FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Ivins, ER James, TS Klemann, V AF Ivins, ER James, TS Klemann, V TI Glacial isostatic stress shadowing by the Antarctic ice sheet SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article DE Antarctic Plate Earthquake; Wilkes Basin; neotectonics; Antarctic ice sheet; Coulomb stress; Transantarctic Mountain Ranges ID SOUTHERN VICTORIA-LAND; SEA-LEVEL CHANGE; UPPER-MANTLE; TRANSANTARCTIC MOUNTAINS; PLATE EARTHQUAKE; LATE-PLEISTOCENE; EAST ANTARCTICA; THERMAL STRUCTURE; NORTHERN NORWAY; MOMENT TENSOR AB [1] Numerous examples of fault slip that offset late Quaternary glacial deposits and bedrock polish support the idea that the glacial loading cycle causes earthquakes in the upper crust. A semianalytical scheme is presented for quantifying glacial and postglacial lithospheric fault reactivation using contemporary rock fracture prediction methods. It extends previous studies by considering differential Mogi-von Mises stresses, in addition to those resulting from a Coulomb analysis. The approach utilizes gravitational viscoelastodynamic theory and explores the relationships between ice mass history and regional seismicity and faulting in a segment of East Antarctica containing the great Antarctic Plate (Balleny Island) earthquake of 25 March 1998 (M-w 8.1). Predictions of the failure stress fields within the seismogenic crust are generated for differing assumptions about background stress orientation, mantle viscosity, lithospheric thickness, and possible late Holocene deglaciation for the D91 Antarctic ice sheet history. Similar stress fracture fields are predicted by Mogi-von Mises and Coulomb theory, thus validating previous rebound Coulomb analysis. A thick lithosphere, of the order of 150-240 km, augments stress shadowing by a late melting (middle-late Holocene) coastal East Antarctic ice complex and could cause present-day earthquakes many hundreds of kilometers seaward of the former Last Glacial Maximum grounding line. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Geol Survey Canada, Sidney, BC V8L 4B2, Canada. Geoforschungszentrum Potsdam, D-14473 Potsdam, Germany. RP Ivins, ER (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 300-233, Pasadena, CA 91109 USA. EM eri@fryxell.jpl.nasa.gov RI James, Thomas/D-9301-2013; Klemann, Volker/H-3660-2013 OI James, Thomas/0000-0001-7321-047X; Klemann, Volker/0000-0002-8342-8947 NR 94 TC 15 Z9 15 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD DEC 12 PY 2003 VL 108 IS B12 AR 2560 DI 10.1029/2002JB002182 PG 21 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 756RD UT WOS:000187494000002 ER PT J AU Povich, MS Raymond, JC Jones, GH Uzzo, M Ko, YK Feldman, PD Smith, PL Marsden, BG Woods, TN AF Povich, MS Raymond, JC Jones, GH Uzzo, M Ko, YK Feldman, PD Smith, PL Marsden, BG Woods, TN TI Doubly ionized carbon observed in the plasma tail of comet Kudo-Fujikawa SO SCIENCE LA English DT Article ID BETA-PICTORIS; SOLAR; DUST; CO AB Comet C/2002 X5 (Kudo-Fujikawa) was observed near its perihelion of 0.19 astronomical unit by the Ultraviolet Coronagraph Spectrometer aboard the Solar and Heliospheric Observatory spacecraft. Images of the comet reconstructed from high-resolution spectra reveal a quasi-spherical cloud of neutral hydrogen and a variable tail of C+ and C2+ that disconnects from the comet and subsequently regenerates. The high abundance of C2+ and C+, at least 24% relative to water, cannot be explained by photodissociation of carbon monoxide and is instead attributed to the evaporation and subsequent photoionization of atomic carbon from organic refractory compounds present in the cometary dust grains. This result serves to strengthen the connection between comets and the material from which the Solar System formed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA. RP Povich, MS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Jones, Geraint/C-1682-2008; OI Jones, Geraint/0000-0002-5859-1136 NR 21 TC 17 Z9 17 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 DEC 12 PY 2003 VL 302 IS 5652 BP 1949 EP 1952 DI 10.1126/science.1092142 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 752NL UT WOS:000187174000056 PM 14671299 ER PT J AU Fisk, MR Storrie-Lombardi, MC Douglas, S Popa, R McDonald, G Di Meo-Savoie, C AF Fisk, MR Storrie-Lombardi, MC Douglas, S Popa, R McDonald, G Di Meo-Savoie, C TI Evidence of biological activity in Hawaiian subsurface basalts SO GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS LA English DT Article DE Hawaiian deep drilling; basalt; microorganisms; DNA staining; Raman spectroscopy; environmental scanning electron microscope ID ULTRAVIOLET RESONANCE RAMAN; SCIENTIFIC DRILLING PROJECT; MARINE PLANKTONIC ARCHAEA; ENDOGENOUS AMINO-ACIDS; CLAY-DYE SYSTEMS; ACRIDINE-ORANGE; MICROBIAL ACTIVITY; OCEAN CRUST; SPECTROSCOPY; DEEP AB [1] The Hawaii Scientific Drilling Program (HSDP) cored and recovered igneous rock from the surface to a depth of 3109 m near Hilo, Hawaii. Much of the deeper parts of the hole is composed of hyaloclastite ( fractured basalt glass that has been cemented in situ with secondary minerals). Some hyaloclastite units have been altered in a manner attributed to microorganisms in volcanic rocks. Samples from one such unit ( 1336 m to 1404 m below sea level) were examined to test the hypothesis that the alteration was associated with microorganisms. Deep ultraviolet native fluorescence and resonance Raman spectroscopy indicate that nucleic acids and aromatic amino acids are present in clay inside spherical cavities ( vesicles) within basalt glass. Chemical mapping shows that phosphorus and carbon were enriched at the boundary between the clay and volcanic glass of the vesicles. Environmental scanning electron microscopy (ESEM) reveals two to three micrometer coccoid structures in these same boundaries. ESEM-linked energy dispersive spectroscopy demonstrated carbon, phosphorous, chloride, and magnesium in these bodies significantly differing from unoccupied neighboring regions of basalt. These observations taken together indicate the presence of microorganisms at the boundary between primary volcanic glass and secondary clays. Amino acids and nucleic acids were extracted from bulk samples of the hyaloclastite unit. Amino acid abundance was low, and if the amino acids are derived from microorganisms in the rock, then there are less than 100,000 cells per gram of rock. Most nucleic acid sequences extracted from the unit were closely related to sequences of Crenarchaeota collected from the subsurface of the ocean floor. C1 Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA. Kinohi Inst, Pasadena, CA USA. CALTECH, Jet Prop Lab, NASA, Astrobiol Inst, Pasadena, CA USA. Univ So Calif, Dept Earth Sci, Los Angeles, CA USA. Med Univ S Carolina, Charleston, SC 29425 USA. RP Fisk, MR (reprint author), Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA. NR 80 TC 36 Z9 36 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1525-2027 J9 GEOCHEM GEOPHY GEOSY JI Geochem. Geophys. Geosyst. PD DEC 11 PY 2003 VL 4 AR 1103 DI 10.1029/2002GC000387 PG 24 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 756NX UT WOS:000187488900001 ER PT J AU Kwok, R Cunningham, GF Hibler, WD AF Kwok, R Cunningham, GF Hibler, WD TI Sub-daily sea ice motion and deformation from RADARSAT observations SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB We find a persistent level of oscillatory sea ice motion and deformation, superimposed on the large-scale wind-driven field, in May 2002 (spring) and February 2003 (midwinter), in the high Arctic over a region centered at similar to(85degreesN, 135degreesW). At this latitude, the RADARSAT wide-swath SAR coverage provides 4-5 sequential observations every day, for ice motion retrieval, with a sampling interval at the orbital period of similar to101 minutes. Periodic correlations in ice motion and deformation can be seen in length scales from 10 km and above, and suggest a 12-hr oscillation that is more likely associated with inertial rather than tidal frequencies. Divergence/convergence of similar to0.1-0.2% peak-to-peak or rates of similar to10(-7)/s is seen in both datasets, with the mid-winter dataset having smaller values. These observations are remarkable in that short-period ice motion is previously believed to be inhibited by the strength of the ice pack in the high Arctic during winter. New ice production due to the recurrent openings and closings at these temporal scales, if ubiquitous, could be significant within the winter pack. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Alaska, IARC Frontier, Fairbanks, AK 99701 USA. RP 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 7 TC 32 Z9 33 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 DEC 11 PY 2003 VL 30 IS 23 AR 2218 DI 10.1029/2003GL018723 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 756PE UT WOS:000187489600004 ER PT J AU Poole, LR Trepte, CR Harvey, VL Toon, GC VanValkenburg, RL AF Poole, LR Trepte, CR Harvey, VL Toon, GC VanValkenburg, RL TI SAGE III observations of Arctic polar stratospheric clouds - December 2002 SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SAM-II; POAM-II; AEROSOL; CLIMATOLOGY; PARTICLES; DEPLETION; VORTEX; GROWTH; OZONE AB Stratospheric Aerosol and Gas Experiment (SAGE) III aerosol extinction data from the Arctic in December 2002 are presented and used to illustrate the instrument's capability for polar stratospheric cloud (PSC) observations. Numerous PSCs were observed during the month at potential temperatures from about 450-700 K, and Types 1a and 1b PSCs could be discriminated in plots of 1022-nm extinction versus color ratio (the ratio of 1022-nm and 449-nm extinctions). Type 1a (1b) PSCs were observed primarily above (below) a threshold temperature of 4 K below the nitric acid trihydrate (NAT) equilibrium temperature. Mie calculations show that some of the Type 1a PSC observations are consistent with a mixture of background aerosol and very few large NAT particles. This suggests that SAGE III offers the potential for systematic observations of these clouds, which would greatly improve our understanding of how they form and lead to stratospheric denitrification. C1 NASA, Langley Res Ctr, Hampton, VA 23665 USA. Sci Applicat Int Corp, Hampton, VA USA. CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Poole, LR (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. EM lamont.r.poole@nasa.gov NR 15 TC 15 Z9 15 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 DEC 11 PY 2003 VL 30 IS 23 AR 2216 DI 10.1029/2003GL018496 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 756PE UT WOS:000187489600002 ER PT J AU Tuck, AF Hovde, SJ Kelly, KK Mahoney, MJ Proffitt, MH Richard, EC Thompson, TL AF Tuck, AF Hovde, SJ Kelly, KK Mahoney, MJ Proffitt, MH Richard, EC Thompson, TL TI Exchange between the upper tropical troposphere and the lower stratosphere studied with aircraft observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE upper tropical troposphere; multifractal ID WATER-VAPOR; TROPOPAUSE TEMPERATURES; TRANSPORT; OZONE; MONSOON; AIR; CIRCULATION; PERSISTENCE; HUMIDITY; FOUNTAIN AB Exchange between the upper tropical troposphere and the lower stratosphere is considered by examining WB57F and ER-2 aircraft observations of water, ozone, wind, and temperature in the potential temperature range 360 0.32). The average spectrum of the burst is well fitted by a Band function (low-energy power-law index alpha = -0.805(-0.105)(+0-112); high-energy power-law index beta = -2.37(-0.31)(+0.18);; and energy of the peak of the spectrum in vF(v), E-peak(obs) = 46.8(-5.1)(+5.8) keV). The near-real-time optical follow-up of GRB 021211 made possible by HETE-2 led to the detection of an optical afterglow for what otherwise would quite likely have been classified as an "optically dark" GRB, since the optical transient faded rapidly (from R < 14 to R &AP; 19) within the first 20 minutes, and was fainter than R &AP; 23 within 24 hr after the burst. GRB 021211 demonstrates that some fraction of burst afterglows are optically dark because their optical afterglows at times greater than 1 hr after the burst are very faint, and previously have often escaped detection. Such bursts are "optically dim" rather than truly optically dark. GRB 021211 also shows that even such optically dim bursts can have very bright optical afterglows at times less than 20 minutes after the burst. C1 MIT, Ctr Space Res, Cambridge, MA 02139 USA. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. Observ Midi Pyrenees, Astrophys Lab, F-31400 Toulouse, France. Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528551, Japan. RIKEN, Inst Phys & Chem Res, Wako, Saitama 3510198, Japan. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Natl Astron Observ, Tokyo 1818588, Japan. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Aoyama Gakuin Univ, Dept Phys, Setagaya Ku, Tokyo 1578572, Japan. Natl Space Dev Agcy Japan, Tsukuba Space Ctr, Tsukuba, Ibaraki 3058505, Japan. Observ Midi Pyrenees, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, Brazil. Tata Inst Fundamental Res, Dept Astron & Astrophys, Bombay 400005, Maharashtra, India. CNR, IASF, I-40129 Bologna, Italy. Miyazaki Univ, Fac Engn, Miyazaki 8892192, Japan. RP Crew, GB (reprint author), MIT, Ctr Space Res, 70 Vassar St, Cambridge, MA 02139 USA. OI Boer, Michel/0000-0001-9157-4349 NR 49 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 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2003 VL 599 IS 1 BP 387 EP 393 DI 10.1086/379222 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 752FN UT WOS:000187149600031 ER PT J AU Reginald, NL St Cyr, OC Davila, JM Brosius, JW AF Reginald, NL St Cyr, OC Davila, JM Brosius, JW TI Electron temperature and speed measurements in the low solar corona: Results from the 2001 June eclipse SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; Sun : atmospheric motions; Sun : corona; Sun : UV radiation ID EXTREME-ULTRAVIOLET; SOHO; WIND; SPECTROMETER; EIT; VELOCITY; PROTON; SUN AB We present measurements of electron temperature and bulk flow speed low in the solar corona derived from white-light spectra obtained during the total solar eclipse of 2001 June 21. Observations were obtained at two locations in the solar corona, one within a helmet streamer at the east limb and the second in a streamer cluster in the southwest. Both points were at an altitude of about 1.1 R-circle dot from the solar center. The east limb and southwest locations yielded electron temperatures of 0.96+/-0.05 and 1.2+/-0.2 MK and bulk flow speeds of 72.0(-72.0)(+281.0) and 257.0(-257.0)(+443.0) km s(-1), respectively. These measurements are unique in that they simultaneously provide both the electron temperature and its bulk flow speed; few previous measurements of electron parameters in the corona are available. The results presented here demonstrate the potential for this technique: if the instrument were used with a coronagraph, it would provide routine synoptic maps of electron temperature and bulk flow speed. C1 NASA, Goddard Space Flight Ctr, Catholic Univ Amer, Greenbelt, MD 20771 USA. RP Reginald, NL (reprint author), NASA, Goddard Space Flight Ctr, Catholic Univ Amer, MC 682, Greenbelt, MD 20771 USA. NR 30 TC 8 Z9 8 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2003 VL 599 IS 1 BP 596 EP 603 DI 10.1086/379148 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 752FN UT WOS:000187149600048 ER PT J AU Bogdan, TJ Hansteen, MCV McMurry, A Rosenthal, CS Johnson, M Petty-Powell, S Zita, EJ Stein, RF McIntosh, SW Nordlund, A AF Bogdan, TJ Hansteen, MCV McMurry, A Rosenthal, CS Johnson, M Petty-Powell, S Zita, EJ Stein, RF McIntosh, SW Nordlund, A TI Waves in the magnetized solar atmosphere. II. Waves from localized sources in magnetic flux concentrations SO ASTROPHYSICAL JOURNAL LA English DT Review DE MHD; Sun : chromosphere; Sun : magnetic fields; Sun : oscillations; sunspots ID CORONAL MAGNETOSTATIC ARCADES; SLOW MAGNETOACOUSTIC WAVES; ACOUSTIC-GRAVITY WAVES; FIELD LINE RESONANCES; PLANE SOUND-WAVES; MAGNETOHYDRODYNAMIC WAVES; GRAVITATIONAL ATMOSPHERE; STRATIFIED ATMOSPHERE; PHOTOSPHERIC NETWORK; HYDROMAGNETIC-WAVES AB Numerical simulations of wave propagation in a two-dimensional stratified magneto-atmosphere are presented for conditions that are representative of the solar photosphere and chromosphere. Both the emergent magnetic flux and the extent of the wave Source. are spatially localized at the lower photospheric boundary of the simulation. The calculations show that the coupling between the fast and slow magneto-acoustic-gravity (MAG) waves is confined to thin quasi-one-dimensional atmospheric layers where the sound speed and the Alfven velocity are comparable in magnitude. Away from this wave conversion zone, which we call the magnetic canopy, the two MAG waves are effectively decoupled because either the magnetic pressure (B-2/8pi) or the plasma pressure (p=Nk(B)T) dominates over the other. The character of the fluctuations observed in the magneto-atmosphere depend sensitively on the relative location and orientation of the magnetic canopy with respect to the wave source and the observation point. Several distinct wave trains may converge on and simultaneously pass through a given location. Their coherent superposition presents a bewildering variety of Doppler and intensity time series because (1) some waves come directly from the source while others emerge from the magnetic canopy following mode conversion, (2) the propagation directions of the individual wave trains ate neither co-aligned with each other nor with the observer's line of sight, and (3) the wave trains may be either fast or slow MAG waves that exhibit different characteristics depending on whether they are observed in high-beta or low-beta plasmas (betaequivalent to8pip/B-2). Through the analysis of four numerical experiments a coherent and physically intuitive picture emerges of how fast and slow MAG waves interact within two-dimensional magneto-atmospheres. C1 Natl Sci Fdn, Arlington, VA 22203 USA. USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA. Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. Evergreen State Coll, Olympia, WA 98505 USA. Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. Univ Space Res Assoc, CPSS, Seabrook, MD 20770 USA. Univ Copenhagen, Niels Bohr Inst Astron Phys & Geophys, DK-2100 Copenhagen O, Denmark. RP Natl Sci Fdn, Arlington, VA 22203 USA. RI Nordlund, Aake/M-4528-2014 OI Nordlund, Aake/0000-0002-2219-0541 NR 105 TC 174 Z9 175 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2003 VL 599 IS 1 BP 626 EP 660 DI 10.1086/378512 PN 1 PG 35 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 752FN UT WOS:000187149600051 ER PT J AU Studinger, M Karner, GD Bell, RE Levin, V Raymond, CA Tikku, AA AF Studinger, M Karner, GD Bell, RE Levin, V Raymond, CA Tikku, AA TI Geophysical models for the tectonic framework of the Lake Vostok region, East Antarctica SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Lake Vostok; East Antarctica; airborne geophysics; gravity; magnetics; tectonics ID UPPER-MANTLE STRUCTURE; GRAVITY-ANOMALIES; SPECTRAL CORRELATION; ICE-SHEET; CRUSTAL; LITHOSPHERE; ANISOTROPY; FLEXURE; EVENTS; PLATE AB Aerogeophysical and seismological data from a geophysical survey in the interior of East Antarctica were used to develop a conceptual tectonic model for the Lake Vostok region. The model is constrained using three independent data sets: magnetic, seismic, and gravimetric. A distinct change in the aeromagnetic anomaly character across Lake Vostok defines a crustal boundary. Depth to magnetic basement estimates image a 400-km-wide and more than 10-km-deep sedimentary basin west of the lake. Analysis of teleseismic earthquakes suggests a relatively thin crust beneath Lake Vostok consistent with predictions from kinematic and flexural gravity modelling. Magnetic, gravity, and subglacial topography data reveal a tectonic boundary within East Antarctica. Based on our kinematic and flexural gravity modelling, this tectonic boundary appears to be the result of thrust sheet emplacement onto an earlier passive continental margin. No data presently exist to date directly either the timing of passive margin formation or the subsequent shortening phase. The preserved thrust sheet thickness is related to the thickness of the passive margin crust. Because a significant amount of time is required to erode the thrust sheet topography, we suggest that these tectonic events are Proterozoic in age. Minor normal reactivation of the thrust sheet offers a simple mechanism to explain the formation of the Lake Vostok Basin. A low level of seismicity exists in the vicinity of this tectonic boundary. The existence of a crustal boundary in the Antarctic interior provides new constraints on the Proterozoic architecture of the East Antarctic craton. Published by Elsevier B.V. C1 Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. Rutgers State Univ, Piscataway, NJ 08854 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Studinger, M (reprint author), Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. NR 41 TC 55 Z9 56 U1 1 U2 15 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 DEC 10 PY 2003 VL 216 IS 4 BP 663 EP 677 DI 10.1016/S0012-821X(03)00548-X PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 756JK UT WOS:000187461800017 ER PT J AU Sjogreen, B Yee, HC AF Sjogreen, B Yee, HC TI Low dissipative high-order numerical simulations of supersonic reactive flows SO INTERNATIONAL JOURNAL FOR NUMERICAL METHODS IN FLUIDS LA English DT Article DE high-order finite-difference method; shock waves; supersonic combustion ID NONLINEAR DIFFERENTIAL-EQUATIONS; REACTION-CONVECTION EQUATIONS; HYPERBOLIC CONSERVATION-LAWS; SOURCE TERMS; DYNAMICAL-APPROACH; RESOLUTION; ENTROPY AB We report the performance of a newly developed low dissipative sixth-order spatial and fourth-order temporal scheme (J. Comput. Phys. 1999; 150:199; RIACS Report 01.01, NASA Ames Research Centre, October 2000) for multiscale supersonic reactive flows that contain shock waves. The accuracy and efficiency of the scheme are compared with a low-dissipative fifth-order weighted ENO (WENO) scheme (ICASE Report No. 95-73, 1995). This paper confirms and complements the grid convergence study of Sjogreen and Yee where a complex shock/shear/boundary-layer interactions model was also included. A 2D viscous flow consisting of a planar Mach 2 in air interacting with a circular zone of hydrogen bubbles in two different initial configurations is considered. The two initial configurations are a single bubble and two non-aligned bubbles. The gradient in pressure across the shock in conjunction with the gradient in fluid density between the air and hydrogen produce a large increase in vorticity as the shock passes through the hydrogen fuel. As can be seen in the study of Don and Quillen (J. Comput. Phys. 1995; 122:244), Don and Gottlieb (SIAM J. Numer. Anal. 1998; 35:2370) and the present grid convergence study, the size, spacing and velocity of the fine-scale vortical structures are very difficult to accurately simulate numerically. The difficulty in obtaining well-resolved multiscale combustion flows by all methods considered will be illustrated. Published in 2003 by John Wiley Sons, Ltd. C1 Royal Inst Technol, NADA, S-10044 Stockholm, Sweden. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Sjogreen, B (reprint author), Royal Inst Technol, NADA, S-10044 Stockholm, Sweden. NR 22 TC 6 Z9 6 U1 0 U2 5 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND SN 0271-2091 J9 INT J NUMER METH FL JI Int. J. Numer. Methods Fluids PD DEC 10 PY 2003 VL 43 IS 10-11 BP 1221 EP 1238 DI 10.1002/fld.507 PG 18 WC Computer Science, Interdisciplinary Applications; Mathematics, Interdisciplinary Applications; Mechanics; Physics, Fluids & Plasmas SC Computer Science; Mathematics; Mechanics; Physics GA 748CQ UT WOS:000186845000005 ER PT J AU Sockol, PM AF Sockol, PM TI Multigrid solution of the Navier-Stokes equations at low speeds with large temperature variations SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE multigrid; implicit smoothers; time-derivative preconditioning; flux-difference splitting; defect correction; Navier-Stokes ID FLOWS; IMPLICIT; ALGORITHMS AB Multigrid methods for the Navier-Stokes equations at low speeds and large temperature variations are investigated. The compressible equations with time-derivative preconditioning and preconditioned flux-difference splitting of the inviscid terms are used. Three implicit smoothers have been incorporated into a common multigrid procedure. Both full coarsening and semi-coarsening with directional fine-grid defect correction have been studied. The resulting methods have been tested on four 2D laminar problems over a range of Reynolds numbers on both uniform and highly stretched grids. Two of the three methods show efficient and robust performance over the entire range of conditions. In addition, none of the methods has any difficulty with the large temperature variations. (C) 2003 Published by Elsevier B.V. C1 NASA, Glenn Res Ctr, Turbomachinery & Propuls Syst, Cleveland, OH 44135 USA. RP NASA, Glenn Res Ctr, Turbomachinery & Propuls Syst, Mail Stop 5-10, Cleveland, OH 44135 USA. EM psockol@nasa.gov NR 22 TC 0 Z9 0 U1 0 U2 1 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0021-9991 EI 1090-2716 J9 J COMPUT PHYS JI J. Comput. Phys. PD DEC 10 PY 2003 VL 192 IS 2 BP 570 EP 592 DI 10.1016/j.jcp.2003.07.033 PG 23 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA 747ZX UT WOS:000186838000010 ER PT J AU Golombek, MP Grant, JA Parker, TJ Kass, DM Crisp, JA Squyres, SW Haldemann, AFC Adler, M Lee, WJ Bridges, NT Arvidson, RE Carr, MH Kirk, RL Knocke, PC Roncoli, RB Weitz, CM Schofield, JT Zurek, RW Christensen, PR Fergason, RL Anderson, FS Rice, JW AF Golombek, MP Grant, JA Parker, TJ Kass, DM Crisp, JA Squyres, SW Haldemann, AFC Adler, M Lee, WJ Bridges, NT Arvidson, RE Carr, MH Kirk, RL Knocke, PC Roncoli, RB Weitz, CM Schofield, JT Zurek, RW Christensen, PR Fergason, RL Anderson, FS Rice, JW TI Selection of the Mars Exploration Rover landing sites SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Review DE Mars Exploration Rover; landing sites; remote sensing; aqueous climatic and geologic histories; Meridiani; Gusev ID ORBITER LASER ALTIMETER; THERMAL EMISSION SPECTROMETER; GENERAL-CIRCULATION MODEL; SIZE-FREQUENCY DISTRIBUTIONS; REMOTE-SENSING DATA; GLOBAL SURVEYOR; PHYSICAL-PROPERTIES; MARTIAN ATMOSPHERE; MAADIM-VALLIS; SCALE ROUGHNESS AB [1] The selection of Meridiani Planum and Gusev crater as the Mars Exploration Rover landing sites took over 2 years, involved broad participation of the science community via four open workshops, and narrowed an initial -155 potential sites (80-300 x 30 km) to four finalists based on science and safety. Engineering constraints important to the selection included (1) latitude (10degreesN-15degreesS) for maximum solar power, (2) elevation (less than -1.3 km) for sufficient atmosphere to slow the lander, (3) low horizontal winds, shear, and turbulence in the last few kilometers to minimize horizontal velocity, (4) low 10-m-scale slopes to reduce airbag spin-up and bounce, (5) moderate rock abundance to reduce abrasion or strokeout of the airbags, and (6) a radar-reflective, load-bearing, and trafficable surface safe for landing and roving that is not dominated by fine-grained dust. The evaluation of sites utilized existing as well as targeted orbital information acquired from the Mars Global Surveyor and Mars Odyssey. Three of the final four landing sites show strong evidence for surface processes involving water and appear capable of addressing the science objectives of the missions, which are to determine the aqueous, climatic, and geologic history of sites on Mars where conditions may have been favorable to the preservation of evidence of possible prebiotic or biotic processes. The evaluation of science criteria placed Meridiani and Gusev as the highest-priority sites. The evaluation of the three most critical safety criteria (10-m-scale slopes, rocks, and winds) and landing simulation results indicated that Meridiani and Elysium Planitia are the safest sites, followed by Gusev and Isidis Planitia. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Washington Univ, Dept Earth & Space Sci, St Louis, MO 63130 USA. US Geol Survey, Menlo Pk, CA 94025 USA. US Geol Survey, Geol Div, Branch Astrogeol, Flagstaff, AZ 86001 USA. NASA Headquarters, Washington, DC 20546 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. Univ Hawaii, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mgolombek@jpl.nassa.gov; grantj@nasm.si.edu; timothy.j.parker@jpl.nasa.gov; david.m.kass@jpl.nasagov; joy.crisp@jpl.nasa.gov; squyres@astrosun.tn.cornell.edu; albert@shannon.jpl.nasa.gov; joy@glassy.jpl.nasa.gov; wayne@cranberry.jpl.nasa.gov; nathan.bridges@jpl.nasa.gov; arvidson@wunder.wustl.edu; carr@usgs.gov; rkirk@usgs.gov; philip.c.knocke@jpl.nasa.gov; ralph.b.roncoli@jpl.nasa.gov; cweitz@hq.nasa.gov; tim@scn1.jpl.nasa.gov; rzurek@jpl.nasa.gov; phil.christensen@asu.edu; robin.fergason@asu.edu; anderson@higp.hawaii.edu; james.rice@asu.edu RI Bridges, Nathan/D-6341-2016; Crisp, Joy/H-8287-2016 OI Crisp, Joy/0000-0002-3202-4416 NR 120 TC 86 Z9 88 U1 1 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 10 PY 2003 VL 108 IS E12 AR 8072 DI 10.1029/2003JE002074 PG 48 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 756QU UT WOS:000187493100001 ER PT J AU Richardson, JD Wang, C Burlaga, LF AF Richardson, JD Wang, C Burlaga, LF TI Correlated solar wind speed, density, and magnetic field changes at Voyager 2 SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB The character of the solar wind plasma data observed by Voyager 2 recently changed to a regime in which the speed, density and magnetic field magnitude are positively correlated. In the inner heliosphere, the density and speed are generally anti-correlated. As streams interact while propagating outward, this correlation weakens. Outside 65 AU, Voyager observed large, in-phase, fluctuations of speed, density, and magnetic field magnitude with time scales of 6-12 months. The dynamic pressure varies by a factor of ten in these fluctuations, which should produce motions in the termination shock. We use ACE data from 1 AU as input to a 1-D MHD model which includes pickup ions to model the radial evolution of the solar wind. The model reproduces the basic character (but not the details) of the observations, predicting correlated variations in speed, density, and magnetic field with time scales similar to those observed. C1 MIT, Ctr Space Res, Cambridge, MA 02139 USA. NASA, Extraterr Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Chinese Acad Sci, Lab Space Weather, Beijing, Peoples R China. RP Richardson, JD (reprint author), MIT, Ctr Space Res, Cambridge, MA 02139 USA. NR 20 TC 30 Z9 30 U1 1 U2 18 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 9 PY 2003 VL 30 IS 23 AR 2207 DI 10.1029/2003GL018253 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 756PC UT WOS:000187489400002 ER PT J AU Slavin, JA Owen, CJ Dunlop, MW Boralv, E Moldwin, MB Sibeck, DG Tanskanen, E Goldstein, ML Fazakerley, A Balogh, A Lucek, E Richter I Reme, H Bosqued, JM AF Slavin, JA Owen, CJ Dunlop, MW Boralv, E Moldwin, MB Sibeck, DG Tanskanen, E Goldstein, ML Fazakerley, A Balogh, A Lucek, E Richter, I Reme, H Bosqued, JM TI Cluster four spacecraft measurements of small traveling compression regions in the near-tail SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID GEOTAIL OBSERVATIONS; PLASMA SHEET; FLUX ROPE; MIDTAIL; DENSITY AB Cluster observations taken during a substorm on September 19, 2001 have revealed the presence of small traveling compression regions (TCRs) in the near tail. These measurements are used to determine directly the speed and direction of TCR propagation and the amplitude of the underlying bulge in the plasma sheet. The time-of-flight speeds derived from the arrival times of the magnetic perturbations at the different Cluster s/c yielded a mean speed of 413 km/s. For 2 of the TCRs s/c 1, 2 and 4 were located sufficiently close to the plasma sheet that they were immersed in the central plasma sheet plasma as the TCR swept over s/c 3. In this manner the Cluster measurements directly demonstrated that these small TCRs are caused by moving bulges in the plasma sheet-lobe interface. In summary, our analysis of the Cluster measurements has directly demonstrated the existence of moving bulges in the north-south thickness of the plasma sheet, most probably due to the formation of flux ropes, and their role in producing traveling compression regions. C1 NASA, Goddard Space Flight Ctr, Extraterr Phys Lab, Greenbelt, MD 20771 USA. Mullard Space Sci Lab, Surrey, England. Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. Swedish Inst Space Phys, S-75121 Uppsala, Sweden. Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA. Univ London Imperial Coll Sci Technol & Med, London SW7 2BZ, England. Tech Univ Braunschweig, Inst Geophys & Meteorol, D-38106 Braunschweig, Germany. Ctr Etud Spatiale Rayonnements, Toulouse, France. RP Slavin, JA (reprint author), NASA, Goddard Space Flight Ctr, Extraterr Phys Lab, Greenbelt, MD 20771 USA. EM james.a.slavin@gsfc.nasa.gov RI Owen, Christopher/C-2999-2008; Moldwin, Mark/F-8785-2011; Sibeck, David/D-4424-2012; Goldstein, Melvyn/B-1724-2008; Slavin, James/H-3170-2012 OI Owen, Christopher/0000-0002-5982-4667; Moldwin, Mark/0000-0003-0954-1770; Slavin, James/0000-0002-9206-724X NR 16 TC 30 Z9 30 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 DEC 9 PY 2003 VL 30 IS 23 AR 2208 DI 10.1029/2003GL018438 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 756PC UT WOS:000187489400003 ER PT J AU Burlaga, L Berdichevsky, D Gopalswamy, N Lepping, R Zurbuchen, T AF Burlaga, L Berdichevsky, D Gopalswamy, N Lepping, R Zurbuchen, T TI Merged interaction regions at 1 AU SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE merged interaction regions; magnetic field; shocks; composition; ejecta; magnetic clouds ID CORONAL MASS EJECTIONS; COSMIC-RAY MODULATION; SOLAR-WIND HELIUM; MAGNETIC-FIELDS; GEOMAGNETIC STORMS; LASCO OBSERVATIONS; FORBUSH DECREASES; COMPOUND STREAMS; INTERPLANETARY; EARTH AB We discuss the existence of large, complex merged interaction regions (MIRs) in the solar wind near Earth. MIRs can have configurations that cause more prolonged geomagnetic effects than a single flow structure. A MIR or successive MIRs can produce relatively long lasting Forbush decreases at 1 AU. We illustrate MIRs at 1 AU with two examples (MIR-1 and MIR-2) seen by WIND and ACE in the interval from 18 March through 29 March 2002. We determined the probable structure and origin of each in terms of interacting flows and shocks using in situ and solar observations, but we emphasize that there are uncertainties that cannot be resolved with these data alone. The MIRs were relatively large structures with radial extent approximate to2/3 and 3/4 AU, respectively. MIR-1 was formed by interactions related to at least two complex ejecta, a magnetic cloud, and two shocks. MIR-2 was related to a corotating stream, the heliospheric plasma sheet (HPS), two complex ejecta, a magnetic cloud and at least two shocks. A MIR can evolve significantly while it moves to 1 AU, and memory of the conditions near the Sun is lost in the process. Thus one cannot unambiguously determine the structure of a MIR and the manner in which it formed using observations from a single spacecraft at 1 AU. The magnetic field strength profiles in MIRs are not correlated with the speed and density profiles so that one cannot infer the magnetic field strength in MIRs from remote sensing observation that give density and speed information. It will be possible to better understand the dynamical processes leading to the formation of MIRs with remote sensing observations, but they cannot measure the magnetic fields in MIRs. C1 NASA, Goddard Space Flight Ctr, Extraterr Phys Lab, Greenbelt, MD 20771 USA. EER Syst Inc, L3 Commun, Largo, MD 20774 USA. Univ Michigan, Space Res Lab, Ann Arbor, MI 48109 USA. RP Burlaga, L (reprint author), NASA, Goddard Space Flight Ctr, Extraterr Phys Lab, Code 661, Greenbelt, MD 20771 USA. EM leonard.f.burlaga@nasa.gov; xrdbb@lepvx3.gsfc.nasa.gov; n_gopalswamy@yahoo.com; rpl@leprpl1.gsfc.nasa.gov; thomasz@umich.edu RI Gopalswamy, Nat/D-3659-2012; OI Gopalswamy, Nat/0000-0001-5894-9954 NR 64 TC 22 Z9 23 U1 1 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 9 PY 2003 VL 108 IS A12 AR 1425 DI 10.1029/2003JA010088 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756RF UT WOS:000187494200006 ER PT J AU Bennett, DJ Khusid, B James, CD Galambos, PC Okandan, M Jacqmin, D Acrivos, A AF Bennett, DJ Khusid, B James, CD Galambos, PC Okandan, M Jacqmin, D Acrivos, A TI Combined field-induced dielectrophoresis and phase separation for manipulating particles in microfluidics SO APPLIED PHYSICS LETTERS LA English DT Article ID AC ELECTRIC-FIELDS; POSITIVE DIELECTROPHORESIS; COLLOIDAL SUSPENSIONS; INDUCED AGGREGATION AB Experiments were conducted in microfluidics equipped with dielectrophoretic gates arranged perpendicular to the flow. Under the action of a high-gradient ac field and shear, flowing suspensions were found to undergo a phase separation and to form a distinct front between the regions enriched with and depleted of particles. We demonstrate that this many-body phenomenon, which originates from interparticle electrical interactions, provides a method for concentrating particles in focused regions and for separating biological and nonbiological materials. The evolution of the particle patterns formation is well described by a proposed electrohydrodynamic model. (C) 2003 American Institute of Physics. C1 New Jersey Inst Technol, Newark, NJ 07102 USA. Sandia Natl Labs, Albuquerque, NM 87185 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. CUNY City Coll, New York, NY 10031 USA. RP Bennett, DJ (reprint author), New Jersey Inst Technol, Univ Hts, Newark, NJ 07102 USA. OI Khusid, Boris/0000-0002-8604-1051 NR 16 TC 34 Z9 35 U1 0 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 DEC 8 PY 2003 VL 83 IS 23 BP 4866 EP 4868 DI 10.1063/1.1629789 PG 3 WC Physics, Applied SC Physics GA 750AY UT WOS:000186970200060 ER PT J AU Mazolli, A Neto, PAM Nussenzveig, HM AF Mazolli, A Neto, PAM Nussenzveig, HM TI Theory of trapping forces in optical tweezers SO PROCEEDINGS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES LA English DT Article DE optical traps; semiclassical limit; Mie scattering ID FOCUSED LASER-BEAM; PARTICLES; TORQUE; FIELD AB Starting from a Debye-type integral representation valid for a laser beam focused through a high numerical aperture objective, we derive an explicit partial-wave (Mie) representation for the force exerted on a dielectric sphere of arbitrary radius, position and refractive index. In the semi-classical limit, the ray-optics result is shown to follow from the Mie expansion, holding in the sense of a size average. The equilibrium position and trap stiffness oscillate as functions of the circumference-to-wavelength ratio, a signature of interference, not predicted by previous theories. We also present comparisons with experimental results. C1 Univ Fed Rio de Janeiro, Inst Fis, BR-21945 Rio De Janeiro, Brazil. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Mazolli, A (reprint author), Univ Fed Rio de Janeiro, Inst Fis, Caixa Postal 68528, BR-21945 Rio De Janeiro, Brazil. NR 32 TC 89 Z9 89 U1 2 U2 40 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1364-5021 EI 1471-2946 J9 P ROY SOC A-MATH PHY JI Proc. R. Soc. A-Math. Phys. Eng. Sci. PD DEC 8 PY 2003 VL 459 IS 2040 BP 3021 EP 3041 DI 10.1098/rspa.2003.1164 PG 21 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 751UT UT WOS:000187085900005 ER PT J AU Tilmes, S Muller, R Grooss, JU Hopfner, M Toon, GC Russell, JM AF Tilmes, S Muller, R Grooss, JU Hopfner, M Toon, GC Russell, JM TI Very early chlorine activation and ozone loss in the Arctic winter 2002-2003 SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID HALOGEN OCCULTATION EXPERIMENT; POLAR VORTEX; BALLOON AB Chlorine activation and chemical ozone destruction is investigated in the Arctic winter 2002-03 using the tracer-tracer correlation technique. Consistent with very low temperatures in the early vortex, strong chlorine activation at 520 K potential temperature was observed already in mid-December 2002 by the MkIV balloon and at 400-500 K in early January 2003 from HALOE satellite measurements. Large column ozone loss was derived inside the outer vortex in January (23 +/- 9 DU) and substantially greater losses in February (51 +/- 9 DU) inside the vortex core in 380-550 K. Calculated ozone loss is similar in February in the two completely separated parts of the vortex. Little influence of mixing in of mid-latitude is noticeable after the reunification of the vortex. Further, some ozone loss at lower altitudes likely occurred during March and April consistent with polar stratospheric clouds detected by MIPAS-ENVISAT towards the end of March. C1 Forschungszentrum Julich, Inst Stratospher Res, D-52425 Julich, Germany. Forschungszentrum Karlsruhe, IMK, D-76021 Karlsruhe, Germany. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Hampton Univ, Hampton, VA 23668 USA. RP Tilmes, S (reprint author), Forschungszentrum Julich, Inst Stratospher Res, Postfach 1913, D-52425 Julich, Germany. EM simone.tilmes@t-online.de; ro.mueller@fz-juelich.de RI Muller, Rolf/A-6669-2013; GrooSS, Jens-Uwe/A-7315-2013; Hopfner, Michael/A-7255-2013 OI Muller, Rolf/0000-0002-5024-9977; GrooSS, Jens-Uwe/0000-0002-9485-866X; Hopfner, Michael/0000-0002-4174-9531 NR 14 TC 22 Z9 24 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 DEC 6 PY 2003 VL 30 IS 23 AR 2201 DI 10.1059/2003GL018079 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 756MF UT WOS:000187482000001 ER PT J AU Brain, DA Bagenal, F Acuna, MH Connerney, JEP AF Brain, DA Bagenal, F Acuna, MH Connerney, JEP TI Martian magnetic morphology: Contributions from the solar wind and crust SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE Mars; crustal magnetism; solar wind interaction; magnetic field topology; Mars Global Surveyor ID MARS GLOBAL SURVEYOR; MAG/ER EXPERIMENT; BOW SHOCK; FIELD; IONOSPHERE; VENUS AB Mars Global Surveyor (MGS) Magnetometer (MAG) data provide constraints on magnetic morphology at Mars, including the relative importance of the solar wind and of crustal magnetic sources. We analyze MAG data to characterize the upstream interplanetary magnetic field (IMF) and confirm trends in the magnetic field expected from the solar wind interaction with a planetary atmosphere, including increases at the shock and magnetic pile-up boundary (MPB), postshock turbulence, and field line draping around the Martian obstacle. Crustal magnetic sources locally modify the solar wind interaction, adding variability to the Martian magnetic environment that depends on planetary rotation. We identify trends in the vector magnetic field with respect to altitude, solar zenith angle, and planetary location. Crustal sources influence the magnetic field to different altitudes above different regions, and the influence of the strongest source extends to 1300-1400 km. The draped IMF partially controls the field topology above crustal sources, and crustal magnetic field lines reconnect to this field in a systematic fashion that depends upon Mars' geography, IMF strength, and IMF orientation. C1 Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Brain, DA (reprint author), Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA. RI connerney, john/I-5127-2013 NR 32 TC 86 Z9 89 U1 3 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 5 PY 2003 VL 108 IS A12 AR 1424 DI 10.1029/2002JA009482 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756NE UT WOS:000187486000001 ER PT J AU Wei, CY Srivastava, D AF Wei, CY Srivastava, D TI Theory of transport of long polymer molecules through carbon nanotube channels SO PHYSICAL REVIEW LETTERS LA English DT Article ID CHAINS; DYNAMICS; MEMBRANE; TRANSLOCATION; SIMULATIONS; NANOPORE; SURFACES AB A theory of transport of long chain polymer molecules through carbon nanotube (CNT) channels is developed using the Fokker-Planck equation and direct molecular dynamics simulations. The mean transport or translocation time tau is found to depend on the chemical potential energy, the entropy, and the diffusion coefficient. A power law dependence tausimilar toN(2) is found, where N is the number of monomers in a molecule. For 10(5)-unit long polyethylene molecules, tau is estimated to be similar to1 mus. The diffusion coefficient of long polymer molecules inside CNTs, like that of short ones, is found to be a few orders of magnitude larger than in ordinary silicate based zeolite systems. 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. NR 22 TC 54 Z9 55 U1 1 U2 13 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 DEC 5 PY 2003 VL 91 IS 23 AR 235901 DI 10.1103/PhysRevLett.91.235901 PG 4 WC Physics, Multidisciplinary SC Physics GA 750PG UT WOS:000187004500038 PM 14683200 ER PT J AU Chesley, SR Ostro, SJ Vokrouhlicky, D Capek, D Giorgini, JD Nolan, MC Margot, JL Hine, AA Benner, LAM Chamberlin, AB AF Chesley, SR Ostro, SJ Vokrouhlicky, D Capek, D Giorgini, JD Nolan, MC Margot, JL Hine, AA Benner, LAM Chamberlin, AB TI Direct detection of the Yarkovsky effect by radar ranging to asteroid 6489 Golevka SO SCIENCE LA English DT Article ID NEAR-EARTH ASTEROIDS; ORDINARY CHONDRITES; THERMAL DRAG; FRAGMENTS; DELIVERY; RADIATION; EVOLUTION; MOBILITY; FORCES; MODEL AB Radar ranging from Arecibo, Puerto Rico, to the 0.5-kilometer near-Earth asteroid 6489 Golevka unambiguously reveals a small nongravitational acceleration caused by the anisotropic thermal emission of absorbed sunlight. The magnitude of this perturbation, known as the Yarkovsky effect, is a function of the asteroid's mass and surface thermal characteristics. Direct detection of the Yarkovsky effect on asteroids will help constrain their physical properties, such as bulk density, and refine their orbital paths. Based on the strength of the detected perturbation, we estimate the bulk density of Golevka to be 2.7(-0.6)(+0.4) grams per cubic centimeter. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Charles Univ, Astron Inst, CZ-18000 Prague, Czech Republic. Natl Astron & Ionosphere Ctr, Arecibo Observ, Arecibo, PR 00612 USA. Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. RP Chesley, SR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. 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 26 TC 95 Z9 98 U1 0 U2 7 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 DEC 5 PY 2003 VL 302 IS 5651 BP 1739 EP 1742 DI 10.1126/science.1091452 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 750AX UT WOS:000186970100040 PM 14657492 ER PT J AU Webster, CR Heymsfield, AJ AF Webster, CR Heymsfield, AJ TI Water isotope ratios D/H, O-18/O-16, O-17/O-16 in and out of clouds map dehydration pathways SO SCIENCE LA English DT Article ID STRATOSPHERIC WATER; TROPICAL TROPOPAUSE; OZONE DEPLETION; CLIMATE-CHANGE; CIRRUS CLOUDS; VAPOR; TRANSPORT; DEUTERIUM; O-18; MECHANISM AB Water isotope ratios have been measured by laser absorption spectroscopy in and out of cirrus clouds formed in situ and convectively generated in anvils over subtropical regions. Water vapor in the tropical and subtropical upper troposphere shows a wide range of isotopic depletion not observed previously. The range suggests that dehydration of upper tropospheric air occurs both by convective dehydration and by gradual dehydration mechanisms. Twenty-five percent of upper tropospheric water sampled is in ice particles whose isotopic signatures are used to identify those grown in situ from those lofted from below. C1 CALTECH, Jet Prop Lab, Div Space Sci, Pasadena, CA 91109 USA. Natl Ctr Atmospher Res, Boulder, CO 80301 USA. RP Webster, CR (reprint author), CALTECH, Jet Prop Lab, Div Space Sci, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Heymsfield, Andrew/E-7340-2011 NR 48 TC 121 Z9 122 U1 1 U2 22 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 DEC 5 PY 2003 VL 302 IS 5651 BP 1742 EP 1745 DI 10.1126/science.1089496 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 750AX UT WOS:000186970100041 PM 14657493 ER PT J AU Khan, H Collier, MR Moore, TE AF Khan, H Collier, MR Moore, TE TI Case study of solar wind pressure variations and neutral atom emissions observed by IMAGE/LENA SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE IMAGE; low-energy neutral atom emission; solar wind pressure; ionospheric outflow ID ION OUTFLOW; SATELLITE-OBSERVATIONS; MASS SPECTROGRAPH; POLAR-CAP; MAGNETOSPHERE; IONOSPHERE; EVENTS AB [1] The Low Energy Neutral Atom (LENA) imager on the IMAGE spacecraft was designed to observe neutral atom emissions at low energy (10 eV - similar to4 keV) from the high-latitude ionosphere. In this study we present data from an ion outflow event on 24 June 2000 showing increases in neutral flux that appear to be associated with dynamic pressure variations in the solar wind. Results from a correlation analysis show the neutral flux to be well correlated (similar to 0.64) with the solar wind dynamic pressure. The neutral atom data are most consistent with a source region at a radial distance of 2.2 - 2.3 R-E, interpreted as the region over which the bulk ion outflow escapes the ionosphere and is partly converted to neutral atoms. Very short time delays (similar to2 min) were calculated between the solar wind pressure increase and neutral atom response, indicating a prompt ionospheric response to the solar wind input. C1 NASA, Goddard Space Flight Ctr, Interplanetary Phys Branch, Greenbelt, MD 20771 USA. RP Khan, H (reprint author), NASA, Goddard Space Flight Ctr, Interplanetary Phys Branch, Code 692, Greenbelt, MD 20771 USA. RI Moore, Thomas/D-4675-2012; Collier, Michael/I-4864-2013 OI Moore, Thomas/0000-0002-3150-1137; Collier, Michael/0000-0001-9658-6605 NR 34 TC 8 Z9 8 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 4 PY 2003 VL 108 IS A12 AR 1422 DI 10.1029/2003JA009977 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756NC UT WOS:000187485700001 ER PT J AU Kurtz, AC Kump, LR Arthur, MA Zachos, JC Paytan, A AF Kurtz, AC Kump, LR Arthur, MA Zachos, JC Paytan, A TI Early Cenozoic decoupling of the global carbon and sulfur cycles SO PALEOCEANOGRAPHY LA English DT Article DE carbon burial; sulfur; Paleogene ID PALEOCENE PLANKTIC FORAMINIFERA; MARINE ORGANIC-MATTER; PALEOPRECIPITATION INDICATORS; CLIMATIC IMPLICATIONS; ISOTOPIC COMPOSITION; ATMOSPHERIC OXYGEN; GEOCHEMICAL CYCLES; SEAWATER SULFATE; PYRITE FORMATION; EOCENE BOUNDARY AB Changes in carbon and sulfur cycling over geologic time may have caused considerable modification of atmospheric and oceanic composition and climate. Here we calculate pyrite sulfur (S-py) and organic carbon (C-org) burial rates from recently improved Cenozoic stable isotope records, and from these rates we infer global changes in C-org burial environments. Given predominantly normal shelf-delta organic carbon burial, the global Spy burial flux should be coupled to C-org burial. However, we find that the major early Cenozoic peak in C-org burial coincides with a minimum in Spy burial. Although the calculated magnitude of variations in global pyrite burial flux is sensitive to our assumptions about the concentration of sulfate in paleoseawater, a non-steady-state isotope mass balance model indicates very low S-py burial rates during the Paleocene and a dramatic increase starting near the Paleocene-Eocene boundary, dropping off to a fairly constant Cenozoic rate beginning in the middle Eocene. High C-org/S-py burial ratios (C/S mole ratio approximate to15-30) coinciding with the Paleocene carbon isotope maximum most likely reflect enhanced accumulation of terrestrial organic carbon in Paleocene terrestrial swamps. We suggest that rapid burning of accumulated Paleocene terrestrial organic carbon could have significantly contributed to the short-lived negative carbon isotope excursion at the Paleocene-Eocene boundary in addition to or possibly even as an alternative to release of gas hydrates from the continental slopes. An early Eocene minimum in calculated C-org/S-py burial ratios (C/S mole ratio approximate to2-4) suggests that the predominant locus of organic carbon burial shifted to euxinic environments in a warm early Eocene ocean. C1 Boston Univ, Dept Earth Sci, Boston, MA 02215 USA. Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. Penn State Univ, NASA, Astrobiol Inst, University Pk, PA 16802 USA. Univ Calif Santa Cruz, Dept Earth Sci, Santa Cruz, CA 95064 USA. Stanford Univ, Dept Geog & Environm Sci, Stanford, CA 94305 USA. RP Kurtz, AC (reprint author), Boston Univ, Dept Earth Sci, Boston, MA 02215 USA. RI Zachos, James/A-7674-2008; Kump, Lee/H-8287-2012; Arthur, Michael/E-2872-2014 OI Arthur, Michael/0000-0002-3028-6279 NR 93 TC 167 Z9 173 U1 3 U2 46 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0883-8305 J9 PALEOCEANOGRAPHY JI Paleoceanography PD DEC 4 PY 2003 VL 18 IS 4 AR 1090 DI 10.1029/2003PA000908 PG 14 WC Geosciences, Multidisciplinary; Oceanography; Paleontology SC Geology; Oceanography; Paleontology GA 756NF UT WOS:000187486200002 ER PT J AU Carpenter, DL Bell, TF Inan, US Benson, RF Sonwalkar, VS Reinisch, BW Gallagher, DL AF Carpenter, DL Bell, TF Inan, US Benson, RF Sonwalkar, VS Reinisch, BW Gallagher, DL TI Z-mode sounding within propagation "cavities" and other inner magnetospheric regions by the RPI instrument on the IMAGE satellite SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE Z-mode sounding; Z-mode propagation; Z-mode trapping; wave ducting; echo inversion; IMAGE satellite ID RADIO PLASMA IMAGER; AURORAL KILOMETRIC RADIATION; ELECTRON-DENSITY; TOPSIDE IONOGRAMS; WAVE MODES; FIELD; EMISSIONS; SOUNDERS; ECHOES AB When the Radio Plasma Imager (RPI) on the IMAGE satellite operates in the inner plasmasphere and at moderate to low altitudes over the poles, pulses emitted at the low end of the RPI 3 kHz to 3 MHz sounding frequency range can propagate in the Z mode as well as the whistler mode. At medium altitudes within the plasmasphere, discrete Z-mode echoes with turning points Earthward of IMAGE are often observed, analogous in form to the regular and oblique Z-mode echoes found on topside sounder records. In the polar regions, where f(pe)/f(ce)<1 usually obtains, the Z-mode echoes tend to be diffuse and to exhibit properties such as an intensity decrease at the local value of f(ce), where there is a significant change with frequency in the topology of the Z-mode refractive index surface. At altitudes up to a few thousand km in polar or near-polar regions, Z-mode soundings regularly provide information on the local value of f(pe), whereas passive recordings that depend upon indications of the upper hybrid resonance frequency f(uh) usually fail to do so. Within the transition region from the auroral zone to the plasmasphere and within the plasmasphere itself, at altitudes from &AP;2000 km upward, we find evidence of the Z-mode trapping phenomenon, noted previously in connection with natural wave emissions detected at polar latitudes. This phenomenon involves echoes returning both from turning points in denser regions Earthward of the sounder and from more tenuous regions above. Within Z-mode "cavities,'' discrete Z-mode echoes are found to propagate back and forth along geomagnetic-field-aligned paths between upper and lower altitude reflection points. The echoes present unique forms, depending upon whether IMAGE is located above or below a minimum in the altitude profile of the Z-mode cutoff frequency. Through an inversion process, such echoes make possible determination of the electron density profile along geomagnetic field lines to distances of thousands of km above the location of IMAGE, all on the basis of echo delay information within frequency bands only &AP;20 to 30 kHz wide. The forms of such density profiles are in general agreement with results reported from conventional RPI X-mode sounding from higher altitudes, as well as with predictions based upon a diffusive equilibrium model of density along plasmasphere field lines. C1 Stanford Univ, Space Telecommun & Radiosci Lab, Stanford, CA 94305 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Alaska, Dept Elect Engn, Fairbanks, AK 99775 USA. Univ Massachusetts, Ctr Atmospher Res, Lowell, MA 01845 USA. NASA, Dept Space Sci, Natl Space Sci & Technol Ctr, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. RP Carpenter, DL (reprint author), Stanford Univ, Space Telecommun & Radiosci Lab, Packard Bldg, Stanford, CA 94305 USA. NR 37 TC 15 Z9 15 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 3 PY 2003 VL 108 IS A12 AR 1421 DI 10.1029/2003JA010025 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756NB UT WOS:000187485500006 ER PT J AU Khazanov, GV Gamayunov, KV Jordanova, VK AF Khazanov, GV Gamayunov, KV Jordanova, VK TI Self-consistent model of magnetospheric ring current and electromagnetic ion cyclotron waves: The 2-7 May 1998 storm SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE ring current; wave-particle interaction; numerical modeling; magnetosphere-inner ID LINEAR DIFFUSION-COEFFICIENTS; EARTHS INNER MAGNETOSPHERE; ELECTRON-SCATTERING LOSS; 1-2 MAGNETIC PULSATIONS; ALFVEN WAVES; EQUATORIAL MAGNETOSPHERE; PARTICLE INTERACTIONS; LARGE-SCALE; RESONANT INTERACTIONS; GEOMAGNETIC STORMS AB A complete description of a self-consistent model of magnetospheric ring current interacting with electromagnetic ion cyclotron waves is presented. The model is based on the system of two kinetic equations; one equation describes the ring current ion dynamics, and another equation describes the wave evolution. The effects on ring current ions interacting with electromagnetic ion cyclotron waves and back on waves are considered self-consistently by solving both equations on a global magnetospheric scale under nonsteady state conditions. The developed model is employed to simulate the entire 2-7 May 1998 storm period. First, the trapped number fluxes of the ring current protons are calculated and presented along with comparison with the data measured by the three-dimensional hot plasma instrument Polar/HYDRA. Incorporating in the model the wave-particle interaction leads to much better agreement between the experimental data and the model results. Second, examining of the wave (MLT, L shell) distributions produced by the model during the storm progress reveals an essential intensification of the wave emission about 2 days after the main phase of the storm. This result is well consistent with the earlier ground-based observations. Finally, the theoretical shapes and the occurrence rates of the wave power spectral densities are studied. It is found that about 2 days after the storm's main phase on 4 May, mainly non-Gaussian shapes of power spectral densities are produced. C1 NASA, Dept Space Sci, Natl Space Sci & Technol Ctr, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA. Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. RP Khazanov, GV (reprint author), NASA, Dept Space Sci, Natl Space Sci & Technol Ctr, George C Marshall Space Flight Ctr, 320 Sparkman Dr, Huntsville, AL 35805 USA. RI Gamayunov, Konstantin/A-8505-2009; OI Gamayunov, Konstantin/0000-0002-8768-8527; Jordanova, Vania/0000-0003-0475-8743 NR 77 TC 34 Z9 34 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 DEC 3 PY 2003 VL 108 IS A12 AR 1419 DI 10.1029/2003JA009856 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756NB UT WOS:000187485500004 ER PT J AU Merkine, VG Papadopoulos, K Milikh, G Sharma, AS Shao, X Lyon, J Goodrich, C AF Merkine, VG Papadopoulos, K Milikh, G Sharma, AS Shao, X Lyon, J Goodrich, C TI Effects of the solar wind electric field and ionospheric conductance on the cross polar cap potential: Results of global MHD modeling SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SATURATION; MAGNETOSPHERE; STORM AB The behavior of the cross polar cap potential, Phi(PC), under strong solar wind conditions is studied using global MHD simulations. Simulations using two typical values of the ionospheric Pedersen conductance in agreement with others show that the cross polar cap potential is reduced compared to the corresponding potential in the solar wind due to the stagnation of the magnetosheath flow and the existence of parallel potentials. However, it is the ionospheric conductance that affects the value of Phi(PC) the most: the transpolar potential saturates only for high enough ionospheric conductance. A mechanism in which the ionospheric conductance changes the properties of the magnetosheath flow is proposed. This mechanism assumes mapping of the electrostatic potential in the ideal MHD system and yields a self-consistent response of the reconnection and transpolar potentials to changes in the ionospheric conductance. C1 Univ Maryland, Dept Phys, College Pk, MD 20742 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. Boston Univ, Dept Astron, Boston, MA 02215 USA. RP Merkine, VG (reprint author), Univ Maryland, Dept Phys, College Pk, MD 20742 USA. RI Merkin, Viacheslav/D-5982-2016 OI Merkin, Viacheslav/0000-0003-4344-5424 NR 10 TC 38 Z9 40 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 2 PY 2003 VL 30 IS 23 AR 2180 DI 10.1029/2003GL017903 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 756MB UT WOS:000187481400001 ER PT J AU Ziemke, JR Chandra, S AF Ziemke, JR Chandra, S TI A Madden-Julian Oscillation in tropospheric ozone SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Madden-Julian Oscillation; MJO; intraseasonal oscillations; tropospheric ozone; tropospheric water vapor ID LOW-FREQUENCY OSCILLATIONS; 1997-1998 EL-NINO; WATER-VAPOR; PACIFIC; FIELD AB This study shows evidence of a Madden-Julian Oscillation (MJO) in tropospheric ozone. Tropospheric ozone is derived using differential measurements of total column ozone and stratospheric column ozone from total ozone mapping spectrometer (TOMS) and microwave limb sounder (MLS) instruments. Two broad regions of significant MJO signal are identified in the tropics, one in the western Pacific and the other in the eastern Pacific. Over both regions, MJO variations in tropospheric ozone represent 5-10 Dobson Unit (DU) peak-to-peak anomalies. These variations are significant compared to mean background amounts of around 20 DU or less over most of the tropical Pacific. MJO signals of this magnitude would need to be considered when investigating and interpreting particular pollution events since ozone is a precursor of the Hydroxyl (OH) radical, the main oxidizing agent of pollutants in the lower atmosphere. C1 Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol, Baltimore, MD 21228 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ziemke, JR (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol, Baltimore, MD 21228 USA. NR 17 TC 16 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 DEC 2 PY 2003 VL 30 IS 23 AR 2182 DI 10.1029/2003GL018523 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 756MB UT WOS:000187481400003 ER PT J AU Fitzenreiter, RJ Ogilvie, KW Bale, SD Vinas, AF AF Fitzenreiter, RJ Ogilvie, KW Bale, SD Vinas, AF TI Modification of the solar wind electron velocity distribution at interplanetary shocks SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE solar wind electrons; interplanetary shock ID EARTHS BOW SHOCK; PHASE-SPACE SIGNATURES; FORESHOCK; WAVES; RADIO AB We analyze a small selection of interplanetary shocks of moderate strength, observed by instruments aboard the Wind spacecraft. We find electron signatures of heating and acceleration that are similar to those found at Earth's high Mach number bow shock. Upstream, velocity distributions have the signature of shock-accelerated electrons with the characteristic time of flight velocity cutoff with bump-on-tail reduced distributions observed in coincidence with Langmuir waves. Downstream, the distributions broaden with the stronger shocks showing flat-topped distributions and accompanying beams, such as are seen on the high entropy side of Earth's bow shock. We apply the Liouville mapping analysis of Hull et al. [1998, 2001] to one of the interplanetary shocks and compute the deHoffman-Teller electrostatic potential across the shock using the electron moments to map the observed upstream distribution to the downstream region. The mapping successfully reproduces the inflated phase density and beam signatures of the observed downstream electron velocity distribution. C1 NASA, Extraterr Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Fitzenreiter, RJ (reprint author), NASA, Extraterr Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Bale, Stuart/E-7533-2011 OI Bale, Stuart/0000-0002-1989-3596 NR 19 TC 13 Z9 15 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 DEC 2 PY 2003 VL 108 IS A12 AR 1415 DI 10.1029/2003JA009865 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756MZ UT WOS:000187485300001 ER PT J AU Kundu, PK Bell, TL AF Kundu, PK Bell, TL TI A stochastic model of space-time variability of mesoscale rainfall: Statistics of spatial averages SO WATER RESOURCES RESEARCH LA English DT Article DE rainfall statistics; stochastic model; scaling; fractal behavior; precipitation spectrum; TOGA-COARE data modeling ID 40-50 DAY OSCILLATION; TOGA-COARE; SAMPLING ERRORS; MULTISCALING PROPERTIES; SATELLITE-OBSERVATIONS; PRECIPITATION FIELDS; RANDOM CASCADES; DESIGNS; SCALE; RADAR AB A characteristic feature of rainfall statistics is that they depend on the space and time scales over which rain data are averaged. A previously developed spectral model of rain statistics that is designed to capture this property predicts power law scaling behavior for the second moment statistics of area-averaged rain rate on the averaging length scale L as L --> 0. In the present work a more efficient method of estimating the model parameters is presented and used to fit the model to the statistics of area-averaged rain rate derived from gridded radar precipitation data from TOGA-COARE. Statistical properties of the data and the model predictions are compared over a wide range of averaging scales. An extension of the spectral model scaling relations to describe the dependence of the average fraction of grid boxes within an area containing nonzero rain (the "`rainy area fraction") on the grid scale L is also explored. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. RP Kundu, PK (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 913, Greenbelt, MD 20771 USA. RI Bell, Thomas/G-5425-2012; Kundu, Prasun/C-7212-2013 OI Kundu, Prasun/0000-0002-2284-9852 NR 45 TC 21 Z9 21 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 J9 WATER RESOUR RES JI Water Resour. Res. PD DEC 2 PY 2003 VL 39 IS 12 AR 1328 DI 10.1029/2002WR001802 PG 15 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 756NP UT WOS:000187487800002 ER PT J AU Cline, LFH Gibbs, G AF Cline, LFH Gibbs, G TI Re-negotiation of the International Space Station Agreements - 1993-1997 SO ACTA ASTRONAUTICA LA English DT Article AB During the Spring of 1993, at the request of the US President, the Space Station partners, under the leadership of the US National Aeronautics and Space Administration (NASA), undertook a fundamental redesign of the Space Station and the manner by which NASA would manage the program. Coincident with the 1993 redesign, NASA initiated discussions with the Russian Federation with the view to Russia becoming a partner in the Space Station Program. This resulted in the partners (the United States, Canada, Europe and Japan) issuing, on December 6, 1993, an invitation to Russia to enter into negotiations to become a partner in the International Space Station Program. Originally, the negotiations were intended to center exclusively around the changes required to the government and agency-level Space Station Agreements to bring Russia into the partnership, and to reflect the changes resulting from the 1993 redesign. After the commencement of the negotiations it became necessary to also reflect changes due to restructuring of the European and Canadian partners' programs, and various desires of the partners to confirm in the legal framework new provisions for dealing with cost control and common operations activities. This paper provides a summary of the complex legal and programmatic multinational negotiations that took place between 1993 and 1997 on a multilateral Intergovernmental Agreement and four bilateral space agency-level Memoranda of Understanding. This paper puts these most recent negotiations in the context of the first set of agreements which were signed in September 1988, explains the process the original partners put in place for the 1993-1997 Round of negotiations, and the substantive issues that resulted together with the solutions agreed. The paper captures in one document the most relevant aspects of these important international negotiations, and complements those papers previously presented by the authors at the 45th and 47th Congresses of the International Astronautical Federation.(C) 2003 Published by Elsevier Ltd. C1 US Natl Aeronaut & Space Adm, Washington, DC 20546 USA. Canadian Space Agcy, Washington Operat, Washington, DC USA. RP Cline, LFH (reprint author), US Natl Aeronaut & Space Adm, 300 E St SW, Washington, DC 20546 USA. NR 0 TC 6 Z9 6 U1 1 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD DEC PY 2003 VL 53 IS 11 BP 917 EP 925 AR PII S0094-5765(02)00210-2 DI 10.1016/S0094-5765(02)00210-2 PG 9 WC Engineering, Aerospace SC Engineering GA 707HE UT WOS:000184504600006 ER PT J AU Zappoli, B Kuhl, R Robey, J Ivanov, A AF Zappoli, B Kuhl, R Robey, J Ivanov, A TI Cooperative research in microgravity sciences during the French manned MIR missions SO ACTA ASTRONAUTICA LA English DT Article; Proceedings Paper CT 51st International Astronautical Congress CY OCT 02-06, 2000 CL RIO DE JANEIRO, BRAZIL ID TRANSITION AB During the past ten years the French laboratories working in the field of fluids and material sciences had access to regular. long-lasting manned missions onboard the Russian MIR Space Station. Beyond the French scientific program that was performed with the ALICE apparatus, a cooperative research program was developed with DLR, NASA and RSA. This cooperation was based on bartered agreements that included the joint utilization of the instruments onboard the MIR station (ALICE, TITUS furnace from DLR, vibration device from RKK Energia) and the funding of dedicated cartridges (DLR) or thermostats (DLR and NASA), as well as launch services (NASA) by the Cooperating Agencies. We present a review of this program with a particular emphasis on its scientific results and on the progress that has been achieved in science and applications. They covered a large field of condensed matter physics, from material sciences to near-critical and off-critical phase separation kinetics and near critical fluid hydrodynamics (thermoacoustic heat transport and vibrational convection). The high microgavity relevance of all these investigations naturally led to outstanding results that was published in the world's best scientific journals. The analysis of the latest experiments performed during the PEGASUS mission shows they will not be an exception to that evaluation. Off-critical phase separation with NASA, pressure-driven piston effect and equiaxed solidification with DLR, heat transport under calibrated vibrations with RKK Energia, all will be presented. The conclusion will stress the international character of this microgravity research program, the conditions of its success and what can be gained from it in the perspective of the space station utilization. (C) 2003 Elsevier Ltd. All rights reserved. C1 CNES HQ, F-31401 Toulouse, France. DLR HQ Linder Hohe, D-5000 Cologne, Germany. NASA HQ, Washington, DC 20546 USA. RKK Energia, Korolev 141070, Moscow Region, Russia. RP Zappoli, B (reprint author), CNES HQ, 18 Ave E Belin, F-31401 Toulouse, France. NR 9 TC 2 Z9 2 U1 1 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD DEC PY 2003 VL 53 IS 12 BP 963 EP 970 DI 10.1016/S0094-5765(02)00273-4 PG 8 WC Engineering, Aerospace SC Engineering GA 732KD UT WOS:000185942200003 ER PT J AU Schlagheck, RA Trach, BL AF Schlagheck, RA Trach, BL TI Microgravity research results and experiences from the NASA/MIR space station program SO ACTA ASTRONAUTICA LA English DT Article AB The Microgravity Research Program (MRP) participated aggressively in Phase I of the International Space Station Program using, the Russian Mir Space Station. The Mir Station offered an otherwise unavailable opportunity to explore the advantages and challenges of long duration microgravity space research. Payloads with both National Aeronautics and Space Agency (NASA) and commercial backing were included as well as cooperative research with the Canadian Space Agency (CSA). From this experience, much was learned about long-duration on-orbit science utilization and developing new working relationships with our Russian partner to promote efficient planning, operations, and integration to solve complexities associated with a multiple partner program. This paper focuses on the microgravity research conducted onboard the Mir space station. It includes the Program preparation and planning necessary to support this type of cross increment research experience; the payloads which were flown; and summaries of significant microgravity science findings. Published by Elsevier Ltd. C1 NASA, Marshall Space Flight Ctr, Huntsville, AL 35811 USA. Boeing Co, Huntsville, AL 35824 USA. RP Schlagheck, RA (reprint author), NASA, Marshall Space Flight Ctr, Huntsville, AL 35811 USA. NR 14 TC 1 Z9 2 U1 1 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD DEC PY 2003 VL 53 IS 12 BP 983 EP 996 DI 10.1016/S0094-5765(02)00275-8 PG 14 WC Engineering, Aerospace SC Engineering GA 732KD UT WOS:000185942200005 PM 14503490 ER PT J AU Vahedi-Faridi, A Lovelace, J Bellamy, HD Snell, EH Borgstahl, GEO AF Vahedi-Faridi, A Lovelace, J Bellamy, HD Snell, EH Borgstahl, GEO TI Physical and structural studies on the cryocooling of insulin crystals SO ACTA CRYSTALLOGRAPHICA SECTION D-BIOLOGICAL CRYSTALLOGRAPHY LA English DT Article ID PROTEIN CRYSTALS; ANGSTROM RESOLUTION; MOSAIC SPREAD; MICROGRAVITY; CRYOCRYSTALLOGRAPHY; PERFECTION; GROWTH; CRYSTALLIZATION; EARTH AB Reflection profiles were analyzed from microgravity-grown (mug) and earth-grown insulin crystals to measure mosaicity (eta) and to reveal mosaic domain structure and composition. The effects of cryocooling on single-domain and multi-domain crystals were compared. The effects of cryocooling on insulin structure were also re-examined. Microgravity crystals were of larger volume, were more homogeneous and were of higher quality than earth crystals. Several m g crystals contained a single mosaic domain which encompassed all or nearly all of the crystal with an eta(avg) of 0.005degrees. The earth crystals varied in quality and all contained multiple domains with an eta(avg) of 0.031degrees. Cryocooling caused a 43-fold increase in eta for mug crystals (eta(avg) = 0.217degrees) and an eightfold increase for earth crystals (eta(avg) = 0.246degrees). These results indicate that very well ordered crystals are not completely protected from the stresses associated with cryocooling, especially when structural perturbations occur. However, there were differences in the reflection profiles. For multi-mosaic domain crystals, each domain individually broadened and separated from the other domains upon cryocooling. Cryocooling did not cause an increase in the number of domains. A crystal composed of a single domain retained this domain structure and the reflection profiles simply broadened. Therefore, an improved signal-to-noise ratio for each reflection was measured from cryocooled single-domain crystals relative to cryocooled multi-domain crystals. The improved signal from m g crystals, along with the increase in crystal size, facilitated the measurement of the weaker high-resolution reflections. The observed broadening of reflection profiles indicates increased variation in unit-cell parameters, which may be linked to cryocooling-associated structural changes and disorder. C1 Nebraska Med Ctr 987696, Eppley Inst Res Canc, Omaha, NE 68198 USA. Univ Toledo, Dept Chem, Toledo, OH 43606 USA. Stanford Synchrotron Radiat Lab, Menlo Pk, CA 94025 USA. NASA, George C Marshall Space Flight Ctr, Struct Biol Lab, Huntsville, AL 35812 USA. RP Borgstahl, GEO (reprint author), Nebraska Med Ctr 987696, Eppley Inst Res Canc, Omaha, NE 68198 USA. NR 39 TC 11 Z9 11 U1 1 U2 1 PU BLACKWELL MUNKSGAARD PI COPENHAGEN PA 35 NORRE SOGADE, PO BOX 2148, DK-1016 COPENHAGEN, DENMARK SN 0907-4449 J9 ACTA CRYSTALLOGR D JI Acta Crystallogr. Sect. D-Biol. Crystallogr. PD DEC PY 2003 VL 59 BP 2169 EP 2182 DI 10.1107/S0907444903019668 PN 12 PG 14 WC Biochemical Research Methods; Biochemistry & Molecular Biology; Biophysics; Crystallography SC Biochemistry & Molecular Biology; Biophysics; Crystallography GA 748WM UT WOS:000186884000015 PM 14646075 ER PT J AU Williams, BC Ingham, MD Chung, S Elliott, P Hofbaur, M Sullivan, GT AF Williams, BC Ingham, MD Chung, S Elliott, P Hofbaur, M Sullivan, GT TI Model-based programming of fault-aware systems SO AI MAGAZINE LA English DT Article AB A wide range of sensor-rich, networked embedded systems are being created that must operate robustly for years in the face of novel failures by managing complex autonomic processes. These systems are being composed, for example, into vast networks of space, air, ground, and underwater vehicles. Our objective is to revolutionize the way in which we control these new artifacts by creating reactive model-based programming languages that enable everyday systems to reason intelligently and enable machines to explore other worlds. A model-based program is state and fault aware; it elevates the programming task to specifying intended state evolutions of a system. The program's executive automatically coordinates system interactions to achieve these states, entertaining known and potential failures, using models of its constituents and environment. At the executive's core is a method, called CONFLICT-DIRECTED A*, which quickly prunes promising but infeasible solutions, using a form of one-shot learning. This approach has been demonstrated on a range of systems, including the National Aeronautics and Space Administration's Deep Space One probe. Model-based programming is being generalized to hybrid discrete-continuous systems and the coordination of networks of robotic vehicles. C1 MIT Fac, Model Based Embedded & Robot Syst Grp, Cambridge, MA USA. Graz Univ Technol, Dept Automat Control, A-8010 Graz, Austria. MIT, Artificial Intelligence Lab, Cambridge, MA 02139 USA. CALTECH, Jet Prop Lab, Artificial Intelligence Grp, Pasadena, CA 91125 USA. MIT, Space Syst Lab, Cambridge, MA 02139 USA. EM liams@mit.edu; michel.ingham@jpl.nasa.gov; chung@mit.edu; pelliott@mit.edu; hofbaur@irt.tugraz.ac.at; gregs@ai.mit.edu NR 22 TC 7 Z9 7 U1 0 U2 2 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 WIN PY 2003 VL 24 IS 4 BP 61 EP 75 PG 15 WC Computer Science, Artificial Intelligence SC Computer Science GA 756TX UT WOS:000187500200005 ER PT J AU Pindera, MJ Aboudi, J Arnold, SM AF Pindera, MJ Aboudi, J Arnold, SM TI Analysis of locally irregular composites using high-fidelity generalized method of cells SO AIAA JOURNAL LA English DT Article; Proceedings Paper CT AIAA/ASME/ASCE/AHS/ASC 44th Structures Structural Dynamics and Materials Conference CY APR 07-10, 2003 CL NORFOLK, VIRGINIA SP AIAA, ASME, ASCE, AHS, ASC ID METAL-MATRIX COMPOSITES; HIGHER-ORDER THEORY; DEFORMATION; MODEL; SHAPE AB The generalized method of cells is a micromechanics model that is generally quite accurate at the macrolevel but not always accurate at the microlevel. This is due to the absence of so-called shear coupling, which provides the required bridge between macroscopically applied normal (shear) stresses and the microscopic shear (normal) stresses necessary for an accurate estimate of microlevel quantities. To overcome this deficiency, a new micromechanics model has been developed for the response of multiphase materials with arbitrary periodic microstructures, named high-fidelity generalized method of cells in part because it employs the same microstructural discretization as the original generalized method of cells. The model's framework is based on the homogenization theory, but the method of solution for the local fields borrows concepts previously employed in constructing the higher-order theory for functionally graded materials, in contrast with the typical finite element-based solution strategies. The model generates the average stress-strain response of heterogeneous materials such as ceramic, metal, and polymeric matrix composites, as well as the internal or microlevel stress and strain fields, with excellent accuracy. The model is employed to investigate the response of a metal matrix composite with locally irregular, but periodic, fiber distributions, and it is shown that irregular architectures affect shear and normal stress-strain response in a different manner. The new model's ability to capture these differences is attributed to the shear-coupling effect absent in the original model. C1 Univ Virginia, Charlottesville, VA 22904 USA. Tel Aviv Univ, Dept Solid Mech Mat & Struct, IL-69978 Tel Aviv, Israel. NASA, John H Glenn Res Ctr, Struct Fatigue Branch, Cleveland, OH 44135 USA. RP Pindera, MJ (reprint author), Univ Virginia, Charlottesville, VA 22904 USA. NR 14 TC 5 Z9 5 U1 0 U2 5 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD DEC PY 2003 VL 41 IS 12 BP 2331 EP 2340 DI 10.2514/2.6857 PG 10 WC Engineering, Aerospace SC Engineering GA 754NE UT WOS:000187322600003 ER PT J AU Okong'o, N Bellan, J AF Okong'o, N Bellan, J TI Real-gas effects on mean flow and temporal stability of binary-species mixing layers SO AIAA JOURNAL LA English DT Article ID DIRECT NUMERICAL SIMULATIONS; INVISCID SPATIAL STABILITY; SUPERCRITICAL CONDITIONS; NITROGEN; HEPTANE; PRESSURES; MIXTURES; HYDROGEN; MODEL AB Real-gas effects on the mean flow and inviscid stability of temporal mixing layers are examined for supercritical heptane/nitrogen and oxygen/hydrogen mixtures. The analysis is based on the compressible Navier-Stokes equations for conservation of mass, momentum, total energy, and species mass, with heat and species-mass fluxes derived from fluctuation-dissipation theory and incorporating Soret and Dufour effects. An approximate form of the equations is used to obtain a system of similarity equations for the streamwise velocity, the temperature, and the mass fraction. The similarity profiles show important real-gas nonideal-mixture effects, particularly for the temperature, in departing from the incompressible error-function similarity solution. Realistic Schmidt and Prandtl numbers were found to be important to the similarity profiles. A linear, inviscid stability analysis is then performed using the similarity profile, as well as analytical error-function profiles, as its basic flow. The stability analysis shows that the similarity profile has larger growth rates at a given wavelength and a shorter more unstable wavelength than the error-function profiles and than an incompressible flow. The similarity profile also has a larger range of unstable wavelengths than the error-function profiles. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Okong'o, N (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 24 TC 17 Z9 18 U1 1 U2 2 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD DEC PY 2003 VL 41 IS 12 BP 2429 EP 2443 DI 10.2514/2.6842 PG 15 WC Engineering, Aerospace SC Engineering GA 754NE UT WOS:000187322600015 ER PT J AU Cutler, AD Danehy, PM Springer, RR O'Byrne, S Capriotti, DP DeLoach, R AF Cutler, AD Danehy, PM Springer, RR O'Byrne, S Capriotti, DP DeLoach, R TI Coherent anti-stokes Raman spectroscopic thermometry in a supersonic combustor SO AIAA JOURNAL LA English DT Article; Proceedings Paper CT AIAA 40th Aerospace Sciences Meeting CY JAN 14-18, 2002 CL RENO, NEVADA SP Amer Inst Aeronaut & Astronaut ID TEMPERATURE; FLOW; SCATTERING; JET AB An experiment has been conducted to acquire data for the validation of computational fluid dynamics codes used in the design of supersonic combustors. The How in a supersonic combustor, consisting of a diverging duct with a single downstream-angled wall injector, is studied. Combustor entrance Mach number is 2 and enthalpy nominally corresponds to Mach 7 flight. The primary measurement technique is coherent anti-Stokes Raman spectroscopy, but surface pressures and temperatures have also been acquired. Modern design of experiment techniques have been used to maximize the quality of the data set (for the given level of effort) and to minimize systematic errors. Temperature maps are obtained at several planes in the flow for a case in which the combustor is piloted by injecting fuel upstream of the main injector and one case in which it is not piloted. Boundary conditions and uncertainties are characterized. C1 George Washington Univ, Hampton, VA 23681 USA. NASA, Langley Res Ctr, Instrumentat Syst Dev Branch, Hampton, VA 23681 USA. NASA, Langley Res Ctr, Hyperson Airbreathing Prop Branch, Hampton, VA 23681 USA. RP Cutler, AD (reprint author), George Washington Univ, MS 335, Hampton, VA 23681 USA. NR 27 TC 16 Z9 16 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 DEC PY 2003 VL 41 IS 12 BP 2451 EP 2459 DI 10.2514/2.6844 PG 9 WC Engineering, Aerospace SC Engineering GA 754NE UT WOS:000187322600017 ER PT J AU Chen, F Xue, YY Hadjiev, VG Chu, CW Nikolaev, P Arepalli, S AF Chen, F Xue, YY Hadjiev, VG Chu, CW Nikolaev, P Arepalli, S TI Fast characterization of magnetic impurities in single-walled carbon nanotubes SO APPLIED PHYSICS LETTERS LA English DT Article ID COBALT PARTICLES; HIPCO PROCESS; MONOXIDE AB We have demonstrated that the magnetic susceptibility measurement is a nondestructive, fast, and accurate method to determine the residual metal catalysts in a few microgram single-walled carbon nanotube (SWCNT) sample. We have studied magnetic impurities in raw and purified SWCNTs by magnetic susceptibility measurements, transmission electron microscopy, and thermogravimetry. The data suggest that the saturation magnetic moment and the effective field, which are caused by the interparticle interactions, decrease and increase, respectively, with the decrease of the particle size. Methods are suggested to overcome the uncertainty associated. (C) 2003 American Institute of Physics. C1 Univ Houston, Texas Ctr Superconduct & Adv Mat, Houston, TX 77204 USA. GB Tech NASA JSC, Houston, TX 77058 USA. Lawrence Berkeley Lab, Berkeley, CA 94720 USA. Hong Kong Univ Sci & Technol, Hong Kong, Hong Kong, Peoples R China. RP Chen, F (reprint author), Univ Houston, Texas Ctr Superconduct & Adv Mat, Houston, TX 77204 USA. EM fchen@uh.edu RI Arepalli, Sivaram/A-5372-2010; Nikolaev, Pavel/B-9960-2009; Hadjiev, Viktor/A-7069-2008 OI Hadjiev, Viktor/0000-0001-8579-9357 NR 11 TC 21 Z9 21 U1 0 U2 3 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0003-6951 EI 1077-3118 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD DEC 1 PY 2003 VL 83 IS 22 BP 4601 EP 4603 DI 10.1063/1.1630854 PG 3 WC Physics, Applied SC Physics GA 747CF UT WOS:000186787100045 ER PT J AU Corsetti, FA Storrie-Lombardi, MC AF Corsetti, FA Storrie-Lombardi, MC TI Lossless compression of stromatolite images: A biogenicity index? SO ASTROBIOLOGY LA English DT Article DE stromatolites; lossless compression; biosignatures; complexity analysis ID CELLULAR-AUTOMATA; COMPLEXITY; ORIGIN AB It has been underappreciated that inorganic processes can produce stromatolites (laminated macroscopic constructions commonly attributed to microbiological activity), thus calling into question the long-standing use of stromatolites as de facto evidence for ancient life. Using lossless compression on unmagnified reflectance red-green-blue (RGB) images of matched stromatolite-sediment matrix pairs as a complexity metric, the compressibility index (delta(c) the log of the ratio of the compressibility of the matrix versus the target) of a putative abiotic test stromatolite is significantly less than the delta(c) of a putative biotic test stromatolite. There is a clear separation in delta(c) between the different stromatolites discernible at the outcrop scale. In terms of absolute compressibility, the sediment matrix between the stromatolite columns was low in both cases, the putative abiotic stromatolite was similar to the intracolumnar sediment, and the putative biotic stromatolite was much greater (again discernible at the outcrop scale). We propose that this metric would be useful for evaluating the biogenicity of images obtained by the camera systems available on every Mars surface probe launched to date including Viking, Pathfinder, Beagle, and the two Mars Exploration Rovers. C1 Univ So Calif, Dept Earth Sci, Los Angeles, CA USA. CALTECH, Jet Propuls Lab, Ctr Life Detect, Pasadena, CA USA. RP Storrie-Lombardi, MC (reprint author), Kinohi Inst, Pasadena, CA 91101 USA. EM mike@kinohi.org NR 31 TC 16 Z9 16 U1 1 U2 6 PU MARY ANN LIEBERT INC PUBL PI LARCHMONT PA 2 MADISON AVENUE, LARCHMONT, NY 10538 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD WIN PY 2003 VL 3 IS 4 BP 649 EP 655 DI 10.1089/153110703322735980 PG 7 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 773BG UT WOS:000188877400001 PM 14994715 ER PT J AU Segura, A Krelove, K Kasting, JF Sommerlatt, D Meadows, V Crisp, D Cohen, M Mlawer, E AF Segura, A Krelove, K Kasting, JF Sommerlatt, D Meadows, V Crisp, D Cohen, M Mlawer, E TI Ozone concentrations and ultraviolet fluxes on Earth-like planets around other stars SO ASTROBIOLOGY LA English DT Article DE terrestrial planet finder; biomarkers; ozone; extrasolar planets ID PROTEROZOIC OCEAN CHEMISTRY; OXYGEN GEOCHEMICAL CYCLE; MAIN-SEQUENCE STARS; ATMOSPHERIC OZONE; MULTIPLE-SCATTERING; RADIATIVE-TRANSFER; HABITABLE ZONES; SULFUR CYCLE; LIFE; EVOLUTION AB Coupled radiative-convective/photochemical modeling was performed for Earth-like planets orbiting different types of stars (the Sun as a G2V, an F2V, and a K2V star). O-2 concentrations between 1 and 10(-5) times the present atmospheric level (PAL) were simulated. The results were used to calculate visible/near-IR and thermal-IR spectra, along with surface UV fluxes and relative dose rates for erythema and DNA damage. For the spectral resolution and sensitivity currently planned for the first generation of terrestrial planet detection and characterization missions, we find that O-2 should be observable remotely in the visible for atmospheres containing at least 10(-2) PAL of O-2. O-3 should be visible in the thermal-IR for atmospheres containing at least 10(-3) PAL of O-2. CH4 is not expected to be observable in 1 PAL O-2 atmospheres like that of modern Earth, but it might be observable at thermal-IR wavelengths in "mid-Proterozoic-type" atmospheres containing similar to10(-1) PAL of O-2. Thus, the simultaneous detection of both O-3 and CH4-considered to be a reliable indication of life-is within the realm of possibility. High-O-2 planets orbiting K2V and F2V stars are both better protected from surface UV radiation than is modern Earth. For the F2V case the high intrinsic UV luminosity of the star is more than offset by the much thicker ozone layer. At O-2 levels below similar to10(-2) PAL, planets around all three types of stars are subject to high surface UV fluxes, with the F2V planet exhibiting the most biologically dangerous radiation environment. Thus, while advanced life is theoretically possible on high-O-2 planets around F stars, it is not obvious that it would evolve as it did on Earth. C1 Penn State Univ, Dept Geosci, State Coll, PA USA. NASA, CALTECH, Jet Propuls Lab, Pasadena, CA USA. Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. Atmospher & Environm Res Inc, Lexington, MA USA. RP Segura, A (reprint author), 443 Deike Bldg,Univ Pk, State Coll, PA 16803 USA. EM antigona@essc.psu.edu NR 58 TC 136 Z9 140 U1 2 U2 27 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 WIN PY 2003 VL 3 IS 4 BP 689 EP 708 DI 10.1089/153110703322736024 PG 20 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 773BG UT WOS:000188877400005 PM 14987475 ER PT J AU Benardini, JN Sawyer, J Venkateswaran, K Nicholson, WL AF Benardini, JN Sawyer, J Venkateswaran, K Nicholson, WL TI Spore UV and acceleration resistance of endolithic Bacillus pumilus and Bacillus subtilis isolates obtained from Sonoran desert basalt: Implications for lithopanspermia SO ASTROBIOLOGY LA English DT Article DE bacterial spores; Bacillus pumilus; Bacillus subtilis; UV resistance; extreme acceleration; lithopanspermia ID ENDOSPORES; TERRESTRIAL; ENVIRONMENT; ANTHRACIS; SEQUENCE; IMPACT; EJECTA; EARTH; SPACE; MARS AB Bacterial spores have been used as model systems for studying the theory of interplanetary transport of life by natural processes such as asteroidal or cometary impacts (i.e., lithopanspermia). Because current spallation theory predicts that near-surface rocks are ideal candidates for planetary ejection and surface basalts are widely distributed throughout the rocky planets, we isolated spore-forming bacteria from the interior of near-subsurface basalt rocks collected in the Sonoran desert near Tucson, Arizona. Spores were found to inhabit basalt at very low concentrations (less than or equal to28 colony-forming units/g) in these samples. Six isolates identified as being most closely related to Bacillus pumilus and one Bacillus subtilis isolate were recovered from near-subsurface basalt samples. Populations of purified spores prepared from the isolated strains were subjected to 254-nm UV and ballistics tests in order to assess their resistance to UV radiation and to extreme acceleration shock, two proposed lethal factors for spores during interplanetary transfer. Specific natural isolates of B. pumilus were found to be substantially more resistant to UV and extreme acceleration than were reference laboratory strains of B. subtilis, the benchmark organism, suggesting that spores of environmental B. pumilus isolates may be more likely to survive the rigors of interplanetary transfer. C1 Univ Arizona, Dept Vet Sci & Microbiol, Tucson, AZ USA. NASA, Jet Propuls Lab, Planetary Protect Technol Grp, Pasadena, CA USA. RP Nicholson, WL (reprint author), Dept Microbiol & Cell Sci, Space Life Sci Lab, Bldg M6-1025-SLSL,Room 201B,Kennedy Pkwy & 5th St, Kennedy Space Ctr, FL 32899 USA. EM WLN@ufl.edu NR 32 TC 41 Z9 43 U1 2 U2 8 PU MARY ANN LIEBERT INC PUBL PI LARCHMONT PA 2 MADISON AVENUE, LARCHMONT, NY 10538 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD WIN PY 2003 VL 3 IS 4 BP 709 EP 717 DI 10.1089/153110703322736033 PG 9 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 773BG UT WOS:000188877400006 PM 14987476 ER PT J AU Lindsay, JF McKay, DS Allen, CC AF Lindsay, JF McKay, DS Allen, CC TI Earth's earliest biosphere - A proposal to develop a collection of curated archean geologic reference materials SO ASTROBIOLOGY LA English DT Review DE geologic curated collection; archean; western Australia; early life on earth ID MASSIVE SULFIDE DEPOSIT; BILLION YEARS AGO; WESTERN-AUSTRALIA; PILBARA-CRATON; TECTONIC EVOLUTION; WARRAWOONA GROUP; NORTH-POLE; PALAEOPROTEROZOIC BRYAH; STROMATOLITES OLDER; ABIOLOGICAL ORIGIN AB The discovery of evidence indicative of life in a Martian meteorite has led to an increase in interest in astrobiology. As a result of this discovery, and the ensuing controversy, it has become apparent that our knowledge of the early development of life on Earth is limited. Archean stratigraphic successions containing evidence of Earth's early biosphere are well preserved in the Pilbara Craton of Western Australia. The craton includes part of a protocontinent consisting of granitoid complexes that were emplaced into, and overlain by, a 3.51-2.94 Ga volcanigenic carapace-the Pilbara Supergroup. The craton is overlain by younger supracrustal basins that form a time series recording Earth history from approximately 2.8 Ga to approximately 1.9 Ga. It is proposed that a well-documented suite of these ancient rocks be collected as reference material for Archean and astrobiological research. All samples would be collected in a well-defined geological context in order to build a framework to test models for the early evolution of life on Earth and to develop protocols for the search for life on other planets. C1 Lunar & Planetary Inst, Houston, TX 77058 USA. NASA, Johnson Space Ctr, Houston, TX USA. RP Lindsay, JF (reprint author), Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77058 USA. EM john.f.lindsay@jsc.nasa.gov NR 103 TC 8 Z9 8 U1 0 U2 7 PU MARY ANN LIEBERT INC PUBL PI LARCHMONT PA 2 MADISON AVENUE, LARCHMONT, NY 10538 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD WIN PY 2003 VL 3 IS 4 BP 739 EP 758 DI 10.1089/153110703322736060 PG 20 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 773BG UT WOS:000188877400009 PM 14987479 ER PT J AU Greeley, R Morrison, D AF Greeley, R Morrison, D TI Europa - Introduction SO ASTROBIOLOGY LA English DT Editorial Material C1 Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Greeley, R (reprint author), Arizona State Univ, Dept Geol Sci, Box 871404, Tempe, AZ 85287 USA. EM greeley@asu.edu NR 0 TC 1 Z9 1 U1 0 U2 1 PU MARY ANN LIEBERT INC PUBL PI LARCHMONT PA 2 MADISON AVENUE, LARCHMONT, NY 10538 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD WIN PY 2003 VL 3 IS 4 BP 759 EP 759 DI 10.1089/153110703322736079 PG 1 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 773BG UT WOS:000188877400010 ER PT J AU Dalton, JB AF Dalton, JB TI Spectral behavior of hydrated sulfate salts: implications for Europa mission spectrometer design SO ASTROBIOLOGY LA English DT Article DE hydrated salts; Europa; infrared spectroscopy; remote sensing ID GALILEAN SATELLITES; WATER ICE; IMPACT FEATURES; MU-M; LIFE; SURFACE; SYSTEM; SEARCH; EARTH; OCEAN AB Remote sensing of the surface of Europa with near-infrared instruments has suggested the presence of hydrated materials, including sulfate salts. Attention has been focused on these salts for the information they might yield regarding the evolution of a putative interior ocean, and the evaluation of its astrobiological potential. These materials exhibit distinct infrared absorption features due to bound water. The interactions of this water with the host molecules lead to fine structure that can be used to discriminate among these materials on the basis of their spectral behavior. This fine structure is even more pronounced at the low temperatures prevalent on icy satellites. Examination of hydrated sulfate salt spectra measured under cryogenic temperature conditions provides realistic constraints for future remote-sensing missions to Europa. In particular, it suggests that a spectrometer system capable of 2-5 nm spectral resolution or better, with a spatial resolution approaching 100 m, would be able to differentiate among proposed hydrated surface materials, if present, and constrain their distributions across the surface. Such information would provide valuable insights into the evolutionary history of Europa. C1 NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. RP Dalton, JB (reprint author), NASA, Ames Res Ctr, SETI Inst, MS 245-3, Moffett Field, CA 94035 USA. EM dalton@mail.arc.nasa.gov NR 62 TC 27 Z9 27 U1 1 U2 12 PU MARY ANN LIEBERT INC PUBL PI LARCHMONT PA 2 MADISON AVENUE, LARCHMONT, NY 10538 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD WIN PY 2003 VL 3 IS 4 BP 771 EP 784 DI 10.1089/153110703322736097 PG 14 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 773BG UT WOS:000188877400012 PM 14987482 ER PT J AU Soffel, M Klioner, SA Petit, G Wolf, P Kopeikin, SM Bretagnon, P Brumberg, VA Capitaine, N Damour, T Fukushima, T Guinot, B Huang, TY Lindegren, L Ma, C Nordtvedt, K Ries, JC Seidelmann, PK Vokrouhlicky, D Will, CM Xu, C AF Soffel, M Klioner, SA Petit, G Wolf, P Kopeikin, SM Bretagnon, P Brumberg, VA Capitaine, N Damour, T Fukushima, T Guinot, B Huang, TY Lindegren, L Ma, C Nordtvedt, K Ries, JC Seidelmann, PK Vokrouhlicky, D Will, CM Xu, C TI The IAU 2000 resolutions for astrometry, celestial mechanics, and metrology in the relativistic framework: Explanatory supplement SO ASTRONOMICAL JOURNAL LA English DT Article DE astrometry; celestial mechanics; reference systems; time ID REFERENCE SYSTEMS; TIME EPHEMERIS; MOTION; EARTH; DEFINITION; DEFLECTION; EQUATIONS; FOUNTAIN; VICINITY; WAVES AB We discuss the IAU resolutions B1.3, B1.4, B1.5, and B1.9 that were adopted during the 24th General Assembly in Manchester, 2000, and provides details on and explanations for these resolutions. It is explained why they present significant progress over the corresponding IAU 1991 resolutions and why they are necessary in the light of present accuracies in astrometry, celestial mechanics, and metrology. In fact, most of these resolutions are consistent with astronomical models and software already in use. The metric tensors and gravitational potentials of both the Barycentric Celestial Reference System and the Geocentric Celestial Reference System are defined and discussed. The necessity and relevance of the two celestial reference systems are explained. The transformations of coordinates and gravitational potentials are discussed. Potential coefficients parameterizing the post-Newtonian gravitational potentials are expounded. Simplified versions of the time transformations suitable for modern clock accuracies are elucidated. Various approximations used in the resolutions are explicated and justified. Some models (e.g., for higher spin moments) that serve the purpose of estimating orders of magnitude have actually never been published before. C1 Tech Univ Dresden, Inst Planetare Geodasie, Lohrmann Observ, D-01062 Dresden, Germany. Bur Int Poids & Mesures, F-92312 Sevres, France. Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA. Bur Longitudes, F-75014 Paris, France. Russian Acad Sci, Inst Appl Astron, St Petersburg 191187, Russia. Observ Paris, F-75014 Paris, France. Inst Hautes Etud Sci, F-91440 Bures Sur Yvette, France. Natl Astron Observ, Tokyo 181, Japan. Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China. Chinese Acad Sci, Natl Astron Observ, Beijing 100864, Peoples R China. Lund Univ, Inst Astron, SE-22100 Lund, Sweden. NASA, Space Geodesy Branch, Terr Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NW Anal, Bozeman, MT 59715 USA. Univ Texas, Ctr Space Res, Austin, TX 78712 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Charles Univ Prague, Astron Ustav, CZ-18000 Prague 8, Czech Republic. Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA. Washington Univ, Dept Phys, St Louis, MO 63130 USA. Nanjing Normal Univ, Dept Phys, Nanjing 210097, Peoples R China. RP Tech Univ Dresden, Inst Planetare Geodasie, Lohrmann Observ, Mommsenstr 13, D-01062 Dresden, Germany. RI Ma, Chopo/D-4751-2012; Kopeikin, Sergei/A-8857-2009; Klioner, Sergei/C-7927-2009 OI Kopeikin, Sergei/0000-0002-4866-1532; NR 50 TC 172 Z9 181 U1 1 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD DEC PY 2003 VL 126 IS 6 BP 2687 EP 2706 DI 10.1086/378162 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 759EN UT WOS:000187725500009 ER PT J AU Doppmann, GW Jaffe, DT AF Doppmann, GW Jaffe, DT TI A spectroscopic technique for measuring stellar properties of pre-main-sequence stars SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared radiation; methods : analytical; stars : fundamental parameters techniques : spectroscopic ID RHO-OPHIUCHI CLOUD; NEAR-INFRARED SPECTRA; T-TAURI STARS; AURIGA MOLECULAR CLOUD; LOW-MASS STARS; H-R DIAGRAM; IRON ABUNDANCES; MU-M; ROTATIONAL VELOCITIES; ECHELLE SPECTROGRAPH AB We describe a technique for deriving effective temperatures, surface gravities, rotation velocities, and radial velocities from high-resolution near-IR spectra. The technique matches the observed near-IR spectra to spectra synthesized from model atmospheres. Our analysis is geared toward characterizing heavily reddened pre-main-sequence stars, but the technique also has potential applications in characterizing main-sequence and post-main-sequence stars when these lie behind thick clouds of interstellar dust. For the pre main-sequence stars, we use the same matching process to measure the amount of excess near-IR emission ( which may arise in the protostellar disks) in addition to the other stellar parameters. The information derived from high-resolution spectra comes from line shapes and the relative line strengths of closely spaced lines. The values for the stellar parameters we derive are therefore independent of those derived from low-resolution spectroscopy and photometry. The new method offers the promise of improved accuracy in placing young stellar objects on evolutionary model tracks. Tests with an artificial noisy spectrum with typical stellar parameters and a signal-to-noise ratio of 50 indicate a 1sigma error of 100 K in T-eff, 2 km s(-1) in v sin i, and 0.13 in continuum veiling for an input veiling of 1. If the flux ratio between the sum of the Na, Sc, and Si lines at 2.2 mum and the (2 - 0) (CO)-C-12 band head at 2.3 mum is known to an accuracy of 10%, the errors in our best-fit value for log g will be Delta log g = 0.1 - 0.2. We discuss the possible systematic effects on our determination of the stellar parameters and evaluate the accuracy of the results derivable from high-resolution spectra. In the context of this evaluation, we quantitatively explore the degeneracy between temperature and gravity that has bedeviled efforts to type young stellar objects using low-resolution spectra. The analysis of high-resolution near-IR spectra of MK standards shows that the technique yields very accurate values for the effective temperature. The greatest uncertainty in comparing our results with optical spectral typing of MK standards is in the spectral type-to-effective temperature conversion for the standards themselves. Even including this uncertainty, the 1sigma difference between the optical and infrared temperatures for dwarfs at 3000 - 5800 K is only 140 K. In a companion paper, we present an analysis of heavily extincted young stellar objects in the rho Ophiuchi molecular cloud. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. RP Doppmann, GW (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA. NR 74 TC 14 Z9 15 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 DEC PY 2003 VL 126 IS 6 BP 3030 EP 3042 DI 10.1086/379292 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 759EN UT WOS:000187725500033 ER PT J AU Doppmann, GW Jaffe, DT White, RJ AF Doppmann, GW Jaffe, DT White, RJ TI Stellar properties of pre-main-sequence stars from high-resolution near-infrared spectra SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared radiation; stars : fundamental parameters; stars : low-mass, brown dwarfs; stars : pre-main-sequence; stars : rotation; techniques : spectroscopic ID T-TAURI STARS; RHO-OPHIUCHI CLOUD; ORION-NEBULA-CLUSTER; H-R DIAGRAM; DARK-CLOUD; YOUNG STARS; DISK ACCRETION; MAGNETOSPHERIC ACCRETION; EVOLUTIONARY STATUS; MOLECULAR CLOUDS AB We present high-resolution (R = 50; 000) spectra at 2.2 mum of 16 young stars in the rho Ophiuchi dark cloud. Photospheric features are detected in the spectra of 11 of these sources, all Class II young stellar objects. The five featureless spectra consist of two Class I, two Class I. 5, and one Class II. One star, GSS 29, is identified as a spectroscopic binary based on radial velocity variations. The radial velocities for the remaining sample are consistent with (CO)-C-12 and H2CO gas velocities and further confirm the membership of the sources in the rho Oph cluster. For the 10 spectroscopically single Class II sources, we measure effective temperatures, continuum veiling, and v sin i rotation from the shapes and strengths of atomic photospheric lines by comparison with spectral synthesis models at 2.2 mum. We measure surface gravities in two stars from the integrated line flux ratio of the (CO)-C-12 line region at 2.3 mum and the Na I line region at 2.2 mum. Although the majority (8/ 10) of the Class II stars have similar effective temperatures (3530 +/- 100 K), they exhibit a large spread in bolometric luminosities (a factor of similar to8), as derived from near-IR photometry. In the two stars for which we have surface gravity measurements from spectroscopy, the photometrically derived luminosities are systematically higher than the spectroscopic luminosities. The spread in the photometrically derived luminosities in our other sources suggests either a large spread in stellar ages or nonphotospheric emission in the J band since anomalous and significant veiling at J has been observed in other T Tauri stars. Our spectroscopic luminosities result in older ages on the Hertzsprung-Russell diagram than are suggested by photometry at J or K. Most of our sources show a larger amount of continuum excess (F-K ex) than stellar flux at 2.2 mum (F-K*), substantially higher in many cases (r(K) = F-K ex/F-K* = 0.3-4.5). The derived veiling values at K (r(K)) appear correlated with mid-IR disk luminosity and with Brackett gamma equivalent width, corrected for veiling. The derived v sin i rotation is substantial (12 - 39 km s(-1)), but systematically less than the rotation measured in Class I. 5 (. at) and Class I sources from other studies in Ophiuchus. In four stars ( Class I and I. 5 sources), the absence of any photospheric lines is likely due to large continuum excess and/or rapid rotation if the stars have late-type photospheres. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. RP Doppmann, GW (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA. NR 85 TC 27 Z9 27 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 DEC PY 2003 VL 126 IS 6 BP 3043 EP 3057 DI 10.1086/378958 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 759EN UT WOS:000187725500034 ER PT J AU Walter, FM Herczeg, G Brown, A Ardila, DR Gahm, GF Johns-Krull, CM Lissauer, JJ Simon, M Valenti, JA AF Walter, FM Herczeg, G Brown, A Ardila, DR Gahm, GF Johns-Krull, CM Lissauer, JJ Simon, M Valenti, JA TI Mapping the circumstellar environment of T Tauri with fluorescent H-2 emission SO ASTRONOMICAL JOURNAL LA English DT Article DE ISM : molecules; stars : individual (T Tauri) ID HUBBLE-SPACE-TELESCOPE; FAR-ULTRAVIOLET SPECTRUM; MAIN-SEQUENCE EVOLUTION; HERBIG-HARO OBJECT-43; YOUNG BINARY-SYSTEM; SPATIAL-DISTRIBUTION; MOLECULAR-HYDROGEN; BURNHAMS NEBULA; RADIO-SOURCE; IUE ATLAS AB We have obtained three long-slit, far-UV spectra of the pre-main-sequence system T Tauri. These Hubble Space Telescope STIS spectra show a strong and variable on-source spectrum composed of both fluoresced H-2 and stellar chromospheric lines. Extended H-2 emission is seen up to 10" from the T Tau system. The on-source and extended H-2 are both pumped by H I Lyalpha. The on-source H-2 is pumped by the red wing of a broad, self-absorbed Lyalpha line, while the progressions seen in the extended gas are pumped from near line center. This suggests that the extended H-2 is pumped locally and not by the stellar Lyalpha line. The H-2 to the north and west coincides with the evacuated cavity bounded by the optical reflection nebulosity; to the south the extended H-2 coincides with the HH 255 outflow from the embedded infrared companion T Tau S. The spatial pro. le of the extended gas shows a prominent dip coincident with the position of T Tau S. This may be absorption by a disk associated with T Tau S. There is no evidence for absorption by a disk surrounding T Tau N large enough to obscure T Tau S. C1 SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. Univ Colorado, JILA, Boulder, CO 80309 USA. Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Stockholm Univ, SE-10691 Stockholm, Sweden. Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA. NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Walter, FM (reprint author), SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. OI Herczeg, Gregory/0000-0002-7154-6065 NR 60 TC 45 Z9 46 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 DEC PY 2003 VL 126 IS 6 BP 3076 EP 3089 DI 10.1086/379557 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 759EN UT WOS:000187725500036 ER PT J AU Walsh, RW Ireland, J AF Walsh, RW Ireland, J TI The heating of the solar corona SO ASTRONOMY AND ASTROPHYSICS REVIEW LA English DT Review DE Sun : corona; Sun : magnetic fields; MHD; Sun : activity; Sun : oscillations ID TRANSITION REGION OSCILLATIONS; SLOW MAGNETOACOUSTIC WAVES; LONGITUDINAL INTENSITY OSCILLATIONS; 3-DIMENSIONAL STEREOSCOPIC ANALYSIS; MAGNETOHYDRODYNAMIC SURFACE-WAVES; PHOTOSPHERIC MAGNETIC-FIELD; AZIMUTHAL FOOTPOINT MOTIONS; EUV TRANSIENT BRIGHTENINGS; MICHELSON DOPPLER IMAGER; SHEAR ALFVEN WAVES AB The heating of the solar corona has been a fundamental astrophysical issue for over sixty years. Over the last decade in particular, space-based solar observatories (Yohkoh, SOHO and TRACE) have revealed the complex and often subtle magnetic-field and plasma interactions throughout the solar atmosphere in unprecedented detail. It is now established that any energy release mechanism is magnetic in origin - the challenge posed is to determine what specific heat input is dominating in a given coronal feature throughout the solar cycle. This review outlines a range of possible magnetohydrodynamic (MHD) coronal heating theories, including MHD wave dissipation and MHD reconnection as well as the accumulating observational evidence for quasi-periodic oscillations and small-scale energy bursts occurring in the corona. Also, we describe current attempts to interpret plasma temperature, density and velocity diagnostics in the light of specific localised energy release. The progress in these investigations expected from future solar missions (Solar-B, STEREO, SDO and Solar Orbiter) is also assessed. C1 Univ Cent Lancashire, Ctr Astrophys, Preston PR1 2HE, Lancs, England. NASA, L3 Commun EER Syst Inc, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Univ Cent Lancashire, Ctr Astrophys, Preston PR1 2HE, Lancs, England. EM rwwalsh@uclan.ac.uk NR 208 TC 63 Z9 65 U1 1 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0935-4956 EI 1432-0754 J9 ASTRON ASTROPHYS REV JI Astron. Astrophys. Rev. PD DEC PY 2003 VL 12 IS 1 BP 1 EP 41 DI 10.1007/s00159-003-0021-9 PG 41 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 752UM UT WOS:000187185600001 ER PT J AU Miroshnichenko, AS Kusakin, AV Bjorkman, KS Drake, NA Rudy, RJ Lynch, DK Mazuk, S Venturini, CC Puetter, RC Perry, RB AF Miroshnichenko, AS Kusakin, AV Bjorkman, KS Drake, NA Rudy, RJ Lynch, DK Mazuk, S Venturini, CC Puetter, RC Perry, RB TI HD 19993 and HD 29035: New bright A-type emission-line stars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques : spectroscopic; techniques : photometric; stars : circumstellar matter; stars : individual : HD 19993, HD 29035 ID INTERMEDIATE-MASS STARS; ATMOSPHERIC PARAMETERS; INFRARED EXCESS; DATA-BASE; F STARS; SUPERGIANTS; ABUNDANCES; COLORS; PHOTOMETRY; EVOLUTION AB We present the results of photometric and spectroscopic observations of two A-type stars (HD19993 and HD29035), optical counterparts of the IRAS sources (F03108+3729 and 04331+5211, respectively). Halpha line emission is found in the optical spectra of both objects for the first time. Our analysis of the spectral line profiles and the photometric information shows that HD19993 is an A7/8 II star (T(eff)similar to7500+/-200 K, log g=2.7+/-0.2, v sin i=35+/-2 km s(-1), M=4.8+/-0.8 M-circle dot) with a mild metal deficit ([Fe/H]similar to-0.3+/-0.1), while HD29035 is a B9/A0 V star (T(eff)similar to10000 K, log gsimilar to4, v sin isimilar to150 km s(-1)). The presence of an IR excess and the Halpha emission in combination with a very different location in the Hertzsprung-Russell diagram suggest the different nature and evolutionary stages of the objects. We conclude that HD29035 is a candidate Herbig Ae type star, a possible member of a group of similar objects. HD19993 seems to be a post-main-sequence object. C1 Univ Toledo, Dept Phys & Astron, Ritter Observ, Toledo, OH 43606 USA. Pulkovo Observ, St Petersburg 196140, Russia. Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119899, Russia. Fesenkov Astrophys Inst, Alma Ata 480068, Kazakhstan. Observ Nacl MCT, BR-20921400 Rio De Janeiro, Brazil. St Petersburg Univ, Sobolev Astron Inst, St Petersburg 198504, Russia. Aerosp Corp, Los Angeles, CA 90009 USA. Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. NASA, Langley Res Ctr, Earth & Space Sci Support Off, Hampton, VA 23681 USA. RP Miroshnichenko, AS (reprint author), Univ Toledo, Dept Phys & Astron, Ritter Observ, Toledo, OH 43606 USA. EM anatoly@physics.utoledo.edu RI Drake, Natalia/K-7232-2013 OI Drake, Natalia/0000-0003-4842-8834 NR 50 TC 5 Z9 5 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2003 VL 412 IS 1 BP 219 EP 228 DI 10.1051/0004-6361:20031416 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 747JC UT WOS:000186800600022 ER PT J AU Tsurutani, B Wu, ST Zhang, TX Dryer, M AF Tsurutani, B Wu, ST Zhang, TX Dryer, M TI Coronal Mass Ejection (CME)-induced shock formation, propagation and some temporally and spatially developing shock parameters relevant to particle energization SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun : corona; Sun : interplanetary shocks; Sun : CME; Sun : MHD ID INTERPLANETARY SHOCKS; MAGNETIC CLOUD; JANUARY 1997; ERUPTIVE PROMINENCE; LASCO OBSERVATIONS; PROTON EVENTS; FLUX ROPE; ACCELERATION; EVOLUTION; STREAMER AB Interplanetary shocks accelerate solar energetic particles (SEPs) from the point of shock formation in the lower corona, and continuously as the shock propagates outward to 1 AU and beyond. In this study, the formation properties of a CME-induced shock and propagation characteristics are studied from the inner corona to 1 AU. We use a 2D, three-component (i.e., 2.5D), time-dependent MHD code in our model. A well-studied CME event (the 1997 January 6-12 Sun-Earth Connection Event) is used as a baseline for this study. The solar wind conditions measured at 1 AU (WIND data) are used to motivate our effort to model the CME driven shock. It is found that the fast forward shock forms originally at similar to3.2 R(s) (solar radii) from the solar surface in the ecliptic plane for the assumed CME and background solar wind parameters. In our model, this occurs similar to2 hrs after CME initiation. The shock formation at higher (similar to30degrees) latitudes measured from the ecliptic plane is further from the Sun (similar to3.6 R(s)) because of higher local magnetosonic speeds that must be exceeded by the original disturbance for shock formation. Finally, the shock becomes symmetric at 16 R(s). In the ecliptic plane at 16 R(s) the fast shock Mach number (M(f)) is similar to3.5, and at 30degrees latitude, M(f)similar to1.7, considerably weaker. A maximum in the fast shock Mach number of 4 is reached at 130 R(s) in the ecliptic plane. The M(f) decreases to 3.5 by 1 AU. Other properties of the shock, as well as its relationship to the local interplanetary properties through which it passes, are discussed. The interplanetary counterpart, ICME, of the coronal CME, is also discussed. These shock properties, we believe, are relevant to the shock's ability to accelerate particles to energies as high as 100 MeV. The actual physical process, however, is not discussed in this paper. C1 Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. CALTECH, Jet Prop Lab, Pasadena, CA USA. NASA, Space Environm Ctr, Boulder, CO 80305 USA. RP Wu, ST (reprint author), Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. EM wus@cspar.uah.edu NR 52 TC 28 Z9 28 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 DEC PY 2003 VL 412 IS 1 BP 293 EP 304 DI 10.1051/0004-6361:20031413 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 747JC UT WOS:000186800600031 ER PT J AU Poulet, F Cruikshank, DP Cuzzi, JN Roush, TL French, RG AF Poulet, F Cruikshank, DP Cuzzi, JN Roush, TL French, RG TI Compositions of Saturn's rings A, B, and C from high resolution near-infrared spectroscopic observations SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planets : rings; radiative transfer ID OPTICAL-CONSTANTS; REFLECTANCE SPECTROSCOPY; SOLAR-SYSTEM; SPECTRA; ICE; SURFACES; SATELLITES; MICROWAVE; CENTAURS; COMETARY AB We used the NASA IRTF spectrograph SpeX to obtain near-infrared spectra (0.9-5.4 mum) of Saturn's rings, achieving spectral resolution lambda/lambdaDelta of about 2000. The spatial resolution (about 1 arcsec) is sufficient to distinguish the three main ring components (A, B and C rings) from one another. These new observations of Saturn's rings are the first to combine an extended spectral range with high spectral resolution and good spatial resolution. We combined these data with recent photometric observations acquired by HST in the 0.3-1.0 mum range. The spectra of the A band B rings are dominated by strong features due to crystalline water ice. The shape and the depth of these absorptions differ for each ring, which indicates different water ice grain sizes and abundances. No spectral evidence for volatile ices other than water ice has been detected. Both the lower albedo and the less blue slope in the near-infrared reflectance of the C ring indicate a concentration of dark material different from that in the A and B rings. The broader triangular Fresnel reflection peak at 3.1 mum may support the presence of some amount of amorphous ice. The C ring spectrum exhibits bands centered at 1.73 and 3.4 mum which agree in position quite well with the C-H bands. Although the detection is probable, it requires confirmation. With a radiative transfer model, we constrain the grain sizes and the relative abundances of water ice, a dark colorless component (amorphous carbon) to adjust the albedo and a second contaminant to reproduce the reddening in the UV-visible range represented here by organic tholins. The dark component of the C ring spectrum is included as an intra-mixture only. The cosmogenic implications of the inferred compositions are discussed. C1 Univ Paris 11, IAS, F-91405 Orsay, France. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Wellesley Coll, Dept Astron, Wellesley, MA 02481 USA. RP Poulet, F (reprint author), Univ Paris 11, IAS, Batiment 121, F-91405 Orsay, France. NR 46 TC 48 Z9 48 U1 1 U2 6 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2003 VL 412 IS 1 BP 305 EP 316 DI 10.1051/0004-6361:20031123 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 747JC UT WOS:000186800600032 ER PT J AU Yudin, RV Evans, A Barrett, P Albinson, JS Davies, JK Hutchinson, MG AF Yudin, RV Evans, A Barrett, P Albinson, JS Davies, JK Hutchinson, MG TI Polarimetry of evolved stars - III. RV Tau and R CrB stars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE polarization; stars : circumstellar matter; stars : variable : general ID CORONAE-BOREALIS STARS; LOW-MASS STARS; MULTIWAVELENGTH OBSERVATIONS; WAVELENGTH DEPENDENCE; VARIABLE-STARS; AC-HERCULIS; INFRARED OBSERVATIONS; LINEAR-POLARIZATION; CEPHEID VARIABLES; MIRA VARIABLES AB We present broadband optical polarimetry, and broadband optical and infrared photometry, of eight RV Tau-type and five R CrB-type stars; much of the photometry and polarimetry was obtained simultaneously. For nine of the objects polarimetric data is reported for the first time. We have estimated and subtracted the interstellar component of polarization, allowing us to determine the level of intrinsic polarization. In some cases this is similar or equal to 1% - 2% even when the star is in a bright photometric state. We consider this to be evidence for the presence of permanent clumpy non-spherical dust shells around the RV Tau and R CrB-type stars we observed. Our polarimetric and photometric data lead us to conclude that, for most of our programme stars, neutral extinction must be significant in their circumstellar envelopes. Apart from the brightness variations due to pulsations and changes in the effective temperature of stars, there is clear evidence of wavelength-independent flux variations - with amplitude from 0.(m)5 to 1.(m)0 - implying the presence of large (a greater than or similar to 0.15 mum) dust particles. Rapid (similar to2 hours) evolution of the infrared flux distribution at the level of similar to0.(m)6 in the JHKL bands was detected in the RV Tau star R Sct. C1 Russian Acad Sci Pulkovo, Cent Astron Observ, St Petersburg 196140, Russia. Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg, Russia. Univ Keele, Astrophys Grp, Sch Chem & Phys, Keele ST5 5BG, Staffs, England. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Joint Astron Ctr, Hilo, HI 96720 USA. RP Yudin, RV (reprint author), Russian Acad Sci Pulkovo, Cent Astron Observ, St Petersburg 196140, Russia. NR 80 TC 5 Z9 5 U1 0 U2 1 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2003 VL 412 IS 2 BP 405 EP + DI 10.1051/0004-6361:20031271 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 748WR UT WOS:000186884400018 ER PT J AU Revnivtsev, M Gilfanov, M Sunyaev, R Jahoda, K Markwardt, C AF Revnivtsev, M Gilfanov, M Sunyaev, R Jahoda, K Markwardt, C TI The spectrum of the cosmic X-ray background observed by RTXE/PCA SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology : observations; diffuse radiation; X-rays : general ID POWER SPECTRUM; ASCA; ROSAT; FLUCTUATIONS; INTENSITY; MISSION; ORIGIN; SKY AB We have analyzed a large set of RXTE/PCA scanning and slewing observations performed between April 1996 and March 1999. We obtained the 3-20 keV spectrum of the cosmic X-ray background (CXB) by subtracting Earth-occulted observations from observations of the X-ray sky at high galactic latitude and far away from sources. The sky coverage is approximately similar to22.6 x 10(3) deg(2). The PCA spectrum of CXB in 3-20 keV energy band is adequately approximated by a single power law with photon index Gamma similar to 1.4 and normalization at 1 keV similar to 9.5 phot/s/cm(2)/keV/sr. Instrumental background uncertainty precludes accurate RXTE/PCA measurements of the spectrum of cosmic X-ray background at energies above 15 keV and therefore we cannot detect the high energy cutoff observed by the HEAO-1 A2 experiment. Deep observations of the 6 high latitude points used to model the PCA background provide a coarse measure of the spatial variation of the CXB. The CXB variations are consistent with a fixed spectral shape and variable normalization characterized by a fractional rms amplitude of similar to7% on angular scales of similar to1 square deg. C1 Max Planck Inst Astrophys, D-85740 Garching, Germany. Russian Acad Sci, Space Res Inst, Moscow 117810, Russia. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Revnivtsev, M (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85740 Garching, Germany. RI Jahoda, Keith/D-5616-2012 NR 39 TC 71 Z9 71 U1 0 U2 1 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2003 VL 411 IS 3 BP 329 EP 334 DI 10.1051/0004-6361:20031386 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 743KQ UT WOS:000186571300009 ER PT J AU Mukherjee, P Banday, AJ Riazuelo, A Gorski, KM Ratra, B AF Mukherjee, P Banday, AJ Riazuelo, A Gorski, KM Ratra, B TI COBE DMR-normalized dark energy cosmogony SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmology : observations; large-scale structure of universe ID PROBE WMAP OBSERVATIONS; VARIABLE COSMOLOGICAL CONSTANT; BACKGROUND ANISOTROPY DATA; EQUATION-OF-STATE; POWER SPECTRUM; SKY MAPS; PARAMETER-ESTIMATION; REDSHIFT DATA; ANGULAR SIZE; CONSTRAINTS AB Likelihood analyses of the COBE Differential Microwave Radiometer (DMR) sky maps are used to determine the normalization of the inverse-power-law potential scalar-field dark energy model. Predictions of the DMR-normalized model are compared with various observations to constrain the allowed range of model parameters. Although the derived constraints are restrictive, evolving dark energy density scalar-field models remains an observationally viable alternative to the constant cosmological constant model. C1 Kansas State Univ, Dept Phys, Manhattan, KS 66506 USA. Max Planck Inst Astrophys, D-85741 Garching, Germany. CEA Saclay, CNRS, DSM,SPhT, Serv Phys Theor,UMR, F-91191 Gif Sur Yvette, France. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Mukherjee, P (reprint author), Univ Oklahoma, Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA. RI Ratra, Bharat/I-4979-2012 NR 87 TC 12 Z9 12 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2003 VL 598 IS 2 BP 767 EP 778 DI 10.1086/378951 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 752FL UT WOS:000187149300005 ER PT J AU Zhang, TJ Pen, UL Zhang, PJ Dubinski, J AF Zhang, TJ Pen, UL Zhang, PJ Dubinski, J TI Optimal weak-lensing skewness measurements SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; cosmology : theory; dark matter; gravitational lensing; large-scale structure of universe ID LARGE-SCALE STRUCTURE; POWER SPECTRUM; COSMIC SHEAR; PERTURBATION-THEORY; STATISTICS; FLUCTUATIONS; ANISOTROPIES; FIELDS; OMEGA; PROBE AB Weak-lensing measurements are starting to provide statistical maps of the distribution of matter in the universe that are increasingly precise and complementary to cosmic microwave background maps. The most common measurement is the correlation in alignments of background galaxies, which can be used to infer the variance of the projected surface density of matter. This measurement of the fluctuations is insensitive to the total mass content and is analogous to using waves on the ocean to measure its depths. However, when the depth is shallow, as happens near a beach, waves become skewed. Similarly, a measurement of skewness in the projected matter distribution directly measures the total matter content of the universe. While skewness has already been convincingly detected, its constraint on cosmology is still weak. We address optimal analyses for the Canada-France-Hawaii Telescope Legacy Survey in the presence of noise. We show that a compensated Gaussian filter with a width of 2.'5 optimizes the cosmological constraint, yielding DeltaOmega(m)/Omega(m) similar to 10%. This is significantly better than other filters that have been considered in the literature. This can be further improved with tomography and other sophisticated analyses. C1 Beijing Normal Univ, Dept Astron, Beijing 100875, Peoples R China. Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. NASA, Fermilab Astrophys Grp, Fermi Natl Accelerator Lab, Batavia, IL 60510 USA. Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. RP Beijing Normal Univ, Dept Astron, Beijing 100875, Peoples R China. EM tjzhang@bnu.edu.cn; pen@cita.utoronto.ca; zhangpj@fnal.gov; dubinski@cita.utoronto.ca RI ZHANG, PENGJIE/O-2825-2015 NR 31 TC 18 Z9 21 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 DEC 1 PY 2003 VL 598 IS 2 BP 818 EP 826 DI 10.1086/379119 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 752FL UT WOS:000187149300009 ER PT J AU Turner, TJ Kraemer, SB AF Turner, TJ Kraemer, SB TI XMM-Newton observation of FeK alpha emission from a broad absorption line quasar: Markarian 231 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (Markarian 231); galaxies : nuclei; galaxies : Seyfert; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; ULTRALUMINOUS INFRARED GALAXIES; STELLAR OBJECTS; ECHELLE SPECTROSCOPY; ASCA OBSERVATIONS; DISK WINDS; CHANDRA; REFLECTION; MATTER; MODELS AB We present results from a 20 ks XMM-Newton observation of Mrk 231. The European Photon Imaging Camera (EPIC) spectral data reveal strong line emission due to Fe Kalpha, which has rarely been detected in this class, as broad absorption line quasars (BAL QSOs) are very faint in the X-ray band. The line energy is consistent with an origin in neutral Fe. The width of the line is equivalent to a velocity dispersion similar to18,000 km s(-1), and thus the line may be attributed to transmission and/or reflection from a distribution of emitting clouds. If, instead, the line originates in the accretion disk, then the line strength and. at X-ray continuum support some contribution from a reflected component, although the data disfavor a model in which the hard X-ray band is purely reflected X-rays from a disk. The line parameters are similar to those obtained for the Fe Kalpha line detected in another BAL QSO, H1413+117. C1 Univ Maryland Baltimore Cty, Dept Phys, Joint Ctr Astrophys, Baltimore, MD 21250 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Turner, TJ (reprint author), Univ Maryland Baltimore Cty, Dept Phys, Joint Ctr Astrophys, 1000 Hilltop Circle, Baltimore, MD 21250 USA. NR 33 TC 6 Z9 6 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2003 VL 598 IS 2 BP 916 EP 921 DI 10.1086/379100 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 752FL UT WOS:000187149300016 ER PT J AU Schlegel, E Holt, SS Petre, R AF Schlegel, E Holt, SS Petre, R TI A Chandra observation of the diffuse emission in the face-on spiral NGC 6946 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 6946); galaxies : ISM; galaxies : spiral; X-rays : galaxies ID X-RAY-EMISSION; INTERSTELLAR-MEDIUM; SUPERNOVA-REMNANTS; GALAXY NGC-6946; ROSAT HRI; GAS; RADIATION; PLASMAS; IMAGES; M101 AB This paper describes the Chandra observation of the diffuse emission in the face-on spiral NGC 6946. Overlaid on optical and Halpha images, the diffuse emission follows the spiral structure of the galaxy. An overlay on a 6 cm polarized radio intensity map confirms the phase offset of the polarized emission. We then extract and fit the spectrum of the unresolved emission with several spectral models. All model fits show a consistent continuum thermal temperature with a mean value of 0.25 +/- 0..03 keV. Additional degrees of freedom are required to obtain a good fit, and any of several models satisfy that need; one model uses a second continuum component with a temperature of 0.70 +/- 0.10 keV. An abundance measure of 3(-1.90)(+1.95) for Si differs from the solar value at the 90% confidence level; the net diffuse spectrum shows that the line lies above the instrumental Si feature. For Fe the abundance measure of 0.67 +/- 0.13 is significant at 99%. Multiple Gaussians also provide a good fit. Two of the fitted Gaussians capture the O VII and O VIII emission; the fitted emission is consistent with an XMM-Newton RGS spectrum of diffuse gas in M81. The ratio of the two lines is less than 0.6-0.7 and suggests the possibility of nonequilibrium ionization conditions existing in the interstellar medium of NGC 6946. An extrapolation of the point-source luminosity distribution shows that the diffuse component is not the sum of unresolved point sources; their contribution is at most 25%. C1 Harvard Smithsonian Ctr Astrophys, High Energy Astrophys Div, Cambridge, MA 02138 USA. Olin Coll Egn, Needham, MA 02492 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Schlegel, E (reprint author), Harvard Smithsonian Ctr Astrophys, High Energy Astrophys Div, 60 Garden St, Cambridge, MA 02138 USA. NR 40 TC 13 Z9 13 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2003 VL 598 IS 2 BP 982 EP 992 DI 10.1086/378937 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 752FL UT WOS:000187149300021 ER PT J AU Dyks, J Rudak, B AF Dyks, J Rudak, B TI Two-pole caustic model for high-energy light curves of pulsars SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : theory; pulsars : general; stars : neutron ID GAMMA-RAY PULSARS; RAPIDLY SPINNING PULSARS; OUTER GAP ACCELERATOR; BRIGHT EGRET PULSARS; CRAB PULSAR; GEMINGA PULSAR; VELA PULSAR; EMISSION; RADIATION; SPECTRUM AB We present a new model of high-energy light curves from rotation-powered pulsars. The key ingredient of the model is the gap region (i.e., the region where particle acceleration is taking place and high-energy photons originate) that satisfies the following assumptions: (1) the gap region extends from each polar cap to the light cylinder; (2) the gap is thin and confined to the surface of last open magnetic-field lines; (3) photon emissivity is uniform within the gap region. The model light curves are dominated by strong peaks ( either double or single) of caustic origin. Unlike other pulsar models with caustic effects, the double peaks arise from a crossing two caustics, each of which is associated with a different magnetic pole. The generic features of the light curves are consistent with the observed characteristics of pulsar light curves: ( 1) the most natural ( in terms of probability) shape consists of two peaks ( separated by 0.4 to 0.5 in phase for large viewing angles); ( 2) the peaks possess well-developed wings; ( 3) there is a bridge (interpeak) emission component; (4) there is a nonvanishing off-pulse emission level; (5) the radio pulse occurs before the leading high-energy peak. The model is well suited for four gamma-ray pulsars - Crab, Vela, Geminga, and B1951+ 32 - with double-peak light curves exhibiting the peak separation of 0.4 to 0.5 in phase. Here we apply the model to the Vela pulsar. Moreover, we indicate the limitation of the model in accurate reproducing of the light curves with single pulses and narrowly separated ( about 0.2 in phase) pulse peaks. We also discuss the optical polarization properties for the Crab pulsar in the context of the two-pole caustic model. C1 NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Nicolaus Copernicus Astron Ctr, PL-87100 Torun, Poland. RP Dyks, J (reprint author), NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. NR 34 TC 168 Z9 168 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2003 VL 598 IS 2 BP 1201 EP 1206 DI 10.1086/379052 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 752FL UT WOS:000187149300039 ER PT J AU Haghighipour, N Boss, AP AF Haghighipour, N Boss, AP TI On gas drag-induced rapid migration of solids in a nonuniform solar nebula SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems : formation; planetary systems : protoplanetary disks; solar system : formation ID TURBULENT PROTOPLANETARY DISKS; ICY PLANETESIMALS; GLOBAL EVOLUTION; DUST PARTICLES; AERODYNAMICS; MATTER AB We study the motions of small solids, ranging from micron-sized dust grains to meter-sized objects, in the vicinity of local pressure enhancements of a gaseous nebula. Integrating numerically, we show that as a result of the combined effect of gas drag and pressure gradients, solids tend to accumulate at the locations where the pressure of the gas maximizes. The rate of migration of solids varies with their sizes and densities and also with the physical properties of the gas. The results of our numerical simulations indicate that such migrations are most rapid for meter-sized objects. The applicability of the results to the enhancement of the collision and coagulation of solids and also to the growth rate of planetesimals is discussed. C1 Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. Carnegie Inst Washington, NASA Astrobiol Inst, Washington, DC 20015 USA. RP Haghighipour, N (reprint author), Carnegie Inst Washington, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. NR 10 TC 58 Z9 58 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2003 VL 598 IS 2 BP 1301 EP 1311 DI 10.1086/378950 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 752FL UT WOS:000187149300049 ER PT J AU Cane, HV AF Cane, HV TI Near-relativistic solar electrons and type III radio bursts SO ASTROPHYSICAL JOURNAL LA English DT Article DE interplanetary medium; Sun : flares; Sun : particle emission ID ADVANCED-COMPOSITION-EXPLORER; WIND SPACECRAFT; ALPHA-MONITOR; EVENTS; PLASMA; PROPAGATION; FREQUENCY; EMISSION; WAVES AB Recently, it has been found that the inferred injection times of >25 keV electrons are up to 30 minutes later than the start times of the associated type III radio bursts at the Sun. Thus, it has been suggested that the electrons that produce type III bursts do not belong to the same population as those observed above 25 keV. This paper examines the characteristics and circumstances of 79 solar electron beam events measured on the Advanced Composition Explorer (ACE) spacecraft. Particular attention is paid to the very low frequency emissions of the associated radio bursts and the ambient conditions at the arrival times of the electrons at the spacecraft. It is found that the inferred >25 keV electron injection delays are correlated with the times required for the associated radio bursts to drift to the lowest frequencies. This suggests that the electrons responsible for the radio emission, and those observed above 25 keV, are part of a single population and that the electrons both above and below 25 keV are delayed in the interplanetary medium. Further evidence for a single population is the general correspondence between electron and local radio intensities and temporal profiles. It is found that the delays increase with the ambient solar wind density, consistent with the propagation times of the electrons being determined by the characteristics of the interplanetary medium. However, it is known that particle arrival times at 1 AU are a linear function of inverse particle speed. Conventionally, such a relationship is taken to indicate scatter-free propagation when inferred path lengths lie close to 1.2 AU, as they do for the electron events studied here. These conflicting interpretations require further investigation. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Tasmania, Sch Math & Phys, Hobart, Tas, Australia. RP Cane, HV (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 16 TC 43 Z9 43 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2003 VL 598 IS 2 BP 1403 EP 1408 DI 10.1086/379007 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 752FL UT WOS:000187149300058 ER PT J AU McKernan, B Yaqoob, T Mushotzky, R George, IM Turner, TJ AF McKernan, B Yaqoob, T Mushotzky, R George, IM Turner, TJ TI A warm/hot intergalactic medium toward 3C 120? SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (3C 120); galaxies : Seyfert; techniques : spectroscopic; X-rays : galaxies ID X-RAY FOREST; ENERGY GRATING SPECTROSCOPY; PHYSICAL CONDITIONS; CHANDRA DETECTION; ALPHA ABSORPTION; IONIZED-GAS; KINEMATICS; GALAXIES; SPECTRA; BARYONS AB We observed the Seyfert I active/broad-line radio galaxy 3C 120 with the Chandra high-energy transmission gratings and present an analysis of the soft X-ray spectrum. We identify the strongest absorption feature (detected at >99.9% confidence) with O VIII Lyalpha (FWHM = 1010(-265)(+295) kms s(-1)), blueshifted by -5500 +/- 140 km s(-1) from systemic velocity. The absorption may be due to missing baryons in a warm/hot intergalactic medium (WHIGM) along the line of sight to 3C 120 at z = 0.0147 +/- 0.0005, or it could be intrinsic to the jet of 3C 120. Assuming metallicities of similar to0.1 Z., we estimate an ionic column density of N-O VIII > 3.4 x 10(16) cm(-2) for the WHIGM and a filament depth of less than 19 h(70)(-1) Mpc. We find a baryon overdensity greater than 56 relative to the critical density of a Lambda-dominated cold dark matter universe, which is in reasonable agreement with WHIGM simulations. We detect, at marginal significance, absorption of O VIII Lyalpha at z similar to 0 due to a hot medium in the Local Group. We also detect an unidentified absorption feature at similar to0.71 keV. Absorption features that might be expected along with O VIII Lyalpha were not significant statistically. Relative abundances of metals in the WHIGM and local absorbers may therefore be considerably different from solar. C1 Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. NASA, High Energy Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Baltimore, MD 21250 USA. RP McKernan, B (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. NR 24 TC 23 Z9 23 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2003 VL 598 IS 2 BP L83 EP L86 DI 10.1086/380775 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 752FM UT WOS:000187149400004 ER PT J AU Runyan, MC Ade, PAR Bhatia, RS Bock, JJ Daub, MD Goldstein, JH Haynes, CV Holzapfel, WL Kuo, CL Lange, AE Leong, J Lueker, M Newcomb, M Peterson, JB Reichardt, C Ruhl, J Sirbi, G Torbet, E Tucker, C Turner, AD Woolsey, D AF Runyan, MC Ade, PAR Bhatia, RS Bock, JJ Daub, MD Goldstein, JH Haynes, CV Holzapfel, WL Kuo, CL Lange, AE Leong, J Lueker, M Newcomb, M Peterson, JB Reichardt, C Ruhl, J Sirbi, G Torbet, E Tucker, C Turner, AD Woolsey, D TI ACBAR: The arcminute cosmology bolometer array receiver SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmic microwave background; galaxies : clusters : general instrumentation : miscellaneous ID MICROWAVE BACKGROUND ANISOTROPY; SPECTRUM RADIO-SOURCES; CORRUGATED FEED HORNS; INTENSITY FLUCTUATIONS; MILLIMETER WAVELENGTHS; SEST OBSERVATIONS; GAUSSIAN LIGHT; SUBMILLIMETER; PHOTOMETER; RADIATION AB We describe the Arcminute Cosmology Bolometer Array Receiver (ACBAR); a multifrequency millimeter-wave receiver designed for observations of the cosmic microwave background and the Sunyaev-Zel'dovich effect in clusters of galaxies. The ACBAR focal plane consists of a 16 pixel, background-limited, 240 mK bolometer array that can be configured to observe simultaneously at 150, 220, 280, and 350 GHz. With 4' - 5' FWHM beams and a 3degrees azimuth chop, ACBAR is sensitive to a wide range of angular scales. ACBAR was installed on the 2 m Viper telescope at the South Pole in 2001 January. We describe the design of the instrument and its performance during the 2001 and 2002 observing seasons. C1 CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. European Space Agcy, NL-2200 AG Noordwijk, Netherlands. CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA. Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. RP Runyan, MC (reprint author), Univ Chicago, Enrico Fermi Inst, LASR-132, Chicago, IL 60637 USA. RI Peterson, Jeffrey/O-4794-2014; Holzapfel, William/I-4836-2015; OI Peterson, Jeffrey/0000-0003-1340-818X; Reichardt, Christian/0000-0003-2226-9169 NR 65 TC 56 Z9 56 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD DEC PY 2003 VL 149 IS 2 BP 265 EP 287 DI 10.1086/379099 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 754DH UT WOS:000187287100001 ER PT J AU Jackson, T Werner, M Gautier, TN AF Jackson, T Werner, M Gautier, TN TI A catalog of bright filamentary structures in the interstellar medium SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; infrared : ISM; ISM : structure; methods : data analysis; techniques : image processing ID GALACTIC DUST EMISSION; POLARIMETRY; CIRRUS; CLOUDS; MAPS AB We present a listing of prominent filamentary structures in the interstellar cirrus, selected with an eye toward current and planned far-infrared and submillimeter polarimetry facilities. The. laments were identified on the 100 mum plates of the IRAS Sky Survey Atlas (ISSA), using a computer vision algorithm that is unbiased with respect to source intensity. Our catalog is two-tiered: the selection criteria in the Galactic plane are based on the sensitivity limits of airborne polarimeters such as the proposed HALE instrument for SOFIA, and away from the plane the limits are dictated by the sensitivities of balloon-borne cosmic microwave background experiments, such as BOOMERanG and MAXIMA. Infrared detector technology is currently at the point where detecting the polarization of the interstellar cirrus is feasible, and we hope this catalog will assist any experimenter undertaking this task. C1 Princeton Univ Observ, Princeton, NJ 08544 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Jackson, T (reprint author), Princeton Univ Observ, Peyton Hall, Princeton, NJ 08544 USA. NR 23 TC 4 Z9 4 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD DEC PY 2003 VL 149 IS 2 BP 365 EP 373 DI 10.1086/378671 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 754DH UT WOS:000187287100006 ER PT J AU Stowe, RP Sams, CF Pierson, DL AF Stowe, RP Sams, CF Pierson, DL TI Effects of mission duration on neuroimmune responses in astronauts SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE spaceflight; microgravity; neuroimmunity; catecholamines; adrenocortical response; glucocorticoids; leucocytes; lymphocytes ID SHORT-TERM SPACEFLIGHT; EPSTEIN-BARR-VIRUS; CELLS IN-VITRO; IMMUNE-RESPONSES; SPACE-FLIGHT; GLUCOCORTICOIDS; REACTIVATION; SUBPOPULATIONS; THERAPY; ENHANCE AB STOWE RP, SAMS CF, PIERSON DL. Effects of mission duration on neuroimmune responses in astronauts, Aviat Space Environ Med 2003; 74:1281-4. Background: Spaceflight poses a unique stress to humans that can impair cellular immune responses and reactivate latent herpes viruses. Notably, prior studies have suggested that mission length may be an important factor in the variability of immune alterations observed after spaceflight. In this study, adrenocortical responses and circulating leukocytes were compared between astronauts who participated in either 9- or 16-d missions. Hypothesis: Mission duration will differentially affect neuroimmune responses after spaceflight. Methods. Blood and urine samples, collected from 28 crew-members who flew on 5 Space Shuttle missions, were analyzed for levels of plasma and urinary cortisol, urinary catecholamines, leukocyte and lymphocyte subsets, and total IgE. Results: After spaceflight, plasma cortisol was significantly decreased after the 9-d missions but increased after the 16-d missions. In contrast, urinary epinephrine and norepinephrine levels were greater after the 9-d missions than the 16-d missions. Total IgE was significantly increased after the 16-d missions and correlated with urinary cortisol. The number of white blood cells, polymorphonuclear leukocytes, and CD4(+) T cells were significantly increased postflight. After the 9-d missions, monocytes were increased while natural killer cells were decreased. However, monocytes were decreased after the 16-d missions; no change occurred in natural killer cells. Conclusions. These results suggest that sympathetic nervous system responses predominate after shorter spaceflights, while longer flights are characterized by glucocorticoid-mediated changes at landing that may result from the accumulative effects of microgravity (i.e., physiological deconditioning) over time. C1 Univ Texas, Med Branch, Dept Pathol, Galveston, TX 77555 USA. NASA, Lyndon B Johnson Space Ctr, Space & Life Sci Directorate, Houston, TX 77058 USA. RP Stowe, RP (reprint author), Univ Texas, Med Branch, Dept Pathol, Galveston, TX 77555 USA. NR 27 TC 49 Z9 55 U1 0 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 DEC PY 2003 VL 74 IS 12 BP 1281 EP 1284 PG 4 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 751XH UT WOS:000187115000011 PM 14692473 ER PT J AU Zelnick, SD Mattie, DR Stepaniak, PC AF Zelnick, SD Mattie, DR Stepaniak, PC TI Occupational exposure to hydrazines: Treatment of acute central nervous system toxicity SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Review DE aviation; hydrazine; treatment ID UREA CYCLE DISORDERS; ISONIAZID OVERDOSE; UDMH INTOXICATION; PYRIDOXINE; MANAGEMENT; THERAPY; INHIBITION; ENZYMES; INVIVO; RAT AB ZELNICK SD, MATTIE DR, STEPANIAK PC. Occupational exposure to hydrazines: treatment of acute central nervous system toxicity. Aviat Space Environ Med 2003; 74:1285-91. Exposure to hydrazine and hydrazines' alkylated derivatives is an important occupational health issue, which will increase in significance as space applications increase. Despite their widespread usage as rocket fuels in manned and unmanned space and missile systems, serious exposures to hydrazines are rare. While a significant number of experimental studies were performed in the late 1950s through the mid-1960s, conflicting information exists concerning the most appropriate treatment for these exposures. A cross-sectional study evaluating the most common rocket fuels such as hydrazine; 1,1-dimethylhydrazine (UDMH); mono-methylhydrazine (MMH); and Aerozine-50 against the most commonly suggested therapies, such as pyridoxine, traditional antiseizure therapies, and arginine is needed to clarify the treatment implications for human exposure. Treatments that have been useful for hyperammonemic states, such as those for the six inherited urea cycle defects, have significant potential for the improvement of hydrazine exposure treatment. C1 US Dept Def, Manned Space Flight Off, Div Med, Patrick AFB, FL USA. USAF, Res Lab, Wright Patterson AFB, OH 45433 USA. NASA, Contingency Med Operat Grp, Space Med & Crew Hlth Syst, Houston, TX USA. RP Zelnick, SD (reprint author), US Dept Def, Manned Space Flight Off, Div Med, 1201 Edward H White II St,MS 7101,Bldg 423,Room S, Patrick AFB, FL USA. NR 47 TC 98 Z9 102 U1 3 U2 15 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 DEC PY 2003 VL 74 IS 12 BP 1285 EP 1291 PG 7 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 751XH UT WOS:000187115000012 PM 14692474 ER PT J AU Truccolo, W Knuth, KH Shah, A Bressler, SL Schroeder, CE Ding, MZ AF Truccolo, W Knuth, KH Shah, A Bressler, SL Schroeder, CE Ding, MZ TI Estimation of single-trial multicomponent ERPs: Differentially variable component analysis (dVCA) SO BIOLOGICAL CYBERNETICS LA English DT Article ID EVENT-RELATED POTENTIALS; VISUAL-SYSTEM; EVOKED-POTENTIALS; VARIABILITY; MACAQUE; SIGNAL AB A Bayesian inference framework for estimating the parameters of single-trial, multicomponent, event-related potentials is presented. Single-trial recordings are modeled as the linear combination of ongoing activity and multicomponent waveforms that are relatively phase-locked to certain sensory or motor events. Each component is assumed to have a trial-invariant waveform with trial-dependent amplitude scaling factors and latency shifts. A Maximum a Posteriori solution of this model is implemented via an iterative algorithm from which the component's waveform, single-trial amplitude scaling factors and latency shifts are estimated. Multiple components can be derived from a single-channel recording based on their differential variability, an aspect in contrast with other component analysis techniques (e.g., independent component analysis) where the number of components estimated is equal to or smaller than the number of recording channels. Furthermore, we show that, by subtracting out the estimated single-trial components from each of the single-trial recordings, one can estimate the ongoing activity, thus providing additional information concerning task-related brain dynamics. We test this approach, which we name differentially variable component analysis (dVCA), on simulated data and apply it to an experimental dataset consisting of intracortically recorded local field potentials from monkeys performing a visuomotor pattern discrimination task. C1 Florida Atlantic Univ, Ctr Complex Syst & Brain Sci, Boca Raton, FL 33431 USA. Brown Univ, Dept Neurosci, Providence, RI 02912 USA. NASA, Ames Res Ctr, Computat Sci Div, Moffett Field, CA 94035 USA. Albert Einstein Coll Med, Dept Neurosci, Bronx, NY 10461 USA. Nathan S Kline Inst Psychiat Res, Cognit Neurosci & Schizophrenia Dept, Orangeburg, NY 10962 USA. RP Ding, MZ (reprint author), Florida Atlantic Univ, Ctr Complex Syst & Brain Sci, 777 Glades Rd, Boca Raton, FL 33431 USA. EM ding@fau.edu FU NIMH NIH HHS [MH 62404, MH 42900]; PHS HHS [T32 M 07288] NR 28 TC 56 Z9 58 U1 0 U2 1 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0340-1200 J9 BIOL CYBERN JI Biol. Cybern. PD DEC PY 2003 VL 89 IS 6 BP 426 EP 438 DI 10.1007/s00422-003-0433-7 PG 13 WC Computer Science, Cybernetics; Neurosciences SC Computer Science; Neurosciences & Neurology GA 766FJ UT WOS:000188355800003 PM 14673654 ER PT J AU Koren, I Joseph, JH Israelevich, P AF Koren, I Joseph, JH Israelevich, P TI Detection of dust plumes and their sources in northeastern Libya SO CANADIAN JOURNAL OF REMOTE SENSING LA English DT Article ID METEOSAT AB The common source area of long and narrow dust plumes that emanate frequently from an area southeast of Benghazi in Libya is identified by computerized image analysis. Four examples are shown in SeaWiFS data at that location. Similar plumes are found in many locations over the globe. The direction of propagation of plumes from the source depends on the synoptic situation. Plumes travel both northwards, reaching the Mediterranean Sea, and southwards, to the interior of the Sahara. Such plumes may ultimately assemble into massive dust palls that frequently travel long distances out of North Africa. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. CNR, Washington, DC 20001 USA. Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel. RP Koren, I (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM ilank@climate.gsfc.nasa.gov RI Koren, Ilan/K-1417-2012 OI Koren, Ilan/0000-0001-6759-6265 NR 11 TC 10 Z9 10 U1 0 U2 1 PU CANADIAN AERONAUTICS SPACE INST PI OTTAWA PA 1685 RUSSELL RD, UNIT 1-R, OTTAWA, ON K1G 0N1, CANADA SN 0703-8992 J9 CAN J REMOTE SENS JI Can. J. Remote Sens. PD DEC PY 2003 VL 29 IS 6 BP 792 EP 796 PG 5 WC Remote Sensing SC Remote Sensing GA 763MB UT WOS:000188088800014 ER PT J AU Paillou, P Rosenqvist, A Malezieux, JM Reynard, B Farr, T Heggy, E AF Paillou, P Rosenqvist, A Malezieux, JM Reynard, B Farr, T Heggy, E TI Discovery of a double impact crater in Libya: the astrobleme of Arkenu SO COMPTES RENDUS GEOSCIENCE LA English DT Article DE impact; crater; Libya; radar; Arkenu ID EASTERN SAHARA; RADAR; CHAD; AOROUNGA; ORIGIN; QUARTZ AB Using orbital imaging radar, we detected a double circular structure, located in the southeastern part of the Libyan Desert, which is partially hidden under sandy sediments. Fieldwork confirmed it to be an unknown double impact crater, each crater having a diameter of about 10 km, younger than 140 Ma. Sampling on the site enabled the observation of quantities of shatter cone structures and impact breccias containing planar fractures. (C) 2003 Academie des sciences. Published by Elsevier SAS. All rights reserved. C1 Observ Aquitain Sci Univers, UMR 5804, F-33270 Floirac, France. Earth Observat Res Ctr, NASDA, Tokyo, Japan. Univ Bordeaux 3, Inst EGID, Bordeaux, France. ENS, UMR 5570, Lab Sci Terre, Lyon, France. CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. Cairo Univ, Dept Astron, Giza, Egypt. RP Paillou, P (reprint author), Observ Aquitain Sci Univers, UMR 5804, 2 Rue Observ,BP 89, F-33270 Floirac, France. EM paillou@obs.u-bordeaux1.fr RI Heggy, Essam/E-8250-2013; Reynard, Bruno/C-8301-2012 OI Heggy, Essam/0000-0001-7476-2735; Reynard, Bruno/0000-0002-4782-6163 NR 26 TC 26 Z9 26 U1 0 U2 2 PU ELSEVIER FRANCE-EDITIONS SCIENTIFIQUES MEDICALES ELSEVIER PI PARIS PA 23 RUE LINOIS, 75724 PARIS, FRANCE SN 1631-0713 J9 CR GEOSCI JI C. R. Geosci. PD DEC PY 2003 VL 335 IS 15 BP 1059 EP 1069 DI 10.1016/j.crte.2003.09.008 PG 11 WC Geosciences, Multidisciplinary SC Geology GA 767UH UT WOS:000188470700003 ER PT J AU Cao, YZ Hussaini, MY Zang, TA AF Cao, YZ Hussaini, MY Zang, TA TI An efficient Monte Carlo method for optimal control problems with uncertainty SO COMPUTATIONAL OPTIMIZATION AND APPLICATIONS LA English DT Article DE Monte Carlo method; optimal control; Burger's equation; uncertainty quantification; sensitivity derivatives ID QUANTIFICATION AB A general framework is proposed for what we call the sensitivity derivative Monte Carlo (SDMC) solution of optimal control problems with a stochastic parameter. This method employs the residual in the first-order Taylor series expansion of the cost functional in terms of the stochastic parameter rather than the cost functional itself. A rigorous estimate is derived for the variance of the residual, and it is verified by numerical experiments involving the generalized steady-state Burgers equation with a stochastic coefficient of viscosity. Specifically, the numerical results show that for a given number of samples, the present method yields an order of magnitude higher accuracy than a conventional Monte Carlo method. In other words, the proposed variance reduction method based on sensitivity derivatives is shown to accelerate convergence of the Monte Carlo method. As the sensitivity derivatives are computed only at the mean values of the relevant parameters, the related extra cost of the proposed method is a fraction of the total time of the Monte Carlo method. C1 Florida A&M Univ, Dept Math, Tallahassee, FL 32307 USA. Florida State Univ, Sch Computat Sci & Informat Technol, Tallahassee, FL 32306 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Cao, YZ (reprint author), Florida A&M Univ, Dept Math, Tallahassee, FL 32307 USA. NR 14 TC 15 Z9 15 U1 0 U2 6 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0926-6003 J9 COMPUT OPTIM APPL JI Comput. Optim. Appl. PD DEC PY 2003 VL 26 IS 3 BP 219 EP 230 DI 10.1023/A:1026079021836 PG 12 WC Operations Research & Management Science; Mathematics, Applied SC Operations Research & Management Science; Mathematics GA 727MJ UT WOS:000185662300001 ER PT J AU Shebalin, JV AF Shebalin, JV TI A spectral algorithm for solving the relativistic Vlasov-Maxwell equations SO COMPUTER PHYSICS COMMUNICATIONS LA English DT Article DE spectral methods; relativistic plasma; Vlasov-Maxwell; kinetic theory ID PLASMA OSCILLATIONS; POISSON EQUATION; PHASE-SPACE AB A spectral method algorithm is developed for the numerical solution of the full six-dimensional Vlasov-Maxwell system of equations. Here, the focus is on the electron distribution function, with positive ions providing a constant background. The algorithm consists of a Jacobi polynomial-spherical harmonic formulation in velocity space and a trigonometric formulation in position space. A transform procedure is used to evaluate nonlinear terms. The algorithm is suitable for performing moderate resolution simulations on currently available supercomputers for both scientific and engineering applications. (C) 2003 Elsevier B.V. All rights reserved. C1 NASA, Lyndon B Johnson Space Ctr, Adv Space Prop Lab, Houston, TX 77058 USA. RP Shebalin, JV (reprint author), NASA, Lyndon B Johnson Space Ctr, Adv Space Prop Lab, Houston, TX 77058 USA. NR 25 TC 2 Z9 2 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0010-4655 J9 COMPUT PHYS COMMUN JI Comput. Phys. Commun. PD DEC 1 PY 2003 VL 156 IS 1 BP 86 EP 94 DI 10.1016/S0010-4655(03)00438-7 PG 9 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA 750MW UT WOS:000187001200007 ER PT J AU De Chant, LJ Seidel, JA Kline, TR AF De Chant, LJ Seidel, JA Kline, TR TI Extension of a combined analytical/numerical initial value problem solver for turbulent mixing with combustion SO COMPUTERS & FLUIDS LA English DT Article DE elementary combustion model; combined analytical/numerical method; aerodynamic mixing; ejector nozzle; preliminary design ID PERFORMANCE AB Here, we describe the development of a reacting flow multi-species/combustion methodology, implemented as an extension to the differential reduced ejector analysis (DREA) computer program [Mathematical and computer modeling, vol. 31, 2000, p. 21; Appl. Math. Model. 25 (2001) 427; Comput. Math. Appl. 43(10-11); NASA Contractor Report, 1998]. Use of the single fluid IVP solver framework that was developed for the original DREA model has been directly coupled into the combustion formulation. With these modifications, the analysis has an elementary single step reaction Fuel + Oxidizer --> Product combustion capability. Though approximate in nature, the simplicity and efficiency of the DREA formulation make it suitable for its original niche, namely design and preliminary design environments where more complex and expensive models may be inappropriate. (C) 2003 Elsevier Science Ltd. All rights reserved. C1 Analyt Entrainmenmt LLC, Albuquerque, NM 87112 USA. NASA, Glenn Res Ctr, Prop Syst Anal Off, Cleveland, OH 44135 USA. RP De Chant, LJ (reprint author), Analyt Entrainmenmt LLC, 1541 Summit Hills Dr, Albuquerque, NM 87112 USA. NR 24 TC 1 Z9 1 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0045-7930 J9 COMPUT FLUIDS JI Comput. Fluids PD DEC PY 2003 VL 32 IS 10 BP 1435 EP 1452 DI 10.1016/S0045-7930(03)0003-3 PG 18 WC Computer Science, Interdisciplinary Applications; Mechanics SC Computer Science; Mechanics GA 693WK UT WOS:000183741200005 ER PT J AU Ricketts, T Imhoff, M AF Ricketts, T Imhoff, M TI Biodiversity, urban areas, and agriculture: Locating priority ecoregions for conservation SO CONSERVATION ECOLOGY LA English DT Article ID UNITED-STATES; BIOLOGICAL DIVERSITY; CITY LIGHTS; INDICATOR; HOTSPOTS; URBANIZATION; ECOSYSTEMS; SATELLITE; GRADIENT; THREATS AB Urbanization and agriculture are two of the most important threats to biodiversity worldwide. The intensities of these land-use phenomena, however, as well as levels of biodiversity itself, differ widely among regions. Thus, there is a need to develop a quick but rigorous method of identifying where high levels of human threats and biodiversity coincide. These areas are clear priorities for biodiversity conservation. In this study, we combine distribution data for eight major plant and animal taxa (comprising over 20,000 species) with remotely sensed measures of urban and agricultural land use to assess conservation priorities among 76 terrestrial ecoregions in North America. We combine the species data into overall indices of richness and endemism. We then plot each of these indices against the percent cover of urban and agricultural land in each ecoregion, resulting in four separate comparisons. For each comparison, ecoregions that fall above the 66th quantile on both axes are identified as priorities for conservation. These analyses yield four "priority sets" of 6-16 ecoregions (8-21% of the total number) where high levels of biodiversity and human land use coincide. These ecoregions tend to be concentrated in the southeastern United States, California, and, to a lesser extent, the Atlantic coast, southern Texas, and the U.S. Midwest. Importantly, several ecoregions are members of more than one priority set and two ecoregions are members of all four sets. Across all 76 ecoregions, urban cover is positively correlated with both species richness and endemism. Conservation efforts in densely populated areas therefore may be equally important (if not more so) as preserving remote parks in relatively pristine regions. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 45 TC 64 Z9 67 U1 4 U2 52 PU RESILIENCE ALLIANCE PI WOLFVILLE PA ACADIA UNIV, BIOLOGY DEPT, WOLFVILLE, NS B0P 1X0, CANADA SN 1195-5449 J9 CONSERV ECOL JI Conserv. Ecol. PD DEC PY 2003 VL 8 IS 2 AR 1 PG 15 WC Ecology SC Environmental Sciences & Ecology GA 900FG UT WOS:000227200200001 ER PT J AU Behrenfeld, MJ Boss, E AF Behrenfeld, MJ Boss, E TI The beam attenuation to chlorophyll ratio: an optical index of phytoplankton physiology in the surface ocean? SO DEEP-SEA RESEARCH PART I-OCEANOGRAPHIC RESEARCH PAPERS LA English DT Article DE beam attenuation; phytoplankton; photosynthesis ID ATLANTIC TIME-SERIES; PARTICULATE ORGANIC-CARBON; EQUATORIAL PACIFIC; LIGHT-SCATTERING; PHAEODACTYLUM-TRICORNUTUM; SEASONAL VARIABILITY; SARGASSO SEA; PHOTOSYNTHESIS; BACKSCATTERING; MICROORGANISMS AB The particulate beam attenuation coefficient (c(p)) is proportional to the concentration of suspended particles in a size domain overlapping that of the phytoplankton assemblage. c(p) is largely insensitive to changes in intracellular chlorophyll concentration, which varies with growth irradiance (a process termed 'photoacclimation'). Earlier studies have shown that the ratio of c(p):chlorophyll (i.e., c(p)*) exhibits depth-dependent changes that are consistent with photoacclimation. Similar relationships may likewise be expected in the horizontal and temporal dimensions, reflecting changes in mixing depth, incident irradiance, and light attenuation. A link between c(p)* and more robust photoadaptive variables has never been explicitly tested in the field. Here we use five historical field data sets to directly compare spatial and temporal variability in c(p)* with two independent indices of photoacclimation: the light-saturated, chlorophyll-normalized photosynthetic rate, p(opt)(b)-saturation index, E-k. For the variety of oceanographic conditions. and the light considered. a first-order correlation emerged between c(p)* and p(opt)(b) or E-k. These simple empirical results suggest that a relationship exists between a bio-optical variable that can potentially be retrieved remotely (c(p)*) and physiological variables crucial for estimating primary productivity in the sea. (C) 2003 Elsevier Ltd. All rights reserved. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maine, Sch Marine Sci, Orono, ME 04469 USA. RP Behrenfeld, MJ (reprint author), NASA, Goddard Space Flight Ctr, Code 971,Bldg 22, Greenbelt, MD 20771 USA. EM mjb@neptune.gsfc.nasa.gov RI Boss, Emmanuel/C-5765-2009 OI Boss, Emmanuel/0000-0002-8334-9595 NR 58 TC 56 Z9 62 U1 2 U2 9 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0967-0637 J9 DEEP-SEA RES PT I JI Deep-Sea Res. Part I-Oceanogr. Res. Pap. PD DEC PY 2003 VL 50 IS 12 BP 1537 EP 1549 DI 10.1016/j.dsr.2003.09.002 PG 13 WC Oceanography SC Oceanography GA 767PD UT WOS:000188458900008 ER PT J AU Hurst, TP Conover, DO AF Hurst, TP Conover, DO TI Seasonal and interannual variation in the allometry of energy allocation.in juvenile striped bass SO ECOLOGY LA English DT Article DE allometry; energy allocation; Hudson River; USA; lipid reserves; Morone saxatilis; seasonality; striped bass; juvenile ID DEPENDENT WINTER MORTALITY; MORONE-SAXATILIS; BODY-SIZE; LIFE-HISTORY; FAT STORAGE; POPULATION; SURVIVAL; SALMON; FISH; TEMPERATURE AB Survival rates during the first winter of life are strongly size dependent and variable in many temperate fish populations. Starvation is often implicated as the cause of size-dependent first-winter mortality, and interannual variation in energy accumulation and the allocation between growth and storage is a likely source of variability. We examined these processes in young-of-the-year Hudson River striped bass Morone saxatilis, which are known to experience size-selective winter mortality and a winter energy deficit. Neutral-lipid and lean-tissue masses were determined for fish of five consecutive year classes collected through the first year of life. Differences in scaling relationships between body length and neutral-lipid and lean-tissue mass were used to infer patterns of resource allocation. Lipid reserves scaled isometrically with body length in summer but increased at a greater rate than did body length in autumn and winter. Lean-tissue allometries were less variable but followed a similar seasonal cycle. Allometric slopes were homogeneous across years, but significant interannual variation in length-specific lipid content and lean-tissue mass in the later half of the growing season indicated variable allocation patterns. During winter, up to 21% of total energy content and 50% of neutral-lipid stores were depleted. The-results indicate that energy allocation patterns result from interactions among season, ontogenetic stage, and body size. The variation in growth, allocation, and severity of the winter energy deficit likely interact to determine first-winter survival. C1 SUNY Stony Brook, Marine Sci Res Ctr, Stony Brook, NY 11794 USA. RP Hurst, TP (reprint author), NOAA, Fisheries Behav Ecol Program, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv,Hatfield Marine Sci Ct, Newport, OR 97365 USA. EM thomas.hurst@noaa.gov RI Hurst, Thomas/N-1401-2013 NR 53 TC 56 Z9 58 U1 1 U2 16 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1707 H ST NW, STE 400, WASHINGTON, DC 20006-3915 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD DEC PY 2003 VL 84 IS 12 BP 3360 EP 3369 DI 10.1890/02-0562 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 762LN UT WOS:000187973500025 ER PT J AU Floss, C Crozaz, G McKay, G Mikouchi, T Killgore, M AF Floss, C Crozaz, G McKay, G Mikouchi, T Killgore, M TI Petrogenesis of angrites SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID ANGRA-DOS-REIS; RARE-EARTH-ELEMENTS; ANTARCTIC ANGRITES; LEWIS CLIFF-86010; SAHARA 99555; METEORITES; PYROXENE; CHONDRULES; OLIVINE; GEOCHEMISTRY AB The recent discovery of two new angrites, Sahara 99555 and D'Orbigny, has revived interest in this small group of achondrites. We measured trace element abundances in the individual minerals of these two angrites and compared them with the three Antarctic angrites, LEW 86010, LEW 87051 and Asuka 881371. Trace element variations in four of these meteorites (LEW 87051, Asuka 881371, Sahara 99555 and D'Orbigny) indicate rapid crystallization under near closed system conditions, consistent with their mineralogical and textural features. All four appear to be closely related and crystallized from very similar magmas. Discrepancies between their bulk REE compositions and melts calculated to be in equilibrium with the major phases may be due in part to kinetic effects of rapid crystallization. Prior crystallization of olivine and/or plagioclase may also account for the elevated parent melt composition of clinopyroxene in some of the angrites, such as Asuka 881371. LEW 86010 also crystallized from a melt and represents a liquid composition, but trace element trends in clinopyroxene and olivine differ from those of the other angrites. This meteorite seems to have crystallized from a different source magma. Copyright (C) 2003 Elsevier Ltd. C1 Washington Univ, Space Sci Lab, St Louis, MO 63130 USA. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Univ Tokyo, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan. SW Meteorite Lab, Payson, AZ 85547 USA. RP Floss, C (reprint author), Washington Univ, Space Sci Lab, St Louis, MO 63130 USA. NR 57 TC 25 Z9 25 U1 2 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD DEC PY 2003 VL 67 IS 24 BP 4775 EP 4789 DI 10.1016/S0016-7037(03)00310-7 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 754NQ UT WOS:000187323600009 ER PT J AU Flynn, GJ Keller, LP Feser, M Wirick, S Jacobsen, C AF Flynn, GJ Keller, LP Feser, M Wirick, S Jacobsen, C TI The origin of organic matter in the solar system: Evidence from the interplanetary dust particles SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID COMET HALLEY; SPECTROSCOPY; METEORITE; MICROMETEORITES; IDENTIFICATION; STRATOSPHERE; CONSTRAINTS; ABSORPTION; MOLECULES; DISCOVERY AB The detailed examination of meteorites and interplanetary dust particles provides an opportunity to infer the origin of the organic matter found in primitive Solar System materials. If this organic matter were produced by aqueous alteration of elemental (graphitic or amorphous) carbon on an asteroid, then we would expect to see the organic matter occurring preferentially in interplanetary materials that exhibit evidence of aqueous activity, such as the presence of hydrated silicates. On the other hand, if the organic matter were produced either during the nebula phase of Solar System evolution or in the interstellar medium, we might expect this organic matter to be incorporated into the dust as it formed. In that case pre-biotic organic matter would be present in both the anhydrous and the hydrated interplanetary materials. We have performed carbon X-ray absorption near-edge structure spectroscopy and infrared spectroscopy on primitive anhydrous and hydrated interplanetary dust particles (IDPs) collected by NASA from the Earth's stratosphere. We find that organic matter is present in similar types and abundances in both the anhydrous and the hydrated IDPs, and, in the anhydrous IDPs some of this organic matter is the "glue" that holds grains together. These measurements provide the first direct, experimental evidence from the comparison of extraterrestrial samples that the bulk of the pre-biotic organic matter occurs in similar types and abundances in both hydrated and anhydrous samples. This indicates that the bulk of the pre-biotic organic matter in the Solar System did not form by aqueous processing, but, instead, had already formed at the time that primitive, anhydrous dust was being assembled. Thus, the bulk of the pre-biotic organic matter in the Solar System was formed by non-aqueous processing, occurring in either the Solar nebula or in an interstellar environment. Aqueous processing on asteroids may have altered this pre-existing organic matter, but such processing did not affect in any substantial way the C=O content of the organic matter, the aliphatic C-H abundance, or the mean aliphatic chain length. Copyright (C) 2003 Elsevier Ltd. C1 SUNY Coll Plattsburgh, Dept Phys, Plattsburgh, NY 12901 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. SUNY Stony Brook, Dept Phys, Stony Brook, NY 11794 USA. RP Flynn, GJ (reprint author), SUNY Coll Plattsburgh, Dept Phys, Plattsburgh, NY 12901 USA. EM george.flynn@plattsburgh.edu RI Jacobsen, Chris/E-2827-2015 OI Jacobsen, Chris/0000-0001-8562-0353 NR 47 TC 115 Z9 115 U1 0 U2 20 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 DEC PY 2003 VL 67 IS 24 BP 4791 EP 4806 DI 10.1016/j.gca.2003.09.001 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 754NQ UT WOS:000187323600010 ER PT J AU Wadhwa, M Shukolyukov, A Davis, AM Lugmair, GW Mittlefehldt, DW AF Wadhwa, M Shukolyukov, A Davis, AM Lugmair, GW Mittlefehldt, DW TI Differentiation history of the mesosiderite parent body: Constraints from trace elements and manganese-chromium isotope systematics in Vaca Muerta silicate clasts SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID EARLY SOLAR-SYSTEM; HF-W CHRONOMETRY; PLANET FORMATION; CORE FORMATION; METEORITES; PETROGENESIS; DIOGENITES; EUCRITES; CHEMISTRY; PETROLOGY AB We report here the results of a study of trace element microdistributions and Mn-53-Cr-53 systematics in several basaltic and orthopyroxenitic clasts from the Vaca Muerta mesosiderite. Ion microprobe analyses of selected trace and minor element abundances in minerals of the silicate clasts indicate that, following igneous crystallization, these clasts underwent extensive metamorphic equilibration that resulted in intra- and inter-grain redistribution of elements. There is also evidence in the elemental microdistributions that these clasts were subsequently affected to varying degrees by alteration resulting from redox reactions involving the indigenous silicates and externally derived reducing agents (such as phosphorus, derived from the mesosiderite metal) at the time of metal-silicate mixing. Furthermore, our results suggest that the varying degrees of alteration by redox reactions recorded in the different clasts were most likely facilitated by different degrees of remelting induced by heating during the metal-silicate mixing event. After taking into account the effects of these postmagmatic secondary processes, comparison of the trace and minor element concentrations and distributions in minerals of basaltic and orthopyroxenitic clasts with those of noncumulate eucrites and diogenites, respectively, suggests that the primary igneous petrogenesis, including parent magma and source compositions, of Vaca Muerta silicates were similar to those of achondritic meteorites of the Howardite-Eucrite-Diogenite (HED) association. Internal Mn-53-Cr-53 isochrons obtained for two basaltic (pebble 16 and 4679) and two orthopyroxenitic (4659 and 4670) clasts show that chromium isotopes are equilibrated within each clast. Nevertheless, just as for noncumulate eucrites and diogenites, Cr-53 excesses in whole-rock samples of the basaltic clasts (similar to1.01 epsilon in pebble 16; similar to1.07 epsilon in 4679) are significantly higher than in the orthopyroxene-rich clasts (similar to0.62 epsilon in 4659; similar to0.53 epsilon in 4670). As in the case of the HED parent body, this suggests that Mn/Cr fractionation in the parent body of the Vaca Muerta silicate clasts occurred very early in the history of the solar system, when Mn-53 was still extant. However, the slope of the Mn-53-Cr-53 isochron 3 155 defined by the whole-rock samples of Vaca Muerta clasts (corresponding to a Mn-53/Mn-55 ratio of 3.3 +/- 0.6 X 10(-6)) is distinctly lower than that defined by the HED whole-rock samples (corresponding to a Mn-53/Mn-55 ratio of 4.7 +/- 0.5 X 10(-6)), indicating that the global Mn/Cr fractionation event that established mantle source reservoirs on the parent body of the Vaca Muerta silicate clasts occurred similar to2 Ma after a similar event on the HED parent body. Copyright (C) 2003 Elsevier Ltd. C1 Field Museum Nat Hist, Dept Geol, Chicago, IL 60605 USA. Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. Max Planck Inst Chem, D-55020 Mainz, Germany. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Wadhwa, M (reprint author), Field Museum Nat Hist, Dept Geol, 1400 S Lake Shore Dr, Chicago, IL 60605 USA. OI Davis, Andrew/0000-0001-7955-6236 NR 61 TC 23 Z9 24 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD DEC PY 2003 VL 67 IS 24 BP 5047 EP 5069 DI 10.1016/j.gca.2003.08.005 PG 23 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 754NQ UT WOS:000187323600024 ER PT J AU Connell, JW Smith, JG Criss, JM AF Connell, JW Smith, JG Criss, JM TI High temperature transfer molding resins: Laminate properties of PETI-298 and PETT-330 SO HIGH PERFORMANCE POLYMERS LA English DT Article; Proceedings Paper CT 23rd High Temple Workshop CY FEB 10-13, 2003 CL JACKSONVILLE, FLORIDA DE resin transfer molding (RTM); high temperature polymers; polyimides; PETI-330; PETI-298; high temperature laminates ID PHENYLETHYNYL; COMPOSITES; DIANHYDRIDE; POLYIMIDES AB Two phenylethynyl terminated oligomers designated PETI-298 and PETI-330 were developed at the NASA Langley Research Center and have emerged as leading candidates for composite applications requiring high temperature performance (i.e. greater than or equal to 288 degreesC for 1000 hours) combined with the ability to be readily processed into composites without the use of an autoclave or complex or lengthy cure or post-cure cycles. These high performance/high temperature composites are potentially useful on advanced aerospace vehicles in structural applications and as aircraft engine components such as inlet frames and compressor vanes. The number designation (i.e. 298, 330) refers to the glass transition temperature in degrees Centigrade as determined on neat resin cured for I hour at 371 degreesC. The resins are processable by non-autoclave techniques such as resin transfer molding (RTM), vacuum assisted RTM (VARTM) and resin infusion (RI). Both resins exhibit low complex melt viscosities (0.1-10 poise) at 280 degreesC and are stable for greater than or equal to 2 hours at this temperature. Typically, the resins are melted, de-gassed and infused or injected at 280 degreesC and subsequently cured at 371 degreesC for 1-2 hours. Virtually no volatiles are evolved during the cure process. The resin synthesis is straightforward and has been scaled-up to 25 kg batches. The chemistry of PETI-298 and PETI-330 and the RTM AS-4 and T-650 carbon fabric laminate properties, and those of BMI-5270 for comparison, are presented. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. M&P Technol Inc, Marietta, GA 30067 USA. RP Connell, JW (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM j.w.connell@nasa.gov NR 25 TC 42 Z9 55 U1 5 U2 22 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 DEC PY 2003 VL 15 IS 4 BP 375 EP 394 DI 10.1177/09540083030154001 PG 20 WC Polymer Science SC Polymer Science GA 763PX UT WOS:000188096200002 ER PT J AU Allred, RE Wesson, SP Shin, EE Inghram, L McCorkle, L Papadopoulos, D Wheeler, D Sutter, JK AF Allred, RE Wesson, SP Shin, EE Inghram, L McCorkle, L Papadopoulos, D Wheeler, D Sutter, JK TI The influence of sizings on the durability of high-temperature polymer composites SO HIGH PERFORMANCE POLYMERS LA English DT Article; Proceedings Paper CT 23rd High Temple Workshop CY FEB 10-13, 2003 CL JACKSONVILLE, FL DE sizing; desizing; carbon fibers; reactive finish; thermal aging; mechanical properties; wetting; surface energy; blistering; interface AB To increase performance and durability of high-temperature composites for potential rocket engine components, it is necessary to optimize wetting and interfacial bonding between high-modulus carbon fibers and high-temperature polyimide resins. Sizings commercially supplied on most carbon fibers are not compatible with polyimides. In this study, the chemistry of sizings on two high-modulus carbon fibers (M40J and M60J, Toray) was characterized as was the chemistry of PMR-11-50 fluorinated polyimide resin. The carbon fibers were characterized using single filament wetting, scanning electron microscopy, Fourier transform infrared spectroscopy, and X-ray photoelectron spectroscopic measurements. The polyimide matrix resins were coated onto glass filaments for characterization by wetting measurements. Surface energy components were obtained by wetting with nondispersive (methylene iodide), acidic (ethylene glycol), and basic (formamide) probes. A continuous desizing system that uses an environmentally friendly chemical-mechanical process was developed for tow level fiber. Composites were fabricated with fibers containing the manufacturer's sizing, desized, and further treated with a reactive finish. Results of room temperature tests after thermal aging show that the reactive finish produces a higher strength and more durable interface compared to the manufacturer's sizing. When exposed to moisture blistering tests, however, the better-bonded composite displayed a tendency to delaminate, presumably due to trapping of volatiles. C1 Adherent Technol Inc, Albuquerque, NM USA. Ohio Aerosp Inst, Cleveland, OH USA. Univ Akron, Akron, OH 44325 USA. NASA, Glenn Res Ctr, Cleveland, OH USA. RP Allred, RE (reprint author), Adherent Technol Inc, Albuquerque, NM USA. NR 9 TC 2 Z9 9 U1 6 U2 18 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 DEC PY 2003 VL 15 IS 4 BP 395 EP 419 PG 25 WC Polymer Science SC Polymer Science GA 763PX UT WOS:000188096200003 ER PT J AU Sutter, JK Miyoshi, K Bowman, C Naik, SK Ma, K Sinatra, R Cupp, R Horan, R Leissler, G AF Sutter, JK Miyoshi, K Bowman, C Naik, SK Ma, K Sinatra, R Cupp, R Horan, R Leissler, G TI Erosion coatings for Polymer Matrix Composites in propulsion applications SO HIGH PERFORMANCE POLYMERS LA English DT Article; Proceedings Paper CT 23rd High Temple Workshop CY FEB 10-13, 2003 CL JACKSONVILLE, FLORIDA DE coatings; composite materials; aerospace/aircraft AB Polymer Matrix Composites (PMCs) offer lightweight and frequently low cost alternatives to other materials in many applications. High temperature PMCs are currently used in limited propulsion applications replacing metals. Yet in most cases, PMC propulsion applications are not in the direct engine flow path since particulate erosion degrades PMC component performance and therefore restricts their use in gas turbine engines. This paper compares two erosion resistant coatings (SANRES and SANPRES) on PMCs that are useful for both low and high temperature propulsion applications. Collaborating over a multi-year period, researchers at NASA Glenn Research Center, AADC, and Rolls-Royce Engines have optimized these coatings in terms of adhesion, surface roughness and erosion resistance. Results are described for vigorous hot gas/particulate erosion rig and engine testing of uncoated and coated PMC fan bypass vanes from the A-E 3007 regional jet gas turbine engine. Moreover, the structural durability of these coatings is described in long-term high cycle fatigue tests. Overall, both coatings performed well in all tests and will be considered for applications in both commercial and defense propulsion applications. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. Roll Royce Corp, Indianapolis, IN 46206 USA. AADC, Indianapolis, IN 46206 USA. QSS Corp, Cleveland, OH 44135 USA. RP Sutter, JK (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM james.k.sutter@nasa.gov NR 10 TC 13 Z9 13 U1 0 U2 12 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 DEC PY 2003 VL 15 IS 4 BP 421 EP 440 DI 10.1177/09540083030154003 PG 20 WC Polymer Science SC Polymer Science GA 763PX UT WOS:000188096200004 ER PT J AU Ndalama, T Vasquez, DL Hirschfeld, DA Sutter, JK AF Ndalama, T Vasquez, DL Hirschfeld, DA Sutter, JK TI Surface modification of polyimide composites by RF plasma and UV/ozone treatments SO HIGH PERFORMANCE POLYMERS LA English DT Article; Proceedings Paper CT 23rd High Temple Workshop CY FEB 10-13, 2003 CL JACKSONVILLE, FLORIDA DE polyimide; composite; surface; RF plasma; UV/ozone; chemical vapor deposition; silica; etching ID DEPOSITION; TEOS AB Graphite-reinforced polyimide composites are being considered for advanced turbine engine applications, which require that the composite be coated with a wear- and oxidation-resistant coating. For this study, the surface properties of PMR-15 and PMR-II-50 composites were examined and modification techniques investigated to improve coating adhesion. RF plasma and UV/ozone treatments were used to modify the surface chemistry of the polyimide composites, and were optimized to increase the surface energy of the polyimide composites, by etching and deposition of SiOx films. Chemical and physical changes of the composite surface were characterized by contact angle analysis and Fourier transform infrared-attenuated total reflectance spectroscopy (FTIR-ATR). Both RF plasma and UV/ozone treatments effectively removed surface contaminants and modified surface chemistry as indicated by increased surface energy. PMR-II-50 and PMR-15 composites responded differently to argon plasma etching and UV/ozone etching because of their structures. Films deposited by plasma-enhanced chemical vapor deposition (PECVD), using tetramethoxysilane, were stoichiometrically closer to SiO2 than the films deposited by PECVD using tetraethoxysilane. C1 New Mexico Inst Min & Technol, Socorro, NM USA. NASA, Glenn Res Ctr, Cleveland, OH USA. RP Hirschfeld, DA (reprint author), New Mexico Inst Min & Technol, Socorro, NM USA. EM hirsch@nmt.edu NR 12 TC 7 Z9 7 U1 2 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 DEC PY 2003 VL 15 IS 4 BP 441 EP 458 DI 10.1177/09540083030154004 PG 18 WC Polymer Science SC Polymer Science GA 763PX UT WOS:000188096200005 ER PT J AU Chuang, KC Bowman, CL Tsotsis, TK Arendt, CP AF Chuang, KC Bowman, CL Tsotsis, TK Arendt, CP TI 6F-Polyhimides with phenylethynyl endcap for 315-370 C-circle applications SO HIGH PERFORMANCE POLYMERS LA English DT Article; Proceedings Paper CT 23rd High Temple Workshop CY FEB 10-13, 2003 CL JACKSONVILLE, FLORIDA DE Polyimides; phenylethynyl endcap; resin infusion; thermal cycling; rapid heating ID COMPOSITES; POLYIMIDES AB 6F-Polyimides with a phenylethynyl endcap (HFPE) were fabricated into carbon fiber composites using the standard polymerization of monomer reactant (PMR) approach via the ester/acid route. T650-35/HFPE carbon fiber composites were evaluated against the corresponding T650-35/PMR-II-50 composites with nadic endcap at 315-370 degreesC (600-700 degreesF) for their physical and mechanical properties as well as thermo-oxidative stability In addition, concentrated HFPE monomer solutions were infused into stitched AS4 and T650-35 preforms and their mechanical properties were compared with those of the commercial BMI-5270 composites from cryogenic temperature to 343 degreesC (650 degreesF). The stitched HFPE composites out-performed BMI-5270 composites in terms of property retention at elevated temperature and microcrack resistance during thermal cycling from -54 to 288 degreesC (-65 to 550 degreesF). The stitched composites also showed more resistance toward blistering and delamination than conventional laminate composites during a rapid heating rate simulating launch and re-entry of reusable launch vehicles (RLV). C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. Boeing Phantom Works, Huntington Beach, CA 94647 USA. RP Chuang, KC (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM Kathy.chuang@grc.nasa.gov NR 19 TC 23 Z9 40 U1 0 U2 4 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 DEC PY 2003 VL 15 IS 4 BP 459 EP 472 DI 10.1177/0954008303015004005 PG 14 WC Polymer Science SC Polymer Science GA 763PX UT WOS:000188096200006 ER PT J AU Ivosevic, M Knight, R Kalidindi, SR Palmese, GR Sutter, JK AF Ivosevic, M Knight, R Kalidindi, SR Palmese, GR Sutter, JK TI Erosion/oxidation resistant coatings for high temperature polymer composites SO HIGH PERFORMANCE POLYMERS LA English DT Article; Proceedings Paper CT 23rd High Temple Workshop CY FEB 10-13, 2003 CL JACKSONVILLE, FLORIDA DE thermal spray; HVOF combustion spray; composite coatings; high temperature polymers; thermosetting polyimide AB Thermally sprayed coatings are being studied and developed as methods of enabling lightweight composites to be used more extensively as structural components in propulsion applications in order to reduce costs and improve efficiency through weight reductions. The primary goal of this work is the development of functionally graded material (FGM) polymer/metal matrix composite coatings to provide improved erosion/oxidation resistance to polyimide-based polymer matrix composite (PMC) substrates. The goal is to grade the coating composition from pure polyimide, similar to the PMC substrate matrix on one side, to 100% WC-Co on the other. Both step-wise and continuous gradation of the WC-Co loading in these coatings are being investigated. Details of the processing parameter development are presented, specifically the high velocity oxy-fuel (HVOF) combustion spraying of pure PMR-II matrix material and layers of various composition PMR-II/WC-Co blends onto steel and PMR-15 composite substrates. Results of the HVOF process optimization, microstructural characterization, and analysis will be presented. The sprayed coatings were evaluated using standard metallographic techniques - optical and scanning electron microscopy (SEM). An SEM + electron dispersive spectroscopy (EDS) technique has also been used to confirm retention of the PMR-II component. C1 Drexel Univ, Dept Mat Sci & Engn, Philadelphia, PA 19104 USA. Drexel Univ, Dept Chem Engn, Philadelphia, PA 19104 USA. NASA, Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA. RP Knight, R (reprint author), Drexel Univ, Dept Mat Sci & Engn, 3141 Chestnut St, Philadelphia, PA 19104 USA. EM knightr@coe.drexel.edu RI Kalidindi, Surya/A-1024-2007; OI Kalidindi, Surya/0000-0001-6909-7507 NR 17 TC 11 Z9 11 U1 1 U2 8 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 DEC PY 2003 VL 15 IS 4 BP 503 EP 517 DI 10.1177/09540083030154007 PG 15 WC Polymer Science SC Polymer Science GA 763PX UT WOS:000188096200008 ER PT J AU Prinzel, LJ Freeman, FG Scerbo, MW Mikulka, PJ Pope, AT AF Prinzel, LJ Freeman, FG Scerbo, MW Mikulka, PJ Pope, AT TI Effects of a psychophysiological system for adaptive automation on performance, workload, and the event-related potential P300 component SO HUMAN FACTORS LA English DT Article ID TASK; EEG; MODEL; ALLOCATION; ATTENTION; RESOURCES; INDEXES; STRESS AB The present study examined the effects of an electroencephalographic- (EEG-) based system for adaptive automation on tracking performance and workload. In addition, event-related potentials (ERPs) to a secondary task were derived to determine whether they would provide an additional degree of workload specificity. Participants were run in an adaptive automation condition, in which the system switched between manual and automatic task modes based on the value of each individual's own EEG engagement index; a yoked control condition; or another control group, in which task mode switches followed a random pattern. Adaptive automation improved performance and resulted in lower levels of workload. Further, the P300 component of the ERP paralleled the sensitivity to task demands of the performance and subjective measures across conditions. These results indicate that it is possible to improve performance with a psychophysiological adaptive automation system and that ERPs may provide an alternative means for distinguishing among levels of cognitive task demand in such systems. Actual or potential applications of this research include improved methods for assessing operator workload and performance. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. Old Dominion Univ, Norfolk, VA USA. RP Prinzel, LJ (reprint author), NASA, Langley Res Ctr, Mail Stop 152, Hampton, VA 23681 USA. EM l.j.prinzel@larc.nasa.gov NR 47 TC 57 Z9 57 U1 1 U2 3 PU HUMAN FACTORS SOC PI SANTA MONICA PA BOX 1369, SANTA MONICA, CA 90406 USA SN 0018-7208 J9 HUM FACTORS JI Hum. Factors PD WIN PY 2003 VL 45 IS 4 BP 601 EP 613 DI 10.1518/hfes.45.4.601.27092 PG 13 WC Behavioral Sciences; Engineering, Industrial; Ergonomics; Psychology, Applied; Psychology SC Behavioral Sciences; Engineering; Psychology GA 800XB UT WOS:000220059900008 PM 15055457 ER PT J AU Carpino, M Milani, A Chesley, SR AF Carpino, M Milani, A Chesley, SR TI Error statistics of asteroid optical astrometric observations SO ICARUS LA English DT Article DE asteroids; data reduction techniques; orbits ID IDENTIFICATION PROBLEM AB Astrometric uncertainty is a crucial component of the asteroid orbit determination process. However, in the absence of rigorous uncertainty information, only very crude weighting schemes are available to the orbit computer. This inevitably leads to a correspondingly crude characterization of the orbital uncertainty and in many cases to less accurate orbits. In this paper we describe a method for carefully assessing the statistical performance of the various observatories that have produced asteroid astrometry, with the ultimate goal of using this statistical characterization to improve asteroid orbit determination. We also include a detailed description of our previously unpublished automatic outlier rejection algorithm used in the orbit determination, which is an important component of the fitting process. To start this study we have determined the best fitting orbits for the first 17,349 numbered asteroids and computed the corresponding O-C astrometric residuals for all observations used in the orbit fitting. We group the residuals into roughly homogeneous bins and compute the root mean square (RMS) error and bias in declination and right ascension for each bin. Results are tabulated for each of the 77 bins containing more than 3000 observations; this comprises roughly two thirds of the data, but only 2% of the bins. There are several interesting results, including substantial bias from several observatories, and some distinct non-Gaussian characteristics that are difficult to explain. Several limitations of our approach and possible future improvements are discussed. The correlation of errors among observations taken closely together in time is in many cases an important issue that has rarely been considered. We have computed the mean correlation between observations with varying time separations and obtained empirical functions that model the results. This has been done for several observatories with very large data sets (the remainder has been lumped into a single mixed batch). These functions could be used for estimating correlation coefficients among different observations of the same observatory, supplying a new observation weighting scheme based upon an empirically tested observational error model. (C) 2003 Elsevier Inc. All rights reserved. C1 Osserv Astron Brera, I-20121 Milan, Italy. Univ Pisa, Dipartmento Matemat, I-56127 Pisa, Italy. Navigat & Mission Design Sect, Jet Prop Lab, Pasadena, CA 91109 USA. RP Carpino, M (reprint author), Osserv Astron Brera, Via Brera 28, I-20121 Milan, Italy. NR 9 TC 33 Z9 32 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 DEC PY 2003 VL 166 IS 2 BP 248 EP 270 DI 10.1016/S0019-1035(03)00051-4 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000187231000003 ER PT J AU Ostro, SJ Giorgini, JD Benner, LAM Hine, AA Nolan, MC Margot, JL Chodas, PW Veillet, C AF Ostro, SJ Giorgini, JD Benner, LAM Hine, AA Nolan, MC Margot, JL Chodas, PW Veillet, C TI Radar detection of asteroid 2002 AA29 SO ICARUS LA English DT Article DE asteroids; radar; photometry ID EARTH AB Radar echoes from Earth co-orbital Asteroid 2002 AA29 yield a total-power radar cross section of 2.9 x 10(-5) km(2) +/-25%, a circular polarization ratio of SC/OC = 0.26 +/- 0.07, and an echo bandwidth of at least 1.5 Hz. Combining these results with the estimate of its visual absolute magnitude, H-V = 25.23 +/- 0.24, from reported Spacewatch photometry indicates an effective diameter of 25 +/- 5 m, a rotation period no longer than 33 min, and an average surface bulk density no larger than 2.0 g cm(-3); the asteroid is radar dark and optically bright, and its statistically most likely spectral class is S. The Hv estimate from LINEAR photometry (23.58 +/- 0.38) is not compatible with either Spacewatch's H-V or our radar results. If a bias this large were generally present in LINEAR's estimates of Hv for asteroids it has discovered or observed, then estimates of the current completeness of the Spaceguard Survey would have to be revised downward. (C) 2003 Elsevier Inc. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Arecibo Observ, Natl Astron & Ionosphere Ctr, Arecibo, PR 00612 USA. CALTECH, Pasadena, CA 91125 USA. Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. RP Ostro, SJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. 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 7 Z9 7 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 DEC PY 2003 VL 166 IS 2 BP 271 EP 275 DI 10.1016/j.icarus.2003.09.001 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000187231000004 ER PT J AU Jones, GH Balogh, A McComas, DJ MacDowall, RJ AF Jones, GH Balogh, A McComas, DJ MacDowall, RJ TI Strong interplanetary field enhancements at Ulysses - evidence of dust trails' interaction with the solar wind? SO ICARUS LA English DT Article DE solar wind; interplanetary medium; interplanetary dust; comets ID NEAR-EARTH ASTEROIDS; SOURCE PICKUP IONS; STATISTICAL PROPERTIES; MAGNETIC HOLES; 2201 OLJATO; ASSOCIATION; ENCOUNTER; ORIGIN; COMET; AU AB Interplanetary field enhancements were first discovered in the vicinity of Venus. These events are characterised by an increase in the magnitude of the heliospheric magnetic field with a near-symmetrical, sometimes thorn-shaped profile, and last from minutes to hours. Surveys of the events near Venus and Earth indicated clustering of the events in inertial space, which suggested that their sources were Solar System objects other than the Sun. A survey is presented of strong events of this type detected by the Ulysses spacecraft from 1990 to late 2001. Most of the events are accompanied by a discontinuity in the field direction near the events' centres. Other discontinuities are often symmetrical about the enhancement. The majority of events last less than two hours. When examined as a whole, the events tend to be accompanied by subtle changes in some plasma parameters. The majority of the enhancements are accompanied by magnetic holes on their fringes. The enhancements' occurrence rate increases with decreasing heliocentric distance. Possible formation mechanisms are discussed. No link was found with solar, or solar wind sources. Several aspects of the survey results are consistent with an origin related to cometary dust trails. Possible processes associated with a dust-solar wind interaction are discussed. (C) 2003 Elsevier Inc. All rights reserved. C1 Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Space & Atmospher Phys Grp, London SW7 2BW, England. SW Res Inst, Space Sci & Engn Div, San Antonio, TX 78228 USA. NASA, Goddard Space Flight Ctr, Extraterr Phys Lab, Greenbelt, MD 20771 USA. RP NASA, Jet Propuls Lab, Pasadena, CA 91109 USA. EM geraint.h.jones@jpl.nasa.gov RI MacDowall, Robert/D-2773-2012; Jones, Geraint/C-1682-2008; OI Jones, Geraint/0000-0002-5859-1136 NR 39 TC 10 Z9 10 U1 0 U2 1 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD DEC PY 2003 VL 166 IS 2 BP 297 EP 310 DI 10.1016/j.icarus.2003.09.007 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000187231000007 ER PT J AU Goldreich, P Rappaport, N AF Goldreich, P Rappaport, N TI Origin of chaos in the Prometheus-Pandora system SO ICARUS LA English DT Article DE satellites of Saturn; orbits; chaos ID SATELLITES AB We demonstrate that the chaotic orbits of Prometheus and Pandora are due to interactions associated with the 121 : 118 mean motion resonance. Differential precession splits this resonance into a quartet of components equally spaced in frequency. Libration widths of the individual components exceed the splitting, resulting in resonance overlap which causes the chaos. Mean motions of Prometheus and Pandora wander chaotically in zones of width 1.8 and 3.1 deg yr(-1), respectively. A model with 1.5 degrees of freedom captures the essential features of the chaotic dynamics. We use it to show that the Lyapunov exponent of 0.3 yr(-1) arises because the critical argument of the dominant member of the resonant quartet makes approximately two separatrix crossings every 6.2 year precessional cycle. (C) 2003 Elsevier Inc. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Inst Adv Study, Princeton, NJ 08540 USA. RP Rappaport, N (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NR 8 TC 27 Z9 27 U1 0 U2 1 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD DEC PY 2003 VL 166 IS 2 BP 320 EP 327 DI 10.1016/j.icarus.2003.09.002 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000187231000009 ER PT J AU Cuzzi, JN Davis, SS Dobrovolskis, AR AF Cuzzi, JN Davis, SS Dobrovolskis, AR TI Blowing in the wind. II. Creation and redistribution of refractory inclusions in a turbulent protoplanetary nebula SO ICARUS LA English DT Article DE origin, solar system; solar nebula; meteorites; mineralogy ID ALUMINUM-RICH INCLUSIONS; DIFFERENTIALLY ROTATING-FLOWS; SOLAR NEBULA; ACCRETION DISKS; CARBONACEOUS CHONDRITES; GLOBAL EVOLUTION; SOLID MATTER; CHONDRULES; PARTICLES; SYSTEM AB Ca-Al rich refractory mineral inclusions (CAIs) found at 1-6% mass fraction in primitive chondrites appear to be 1-3 million years older than the dominant (chondrule) components which were accreted into the same parent bodies. A prevalent concern is that it is difficult to retain CAIs for this long against gas-drag-induced radial drift into the Sun. We reassess the situation in terms of a hot inner (turbulent) nebula context for CAI formation, using analytical models of nebula evolution and particle diffusion. We show that outward radial diffusion in a weakly turbulent nebula can overcome inward drift, and prevent significant numbers of CAI-size particles from being lost into the Sun for times on the order of 106 years. CAIs can form early, when the inner nebula was hot, and persist in sufficient abundance to be incorporated into primitive planetesimals at a much later time. Small (less than or similar to 0.1 mm diameter) CAIs persist for longer times than large (greater than or similar to 5 mm diameter) ones. To obtain a quantitative match to the observed volume fractions of CAIs in chondrites, another process must be allowed for: a substantial enhancement of the inner hot nebula in silicate-forming material, which we suggest was caused by rapid inward drift of meter-sized objects. This early in nebula history, the drifting rubble would have a carbon content probably an order of magnitude larger than even the most primitive (CI) carbonaceous chondrites. Abundant carbon in the evaporating material would help keep the nebula oxygen fugacity low, plausibly solar. as inferred for the formation environment of CAIs. The associated production of a larger than canonical amount of CO(2) might also play a role in mass-independent fractionation of oxygen isotopes, leaving the gas rich in (16)O as inferred from CAIs and other high temperature condensates. Published by Elsevier Inc. C1 NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Cuzzi, JN (reprint author), NASA, Ames Res Ctr, Div Space Sci, Mail Stop 245-3, Moffett Field, CA 94035 USA. EM cuzzi@cosmic.arc.nasa.gov NR 86 TC 76 Z9 77 U1 1 U2 7 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD DEC PY 2003 VL 166 IS 2 BP 385 EP 402 DI 10.1016/j.icarus.2003.08.016 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000187231000014 ER PT J AU Dorn, ED McDonald, GD Storrie-Lombardi, MC Nealson, KH AF Dorn, ED McDonald, GD Storrie-Lombardi, MC Nealson, KH TI Principal component analysis and neural networks for detection of amino acid biosignatures SO ICARUS LA English DT Article DE life detection; exobiology amino acids; meteorites; Murchison; neutral networks; Principal Component Analysis ID MURCHISON METEORITE; NEUTRAL SUGARS; SEDIMENTS; LIGNIN; EARTH; MARS AB We examine the applicability of Principal Component Analysis (PCA) and Artificial Neural Network (ANN) methods of data analysis to biosignature detection. These techniques show promise in classifying and simplifying the representation of patterns of amino acids resulting from biological and non-biological syntheses. PCA correctly identifies glycine and alanine as the amino acids contributing the most information to the task of discriminating biotic and abiotic samples. Trained ANNs correctly classify between 86.1 and 99.5% of a large set of amino acid samples as biotic or abiotic. These and similar techniques are important in the design of automated data analysis systems for robotic missions to distant planetary bodies. Both techniques are robust with respect to noisy and incomplete data. Analysis of the performance of PCA and ANNs also lends insight into the localization of useful information within a particular data set, a feature that may be exploited in the selection of experiments for efficient mission design. (C) 2003 Elsevier Inc. All rights reserved. C1 CALTECH, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Ctr Sci & Technol Life Detect, Pasadena, CA 91109 USA. RP Dorn, ED (reprint author), CALTECH, MSC 139-74,1200 E Calif Blvd, Pasadena, CA 91125 USA. NR 23 TC 10 Z9 11 U1 2 U2 8 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD DEC PY 2003 VL 166 IS 2 BP 403 EP 409 DI 10.1016/j.icarus.2003.08.011 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000187231000015 ER PT J AU Divsalar, D Biglieri, E AF Divsalar, D Biglieri, E TI Upper bounds to error probabilities of coded systems beyond the cutoff rate SO IEEE TRANSACTIONS ON COMMUNICATIONS LA English DT Article; Proceedings Paper CT IEEE International Symposium on Information Theory CY JUN 24-30, 2000 CL SORRENTO, ITALY SP IEEE, Informat Theory Soc DE cutoff rate; error probability; fading channels; low-density parity-check (LDPC) codes; turbo codes ID LINEAR BLOCK-CODES; TURBO-CODES; PERFORMANCE AB A family of upper bounds to error probabilities of coded systems was recently proposed by Divsalar. These bounds are valid for transmission over the additive white Gaussian noise channel, and require only the knowledge of the weight spectrum of the code words. After illustrating these bounds, we extend them to fading channels. Contrary to the union bound, our bounds maintain their effectiveness below the signal-to-noise ratio (SNR) at which the cutoff rate of the channel equals the rate of the code. Some applications are shown. First, we derive upper bounds to the minimum SNR necessary to achieve zero error probability as the code block length increases to infinity. Next, we use our bounds to predict the performance of turbo codes and low-density parity-check codes. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Politecn Torino, Dipartimento Elettron, I-10129 Turin, Italy. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Dariush.Divsalar@jpl.nasa.gov; Biglieri@polito.it RI Biglieri, Ezio/A-2246-2012 OI Biglieri, Ezio/0000-0002-8867-2455 NR 24 TC 26 Z9 26 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0090-6778 EI 1558-0857 J9 IEEE T COMMUN JI IEEE Trans. Commun. PD DEC PY 2003 VL 51 IS 12 BP 2011 EP 2018 DI 10.1109/TCOMM.2003.820746 PG 8 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 763LV UT WOS:000188088100010 ER PT J AU Meyyappan, K McCluskey, P Chen, LY AF Meyyappan, K McCluskey, P Chen, LY TI Thermomechanical analysis of gold-based SiC die-attach assembly SO IEEE TRANSACTIONS ON DEVICE AND MATERIALS RELIABILITY LA English DT Article AB The thermomechanical stresses due to mismatch of the coefficients of thermal expansion (CTE) of the base material (SiC) and the packaging has a significant impact on the stresses in MEMS pressure sensors used in high-temperature applications, to 600 degreesC. The pressure sensor studied essentially consists of a SiC die attached to an AIN substrate using a gold die attach. Characterization of the stress distribution within the die attach, die and substrate along with the fatigue resistance of the die attach At 600 degreesC is essential to estimating the. reliability of the packaging structure. A parametric study has been performed using nonlinear finite element analysis to optimize the die-attach thermomechanical performance at high temperatures. This study includes the effects of varying porosity levels and varying reference temperatures (stress-free temperature). This study also provides information about the mechanical deformations of the pressure sensor due to the thermomechanical load, which must be compensated, for the effective performance of the pressure sensor. The outcome of the study provides guidelines to optimize the design of the pressure sensor. C1 Univ Maryland, CALCE, Elect Prod & Syst Ctr, College Pk, MD 20742 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Meyyappan, K (reprint author), Univ Maryland, CALCE, Elect Prod & Syst Ctr, College Pk, MD 20742 USA. EM karumbu@wam.umd.edu; mcclupa@calce.umd.edu; Liangyu.Chen@grc.nasa.gov RI McCluskey, Patrick/H-6035-2013 NR 4 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 1530-4388 J9 IEEE T DEVICE MAT RE JI IEEE Trans. Device Mater. Reliab. PD DEC PY 2003 VL 3 IS 4 BP 152 EP 158 DI 10.1109/TDMR.2003.821538 PG 7 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 766LD UT WOS:000188377100006 ER PT J AU Gunapala, SD Bandara, SV Liu, JK Rafol, SB Mumolo, JM AF Gunapala, SD Bandara, SV Liu, JK Rafol, SB Mumolo, JM TI 640 x 512 pixel long-wavelength infrared narrowband, multiband, and broadband QWIP focal plane arrays SO IEEE TRANSACTIONS ON ELECTRON DEVICES LA English DT Article DE broadband; focal plane array; infrared camera; long-wavelength infrared; mid-wavelength infrared; multiband; narrowband; quantum-well infrared photodetectors (QWIP) ID PHOTODETECTOR; CAMERA AB A 640 x 512 pixel, long-wavelength cutoff, narrowband (Deltalambda/lambdasimilar to10%) quantum-well infrared photodetector QWIP) focal plane array (M), a four-band QWIP FPA in the 4-15 mum spectral region, and a broadband (Deltalambda/lambda similar to 42%) QWIP FPA having a 15.4 mum cutoff have been demonstrated. In this paper, we discuss the electrical and optical characterization of these FPAs, and their performance. In addition, we discuss the development of a very sensitive (NEDT similar to10.6 mK) 640 x 512 pixel thermal imaging camera having a 9 mum cutoff. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Gunapala, SD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Sarath.d.Gunapala@jpl.nasa.go NR 8 TC 47 Z9 50 U1 2 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9383 J9 IEEE T ELECTRON DEV JI IEEE Trans. Electron Devices PD DEC PY 2003 VL 50 IS 12 BP 2353 EP 2360 DI 10.1109/TED.2003.818818 PG 8 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 762WC UT WOS:000188004300005 ER PT J AU Bolten, JD Lakshmi, V Njoku, EG AF Bolten, JD Lakshmi, V Njoku, EG TI Soil moisture retrieval using the passive/active L- and S-band radar/radiometer SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE microwave; radar; radiometer; remote sensing; soil moisture ID SATELLITE MICROWAVE OBSERVATIONS; SURFACE PARAMETERS; VEGETATION COVER; RADIOMETER; MODEL; CROP; VARIABILITY; SENSITIVITY; EMISSION; SENSOR AB In the present study, remote sensing of soil moisture is carried out using the Passive and Active L- and S-band airborne sensor (PALS). The data in this paper were taken from five days of overflights near Chickasha, OK during the 1999 Southern Great Plains (SGP99) experiment. Presently, we analyze the collected data to understand the relationships between the observed signals (radiometer, brightness temperature and radar backscatter) and surface parameters (surface soil moisture, temperature, vegetation water content, and roughness). In addition, a radiative transfer model and two radar backscatter models are used to simulate the PALS observations. An integration of observations, regression retrievals, and forward modeling is used to derive the best estimates of soil moisture under varying surface conditions. C1 Univ S Carolina, Dept Geol Sci, Columbia, SC 29208 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bolten, JD (reprint author), Univ S Carolina, Dept Geol Sci, Columbia, SC 29208 USA. EM jbolten@geol.sc.edu; vlakshmi@geol.sc.edu; eni.g.njoku@jpl.nasa.gov RI Bolten, John/F-9006-2012; Lakshmi, Venkat/I-3078-2016 OI Lakshmi, Venkat/0000-0001-7431-9004 NR 45 TC 23 Z9 26 U1 1 U2 9 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD DEC PY 2003 VL 41 IS 12 BP 2792 EP 2801 DI 10.1109/TGRS.2003.815401 PN 1 PG 10 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 766KU UT WOS:000188376200011 ER PT J AU Kim, DJ Moon, WM Moller, D Imel, DA AF Kim, DJ Moon, WM Moller, D Imel, DA TI Measurements of ocean surface waves and currents using L- and C-band along-track interferometric SAR SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE along-track interferometric synthetic aperture; radar (ATI-SAR); Bragg-wave phase velocity; dual-frequency; ocean surface current; ocean surface wave ID SYNTHETIC-APERTURE RADAR; MODULATION TRANSFER-FUNCTION; IMAGE SPECTRA; DIRECTIONAL SPECTRA; SEA-SURFACE; SIMULATION; INVERSION; TRANSFORM; ALGORITHM; PLATFORM AB Along-track interferometric synthetic aperture radar (ATI-SAR) is an active coherent imaging system, utilizing two antennas separated along the platform flight direction. The phase information of ATI-SAR from the Doppler shift of the backscattered signal represents the line-of-sight velocity of the water scatterers. While the advent of ATI-SAR provided us with a potentially powerful technique for ocean surface current and wave mapping, the surface current has not been measured exactly from the ATI-SAR velocity because the Doppler shift is not simply proportional to the component of the mean surface current. It also includes other types of contributions associated with the phase velocity of the Bragg waves and orbital motions of all ocean waves that are longer than Bragg waves. In this paper, we review how the phase difference measured by ATI-SAR is related to the mean Doppler frequency, and we develop a new and practically useful method to extract the surface current component utilizing simultaneously measured Land C-band ATI-SAR data. Since the measured ATI-SAR velocity shows a different value at a different radar-frequency, we investigate the influence of Bragg-resonant waves and long ocean wave motions on the ATI-SAR velocity according to the radar frequency. The Bragg-wave phase velocity component, which is a significant source of error for extracting the surface current, can be effectively eliminated by using L- and C-band ATI-SAR. The method is applied to L- and C-band ATI-SAR measurements acquired at the Ulsan coast in the southeastern part of the Korean peninsula. The resulting ocean surface current vectors are compared with in situ measurements collected by recording current meter. We furthermore extract ocean surface wave information from the ATI-SAR phase image using a quasi-linear transform. C1 Seoul Natl Univ, Sch Earth & Environm Sci, ESI3 Lab, Seoul 151747, South Korea. Univ Manitoba, Dept Geophys, Winnipeg, MB R3T 2N2, Canada. Jet Prop Lab, Radar Sci & Engn Sect, Pasadena, CA 91109 USA. RP Kim, DJ (reprint author), Seoul Natl Univ, Sch Earth & Environm Sci, ESI3 Lab, Seoul 151747, South Korea. EM wmoon@eos1.snu.ac.kr RI Kim, Duk-jin/H-4024-2011; OI Imel, David/0000-0002-6118-7396 NR 34 TC 11 Z9 19 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 DEC PY 2003 VL 41 IS 12 BP 2821 EP 2832 DI 10.1109/TGRS.2003.817210 PN 1 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 766KU UT WOS:000188376200014 ER PT J AU Kwiatkowska, EJ Fargion, GS AF Kwiatkowska, EJ Fargion, GS TI Application of machine-learning techniques toward the creation of a consistent and calibrated global chlorophyll concentration baseline dataset using remotely sensed ocean color data SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE chlorophyll; data merger; fusion; machine learning; moderate resolution Imaging spectroradiometer; (MODIS); ocean color; regression; sea-viewing wide field-of-view sensor (SeaWiFS); support vector machines ID SUPPORT VECTOR MACHINES; TEMPERATURE SCANNER; NEURAL-NETWORKS; SEAWIFS; ALGORITHMS; RADIANCE; MODEL; MODIS; ERA AB This paper introduces a machine-learning approach to satellite ocean color sensor cross calibration. The cross-calibration objective is to eliminate incompatibilities among sensor data from different missions and produce merged daily global ocean color coverage. The approach is designed and investigated using data from the Moderate Resolution Imaging Spectroradiometer (MODIS) onboard of the Terra satellite and Sea-viewing Wide Field-of-view Sensor (SeaWiFS). Data from these two sensors show apparent discrepancies originating from differences in sensor design, calibration, processing algorithms, and from the rate of change in the atmosphere and ocean within 1(1/2) h between sensor imaging of the same regions on the ground. The discrepancies have complex, noisy, and often contradictory time and space variabilities. Support vector machines are used to bring MODIS data to the SeaWiFS representation where SeaWiFS data are considered to exemplify a consistent ocean color baseline. Support vector machines are effective in learning and resolving convoluted data relationships between the two sensors given a variety of bio-optical, atmospheric, viewing geometry, and ancillary information. The method works accurately in low chlorophyll waters and shows a potential to eliminate sensor problems, such as scan angle dependencies and seasonal and spatial trends in data. The results illustrate that MODIS and SeaWiFS differences are noisy and highly variable, which makes it difficult to extrapolate the cross-calibration knowledge onto new time and space domains and to define representative global ocean color datasets for support vector machine training. C1 NASA, Goddard Space Flight Ctr, Sci Applicat Int Corp, Greenbelt, MD 20771 USA. RP Kwiatkowska, EJ (reprint author), NASA, Goddard Space Flight Ctr, Sci Applicat Int Corp, Greenbelt, MD 20771 USA. EM gfargion@simbios.gsfc.nasa.gov NR 53 TC 28 Z9 31 U1 1 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 DEC PY 2003 VL 41 IS 12 BP 2844 EP 2860 DI 10.1109/TGRS.2003.818016 PN 1 PG 17 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 766KU UT WOS:000188376200016 ER PT J AU Lotsch, A Friedl, MA Pinzon, J AF Lotsch, A Friedl, MA Pinzon, J TI Spatio-temporal deconvolution of NDVI image sequences using independent component analysis SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE decorrelation; image sequence analysis; independent component analysis (ICA); neural network applications; normalized difference vegetation index (NDVI); remote sensing ID PRINCIPAL COMPONENTS; TIME-SERIES; ROTATION; EOFS AB Independent component analysis (ICA) provides a powerful new method to spatially and temporally deconvolve image sequences into components that capture variability arising from independent physical sources. To do this, ICA uses information contained in higher order cross-moments of multivariate data. We use remotely sensed time series of the normalized difference vegetation index to illustrate the utility of this technique. C1 Boston Univ, Dept Geog, Boston, MA 02215 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lotsch, A (reprint author), Boston Univ, Dept Geog, Boston, MA 02215 USA. EM alotsch@crsa.bu.edu; friedl@crsa.bu.edu; pinzon@negev.gsfc.nasa.gov NR 16 TC 16 Z9 19 U1 0 U2 8 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 DEC PY 2003 VL 41 IS 12 BP 2938 EP 2942 DI 10.1109/TGRS.2003.819868 PN 2 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 766KZ UT WOS:000188376700001 ER PT J AU Cole-Rhodes, AA Johnson, KL LeMoigne, J Zavorin, I AF Cole-Rhodes, AA Johnson, KL LeMoigne, J Zavorin, I TI Multiresolution registration of remote sensing imagery by optimization of mutual information using a stochastic gradient SO IEEE TRANSACTIONS ON IMAGE PROCESSING LA English DT Article DE image registration; mutual information; remote sensing imagery; stochastic optimization; wavelets AB Image registration is the process by which we determine a transformation that provides the most accurate match between two images. The search for the matching transformation can be automated with the use of a suitable metric, but it can be very time-consuming and tedious. In this paper, we introduce a registration algorithm that combines a simple yet powerful search strategy based on a stochastic gradient with two similarity measures, correlation and mutual information, together with a wavelet-based multiresolution pyramid. We limit our study to pairs of images, which are misaligned by rotation and/or translation, and present two main results. First, we demonstrate that in our application mutual information may be better suited for sub-pixel registration as it produces consistently sharper optimum peaks than correlation. Then, we show that the stochastic gradient search combined with either measure produces accurate results when applied to synthetic, as well as multitemporal or multisensor collections of satellite data. Mutual information is generally found to optimize with one-third the number of iterations required by correlation. Results also show that a multiresolution implementation of the algorithm yields significant improvements in terms of both speed and robustness over a single-resolution implementation. C1 Morgan State Univ, Dept Elect & Comp Engn, Baltimore, MD 21251 USA. NASA, Goddard Space Flight Ctr, Appl Informat Sci Branch, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, UMBC, GEST Ctr, Greenbelt, MD 20771 USA. RP Cole-Rhodes, AA (reprint author), Morgan State Univ, Dept Elect & Comp Engn, Baltimore, MD 21251 USA. EM acrhodes@eng.morgan.edu; kjohnson@eng.morgan.edu; lemoigne@backserv.gsfc.nasa.gov; zavorin@backserv.gsfc.nasa.gov NR 23 TC 117 Z9 132 U1 1 U2 21 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1057-7149 J9 IEEE T IMAGE PROCESS JI IEEE Trans. Image Process. PD DEC PY 2003 VL 12 IS 12 BP 1495 EP 1511 DI 10.1109/TIP.2003.819237 PG 17 WC Computer Science, Artificial Intelligence; Engineering, Electrical & Electronic SC Computer Science; Engineering GA 764FV UT WOS:000188197500005 PM 18244705 ER PT J AU Bahoura, M Clairon, A AF Bahoura, M Clairon, A TI Diode laser phase noise influence on the ultimate performance of its frequency stabilization to a Mach-Zehnder interferometer fringe SO IEEE TRANSACTIONS ON INSTRUMENTATION AND MEASUREMENT LA English DT Article DE conversion noise; intermodulation noise; laser frequency stabilization; Mach-Zehnder interferometer; semiconductor laser ID INTERROGATED ATOMIC RESONATOR; STABILITY; SPECTROSCOPY; DEGRADATION; LIMITATION; STANDARDS AB We report a detailed investigation on the effect of semiconductor laser phase noise on the achievable frequency stability when locked to a Mach-Zehnder interferometer fringe. We show that the modulation-demodulation operation produces in the presence of laser phase noise two kinds of excess noise, which could be much above the shot noise limit, namely: conversion noise (PM-to-AM) and intermodulation noise. We show that in typical stabilization conditions, the frequency stability of the locked laser is limited by the intermodulation excess noise. This effect, reported initially in the microwave domain, can be considerably reduced by a convenient choice of the modulation frequency. To our knowledge, this is the first time such a phenomenon is reported in the optical domain. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. Observ Paris, Lab Primaire Temps & Frequences, F-75014 Paris, France. RP Bahoura, M (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 24 TC 2 Z9 2 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 DEC PY 2003 VL 52 IS 6 BP 1846 EP 1853 DI 10.1109/TIM.2003.820493 PG 8 WC Engineering, Electrical & Electronic; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 745KM UT WOS:000186687900022 ER PT J AU Mata, A Su, XW Fleischman, AJ Roy, S Banks, BA Miller, SK Midura, RJ AF Mata, A Su, XW Fleischman, AJ Roy, S Banks, BA Miller, SK Midura, RJ TI Osteoblast attachment to a textured surface in the absence of exogenous adhesion proteins SO IEEE TRANSACTIONS ON NANOBIOSCIENCE LA English DT Article DE cell adhesion; focal adhesion contacts; nanotechnology; osteoblast; surface microtextures ID MICROTEXTURED SILICONE; BONE SIALOPROTEIN; CELL-ADHESION; ORIENTATION; ACTIVATION; DIMENSIONS; MIGRATION; SUBSTRATA; MEMBRANES; GROWTH AB The present study investigated whether osteoblasts could attach to a culture substratum through a surface texture-dependent mechanism. Four test groups were used: (A) untextured, and three texture groups with maximum feature sizes of (B) <0.5 mum, (C) 2 mum, and (D) 4 mum, respectively. All surfaces were coated with the nonadhesive protein bovine serum albumin (BSA). Osteoblasts were allowed to adhere in serum-free medium for either 1 or 4 h, at which time nonadherent cells were removed. At 4 h, untextured surface A exhibited no cell attachment, while textured surfaces B, C, and D exhibited 9%, 32%, and 16% cell adhesion, respectively. At 16 h of incubation, adherent osteoblasts on textured surface C exhibited focal adhesion contacts and microfilament stress-fiber bundles. These results indicate that microtextured surfaces in the absence of exogenous adhesive proteins can facilitate osteoblast adhesion. C1 Cleveland Clin Fdn, Lerner Res Inst, Dept Biomed Engn, Cleveland, OH 44195 USA. NASA, Glenn Res Ctr, Electro Phys Branch, Cleveland, OH 44135 USA. RP Mata, A (reprint author), Cleveland Clin Fdn, Lerner Res Inst, Dept Biomed Engn, ND 20, Cleveland, OH 44195 USA. EM mataa@bme.ri.ccf.org RI Mata, Alvaro/D-6028-2015 OI Mata, Alvaro/0000-0002-6739-9111 FU NIAMS NIH HHS [AR45171] NR 32 TC 31 Z9 31 U1 1 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1536-1241 J9 IEEE T NANOBIOSCI JI IEEE Trans. Nanobiosci. PD DEC PY 2003 VL 2 IS 4 BP 287 EP 294 DI 10.1109/TNB.2003.820268 PG 8 WC Biochemical Research Methods; Nanoscience & Nanotechnology SC Biochemistry & Molecular Biology; Science & Technology - Other Topics GA 780QM UT WOS:000189392900016 PM 15376920 ER PT J AU Culpepper, BJ Keller, RM AF Culpepper, BJ Keller, RM TI Enabling computer decisions based on EEG input SO IEEE TRANSACTIONS ON NEURAL SYSTEMS AND REHABILITATION ENGINEERING LA English DT Article DE brain-computer interface (BCI); electroencephalogram (EEG); independent component analysis (ICA); neural networks ID INTERFACE BCI; COMMUNICATION AB Multilayer neural networks were successfully trained to classify segments of 12-channel electroencephalogram (EEG) data into one of five classes corresponding to five cognitive tasks performed by a subject. Independent component analysis (ICA) was used to segregate obvious artifact EEG components from other sources, and a frequency-band representation was used to represent the sources computed by ICA. Examples of results include an 85% accuracy rate on differentiation between two tasks, using a segment of EEG only 0.05-s-long and a 95% accuracy rate using a 0.5-s-long segment. C1 NASA, Ames Res Ctr, Neuro Engn Lab, Moffett Field, CA 94035 USA. Harvey Mudd Coll, Dept Comp Sci, Claremont, CA 91711 USA. RP Culpepper, BJ (reprint author), NASA, Ames Res Ctr, Neuro Engn Lab, Moffett Field, CA 94035 USA. NR 15 TC 12 Z9 12 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1534-4320 J9 IEEE T NEUR SYS REH JI IEEE Trans. Neural Syst. Rehabil. Eng. PD DEC PY 2003 VL 11 IS 4 BP 354 EP 360 DI 10.1109/TNSRE.2003.819788 PG 7 WC Engineering, Biomedical; Rehabilitation SC Engineering; Rehabilitation GA 768KA UT WOS:000188541100003 PM 14960110 ER PT J AU Johnston, AH AF Johnston, AH TI 2003 Nuclear and Space Radiation Effects Conference - Comments by the General Chairman SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Editorial Material 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 NR 0 TC 0 Z9 0 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 DEC PY 2003 VL 50 IS 6 BP 1762 EP 1763 DI 10.1109/TNS.2003.822119 PN 1 PG 2 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 772JA UT WOS:000188837800001 ER PT J AU Johnston, A AF Johnston, A TI In memoriam - Douglas George Millward SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Biographical-Item C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Johnston, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 0 TC 0 Z9 0 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 DEC PY 2003 VL 50 IS 6 BP 1774 EP 1774 DI 10.1109/TNS.2003.822125 PN 1 PG 1 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 772JA UT WOS:000188837800005 ER PT J AU Lu, Y Cressler, JD Krithivasan, R Li, Y Reed, RA Marshall, PW Polar, C Freeman, G Ahlgren, D AF Lu, Y Cressler, JD Krithivasan, R Li, Y Reed, RA Marshall, PW Polar, C Freeman, G Ahlgren, D TI Proton tolerance of third-generation, 0.12 mu m 185 GHz SiGeHBTs SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 40th Annual Nuclear and Space Radiation Effects conference CY JUL 21-25, 2003 CL MONTEREY, CALIFORNIA SP IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE bipolar transistors; HBT; proton irradiation; silicon-germanium (SiGe) ID PERFORMANCE; TECHNOLOGY AB We present results on the impact of proton irradiation on the dc and ac characteristics of third-generation, 0.12 mum 185 GHz SiGe HBTs. Comparisons with prior technology generations are used to assess how the structural changes needed to enhance performance between second and third generation technology couple to the observed proton response. The results demonstrate that SiGe HBT technologies can successfully maintain their a Mrad-level total dose, hardness, without intentional hardening, even when vertically-scaled in order to achieve unprecedented levels of transistor performance. C1 Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. Auburn Univ, Dept Elect & Comp Engn, Auburn, AL 36849 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Jackson & Tull Chartered Engineers, Washington, DC 20018 USA. IBM Microelect, Hopewell Jct, NY 12533 USA. RP Lu, Y (reprint author), Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. EM luyuan@ece.gatech.edu RI Krithivasan, Ramkumar/D-3549-2011 NR 7 TC 23 Z9 23 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 DEC PY 2003 VL 50 IS 6 BP 1811 EP 1815 DI 10.1109/TNS.2003.820737 PN 1 PG 5 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 772JA UT WOS:000188837800011 ER PT J AU Jin, ZR Johansen, JA Cressler, JD Reed, RA Marshall, PW Joseph, AJ AF Jin, ZR Johansen, JA Cressler, JD Reed, RA Marshall, PW Joseph, AJ TI Using proton irradiation to probe the origins of low-frequency noise variations in SiGeHBTs SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 40th Annual Nuclear and Space Radiation Effects Conference CY JUL 21-25, 2003 CL MONTEREY, CA SP IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE bipolar transistors; heterojunction bipolar transistor (HBT); low-frequency noise; 1 / f noise; proton irradiation; SiGe ID BIPOLAR JUNCTION TRANSISTORS; POLYSILICON EMITTER BJTS; FIELD-EFFECT TRANSISTORS; 1/F NOISE; 1-F NOISE; FLUCTUATIONS; MOBILITY; DIODES; OXIDE AB We use proton irradiation to probe the origins of the geometry-dependent variation of low-frequency noise in 120 GHz SiGe heterojunction bipolar transistors (HBTs). Before irradiation, small-sized transistors show a strong variation in noise magnitude across many samples, whereas the noise in larger devices is more statistically reproducible. Although the noise magnitude shows little degradation after 2 x 10(13) p/cm(2) irradiation, the observed noise variation decreases. Its dependence on both geometry and bias-is quantified. This fundamental geometrical scaling effect is investigated using theoretical calculations based on the superposition of generation/recombination (G/R) noise sources. C1 Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. Univ Tromso, Inst Phys, N-9037 Tromso, Norway. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. IBM Microelect, Essex Jct, VT 05452 USA. RP Jin, ZR (reprint author), Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. EM zhenrong@ece.gatech.edu NR 25 TC 5 Z9 5 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2003 VL 50 IS 6 BP 1816 EP 1820 DI 10.1109/TNS.2003.820739 PN 1 PG 5 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 772JA UT WOS:000188837800012 ER PT J AU Luo, ZZ Chen, TB Cressler, JD Sheridan, D Williams, JR Reed, RA Marshall, PW AF Luo, ZZ Chen, TB Cressler, JD Sheridan, D Williams, JR Reed, RA Marshall, PW TI Impact of proton irradiation on the static and dynamic characteristics of high-voltage 4H-SiC JBS switching diodes SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 40th Annual Nuclear and Space Radiation Effects conference CY JUL 21-25, 2003 CL MONTEREY, CALIFORNIA SP IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE diode; junction barrier Schottky (JBS); proton radiation; Schottky barrier diodes (SBD); silicon carbide (SiC) ID RADIATION; DEVICES AB The effects of. proton irradiation on the static (dc) and dynamic (switching) performance of high-voltage 4H-SiC Junction Barrier Schottky (JBS) diodes are investigated for the first time. In contrast to that observed on a high-voltage Si p - i - n diode control device, these SiC JBS devices show an increase (degradation) in series resistance (R-S) a decrease (improvement) of reverse leakage current, and increase (improvement) in blocking voltage after high-fluence proton exposure. Measured breakdown voltages of post-irradiated SiC diodes increase on average by about 200 V after irradiation. Dynamic reverse recovery transient measurements show good agreement between the various dc observations regarding differences between high-power SiC and Si diodes and show that SiC JBS diodes are very effective in minimizing switching losses for high-power applications, even under high levels of radiation exposure. C1 Auburn Univ, Elect & Comp Engn Dept, Alabama Microelect Sci & Technol Ctr, Auburn, AL 36849 USA. Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. IBM Microelect, Essex Jct, VT 05452 USA. Auburn Univ, Dept Phys, Auburn, AL 36849 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Luo, ZZ (reprint author), Auburn Univ, Elect & Comp Engn Dept, Alabama Microelect Sci & Technol Ctr, Auburn, AL 36849 USA. EM lozhiyu@eng.auburn.edu NR 19 TC 9 Z9 9 U1 1 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 DEC PY 2003 VL 50 IS 6 BP 1821 EP 1826 DI 10.1109/TNS.2003.821806 PN 1 PG 6 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 772JA UT WOS:000188837800013 ER PT J AU Li, Y Cressler, JD Lu, Y Pan, J Niu, GF Reed, RA Marshall, PW Polar, C Palmer, MJ Joseph, AJ AF Li, Y Cressler, JD Lu, Y Pan, J Niu, GF Reed, RA Marshall, PW Polar, C Palmer, MJ Joseph, AJ TI Proton tolerance of multiple-threshold voltage and multiple-breakdown voltage CMOS device design points in a 0.18 mu m system-on-a-chip CMOS technology SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 40th Annual Nuclear and Space Radiation Effects Conference CY JUL 21-25, 2003 CL MONTEREY, CA SP IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE CMOS; proton radiation; RF technology; system-on-chip ID PERFORMANCE AB The paper presents the results of an investigation of the proton tolerance of the multiple-threshold voltage and multiple-breakdown voltage device design points contained in a 0.18 mum system-on-a-chip CMOS technology. The radiation response of the CMOS devices having three different device design configurations are characterized and compared for equivalent gamma doses up to 300 krad(Si), using the threshold voltage, off-state leak age, and effective mobility to assess the dc performance. All three CMOS device configurations show a very slight degradation of threshold voltage and effective mobility with increasing dose. We also present for the first time the frequency response and S-parameters of these RF CMOS devices under proton radiation. The S-parameters and cut-off frequency show little degradation up to 300, krad(Si) total dose. These results suggest that the CMOS devices in this 0.18 mum SoC CMOS technology are well-suited for RF circuit applications in an ionizing radiation environment without intentional total-dose hardening. C1 Auburn Univ, Elect & Comp Engn Dept, Alabama Microelect Sci & Technol, Auburn, AL 36849 USA. Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Jackson & Tull Chartered Engineers, Washington, DC USA. IBM Microelect, Burlington, VT 05401 USA. RP Li, Y (reprint author), Auburn Univ, Elect & Comp Engn Dept, Alabama Microelect Sci & Technol, Auburn, AL 36849 USA. EM yingli@eng.auburn.edu NR 8 TC 8 Z9 10 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2003 VL 50 IS 6 BP 1834 EP 1838 DI 10.1109/TNS.2003.821800 PN 1 PG 5 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 772JA UT WOS:000188837800015 ER PT J AU Miyahira, TF Becker, HN McClure, SS Edmonds, LD Johnston, AH Hishinuma, Y AF Miyahira, TF Becker, HN McClure, SS Edmonds, LD Johnston, AH Hishinuma, Y TI Total dose degradation of MEMS optical mirrors SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 40th Annual Nuclear and Space Radiation Effects conference CY JUL 21-25, 2003 CL MONTEREY, CALIFORNIA SP IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE MEMS micromirror; MOEMS; piezoelectric; radiation damage; total dose ID SYSTEMS MEMS; ACCELEROMETERS; RADIATION AB This paper discusses the effect of ionizing radiation on two types of deformable MEMS mirrors. Little effect was observed in the technology that was based on electrostatic deflection, consistent with the structural design that does not contain insulators between the two sections. Significant changes in the operating characteristics were observed for the second type of mirror, which uses piezoelectric material for actuation. The mirrors required higher total dose levels before they were affected compared with MEMS accelerometers, which can. be explained by the larger interelement spacing used in the mirror arrays. C1 CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. RP Miyahira, TF (reprint author), CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. NR 11 TC 19 Z9 19 U1 4 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 DEC PY 2003 VL 50 IS 6 BP 1860 EP 1866 DI 10.1109/TNS.2003.820764 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 772JA UT WOS:000188837800019 ER PT J AU Li, Y Niu, GF Cressler, JD Patel, J Liu, M Mojarradi, MM Reed, RA Marshall, PW Blalock, BJ AF Li, Y Niu, GF Cressler, JD Patel, J Liu, M Mojarradi, MM Reed, RA Marshall, PW Blalock, BJ TI Probing proton damage in SOICMOS technology by using lateral bipolar action SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 40th Annual Nuclear and Space Radiation Effects conference CY JUL 21-25, 2003 CL MONTEREY, CALIFORNIA SP IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE interface states; interface traps; lateral bipolar; proton radiation; SOI ID CURRENT-VOLTAGE METHOD; INTERFACE TRAPS; GATED-DIODE; SENSITIVE TOOL; SOI MOSFETS; DCIV METHOD; TRANSISTORS; SEPARATION; SURFACE; CHARGE AB We investigate proton damage in SOI CMOS devices on UNIBOND using a variety of lateral bipolar operational modes. We show that, the impact of interface states and oxide charge can be more clearly observed using lateral bipolar action than by using normal FET operational characteristics. We also investigate the radiation-induced interface states at the Si/buried oxide interface and oxide charges in the buried oxide of this SOI CMOS technology using the DCIV method. C1 Auburn Univ, Elect & Comp Engn Dept, Alabama Microelect Sci & Technol Ctr, Auburn, AL 36849 USA. Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Honeywell Solid State Elect Ctr, Plymouth, MN 55441 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Tennessee, Dept Elect & Comp Engn, Knoxville, TN 37996 USA. RP Li, Y (reprint author), Auburn Univ, Elect & Comp Engn Dept, Alabama Microelect Sci & Technol Ctr, Auburn, AL 36849 USA. EM yingli@eng.auburn.edu NR 20 TC 0 Z9 0 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 DEC PY 2003 VL 50 IS 6 BP 1885 EP 1890 DI 10.1109/TNS.2003.822088 PN 1 PG 6 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 772JA UT WOS:000188837800023 ER PT J AU Messenger, SR Burke, EA Xapsos, MA Summers, GP Walters, RJ Jun, I Jordan, T AF Messenger, SR Burke, EA Xapsos, MA Summers, GP Walters, RJ Jun, I Jordan, T TI NIEL for heavy ions: An analytical approach SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 40th Annual Nuclear and Space Radiation Effects conference CY JUL 21-25, 2003 CL MONTEREY, CALIFORNIA SP IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE displacement damage; nortionizing energy loss (NIEL); nuclear stopping power ID RADIATION-DAMAGE; PROTON-RADIATION AB We describe an analytical model, for calculating nonionizing energy loss (NIEL) for heavy ions based on screened Coulomb potentials in the nonrelativistic limit. The model applies to any incident ion on any target material where the Coulomb interaction, is primarily responsible for atomic displacement. Results are compared with previous methods of extracting NIEL from Monte Carlo SRIM runs. Examples of NIEL calculations are given for incident ions having energies ranging from the threshold for atomic displacement to 1 GeV. The incident ions include H, He, B, Si, Fe, Xe, and An. Example targets include Si, GaAs, InP, and SiC. C1 SFA Inc, Largo, MD 20774 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. USN, Res Lab, Washington, DC 20375 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EMP Consultants, Gaithersburg, MD 20885 USA. RP Messenger, SR (reprint author), SFA Inc, Largo, MD 20774 USA. EM messenger@nrl.navy.mil; edaburke@rcn.com; Michael.A.Xapsos@nasa.gov; gsummers@ccf.nrl.navy.mil; rwalters@ccf.nrl.navy.mil; Insoo.Jun@jpl.nasa.gov; tj@empc.com NR 12 TC 52 Z9 55 U1 2 U2 10 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 DEC PY 2003 VL 50 IS 6 BP 1919 EP 1923 DI 10.1109/TNS.2003.820762 PN 1 PG 5 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 772JA UT WOS:000188837800028 ER PT J AU Jun, I Xapsos, MA Messenger, SR Burke, EA Walters, RJ Summers, GR Jordan, T AF Jun, I Xapsos, MA Messenger, SR Burke, EA Walters, RJ Summers, GR Jordan, T TI Proton nonionizing energy loss (NIEL) for device applications SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 40th Annual Nuclear and Space Radiation Effects conference CY JUL 21-25, 2003 CL MONTEREY, CALIFORNIA SP IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE MCNPX; nonionizing energy loss (NIEL); ziegler-biersack-littmark (ZBL) screened potential ID INTRANUCLEAR-CASCADE CALCULATION; DISPLACEMENT DAMAGE; SPACE; PARTICLES; SILICON AB The proton-induced nonionizing energy loss (NIEL) for representative device materials, are presented for the energy range between the displacement damage threshold to 1 GeV. All interaction mechanisms (Coulomb and nuclear elastic/nonelastic) are fully accounted, for in the present NIEL calculations. For Coulomb interactions, them Ziegler-Biersack-Littmark (ZBL) screened potential Was used in the lower energy range (<50 MeV) and the relativistic formulation was used in the higher energy range (less than or equal to50 MeV). A charged particle transport code, MCNPX, was used to compute the NIEL due to nuclear interactions. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. SFA Inc, Largo, MD 20774 USA. USN, Res Lab, Washington, DC 20375 USA. EMP Consultants, Gaithersburg, MD USA. RP Jun, I (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Insoo.Jun@jpl.nasa.gov; Michael.A.Xapsos@nasa.gov; messenger@nrl.navy.mil; ed-aburke@rcn.com; rwalters@ccf.nrl.navy.mil; gsummers@ccf.nrl.navy.mil; tj@empc.com NR 25 TC 93 Z9 99 U1 2 U2 9 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 DEC PY 2003 VL 50 IS 6 BP 1924 EP 1928 DI 10.1109/TNS.2003.820760 PN 1 PG 5 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 772JA UT WOS:000188837800029 ER PT J AU Pickel, JC Reed, RA Marshall, PW Jordan, TM Gee, G Fodness, B McKelvey, M McMurray, RE Ennico, KA Johnson, RR McCreight, C AF Pickel, JC Reed, RA Marshall, PW Jordan, TM Gee, G Fodness, B McKelvey, M McMurray, RE Ennico, KA Johnson, RR McCreight, C TI Proton-induced secondary particle environment for infrared sensor applications SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 40th Annual Nuclear and Space Radiation Effects conference CY JUL 21-25, 2003 CL MONTEREY, CALIFORNIA SP IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE delta electrons; infrared detectors; proton testing; secondary electrons; secondary particles ID CHARGE-COLLECTION AB We present measurements of the proton-induced secondary particle environment in the vicinity of an infrared focal plane array. Measurements were made of the energy depositions from secondary electrons and scattered protons from the interior of a cryogenic test dewar using an infrared detector array. The results are compared with model predictions and analyzed for implications to space-based infrared sensors. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. PR&T Inc, Fallbrook, CA 92028 USA. SGT Inc, Greenbelt, MD 20771 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Pickel, JC (reprint author), PR&T Inc, Fallbrook, CA 92028 USA. EM jim@pickel.net RI Ennico, Kimberly/L-9606-2014 NR 4 TC 2 Z9 2 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 DEC PY 2003 VL 50 IS 6 BP 1954 EP 1959 DI 10.1109/TNS.2003.821603 PN 1 PG 6 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 772JA UT WOS:000188837800034 ER PT J AU Marshall, PW Hubbs, JE Arrington, DC Marshall, CJ Reed, RA Gee, G Pickel, JC Ramos, RA AF Marshall, PW Hubbs, JE Arrington, DC Marshall, CJ Reed, RA Gee, G Pickel, JC Ramos, RA TI Proton-induced transients and charge collection measurements in a LWIR HgCdTe focal plane array SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 40th Annual Nuclear and Space Radiation Effects conference CY JUL 21-25, 2003 CL MONTEREY, CALIFORNIA SP IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE infrared detectors; protons; radiation effects ID ENVIRONMENT AB We compare measurements and modeling of 27 and 63 MeV proton-induced transients in a large-format HgCdTe long wavelength infrared (LWIR) focal plane assembly operating at 40 K. Charge collection measurements describe very limited diffusion of carriers to multiple pixels showing significantly reduced particle induced cross-talk for the lateral diffusion structure. C1 NASA, Goddard Space Flight Ctr, Brookneal, VA 24528 USA. Ball Aerosp & Technol Corp, Infrared Radiat Effects Lab, USAF, Res Lab,Space Vehicles Directorate, Albuquerque, NM 87185 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. SGT Inc, Greenbelt, MD 20771 USA. PRT Inc, Fallbrook, CA 92028 USA. USAF, Res Lab, Vehicles Directorate, Infrared Radiat Effects Lab, Kirtland AFB, NM 87117 USA. RP Marshall, PW (reprint author), NASA, Goddard Space Flight Ctr, Brookneal, VA 24528 USA. EM pwmarshall@aol.com; john.hubbs@kirtland.af.mil; doug.arrington@kirtland.af.mil; cmarshall2@aol.com; Robert.Reed@nasa.gov; George.B.Gee.1@gsfc.nasa.gov; jim@pickel.net; rodolfo.ramos@kirtland.af.mil NR 8 TC 7 Z9 7 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 DEC PY 2003 VL 50 IS 6 BP 1968 EP 1973 DI 10.1109/TNS.2003.820749 PN 1 PG 6 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 772JA UT WOS:000188837800036 ER PT J AU Becker, HN Miyahira, TF Johnston, AH AF Becker, HN Miyahira, TF Johnston, AH TI The influence of structural characteristics on the response of silicon avalanche photodiodes to proton irradiation SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 40th Annual Nuclear and Space Radiation Effects conference CY JUL 21-25, 2003 CL MONTEREY, CALIFORNIA SP IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE avalanche photodiodes; dark current; depletion region; ionization damage; noise; protons ID SOLAR-CELLS; DAMAGE COEFFICIENTS; RADIATION; ELECTRON AB Different silicon avalanche photodiode structures are compared for the effects of 51-MeV protons on dark current, photocurrent, and noise. Large differences in depletion region volumes contributed to differences in sensitivity to bulk dark current increases. At high fluences, ionization damage appeared to be the dominant mechanism for dark current increases in some devices. Increases in 1/f-type noise and supplemental gamma ray testing indicate that these high dark current increases are due to surface damage effects. A discussion of structural parameters that may heighten radiation sensitivity is presented, including doping levels and p-n junction termination techniques. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Becker, HN (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Heidi.N.Becker@jpl.nasa.gov; Testsuo.F.Miyahira@jpl.nasa.gov; Allan.H.Johnston@jpl.nasa.gov NR 16 TC 9 Z9 9 U1 0 U2 3 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 DEC PY 2003 VL 50 IS 6 BP 1974 EP 1981 DI 10.1109/TNS.2003.820731 PN 1 PG 8 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 772JA UT WOS:000188837800037 ER PT J AU Swift, GM Levanas, GC Ratliff, JM Johnston, AH AF Swift, GM Levanas, GC Ratliff, JM Johnston, AH TI In-flight annealing of displacement damage in GaAs LEDs: A Galileo story SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 40th Annual Nuclear and Space Radiation Effects conference CY JUL 21-25, 2003 CL MONTEREY, CALIFORNIA SP IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE annealing; electron radiation effects; extraterrestrial radiation effects; light-emitting diodes; nonionizing energy loss (NIEL); proton radiation effects ID LIGHT-EMITTING-DIODES; PROTON DAMAGE; ENERGY-DEPENDENCE AB A recent failure of Galileo's magnetic recorder was attributed to LED degradation. Annealing the culprit OP133 proved successful: irreplaceable data, taken during the encounter with Jupiter's previously unvisited moon Amalthea, was recovered. Annealing test data for both proton and electron displacement damage combined with a simple device temperature model explains some details of the failure and the partial recovery of recorder motor function. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Swift, GM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM gary.m.swift@jpl.nasa.gov NR 12 TC 5 Z9 5 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 DEC PY 2003 VL 50 IS 6 BP 1991 EP 1997 DI 10.1109/TNS.2003.821374 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 772JA UT WOS:000188837800039 ER PT J AU Irom, F Farmanesh, FH Swift, GM Johnston, AH Yoder, GL AF Irom, F Farmanesh, FH Swift, GM Johnston, AH Yoder, GL TI Single-event upset in evolving commercial silicon-on-insulator microprocessor technologies SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 40th Annual Nuclear and Space Radiation Effects conference CY JUL 21-25, 2003 CL MONTEREY, CALIFORNIA SP IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE alpha particles; beams; cosmic rays; cyclotron; heavy ion beams; heavy ions; microprocessors; neutrons; radiation effect; registers; silicon; silicon on insulator; transistors ID SOI TECHNOLOGIES; CIRCUITS; BULK AB Single-event upset effects from heavy ions are measured. for Motorola and IBM silicon-on-insulator (SOI) microprocessors with different feature sizes and core voltages. Multiple-bit upsets in registers and D-cache were measured and compared with single-bit upsets. Also, the scaling,of the cross section with reduction of feature size for SOI microprocessors is discussed. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX USA. RP Irom, F (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM farokh.irom@jpl.nasa.gov; geoffrey.l.yoder@nasa.gov NR 22 TC 11 Z9 11 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 DEC PY 2003 VL 50 IS 6 BP 2107 EP 2112 DI 10.1109/TNS.2003.821820 PN 1 PG 6 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 772JA UT WOS:000188837800056 ER PT J AU Krithivasan, R Niu, GF Cressler, JD Currie, SM Fritz, KE Reed, RA Marshall, PW Riggs, PA Randall, BA Gilbert, B AF Krithivasan, R Niu, GF Cressler, JD Currie, SM Fritz, KE Reed, RA Marshall, PW Riggs, PA Randall, BA Gilbert, B TI An SEU hardening approach for high-speed SiGe HBT digital logic SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 40th Annual Nuclear and Space Radiation Effects Conference CY JUL 21-25, 2003 CL MONTEREY, CA SP IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE charge collection; circuit modeling; current-steering logic; UBT; SiGe; single-event effects (SEE) ID INDUCED CHARGE COLLECTION; SIMULATION AB A new circuit-level single-event upset (SEU) hardening approach for high-speed SiGe HBT current-steering digital logic is introduced and analyzed using both device and circuit simulations. The workhorse D-type flip-flop circuit architecture is modified in order to significantly improve its SEU immunity. Partial elimination of the effect of cross-coupling at the transistor level in the storage cell of this new circuit decreases its vulnerability to SEU. The SEU response of this new circuit is quantitatively compared with three other D flip-flop architectures, including the. unhardened circuit, a conventional NAND gate based circuit, and a current-sharing hardened (CSH) circuit, at both variable data rate and switching current. The new circuit shows substantial improvement in SEU response over the unhardened version, with little increase in layout complexity and power consumption. While the NAND gate based circuit still shows better SEU response than the other circuits, its high power consumption will preclude its use in space applications. Our results suggest that this new circuit architecture exhibits sufficient SEU tolerance, low layout complexity, and modest power,consumption, and thus. should prove suitable for many. space applications requiring very high-speed digital logic. C1 Georgia Inst Technol, Dept Elect & Comp Engn, Atlanta, GA 30332 USA. Auburn Univ, Dept Elect & Comp Engn, Auburn, AL 36849 USA. Mayo Clin & Mayo Fdn, Rochester, MN 55905 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Krithivasan, R (reprint author), Georgia Inst Technol, Dept Elect & Comp Engn, Atlanta, GA 30332 USA. EM ramkumar@ece.gatech.edu RI Krithivasan, Ramkumar/D-3549-2011 NR 8 TC 33 Z9 33 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2003 VL 50 IS 6 BP 2126 EP 2134 DI 10.1109/TNS.2003.822094 PN 1 PG 9 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 772JA UT WOS:000188837800059 ER PT J AU Wang, JJ Wong, W Wolday, S Cronquist, B McCollum, J Katz, R Kleyner, I AF Wang, JJ Wong, W Wolday, S Cronquist, B McCollum, J Katz, R Kleyner, I TI Single event upset and hardening in 0.15 mu m antifuse-based field programmable gate array SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 40th Annual Nuclear and Space Radiation Effects conference CY JUL 21-25, 2003 CL MONTEREY, CALIFORNIA SP IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE antifuse; device simulation; FPGA; radiation hardening; single event effect (SEE); single event upset (SEU) ID TECHNOLOGIES AB The single event effects and hardening of a 0.15 mum antifuse FPGA, the AX device, were investigated by beam test and computer simulation. The beam test showed no permanent damage mode. Functional failures were observed and attributed to the upsets in a control logic circuit, the startup sequencer. Clock upsets were observed and attributed to the single event transients in the clock network. Upsets were also measured in the user hip-flop and embedded SRAM. The hardening technique dealing With each upset mode is discussed in detail. SPICE and three-dimensional mixed-mode simulations were used to determine the design rules for mitigating the multiple upsets due to glancing angle and charge sharing. The hardening techniques have been implemented in the. newly fabricated RTAXS device. Preliminary heavy-ion-beam test data show that all the hard-wired hardening solutions are working successfully. C1 Actel Corp, Mountain View, CA 94043 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Orbital Sci Corp, Greenbelt, MD 20771 USA. RP Wang, JJ (reprint author), Actel Corp, Mountain View, CA 94043 USA. EM jih-jong.wang@actel.com NR 15 TC 9 Z9 9 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 DEC PY 2003 VL 50 IS 6 BP 2158 EP 2166 DI 10.1109/TNS.2003.822090 PN 1 PG 9 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 772JA UT WOS:000188837800063 ER PT J AU Reed, RA Marshall, PW Pickel, JC Carts, MA Fodness, B Niu, GF Fritz, K Vizkelethy, G Dodd, PE Irwin, T Cressler, JD Krithivasan, R Riggs, P Prairie, J Randall, B Gilbert, B LaBel, KA AF Reed, RA Marshall, PW Pickel, JC Carts, MA Fodness, B Niu, GF Fritz, K Vizkelethy, G Dodd, PE Irwin, T Cressler, JD Krithivasan, R Riggs, P Prairie, J Randall, B Gilbert, B LaBel, KA TI Heavy-ion broad-beam and microprobe studies of single-event upsets in 0.20-mu m SiGe heterojunction bipolar transistors and circuits SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 40th Annual Nuclear and Space Radiation Effects conference CY JUL 21-25, 2003 CL MONTEREY, CALIFORNIA SP IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE ground testing; modeling; SiGe; silicon germanium; single event effect; single event upset ID INDUCED CHARGE COLLECTION; LOGIC AB Combining broad-beam circuit level single-event upset (SEU) response with heavy ion microprobe charge collection measurements on single silicon-germanium heterojunction bipolar transistors improves understanding of the charge collection mechanisms responsible for SEU response of digital SiGe HBT technology. This new understanding of the SEU mechanisms shows that the right rectangular parallele-piped model for the sensitive volume is not applicable to this technology. A new first-order physical model is proposed and calibrated with moderate success. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. PR&T, Fallbrook, CA 92028 USA. Raytheon ITSS, Greenbelt, MD 20771 USA. Auburn Univ, Alabama Microelect Sci & Technol Ctr, Dept Elect & Comp Engn, Auburn, AL 36849 USA. Sandia Natl Labs, Albuquerque, NM 87185 USA. Mayo Clin & Mayo Fdn, Rochester, MN 55905 USA. QSS Grp Inc, Greenbelt, MD 20771 USA. Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. RP Reed, RA (reprint author), NASA, Goddard Space Flight Ctr, Code 561-4, Greenbelt, MD 20771 USA. EM robert.a.reed@nasa.gov; pwmarshall@aol.com; jim@pickel.net; mcarts@pop500.jsfc.nasa.gov; varadmu@eng.aubum.edu; randall.Barbara@mayo.edu; gvizkel@sandia.gov; pedodd@sandia.gov; tirwin@pop500.gsfc.nasa.gov; cressler@ece.gatech.edu; Kenneth.A.Label@nasa.gov RI Krithivasan, Ramkumar/D-3549-2011 NR 11 TC 42 Z9 43 U1 0 U2 3 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 DEC PY 2003 VL 50 IS 6 BP 2184 EP 2190 DI 10.1109/TNS.2003.821815 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 772JA UT WOS:000188837800066 ER PT J AU Varadharajaperumal, M Niu, GF Krithivasan, R Cressler, JD Reed, RA Marshall, PW Vizkelethy, G Dodd, PE Joseph, AJ AF Varadharajaperumal, M Niu, GF Krithivasan, R Cressler, JD Reed, RA Marshall, PW Vizkelethy, G Dodd, PE Joseph, AJ TI 3-D simulation of heavy-ion induced charge collection in SiGeHBTs SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 40th Annual Nuclear and Space Radiation Effects conference CY JUL 21-25, 2003 CL MONTEREY, CALIFORNIA SP IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE deep trench; DESSIS; HBT; LET; mesh; polysilicon emitter; shallow trench; SIMS; SRIM; UHV/CVD AB This paper presents the first 3-D simulation of heavy-ion induced charge collection in a SiGe HBT, together with microbeam testing data. The charge collected by the terminals is a strong function of the ion striking position. The sensitive area of charge collection for each terminal is identified based on analysis of the device structure and simulation results. For a normal strike between the deep trench edges, most of the electrons and holes are collected by the collector and substrate terminals, respectively. For an ion strike between the shallow trench edges surrounding the emitter, the base collects appreciable amount of charge. Emitter collects negligible amount of charge. Good agreement is achieved between the experimental and simulated data. Problems encountered with mesh generation and charge collection simulation are also discussed. C1 Auburn Univ, Alabama Microelect Sci & Technol Ctr, Dept Elect & Comp Engn, Auburn, AL 36849 USA. Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Sandia Natl Labs, Albuquerque, NM 87185 USA. IBM Microelect, Essex Jct, VT 05452 USA. RP Varadharajaperumal, M (reprint author), Auburn Univ, Alabama Microelect Sci & Technol Ctr, Dept Elect & Comp Engn, Auburn, AL 36849 USA. EM varadmu@eng.auburn.edu RI Krithivasan, Ramkumar/D-3549-2011 NR 7 TC 23 Z9 24 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 DEC PY 2003 VL 50 IS 6 BP 2191 EP 2198 DI 10.1109/TNS.2003.820775 PN 1 PG 8 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 772JA UT WOS:000188837800067 ER PT J AU Frederickson, AR Dennison, JR AF Frederickson, AR Dennison, JR TI Measurement of conductivity and charge storage in insulators related to spacecraft charging SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 40th Annual Nuclear and Space Radiation Effects conference CY JUL 21-25, 2003 CL MONTEREY, CALIFORNIA SP IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE charge decay; conductivity; dielectrics; electron emission; insulators; resistivity AB Improved experimental methods are discussed for laboratory measurement of conductivity and electric field in insulating spacecraft material intended for space radiation and plasma environments. These measurement techniques investigate the following features: 1) measurements of conductivity are up to four orders of magnitude smaller than those determined by existing standard methods. 2) Conductivity is altered as radiation accumulates and trapping states fill with electrons. 3) With intense kiloelectronvolt electron irradiation, electrons are continually emitted for hours from the,irradiated surface after the irradiation ceases. 4) Charging induced by electron irradiation is strongly modified by the electron-hole pairs that the irradiation generates in the insulator. 5) High field effects at 10(6) V/cm act strongly on the electron-hole pairs and on electrons in shallow traps to provide extended, conductivity. 6) The capacitance of the sample can be measured in the same apparatus along with the other testing. 7) Visible light can be used to investigate conduction by electrons (or holes) emitted from shallow trapping levels. The qualitative physics of such processes in solid dielectrics has long been known, and instrumentation is developed here for measuring the effects in practical spacecraft charging applications. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Utah State Univ, Dept Phys, Logan, UT 84322 USA. RP Frederickson, AR (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM Frederickson@jpl.nasa.gov; physjrd@cc.usu.edu RI Dennison, John/C-1225-2014; OI Dennison, JR/0000-0002-5504-3353 NR 11 TC 37 Z9 43 U1 2 U2 10 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 DEC PY 2003 VL 50 IS 6 BP 2284 EP 2291 DI 10.1109/TNS.2003.821397 PN 1 PG 8 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 772JA UT WOS:000188837800080 ER PT J AU Gersey, B Wilkins, R Huff, H Dwivedi, RC Takala, B O'Donnell, J Wender, SA Singleterry, RC AF Gersey, B Wilkins, R Huff, H Dwivedi, RC Takala, B O'Donnell, J Wender, SA Singleterry, RC TI Correlation of neutron dosimetry using a silicon equivalent proportional counter microdosimeter and SRAM SEU cross sections for eight neutron energy spectra SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 40th Annual Nuclear and Space Radiation Effects conference CY JUL 21-25, 2003 CL MONTEREY, CALIFORNIA SP IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE neutron dosimetry; neutron radiation; silicon microdosimetry; single-event upsets (SEUs) ID DETECTOR AB A silicon equivalent proportional counter microdosimeter (SEPCM) and 4 Mb SRAM were exposed to eight progressively hardened neutron energy spectra at the LANSCE ICE House facility. As the incident neutron energy spectra were hardened, the lineal energy spectra response from the SEPCM changed both in shape and in the number of lineal energy deposition events per incident neutron. The general trend of the 4 Mb SRAM single event upset (SEU) cross section was an increase for harder incident neutron energy spectra. Resulting dosimetric results were correlated to SEU cross sections. C1 Prairie View A&M Univ, NASA, Ctr Appl Radiat Res, Prairie View, TX 77446 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. NASA, Langley Res Ctr, Analyt & Computat Methods Branch, Radiat Phys Grp, Hampton, VA 23681 USA. RP Gersey, B (reprint author), Prairie View A&M Univ, NASA, Ctr Appl Radiat Res, Prairie View, TX 77446 USA. EM buddyhme@hotmail.com; r_wilkins@pvamu.edu; h_huff@pvamu.edu; r_dwivedi@pvamu.edu; takala@lanl.gov; odonnell@lanl.gov; wender@lanl.gov; r.c.singleterry@larc.nasa NR 13 TC 7 Z9 8 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 DEC PY 2003 VL 50 IS 6 BP 2363 EP 2366 DI 10.1109/TNS.2003.821604 PN 1 PG 4 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 772JA UT WOS:000188837800093 ER PT J AU Scheick, L AF Scheick, L TI Microdose analysis of ion strikes on SRAM cells SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 40th Annual Nuclear and Space Radiation Effects conference CY JUL 21-25, 2003 CL MONTEREY, CALIFORNIA SP IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm DE microdose; single hard error; SRAM; stuck bit ID SIMULATION; TRANSISTORS; DOSIMETRY; MOSFETS; LEAKAGE; DAMAGE; MEMORY; ARRAYS AB A method of measuring the effect from exposure to highly localized ionizing radiation on microstructures is described. The voltage at which a commercial SRAM cell cannot hold a programmed state changes with microdose. The microdose distribution across the array, in addition to the analysis of the occurrence of anomalous shifts in operating bias due to rare, large energy-deposition events is studied. The effect of multiple hits on a SRAM cell is presented. A general theory on multiple hits from which basic device parameters can be extracted is presented. SPICE, as well as analysis of basic device physics, is used to analyze the damage to individual transistors and the response of a SRAM cell. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Scheick, L (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM leif.scheick@jpl.nasa.gov NR 25 TC 10 Z9 10 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 DEC PY 2003 VL 50 IS 6 BP 2399 EP 2406 DI 10.1109/TNS.2003.822130 PN 1 PG 8 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 772JA UT WOS:000188837800099 ER PT J AU Messenger, SR Summers, GP Burke, EA Xapsos, MA Walters, RJ Jackson, EM Weaver, BD AF Messenger, SR Summers, GP Burke, EA Xapsos, MA Walters, RJ Jackson, EM Weaver, BD TI Nonionizing energy loss (NIEL) for heavy ions (vol 46, pg 1595, 1999) SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Correction C1 SFA Inc, Largo, MD 20774 USA. USN, Res Lab, Washington, DC 20375 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Messenger, SR (reprint author), SFA Inc, Largo, MD 20774 USA. EM messenger@nrl.navy.mil; gsummers@ccf.nrl.navy.mil; edaburke@rcn.com; Michael.A.Xapsos@nasa.gov; rwalters@ccf.nrl.navy.mil NR 4 TC 1 Z9 1 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 DEC PY 2003 VL 50 IS 6 BP 2494 EP 2494 DI 10.1109/TNS.2003.822035 PN 2 PG 1 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 772JC UT WOS:000188838000015 ER PT J AU Banger, KK Jin, MHC Harris, JD Fanwick, PE Hepp, AF AF Banger, KK Jin, MHC Harris, JD Fanwick, PE Hepp, AF TI A new facile route for the preparation of single-source precursors for bulk, thin-film, and nanocrystallite I-III-VI semiconductors SO INORGANIC CHEMISTRY LA English DT Article ID SOLAR-CELLS; CHALCOPYRITE MATERIALS; SPRAY CVD; CUINS2; DEPOSITION AB We report a new simplified synthetic procedure for commercial manufacture of ternary single-source precursors (SSPs). This new synthetic process has been successfully implemented to fabricate known SSPs on bulk scale and the first liquid SSPs to the semiconductors CuInSe2 and AgInxSy. Single crystal X-ray determination reveals the first unsolvated ternary AgInS SSP. SSPs prepared via this new route have successfully been used in a spray assisted chemical vapor deposition (CVD) process to deposit polycrystalline thin films, and for preparing ternary nanocrystallites. C1 Ohio Aerosp Inst, Cleveland, OH 44142 USA. Ind Technol Inst, Ctr Thin Film & Nanotechnol, Cleveland, OH 44115 USA. Purdue Univ, Xray Facil, W Lafayette, IN 47907 USA. NASA, Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA. RP Banger, KK (reprint author), Ohio Aerosp Inst, 22800 Cedar Point Rd, Cleveland, OH 44142 USA. NR 16 TC 77 Z9 79 U1 2 U2 19 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0020-1669 J9 INORG CHEM JI Inorg. Chem. PD DEC 1 PY 2003 VL 42 IS 24 BP 7713 EP 7715 DI 10.1021/ic034802h PG 3 WC Chemistry, Inorganic & Nuclear SC Chemistry GA 747YL UT WOS:000186833900008 PM 14632481 ER PT J AU Estes, J Wibbels, T Balazs, G AF Estes, J Wibbels, T Balazs, G TI Evaluation of incubation temperatures in green turtle nests at French Frigate Shoals, northwest Hawaiian Islands. SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY 2004 CL New Orleans, LA SP Soc Integrative Comparative Biol C1 Univ Alabama, Birmingham, AL USA. Natl Marine Fisheries Serv, Honolulu, HI USA. NR 0 TC 0 Z9 0 U1 1 U2 3 PU SOC INTEGRATIVE COMPARATIVE BIOLOGY PI MCLEAN PA 1313 DOLLEY MADISON BLVD, NO 402, MCLEAN, VA 22101 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2003 VL 43 IS 6 BP 806 EP 806 PG 1 WC Zoology SC Zoology GA 831ZI UT WOS:000222235200017 ER PT J AU Rivera, G Savitzky, AH Hinkley, JA AF Rivera, G Savitzky, AH Hinkley, JA TI The integument of the common gartersnake (Thamnophis sirtalis): Mechanical properties and the role of skin in feeding SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY 2004 CL New Orleans, LA SP Soc Integrative Comparative Biol C1 Old Dominion Univ, Norfolk, VA 23529 USA. NASA, Langley Res Ctr, Hampton, VA 23665 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU SOC INTEGRATIVE COMPARATIVE BIOLOGY PI MCLEAN PA 1313 DOLLEY MADISON BLVD, NO 402, MCLEAN, VA 22101 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2003 VL 43 IS 6 BP 826 EP 826 PG 1 WC Zoology SC Zoology GA 831ZI UT WOS:000222235200096 ER PT J AU Li, K Li, BQ de Groh, HC AF Li, K Li, BQ de Groh, HC TI Effect of magnetic field on g-jitter induced convection and solute striation during solidification in space SO INTERNATIONAL JOURNAL OF HEAT AND MASS TRANSFER LA English DT Article ID STOCKBARGER CRYSTAL-GROWTH; LOW GRAVITY TOLERANCE; ACCELERATIONS; MICROGRAVITY; SURFACE AB A 2-D finite element model is presented for the melt growth of single crystals in a microgravity environment with a superimposed DC magnetic field. The model is developed using deforming finite element methodology and predicts steady and transient convective flows, heat transfer, solute distribution, and solidification interface morphology associated with the melt growth of single crystals in microgravity with and without an applied magnetic field. Numerical simulations were carried out for a wide range of parameters including idealized microgravity condition, synthesized g-jitter and real g-jitter data taken by on-board accelerometers during space flights. The results reveal that the time varying g-jitter disturbances, although small in magnitude, cause an appreciable convective flow in the liquid pool, which in turn produces detrimental effects during the space processing of single crystal growth. An applied magnetic field of appropriate strength, superimposed on the microgravity, can be very effective in suppressing the deleterious effects resulting from g-jitter disturbances. (C) 2003 Elsevier Ltd. All rights reserved. C1 Washington State Univ, Sch Mech & Mat Engn, Pullman, WA 99163 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Li, BQ (reprint author), Washington State Univ, Sch Mech & Mat Engn, Pullman, WA 99163 USA. EM li@mme.wsu.edu NR 23 TC 6 Z9 6 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0017-9310 J9 INT J HEAT MASS TRAN JI Int. J. Heat Mass Transf. PD DEC PY 2003 VL 46 IS 25 BP 4799 EP 4811 DI 10.1016/S0017-9310(03)00336-3 PG 13 WC Thermodynamics; Engineering, Mechanical; Mechanics SC Thermodynamics; Engineering; Mechanics GA 724QR UT WOS:000185498700005 ER PT J AU Burt, RR Christiansen, EL AF Burt, RR Christiansen, EL TI An enhanced shutter to protect spacecraft windows from meteoroids and orbital debris SO INTERNATIONAL JOURNAL OF IMPACT ENGINEERING LA English DT Article; Proceedings Paper CT Hypervelocity Impact Symposium CY DEC 07-11, 2003 CL NOORDWIJK, NETHERLANDS DE shielding; meteoroid/orbital debris protection; ballistic limit equations AB Conventional spacecraft window shutters are relatively thin aluminum covers (0.1cm to 0.2cm thick), which provide only modest protection from meteoroid/orbital debris (M/OD) impacts. This paper provides results of an intensive effort to develop an improved shutter design capable of protecting fused-silica glass windows from 1.3cm diameter aluminum projectiles impacting at 7 km/s. Hypervelocity impact tests on a number of shutter concepts under a variety of impact conditions are described. Ballistic limit equations are defined that allow assessment of impact damage to shutter protected spacecraft windows. An immediate application for the enhanced shutter design is to provide robust meteoroid/debris protection for windows of the International Space Station (ISS) Cupola. Enhanced shutter designs provided here would be applicable to protecting other spacecraft windows and sensitive surfaces, whenever high levels of reliability and M/OD protection are desired. (C) 2003 Published by Elsevier Ltd. C1 Boeing Co, Houston, TX 77059 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Burt, RR (reprint author), Boeing Co, Mail Code HM5-20,13100 Space Ctr Blvd, Houston, TX 77059 USA. NR 5 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 0734-743X J9 INT J IMPACT ENG JI Int. J. Impact Eng. PD DEC PY 2003 VL 29 IS 1-10 BP 139 EP 152 DI 10.1016/j.ijimpeng.2003.09.013 PG 14 WC Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA 753LC UT WOS:000187232000012 ER PT J AU Burt, RR Christiansen, EL AF Burt, RR Christiansen, EL TI Hypervelocity impact testing of transparent spacecraft materials SO INTERNATIONAL JOURNAL OF IMPACT ENGINEERING LA English DT Article; Proceedings Paper CT Hypervelocity Impact Symposium CY DEC 07-11, 2003 CL NOORDWIJK, NETHERLANDS DE shielding; meteoroid/orbital debris; penetration equations; glass; fused-silica; polycarbonate AB Transparent materials have been used by NASA as windows since the beginning of the Human Space Flight Program. This paper provides results of an intensive effort to determine hypervelocity impact characteristics and develop damage equations for transparent materials currently used on the International Space Station and Space Shuttle programs. The materials considered here are fused silica glass, tempered glass, and polycarbonate. Hypervelocity impact tests on these materials under a variety of impact conditions are described. Penetration equations are defined that allow assessment of impact damage to windows and are useful in BUMPER code meteoroid/orbital debris (M/OD) assessments. (C) 2003 Published by Elsevier Ltd. C1 Boeing Co, Houston, TX 77059 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Burt, RR (reprint author), Boeing Co, Mail Code HM5-20,13100 Space Ctr Blvd, Houston, TX 77059 USA. NR 10 TC 12 Z9 12 U1 1 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0734-743X J9 INT J IMPACT ENG JI Int. J. Impact Eng. PD DEC PY 2003 VL 29 IS 1-10 BP 153 EP 166 DI 10.1016/j.ijimpeng.2003.09.014 PG 14 WC Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA 753LC UT WOS:000187232000013 ER PT J AU Davison, D Cour-Palais, B Quan, XY Holmquist, TJ Cohen, LM Ramsey, R Cummings, R AF Davison, D Cour-Palais, B Quan, XY Holmquist, TJ Cohen, LM Ramsey, R Cummings, R TI Computer models of micrometeoroid impact on fused silica glass mirrors SO INTERNATIONAL JOURNAL OF IMPACT ENGINEERING LA English DT Article; Proceedings Paper CT Hypervelocity Impact Symposium CY DEC 07-11, 2003 CL NOORDWIJK, NETHERLANDS DE micrometeoroid; impact; glass; equation of state; constitutive model; mirror; JWST AB Analysis of impacts on fused silica was motivated by the design of the mirror for the James Webb Space Telescope (JWST). The JWST is expected to have a large-diameter mirror shaded from sunlight but open to space. One of the candidate mirror materials is fused silica; the other candidate materials are ultra-low expansion (ULE) glass and O-30 beryllium. Historically, most meteoroid tests have concerned themselves with the degraded strength of the substrate; JWST is primarily concerned with maintaining its precise optical figure. Micrometeoroids can have velocities of 50 km/s or higher. Although the velocity in the analysis did not exceed 10 km/s, the computer model included a fit to shock Hugoniot data for fused silica with pressures as high as 700 GPa, typical of impacts at velocities higher than 10 km/s. The computer model also included the first-order phase transformation observed in fused silica. The calculations were made with the AUTODYN hydrocode [1], which includes smooth particle hydrodynamic (SPH) and Lagrange solvers with other modules and features for coupling them together. For the analysis of impact, both SPH and Lagrange methods were used. Using the static relaxation option, the analysis continued from crater formation to a late-time static solution from which the effect of the impact on the optics could be determined. Both low and high energy impacts were computed using the fused silica model. For the low energy impact, the computed crater depth, crater diameter, and spall diameter closely matched both historical data for fused silica and values measured by Auburn University/ Hypervelocity Impact Facility (AU/HIF) for two typical fused silica sites and one ULE site. For the high energy impact, the computed values matched historical data for fused silica but not the data measured by AU/HIF for three typical ULE sites. The discrepancy can be explained by the difference in the response of fused silica and ULE under impact, as seen in historical trends and as observed by AU/HIF. Optical interferometry of the surfaces of one of the mirrors revealed deformation in the vicinity of particle impacts that matched that estimated with a static model, and the deformation was consistent with that computed by AUTODYN. (C) 2003 Published by Elsevier Ltd. C1 Shock Transients Inc, Hopkins, MN 55434 USA. Century Dynam Inc, Concord, CA 94520 USA. SAO, Cambridge, MA 02138 USA. Auburn Univ, Space Res Inst, Leach Sci Ctr 231, Auburn, AL 36849 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Davison, D (reprint author), Shock Transients Inc, POB 5357, Hopkins, MN 55434 USA. NR 9 TC 13 Z9 13 U1 0 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0734-743X J9 INT J IMPACT ENG JI Int. J. Impact Eng. PD DEC PY 2003 VL 29 IS 1-10 BP 203 EP 214 DI 10.1016/j.ijimpeng.2003.09.017 PG 12 WC Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA 753LC UT WOS:000187232000016 ER PT J AU Gurzadyan, VG Ade, PAR De Bernardis, P Bianco, CL Bock, JJ Boscaleri, A Crill, BP De Troia, G Ganga, K Giacometti, M Hivon, E Hristov, VV Kashin, AL Lange, AE Masi, S Mauskopf, PD Montroy, T Natoli, P Netterfield, CB Pascale, E Piacentini, F Polenta, G Ruhl, J AF Gurzadyan, VG Ade, PAR De Bernardis, P Bianco, CL Bock, JJ Boscaleri, A Crill, BP De Troia, G Ganga, K Giacometti, M Hivon, E Hristov, VV Kashin, AL Lange, AE Masi, S Mauskopf, PD Montroy, T Natoli, P Netterfield, CB Pascale, E Piacentini, F Polenta, G Ruhl, J TI Ellipticity analysis of the BOOMERanG CMB maps SO INTERNATIONAL JOURNAL OF MODERN PHYSICS D LA English DT Article DE cosmic microwave background ID MICROWAVE BACKGROUND-RADIATION; ANGULAR POWER SPECTRUM; MULTIPLE PEAKS; GAUSSIANITY; COSMOLOGY; SPACE; STATISTICS; CURVATURE; UNIVERSE AB The properties of the Cosmic Microwave Background (CMB) maps carry valuable cosmological information. Here we report the results of the analysis hot and cold CMB anisotropy spots in the BOOMERanG 150 GHz map in terms of number, area, ellipticity, vs. temperature threshold. We carried out this analysis for the map obtained by summing independent measurement channels (signal plus noise map) and for a comparison map (noise only map) obtained by differencing the same channels. The anisotropy areas (spots) have been identified for both maps for various temperature thresholds and a catalog of the spots has been produced. The orientation (obliquity) of the spots is random for both maps. We computed the mean elongation of spots obtained from the maps at a given temperature threshold using a simple estimator. We found that for the sum map there is a region of temperature thresholds where the average elongation is not dependent on the threshold. Its value is similar to 2.3 for cold areas and similar to 2.2 for hot areas. This is a non-trivial result. The bias of the estimator is less than or similar to +0.4 for areas of size less than or similar to 30', and smaller for larger areas. The presence of noise also biases the ellipticity by less than or similar to +0.3. These biases have not been subtracted in the results quoted above. The threshold independent and random obliquity behaviour in the sum map is stable against pointing reconstruction accuracy and noise level of the data, thus confirming that these are actual properties of the dataset. The data used here give a hint of high ellipticity for the largest spots. Analogous elongation properties of CMB anisotropies had been detected for COBE-DMR 4 year data. If this is due to geodesics mixing, it would point to a non zero curvature of the Universe. C1 Yerevan Phys Inst, Yerevan, Armenia. Univ Roma La Sapienza, Dipartimento Fis, ICRA, I-00185 Rome, Italy. Dept Phys & Astron, Cardiff, S Glam, Wales. Univ Roma La Sapienza, Dipartimento Fis, Rome, Italy. JPL, Pasadena, CA USA. CNR, IROE, I-50127 Florence, Italy. CALTECH, Pasadena, CA 91125 USA. IPAC, Pasadena, CA USA. Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. Dipartimento Fis, Rome, Italy. Univ Toronto, Dept Phys, Toronto, ON, Canada. RP Gurzadyan, VG (reprint author), Yerevan Phys Inst, Yerevan, Armenia. RI Piacentini, Francesco/E-7234-2010; OI Piacentini, Francesco/0000-0002-5444-9327; de Bernardis, Paolo/0000-0001-6547-6446; Masi, Silvia/0000-0001-5105-1439; Polenta, Gianluca/0000-0003-4067-9196; Hivon, Eric/0000-0003-1880-2733 NR 38 TC 11 Z9 11 U1 0 U2 1 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA JOURNAL DEPT PO BOX 128 FARRER ROAD, SINGAPORE 912805, SINGAPORE SN 0218-2718 J9 INT J MOD PHYS D JI Int. J. Mod. Phys. D PD DEC PY 2003 VL 12 IS 10 BP 1859 EP 1873 DI 10.1142/S0218271803004419 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 773YB UT WOS:000188952000004 ER PT J AU Loeb, NG Loukachine, K Manalo-Smith, N Wielicki, BA Young, DF AF Loeb, NG Loukachine, K Manalo-Smith, N Wielicki, BA Young, DF TI Angular distribution models for top-of-atmosphere radiative flux estimation from the Clouds and the Earth's Radiant Energy System instrument on the Tropical Rainfall Measuring Mission satellite. Part II: Validation SO JOURNAL OF APPLIED METEOROLOGY LA English DT Article ID BUDGET EXPERIMENT; SCENE IDENTIFICATION; IRIS HYPOTHESIS; ZENITH ANGLE; ERBE; ALGORITHMS; DEPENDENCE; FEEDBACK; CLIMATE; SCANNER AB Top-of-atmosphere (TOA) radiative fluxes from the Clouds and the Earth's Radiant Energy System (CERES) are estimated from empirical angular distribution models (ADMs) that convert instantaneous radiance measurements to TOA fluxes. This paper evaluates the accuracy of CERES TOA fluxes obtained from a new set of ADMs developed for the CERES instrument onboard the Tropical Rainfall Measuring Mission (TRMM). The uncertainty in regional monthly mean reflected shortwave ( SW) and emitted longwave ( LW) TOA fluxes is less than 0.5W m(-2), based on comparisons with TOA fluxes evaluated by direct integration of the measured radiances. When stratified by viewing geometry, TOA fluxes from different angles are consistent to within 2% in the SW and 0.7% (or 2 W m(-2)) in the LW. In contrast, TOA fluxes based on ADMs from the Earth Radiation Budget Experiment (ERBE) applied to the same CERES radiance measurements show a 10% relative increase with viewing zenith angle in the SW and a 3.5% (9 W m(-2)) decrease with viewing zenith angle in the LW. Based on multiangle CERES radiance measurements, 18 regional instantaneous TOA flux errors from the new CERES ADMs are estimated to be < 10 W m(-2) in the SW and <3.5 W m(-2) in the LW. The errors show little or no dependence on cloud phase, cloud optical depth, and cloud infrared emissivity. An analysis of cloud radiative forcing (CRF) sensitivity to differences between ERBE and CERES TRMM ADMs, scene identification, and directional models of albedo as a function of solar zenith angle shows that ADM and clear-sky scene identification differences can lead to an 8 W m(-2) root-mean-square (rms) difference in 1degrees daily mean SW CRF and a 4 W m(-2) rms difference in LW CRF. In contrast, monthly mean SW and LW CRF differences reach 3 W m(-2). CRF is found to be relatively insensitive to differences between the ERBE and CERES TRMM directional models. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. Sci Applicat Int Corp, Hampton, VA USA. Analyt Serv & Mat Inc, Hampton, VA 23666 USA. RP Loeb, NG (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA. NR 34 TC 52 Z9 52 U1 2 U2 4 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8763 J9 J APPL METEOROL JI J. Appl. Meteorol. PD DEC PY 2003 VL 42 IS 12 BP 1748 EP 1769 DI 10.1175/1520-0450(2003)042<1748:ADMFTR>2.0.CO;2 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 749FJ UT WOS:000186908300005 ER PT J AU Gebremichael, M Krajewski, WF Morrissey, M Langerud, D Huffman, GJ Adler, R AF Gebremichael, M Krajewski, WF Morrissey, M Langerud, D Huffman, GJ Adler, R TI Error uncertainty analysis of GPCP monthly rainfall products: A data-based simulation study SO JOURNAL OF APPLIED METEOROLOGY LA English DT Article ID PRECIPITATION CLIMATOLOGY PROJECT; VERIFICATION; COEFFICIENTS; NETWORKS; SPACE; TIME AB This paper focuses on estimating the error uncertainty of the monthly 2.5degrees x 2.5degrees rainfall products of the Global Precipitation Climatology Project (GPCP) using rain gauge observations. Two kinds of GPCP products are evaluated: the satellite-only ( MS) product, and the satellite-gauge (SG) merged product. The error variance separation (EVS) method has been proposed previously as a means of estimating the error uncertainty of the GPCP products. In this paper, the accuracy of the EVS results is examined for a variety of gauge densities. Three validation sites-two in North Dakota and one in Thailand-all with a large number of rain gauges, were selected. The very high density of the selected sites justifies the assumption that the errors are negligible if all gauges are used. Monte Carlo simulation studies were performed to evaluate sampling uncertainty for selected rain gauge network densities. Results are presented in terms of EVS error uncertainty normalized by the true error uncertainty. These results show that the accuracy of the EVS error uncertainty estimates for the SG product differs from that of the MS product. The key factors that affect the errors of the EVS results, such as the gauge density, the gauge network, and the sample size, have been identified and their influence has been quantified. One major finding of this study is that 8-10 gauges, at the 2.5degrees scale, are required as a minimum to get good error uncertainty estimates for the SG products from the EVS method. For eight or more gauges, the normalized error uncertainty is about 0.86 +/- 0.10 (North Dakota: box 1) and 0.95 +/- 0.10 (North Dakota: box 2). Results show that, despite its error, the EVS method performs better than the root-mean-square error (rmse) approach that ignores the rain gauge sampling error. For the MS products, both the EVS method and the rmse approach give negligible bias. As expected, results show that the SG products give better rainfall estimates than the MS products, according to most of the criteria used. C1 Univ Iowa, Iowa City, IA 52242 USA. Univ Oklahoma, Environm Verificat & Anal Ctr, Norman, OK 73019 USA. N Dakota Atmospher Resource Board, Bismarck, ND USA. Sci Syst & Applicat Inc, Greenbelt, MD USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Krajewski, WF (reprint author), Univ Iowa, Iowa City, IA 52242 USA. RI Gebremichael, Mekonnen/B-3584-2009; Huffman, George/F-4494-2014 OI Huffman, George/0000-0003-3858-8308 NR 23 TC 39 Z9 42 U1 0 U2 8 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8763 J9 J APPL METEOROL JI J. Appl. Meteorol. PD DEC PY 2003 VL 42 IS 12 BP 1837 EP 1848 DI 10.1175/1520-0450(2003)042<1837:EUAOGM>2.0.CO;2 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 749FJ UT WOS:000186908300010 ER PT J AU Yang, RQ Qiu, YM AF Yang, RQ Qiu, YM TI Bipolar cascade lasers with quantum well tunnel junctions SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID 2 MU-M; DIODE-LASERS; OPERATION AB Bipolar cascade lasers with quantum wells (QWs) in tunnel junctions are proposed and demonstrated with emission wavelength near 2 mum based on an InGaAs/InP material system. These bipolar cascade lasers with QW tunnel junctions exhibited superior performance characteristics such as significantly reduced threshold voltage, increased quantum efficiency (>100%) and operation temperature over similar lasers without a QW in the tunnel junction. These broad-area lasers operated at temperatures up to 240 K in continuous wave mode and up to room temperature in pulsed mode. (C) 2003 American Institute of Physics. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Yang, RQ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 16 TC 9 Z9 9 U1 1 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 0021-8979 J9 J APPL PHYS JI J. Appl. Phys. PD DEC 1 PY 2003 VL 94 IS 11 BP 7370 EP 7372 DI 10.1063/1.1624478 PG 3 WC Physics, Applied SC Physics GA 742AM UT WOS:000186492600060 ER PT J AU Plaut, K Maple, RL Wade, CE Baer, LA Ronca, AE AF Plaut, K Maple, RL Wade, CE Baer, LA Ronca, AE TI Effects of hypergravity on mammary metabolic function: gravity acts as a continuum SO JOURNAL OF APPLIED PHYSIOLOGY LA English DT Article DE gravity; mammary gland; rat ID FEMALE RATS; PROLACTIN; SPACEFLIGHT; LACTATION; PREGNANCY AB Mammary metabolic activity in pregnant rats is significantly increased in response to space-flight. To determine whether changes in mammary metabolism are related to gravity load, we exposed pregnant rats to hypergravity and measured mammary metabolic activity. From days 11-20 of gestation (G), animals were centrifuged (20 rpm; 1.5, 1.75, or 2.0 X gravity) or were maintained at I G. On G20, five rats from each group were removed from the centrifuge and euthanized. The remaining dams (n = 5/treatment) were housed at 1 G until parturition. After 2 h of nursing by the pups, the postpartum dams were euthanized (G22). Glucose oxidation to CO2 and incorporation into lipids was measured. Mammary glands from dams euthanized on G20 revealed a strong negative correlation between metabolic rate and increased G load. Approximately 98% of the variation in glucose oxidation and 94% of the variation in glucose incorporation into lipids can be accounted for by differences in G load. Differences in metabolic activity disappeared in the postpartum dams. When we combined previous data from the microgravity with hypergravity environments and plotted the ratio of mammary metabolic rate vs. G load, there was a significant exponential relationship (r(2) = 0.99). These data demonstrate a remarkable continuum of response across the microgravity and hypergravity environments and support the concept that gravitational load influences mammary tissue metabolism. C1 Univ Vermont, Burlington, VT 05405 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Plaut, K (reprint author), Univ Vermont, 570 Main St, Burlington, VT 05405 USA. NR 15 TC 14 Z9 15 U1 0 U2 3 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 DEC PY 2003 VL 95 IS 6 BP 2350 EP 2354 DI 10.1152/japplphysiol.00287.2003 PG 5 WC Physiology; Sport Sciences SC Physiology; Sport Sciences GA 750PF UT WOS:000187004400024 PM 12923115 ER PT J AU Harrison, BC Allen, DL Girten, B Stodieck, LS Kostenuik, PJ Bateman, TA Morony, S Lacey, D Leinwand, LA AF Harrison, BC Allen, DL Girten, B Stodieck, LS Kostenuik, PJ Bateman, TA Morony, S Lacey, D Leinwand, LA TI Skeletal muscle adaptations to microgravity exposure in the mouse SO JOURNAL OF APPLIED PHYSIOLOGY LA English DT Article DE animal enclosure module ID MYOSIN HEAVY-CHAIN; SPACE-SHUTTLE FLIGHT; GROWTH-FACTOR-I; METABOLIC PROPERTIES; HINDLIMB SUSPENSION; APPLIED PHYSIOLOGY; GENETIC MODELS; C57BL/6 MOUSE; MHC ISOFORMS; SPACEFLIGHT AB To investigate the effects of microgravity on murine skeletal muscle fiber size, muscle contractile protein, and enzymatic activity, female C57BL/6J mice, aged 64 days, were divided into animal enclosure module (AEM) ground control and spaceflight (SF) treatment groups. SF animals were flown on the space shuttle Endeavour (STS-108/UF-1) and subjected to similar to11 days and 19 h of microgravity. Immunohistochemical analysis of muscle fiber cross-sectional area revealed that, in each of the muscles analyzed, mean muscle fiber cross-sectional area was significantly reduced (P < 0.0001) for all fiber types for SF vs. AEM control. In the soleus, immunohistochemical analysis of myosin heavy chain (MHC) isoform expression revealed a significant increase in the percentage of muscle fibers expressing MHC IIx and MHC Ilb (P < 0.05). For the gastrocnemius and plantaris, no significant changes in MHC isoform expression were observed. For the muscles analyzed, no alterations in MHC I or MHC IIa protein expression were observed. Enzymatic analysis of the gastrocnemius revealed a significant decrease in citrate synthase activity in SF vs. AEM control. C1 Univ Colorado, Dept Mol Cellular & Dev Biol, Boulder, CO 80309 USA. Univ Colorado, Dept Kinesiol & Appl Physiol, Boulder, CO 80309 USA. Univ Colorado, Dept BioServe Space Technol, Boulder, CO 80309 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Amgen Inc, Metab Disorders Res, Thousand Oaks, CA 91320 USA. Clemson Univ, Dept Bioengn, Clemson, SC 29634 USA. RP Leinwand, LA (reprint author), Univ Colorado, Dept Mol Cellular & Dev Biol, Boulder, CO 80309 USA. NR 53 TC 42 Z9 48 U1 1 U2 4 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 DEC PY 2003 VL 95 IS 6 BP 2462 EP 2470 DI 10.1152/japplphysiol.00603.2003 PG 9 WC Physiology; Sport Sciences SC Physiology; Sport Sciences GA 750PF UT WOS:000187004400038 PM 12882990 ER PT J AU Nalli, NR Smith, WL AF Nalli, NR Smith, WL TI Retrieval of ocean and lake surface temperatures from hyperspectral radiance observations SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID HIGH-RESOLUTION RADIOMETER; TRACK SCANNING RADIOMETER; WATER-VAPOR CORRECTION; DATA-BUOY-CENTER; SEA-SURFACE; SATELLITE RETRIEVALS; MODEL; EMISSIVITY; SPECTRORADIOMETER; INTERFEROMETER AB This paper advances hyperspectral infrared (IR) radiative transfer techniques for retrieving water ( ocean and lake) surface skin temperature from clear-sky radiance observations obtained within the longwave atmospheric window region (800 - 1000 cm(-1)). High spectral resolution has optimal potential for multispectral algorithms because of the capability to resolve, and thus avoid, gas absorption lines that otherwise obscure the surface signal in conventional narrowband radiometers. A hyperspectral radiative transfer model (RTM) is developed for varying satellite zenith angles, atmospheric profiles ( cloud and aerosol free), surface wind speeds and skin temperatures, with atmospheric column transmittance spectra computed from fast models. Wind speed variations in surface emissivity and quasi-specular reflection are both rigorously accounted for. The RTM is then used for deriving retrieval algorithms based upon statistical and physical methodologies. The statistical method is based upon linear regression analyses of brightness temperatures, whereas the physical method is based upon solution of a linear perturbation form of the IR radiative transfer equation valid for window channels. The physical method is unique in its simplicity: It does not solve for atmospheric profiles, but rather relies upon local linearities about guess transmittances for extrapolating the skin temperature. Both algorithms are tested against independent forward calculations and then used to retrieve water surface skin temperatures from the National Polar-orbiting Operational Environmental Satellite System (NPOESS) Airborne Sounder Testbed-Interferometer (NAST-I) flown on board the NASA ER-2. The results demonstrate the capability of hyperspectral radiative transfer for providing an optimal correction for atmospheric gas absorption ( viz., water vapor) from the new suite of environmental satellite IR spectrometers. C1 Univ Wisconsin, Dept Atmospher & Ocean Sci, Madison, WI USA. NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Nalli, NR (reprint author), NOAA, Cooperat Inst Res Atmosphere, NESDIS, ORA, E-RA3,5200 Auth Rd,Room 603-9, Camp Springs, MD 20746 USA. RI Nalli, Nicholas/F-6731-2010 OI Nalli, Nicholas/0000-0002-6914-5537 NR 41 TC 7 Z9 7 U1 0 U2 4 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD DEC PY 2003 VL 20 IS 12 BP 1810 EP 1825 DI 10.1175/1520-0426(2003)020<1810:ROOALS>2.0.CO;2 PG 16 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 758UE UT WOS:000187668000009 ER PT J AU Pickett, MH Tang, WQ Rosenfeld, LK Wash, CH AF Pickett, MH Tang, WQ Rosenfeld, LK Wash, CH TI QuikSCAT satellite comparisons with nearshore buoy wind data off the US West Coast SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID UPWELLING REGION; SCATTEROMETER; CALIFORNIA; NSCAT; TEMPERATURE; ATMOSPHERE; SEAWINDS; ACCURACY; SCHEME; STRESS AB To determine the accuracy of nearshore winds from the QuikSCAT satellite, winds from three satellite datasets ( scientifically processed swath, gridded near-real-time, and gridded science datasets) were compared to those from 12 nearshore and 3 offshore U. S. West Coast buoys. Satellite observations from August 1999 to December 2000 that were within 25 km and 30 min of each buoy were used. Comparisons showed that satellite - buoy wind differences near shore were larger than those offshore. Editing the satellite data by discarding observations recorded in rain and those recorded in light winds improved the accuracy of all three datasets. After removing rain-flagged data and wind speeds less than 3 m s(-1), root-mean-squared differences (satellite minus buoy) for swath data, the best of the three datasets, were 1.4 m s(-1) and 37degrees based on 5741 nearshore comparisons. By removing winds less than 6 m s(-1), these differences were reduced to 1.3 m s(-1) and 26degrees. At the three offshore buoys, the root-mean-squared differences for the swath data, with both rain and winds less than 6 m s(-1) removed, were 1.0 m s(-1) and 15degrees based on 1920 comparisons. Although the satellite's scientifically processed swath data near shore do not match buoy observations as closely as those offshore, they are sufficiently accurate for many coastal studies. C1 NOAA Fisheries, Pacific Fisheries Environm Lab, Pacific Grove, CA 93950 USA. CALTECH, Jet Prop Lab, Pasadena, CA USA. USN, Dept Oceanog, Postgrad Sch, Monterey, CA 93943 USA. USN, Dept Meteorol, Postgrad Sch, Monterey, CA 93943 USA. RP Pickett, MH (reprint author), NOAA Fisheries, Pacific Fisheries Environm Lab, 1352 Lighthouse Ave, Pacific Grove, CA 93950 USA. NR 34 TC 82 Z9 83 U1 0 U2 2 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD DEC PY 2003 VL 20 IS 12 BP 1869 EP 1879 DI 10.1175/1520-0426(2003)020<1869:QSCWNB>2.0.CO;2 PG 11 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 758UE UT WOS:000187668000013 ER PT J AU Smith, SM Davis-Street, JE Fesperman, JV Calkins, DS Bawa, M Macias, BR Meyer, RS Hargens, AR AF Smith, SM Davis-Street, JE Fesperman, JV Calkins, DS Bawa, M Macias, BR Meyer, RS Hargens, AR TI Evaluation of treadmill exercise in a lower body negative pressure chamber as a countermeasure for weightlessness-induced bone loss: A bed rest study with identical twins SO JOURNAL OF BONE AND MINERAL RESEARCH LA English DT Article DE spaceflight; bed rest; simulated weightlessness; bone resorption; bone markers ID SPACE-FLIGHT; UPRIGHT EXERCISE; SIMULATED MICROGRAVITY; BIOCHEMICAL MARKERS; COLLAGEN TURNOVER; CALCIUM; COSMONAUTS; RESORPTION; METABOLISM; BEARING AB Introduction: Bone loss is one of the greatest physiological challenges for extended-duration space missions. The ability of exercise to counteract weightlessness-induced bone loss has been studied extensively, but to date, it has proven ineffective. We evaluated the effectiveness of a combination of two countermeasures-treadmill exercise while inside a lower body negative pressure (LBNP) chamber-on bone loss during a 30-day bed rest study. Materials and Methods: Eight pairs of identical twins were randomized into sedentary (SED) or exercise/LBNP (EX/LBNP) groups. Blood and urine samples were collected before, several times during, and after the 30-day bed rest period. These samples were analyzed for markers of bone and calcium metabolism. Repeated measures ANOVA was used to determine statistical significance. Because identical twins were used, both time and group were treated as repeated variables. Results: Markers of bone resorption were increased during bed rest in samples from sedentary subjects, including the collagen cross-links and serum and urinary calcium concentrations. For N-telopeptide and deoxypyridinoline, there were significant (p < 0.05) interactions between group (SED versus EX/LBNP) and phase of the study (sample collection point). Pyridinium cross-links were increased above pre-bed rest levels in both groups, but the EX/LBNP group had a smaller increase than the SED group. Markers of bone formation were unchanged by bed rest in both groups. Conclusions: These data show that this weight-bearing exercise combined with LBNP ameliorates some of the negative effects of simulated weightlessness on bone metabolism. This protocol may pave the way to counteracting bone loss during spaceflight and may provide valuable information about normal and abnormal bone physiology here on Earth. C1 NASA, Lyndon B Johnson Space Ctr, Nutrit Biochem Lab, Human Adaptat & Countermeasures Off, Houston, TX 77058 USA. Enterprise Advis Serv Inc, Crew Hlth & Res Dept, Houston, TX USA. Wyle Labs, Dept Engn, Houston, TX USA. Univ Calif San Diego, Med Ctr, Dept Orthopaed, San Diego, CA 92103 USA. RP Smith, SM (reprint author), NASA, Lyndon B Johnson Space Ctr, Nutrit Biochem Lab, Human Adaptat & Countermeasures Off, Mail Code SK3, Houston, TX 77058 USA. FU NCRR NIH HHS [M01-RR00827] NR 47 TC 57 Z9 61 U1 1 U2 6 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 DEC PY 2003 VL 18 IS 12 BP 2223 EP 2230 DI 10.1359/jbmr.2003.18.12.2223 PG 8 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 745WB UT WOS:000186712700016 PM 14672358 ER PT J AU Gutsev, GL Bauschlicher, CW Zhai, HJ Wang, LS AF Gutsev, GL Bauschlicher, CW Zhai, HJ Wang, LS TI Structural and electronic properties of iron monoxide clusters FenO and FenO- (n=2-6): A combined photoelectron spectroscopy and density functional theory study SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID TRANSITION-METAL CLUSTERS; GAUSSIAN-BASIS SETS; CORRELATION-ENERGY; GROUND-STATE; OXIDE; FEO; APPROXIMATION; ATOMS; THERMOCHEMISTRY; REPRESENTATION AB We report a combined anion photoelectron spectroscopy and density functional theory (DFT) study on a series of iron monoxide clusters, FenO (n=2-6). Well-resolved photoelectron spectra were obtained for FenO- at variable detachment energies, allowing the ground state and numerous low-lying excited states of FenO to be observed. Sharp threshold photoelectron features were obtained for each species, which suggest rather small geometry changes between the anion and neutral ground states for the monoxide clusters and allows the electron affinities of the neutral clusters to be measured accurately. Extensive DFT calculations using the generalized gradient approximation were carried out for both FenO and FenO-. Optimized geometries of the ground and lowest excited states of both the anion and neutral species are reported along with the ground-state vibrational frequencies and fragmentation energies. Theoretical electron affinities were compared with the experimental measurements to verify the ground states of the iron monoxide clusters obtained from the DFT calculations. (C) 2003 American Institute of Physics. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Washington State Univ, Dept Phys, Richland, WA 99352 USA. Pacific NW Natl Lab, WR Wiley Environm Mol Sci Lab, Richland, WA 99352 USA. RP Gutsev, GL (reprint author), NASA, Ames Res Ctr, Mail Stop 230-3, Moffett Field, CA 94035 USA. NR 42 TC 32 Z9 32 U1 1 U2 14 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD DEC 1 PY 2003 VL 119 IS 21 BP 11135 EP 11145 DI 10.1063/1.1621856 PG 11 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 742AN UT WOS:000186492900017 ER PT J AU Bihary, Z Chaban, GM Gerber, RB AF Bihary, Z Chaban, GM Gerber, RB TI Delayed formation dynamics of HArF and HKrF in rare-gas matrices SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID CHARGE-TRANSFER MOLECULES; TRANSITION-STATE THEORY; SOLID MATRICES; VIBRATIONAL SPECTROSCOPY; ATOMIC-HYDROGEN; KRYPTON; XE; ARGON; KR; PHOTODISSOCIATION AB HArF and HKrF are chemically bound rare-gas compounds that have been produced by photolysis of HF and subsequent thermal annealing in the respective rare-gas matrices. In this paper we present a computational study of the delayed, thermally induced formation of these molecules in the matrix. Using realistic potentials for the molecular and guest-host interactions, the potential energy along the minimum energy paths for formation is evaluated, and thermal transition rates are computed using a Monte Carlo transition state method. A closely packed, dissociated configuration of the molecular fragments is found to play an important role, both as the possible trapping site of the photolyzed fragments, and as an intermediate structure for diffusion-controlled formation. The computed threshold temperatures of formation for the HArF and HKrF molecules at different matrix sites are in good agreement with experimental findings and with previous site assignments for these molecules. (C) 2003 American Institute of Physics. C1 Univ Calif Irvine, Dept Chem, Irvine, CA 92697 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Hebrew Univ Jerusalem, Dept Phys Chem, IL-91904 Jerusalem, Israel. Hebrew Univ Jerusalem, Fritz Haber Res Ctr, IL-91904 Jerusalem, Israel. RP Bihary, Z (reprint author), Univ Calif Irvine, Dept Chem, Irvine, CA 92697 USA. NR 26 TC 13 Z9 13 U1 0 U2 4 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD DEC 1 PY 2003 VL 119 IS 21 BP 11278 EP 11284 DI 10.1063/1.1621851 PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 742AN UT WOS:000186492900032 ER PT J AU Sud, YC Mocko, DM Lau, KM Atlas, R AF Sud, YC Mocko, DM Lau, KM Atlas, R TI Simulating the Midwestern US drought of 1988 with a GCM SO JOURNAL OF CLIMATE LA English DT Article ID SOIL-MOISTURE ANOMALIES; UNITED-STATES; NORTH-AMERICA; GENERAL-CIRCULATION; CLIMATE SIMULATION; MODEL SIMULATIONS; REGIONAL MODEL; SNOW-PHYSICS; PART I; PRECIPITATION AB Past studies have suggested that the drought of the summer of 1988 over the midwestern United States may have been caused by sea surface temperature (SST) anomalies, an evolving stationary circulation, a soil-moisture feedback on circulation and rainfall, or even by remote forcings. The relative importance of various contributing factors is investigated in this paper through the use of Goddard Earth Observing System (GEOS) GCM simulations. Seven different experiments, each containing an ensemble of four simulations, were conducted with the GCM. For each experiment, the GCM was integrated through the summers of 1987 and 1988 starting from an analyzed atmosphere in early January of each year. In the baseline case, only the SST anomalies and climatological vegetation parameters were prescribed, while everything else (such as soil moisture, snow cover, and clouds) was interactive. The precipitation differences (1988 minus 1987) show that the GCM was successful in simulating reduced precipitation in 1988, but the accompanying low-level circulation anomalies in the Midwest were not well simulated. To isolate the influence of the model's climate drift, analyzed winds and analyzed soil moisture were prescribed globally as continuous updates (in isolation or jointly). The results show that remotely advected wind biases (emanating from potential errors in the model's dynamics and physics) are the primary cause of circulation biases over North America. Inclusion of soil moisture helps to improve the simulation as well as to reaffirm the strong feedback between soil moisture and precipitation. In a case with both updated winds and soil moisture, the model produces more realistic evapotranspiration and precipitation differences. An additional case also used soil moisture and winds updates, but only outside North America. Its simulation is very similar to that of the case with globally updated winds and soil moisture, which suggests that North American simulation errors originate largely outside the region. Two additional cases examining the influence of vegetation were built on this case using correct and opposite-year vegetation. The model did not produce a discernible improvement in response to vegetation for the drought year. One may conclude that the soil moisture governs the outcome of the land-atmosphere feedback interaction far more than the vegetation parameters. A primary inference of this study is that even though SSTs have some influence on the drought, model biases strongly influence the prediction errors. It must be emphasized that the results from this study are dependent upon the GEOS model's identified errors and biases, and that the conclusions do not necessarily apply to results from other models. C1 NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. SAIC Gen Sci Operat, Beltsville, MD USA. RP Sud, YC (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RI Atlas, Robert/A-5963-2011; Lau, William /E-1510-2012 OI Atlas, Robert/0000-0002-0706-3560; Lau, William /0000-0002-3587-3691 NR 48 TC 25 Z9 25 U1 0 U2 3 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 J9 J CLIMATE JI J. Clim. PD DEC PY 2003 VL 16 IS 23 BP 3946 EP 3965 DI 10.1175/1520-0442(2003)016<3946:STMUDO>2.0.CO;2 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 745JA UT WOS:000186684500008 ER PT J AU Lee, T Fukumori, I AF Lee, T Fukumori, I TI Interannual-to-decadal variations of tropical-subtropical exchange in the Pacific Ocean: Boundary versus interior pycnocline transports SO JOURNAL OF CLIMATE LA English DT Article ID HEAT-CONTENT VARIABILITY; EQUATORIAL PACIFIC; EL-NINO; NORTH PACIFIC; INDONESIAN THROUGHFLOW; MINDANAO CURRENT; WATER EXCHANGE; MODEL; CIRCULATION; THERMOCLINE AB Interannual-to-decadal variations of tropical - subtropical mass exchange in the Pacific Ocean are investigated using a near-global ocean general circulation model along with satellite observations of sea level and wind and a data assimilation product. The analysis focuses on the variability of pycnocline transports through the western boundary and interior near 10degreesN and 10degreesS. In contrast to time-mean exchange, where boundary and interior pycnocline transports are both equatorward, the variations of boundary and interior pycnocline transports are found to be generally anticorrelated to each other. Moreover, the variation of the boundary pycnocline transport is smaller than that of the interior, again different from time-mean exchange, where the boundary transport at 10degreesN is substantially larger than that through the interior. Interannual variations of the boundary and interior transports are consistent with near-surface geostrophic flow inferred from sea level data. Interior pycnocline flow into the Tropics is weaker in the 1990s than that in the 1980s, in agreement with recent observations. However, approximately half of it is compensated by an opposite change in boundary flow at 10degreesN. The results indicate that the interior pathway is more important to interannual and decadal variability of tropical - subtropical exchange than the boundary pathway, despite a much larger time-mean transport of the western boundary current at 10degreesN. To a large extent, the counteracting tendency of the boundary and interior flow and the larger variation of the latter can be explained by the combined effect of variability in off-equatorial wind stress curl in the western Pacific and near-equatorial zonal wind stress. The former changes the strength of horizontal circulation and results in a variation of boundary pycnocline flow that is opposite in direction but comparable in magnitude to that of the interior pycnocline flow. The latter primarily affects the strength of the shallow meridional overturning circulation with net pycnocline flow ( mostly in the interior) opposing the surface Ekman flow. The covariability of these two forcings leads to an enhancement of interior transport. The relative variability of boundary and interior pycnocline flow is insensitive to whether the Indonesian Throughflow is present or not. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lee, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 300-323, Pasadena, CA 91109 USA. NR 43 TC 63 Z9 69 U1 0 U2 4 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 DEC PY 2003 VL 16 IS 24 BP 4022 EP 4042 DI 10.1175/1520-0442(2003)016<4022:IVOTEI>2.0.CO;2 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 750VN UT WOS:000187019300002 ER PT J AU Shindell, DT Schmidt, GA Miller, RL Mann, ME AF Shindell, DT Schmidt, GA Miller, RL Mann, ME TI Volcanic and solar forcing of climate change during the preindustrial era SO JOURNAL OF CLIMATE LA English DT Article ID NORTHERN-HEMISPHERE WINTER; GENERAL-CIRCULATION MODEL; TREE-RING CHRONOLOGIES; MEDIEVAL WARM PERIOD; MOUNT-PINATUBO; GLOBAL CLIMATE; VARIABILITY; ERUPTIONS; OZONE; OSCILLATION AB The climate response to variability in volcanic aerosols and solar irradiance, the primary forcings during the preindustrial era, is examined in a stratosphere-resolving general circulation model. The best agreement with historical and proxy data is obtained using both forcings, each of which has a significant effect on global mean temperatures. However, their regional climate impacts in the Northern Hemisphere are quite different. While the short-term continental winter warming response to volcanism is well known, it is shown that due to opposing dynamical and radiative effects, the long-term (decadal mean) regional response is not significant compared to unforced variability for either the winter or the annual average. In contrast, the long-term regional response to solar forcing greatly exceeds unforced variability for both time averages, as the dynamical and radiative effects reinforce one another, and produces climate anomalies similar to those seen during the Little Ice Age. Thus, long-term regional changes during the preindustrial appear to have been dominated by solar forcing. C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Columbia Univ, Ctr Climate Syst Res, New York, NY USA. Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. Univ Virginia, Dept Environm Sci, Charlottesville, VA 22903 USA. RP Shindell, DT (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM dshindell@giss.nasa.gov RI Shindell, Drew/D-4636-2012; Schmidt, Gavin/D-4427-2012; Miller, Ron/E-1902-2012; Mann, Michael/B-8472-2017 OI Schmidt, Gavin/0000-0002-2258-0486; Mann, Michael/0000-0003-3067-296X NR 48 TC 161 Z9 167 U1 3 U2 31 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 DEC PY 2003 VL 16 IS 24 BP 4094 EP 4107 DI 10.1175/1520-0442(2003)016<4094:VASFOC>2.0.CO;2 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 750VN UT WOS:000187019300006 ER PT J AU Cummings, D Irizarry, R Huang, N Endy, T Nisalak, A Ungehusak, K Burke, D AF Cummings, D Irizarry, R Huang, N Endy, T Nisalak, A Ungehusak, K Burke, D TI Traveling waves in dengue hemorrhagic fever incidence in Thailand SO JOURNAL OF CLINICAL VIROLOGY LA English DT Meeting Abstract CT 6th Asia Pacific Congress of Medical Virology CY DEC 07-10, 2003 CL KUALA LUMPUR, MALAYSIA SP Malaysian Soc Infect Dis, Chemotherapy Asia Pacific Soc Med Virol C1 Johns Hopkins Bloomberg Sch Publ Hlth, Dept Int Hlth, Baltimore, MD USA. Johns Hopkins Bloomberg Sch Publ Hlth, Dept Biostat, Baltimore, MD USA. NASA, Goddard Space Flight Ctr, Lab Hydrospher Proc, Greenbelt, MD 20771 USA. USA, Med Res Inst Infect Dis, Div Virol, Ft Detrick, MD 21702 USA. Armed Forces Res Inst Med Sci, Dept Virol, Bangkok, Thailand. Minist Publ Hlth, Dept Dis Control, Bangkok, Thailand. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1386-6532 J9 J CLIN VIROL JI J. Clin. Virol. PD DEC PY 2003 VL 28 SU 1 BP S29 EP S29 PG 1 WC Virology SC Virology GA 758ZE UT WOS:000187711900027 ER PT J AU Sallenger, AH Krabill, WB Swift, RN Brock, J List, J Hansen, M Holman, RA Manizade, S Sontag, J Meredith, A Morgan, K Yunkel, JK Frederick, EB Stockdon, H AF Sallenger, AH Krabill, WB Swift, RN Brock, J List, J Hansen, M Holman, RA Manizade, S Sontag, J Meredith, A Morgan, K Yunkel, JK Frederick, EB Stockdon, H TI Evaluation of airborne topographic lidar for quantifying beach changes SO JOURNAL OF COASTAL RESEARCH LA English DT Article DE beach processes; coastal change; storms; surveying; remote sensing; lidar ID GREENLAND ICE-SHEET; LASER ALTIMETRY; ACCURACY AB A scanning airborne topographic lidar was evaluated for its ability to quantify beach topography and changes during the Sandy Duck experiment in 1997 along the North Carolina coast. Elevation estimates, acquired with NASA's Airborne Topographic Mapper (ATM), were compared to elevations measured with three types of ground-based measurements-1) differential GPS equipped all-terrain vehicle (ATV) that surveyed a 3-km reach of beach from the shoreline to the dune, 2) GPS antenna mounted on a stadia rod used to intensely survey a different 100 m reach of beach, and 3) a second GPS-equipped ATV that surveyed a 70-km-long transect along the coast. Over 40,000 individual intercomparisons between ATM and ground surveys were calculated. RMS vertical differences associated with the ATM when compared to ground measurements ranged from 13 to 19 em. Considering all of the intercomparisons together, RMS similar or equal to15 cm. This RMS error represents a total error for individual elevation estimates including uncertainties associated with random and mean errors. The latter was the largest source of error and was attributed to drift in differential GPS. The 15 cm vertical accuracy of the ATM is adequate to resolve beach-change signals typical of the impact of storms. For example, ATM surveys of Assateague Island (spanning the border of MD and VA) prior to and immediately following a severe northeaster showed vertical beach changes in places greater than 2 m, much greater than expected errors associated with the ATM. A major asset of airborne lidar is the high spatial data density. Measurements of elevation are acquired every few m(2) over regional scales of hundreds of kilometers. Hence, many scales of beach morphology and change can be resolved, from beach cusps tens of meters in wavelength to entire coastal cells comprising tens to hundreds of kilometers of coast. Topographic lidars similar to the ATM are becoming increasingly available from commercial vendors and should, in the future, be widely used in beach surveying. C1 US Geol Survey, Ctr Coatal Geol, St Petersburg, FL 33701 USA. NASA, Wallops Fligh Facil, EG&G, Wallops Isl, VA 23337 USA. NOAA, Coastal Serv Ctr, Charleston, SC 29405 USA. US Geol Survey, Woods Hole Field Ctr, Woods Hole, MA 02543 USA. Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA. EG&G Washington, Analyt Serv Ctr, Gaithersburg, MD 20878 USA. RP Sallenger, AH (reprint author), US Geol Survey, Ctr Coatal Geol, 600 4th St S, St Petersburg, FL 33701 USA. OI Stockdon, Hilary/0000-0003-0791-4676 NR 22 TC 118 Z9 120 U1 1 U2 28 PU COASTAL EDUCATION & RESEARCH FOUNDATION PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0749-0208 J9 J COASTAL RES JI J. Coast. Res. PD WIN PY 2003 VL 19 IS 1 BP 125 EP 133 PG 9 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA 669WU UT WOS:000182374100011 ER PT J AU Braverman, A Fetzer, E Eldering, A Nittel, S Leung, K AF Braverman, A Fetzer, E Eldering, A Nittel, S Leung, K TI Semi-streaming quantization for remote sensing data SO JOURNAL OF COMPUTATIONAL AND GRAPHICAL STATISTICS LA English DT Article; Proceedings Paper CT Workshop on Statistical Analysis of Massive Data Streams CY DEC 13-14, 2002 CL WASHINGTON, D.C. DE cluster analysis; data compression; data reduction; massive datasets ID VECTOR QUANTIZATION AB We describe a strategy for reducing the size and complexity of very large, remote sensing datasets acquired from NASA's Earth Observing System. We apply the quantization paradigm from, and algorithms developed in, signal processing to the problem of summarization. Because data arrive in discrete chunks, we formulate a semi-streaming strategy that partially processes chunks as they become available and stores the results. At the end of the summary time period, we re-ingest the partial summaries and summarize them. We show that mean squared errors between the final summaries and the original data can be computed from the mean squared errors incurred at the two stages without directly accessing the original data. The procedure is demonstrated using data from JPL's Atmospheric Infrared Sounder. C1 CALTECH, Jet Prop Lab, Div Earth & Space Sci, Pasadena, CA 91109 USA. Univ Calif Los Angeles, Dept Comp Sci, Los Angeles, CA 90095 USA. Univ Maine, Dept Spatial Informat Sci & Engn, Orono, ME 04469 USA. CALTECH, Jet Prop Lab, Div Earth & Space Sci, Pasadena, CA 91109 USA. RP Braverman, A (reprint author), CALTECH, Jet Prop Lab, Div Earth & Space Sci, 4800 Oak Grove Dr,Mail Stop 169-237, Pasadena, CA 91109 USA. EM Amy.Braverman@jpl.nasa.gov NR 7 TC 7 Z9 7 U1 1 U2 1 PU AMER STATISTICAL ASSOC PI ALEXANDRIA PA 1429 DUKE ST, ALEXANDRIA, VA 22314 USA SN 1061-8600 J9 J COMPUT GRAPH STAT JI J. Comput. Graph. Stat. PD DEC PY 2003 VL 12 IS 4 BP 759 EP 780 DI 10.1198/1061860032535 PG 22 WC Statistics & Probability SC Mathematics GA 761LX UT WOS:000187911200002 ER PT J AU Klimeck, G AF Klimeck, Gerhard TI Quantum and Semi-Classical Transport in NEMO 1-D SO JOURNAL OF COMPUTATIONAL ELECTRONICS LA English DT Article DE transport; classical; quantum; tunneling; diffusion AB The coupling of the fundamentally quantum mechanical nanoelectronic transport simulation through resonant tunneling diodes to semi-classical drift diffusion in the contacts is demonstrated. The coupling between the non-equilibrium Green function formalism used in NEMO to the drift diffusion equation is established by the use of spatially dependent quasi Fermi levels in the reservoirs. The charge distributions are computed quantum mechanically throughout the whole device using the full bandstructure sp3s* tight binding model that includes band non-parabolicity and band warping. The formalism is applied to the simulation of high current density resonant tunneling diodes. Low mobility contacts are shown to introduce a bi-stability in the negative differential resistance region. C1 [Klimeck, Gerhard] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Klimeck, G (reprint author), Purdue Univ, Sch Elect Engn, W Lafayette, IN 47907 USA. EM gekco@purdue.edu NR 13 TC 12 Z9 13 U1 0 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1569-8025 J9 J COMPUT ELECTRON JI J. Comput. Electron. PD DEC PY 2003 VL 2 IS 2-4 SI SI BP 177 EP 182 DI 10.1023/B:JCEL.0000011421.53762.97 PG 6 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA V25LE UT WOS:000208478700021 ER PT J AU Lien, MC Proctor, RW Ruthruff, E AF Lien, MC Proctor, RW Ruthruff, E TI Still no evidence for perfect timesharing with two ideomotor-compatible tasks: A reply to Greenwald (2003) SO JOURNAL OF EXPERIMENTAL PSYCHOLOGY-HUMAN PERCEPTION AND PERFORMANCE LA English DT Article ID PSYCHOLOGICAL REFRACTORY PERIOD; RESPONSE SELECTION; INTERFERENCE; INFORMATION; BOTTLENECK; PARALLEL; THINGS AB For 30 years, A. G. Greenwald and H. G. Shulman's (1973) psychological refractory period (PRP) study has been cited as evidence for perfect timesharing with ideomotor (IM)-compatible tasks. Recently, M.-C. Lien, R. W. Proctor, and P. A. Allen (2002) failed to replicate these results and concluded that IM compatibility is neither necessary nor sufficient to eliminate the PRP effect. A. G. Greenwald (2003) attributed Lien et al.'s nonreplication to the use of (a) a non-IM-compatible task, (b) varied trial spacing, and/or (c) inappropriate instructions. The authors of the present article argue that the first 2 factors are not critical and that instructions merely affect the criterion for speed versus accuracy. In each of Greenwald's experiments, dual-task costs were evident on response time or error rates. Furthermore, the small dual-task costs in his study are consistent with a bottleneck model. Thus, Greenwald (2003) does not provide evidence that IM-compatible tasks enable perfect timesharing. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Purdue Univ, Dept Psychol Sci, W Lafayette, IN 47907 USA. RP Lien, MC (reprint author), NASA, Ames Res Ctr, Mail Stop 262-4, Moffett Field, CA 94035 USA. NR 19 TC 16 Z9 16 U1 3 U2 3 PU AMER PSYCHOLOGICAL ASSOC PI WASHINGTON PA 750 FIRST ST NE, WASHINGTON, DC 20002-4242 USA SN 0096-1523 J9 J EXP PSYCHOL HUMAN JI J. Exp. Psychol.-Hum. Percept. Perform. PD DEC PY 2003 VL 29 IS 6 BP 1267 EP 1272 DI 10.1037/0096-1523.29.6.1267 PG 6 WC Psychology; Psychology, Experimental SC Psychology GA 753EB UT WOS:000187218100012 PM 14640843 ER PT J AU Mahanama, SPP Koster, RD AF Mahanama, SPP Koster, RD TI Intercomparison of soil moisture memory in two land surface models SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID GENERAL-CIRCULATION MODEL; CATCHMENT-BASED APPROACH; ATMOSPHERE SYSTEM; CLIMATE MODELS; PRECIPITATION; VARIABILITY; PERSISTENCE; TRANSPIRATION; VEGETATION; BOUNDARY AB A heavy rain or a dry period can produce an anomaly in soil moisture, and the dissipation of this anomaly may take weeks to months. It is important to understand how land surface models (LSMs) used with atmospheric general circulation models simulate this soil moisture "memory,'' because this memory may have profound implications for long-term weather prediction through land-atmosphere feedback. In order to understand better the effect of precipitation and net radiation on soil moisture memory, the NASA Seasonal-to-Interannual Prediction Project (NSIPP) Catchment LSM and the Mosaic LSM were both forced with a wide variety of idealized climates. The imposed climates had average monthly precipitation ranging from 15 to 500 mm and monthly net radiations (in terms of water equivalent) ranging from 20 to 400 mm, with consequent changes in near-surface temperature and humidity. For an equivalent water holding capacity, the two models maximize memory in distinctly different climate regimes. Memory in the NSIPP Catchment LSM exceeds that in the Mosaic LSM when precipitation and net radiation are of the same order; otherwise, memory in the Mosaic LSM is larger. The NSIPP Catchment and the Mosaic LSMs were also driven offline, globally, for a period of 15 yr (1979-93) with realistic atmospheric forcing. Global distributions of 1-month-lagged autocorrelation of soil moisture for boreal summer were computed. An additional global run with the NSIPP Catchment LSM employing the Mosaic LSM's water holding capacities was also performed. These three global runs show that while some of the intermodel difference in memory can be explained (following traditional interpretations) in terms of differences in water holding capacity and potential evaporation, much of the intermodal difference stems from differences in the parameterizations of evaporation and runoff. C1 NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Hydrol Sci Branch, Greenbelt, MD 20771 USA. Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. RP Mahanama, SPP (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Hydrol Sci Branch, Code 900-3, Greenbelt, MD 20771 USA. RI Koster, Randal/F-5881-2012 OI Koster, Randal/0000-0001-6418-6383 NR 26 TC 16 Z9 16 U1 0 U2 4 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 DEC PY 2003 VL 4 IS 6 BP 1134 EP 1146 DI 10.1175/1525-7541(2003)004<1134:IOSMMI>2.0.CO;2 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 757EB UT WOS:000187534900010 ER PT J AU Adler, RF Huffman, GJ Chang, A Ferraro, R Xie, PP Janowiak, J Rudolf, B Schneider, U Curtis, S Bolvin, D Gruber, A Susskind, J Arkin, P Nelkin, E AF Adler, RF Huffman, GJ Chang, A Ferraro, R Xie, PP Janowiak, J Rudolf, B Schneider, U Curtis, S Bolvin, D Gruber, A Susskind, J Arkin, P Nelkin, E TI The version-2 global precipitation climatology project (GPCP) monthly precipitation analysis (1979-present) SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID SENSOR MICROWAVE IMAGER; PROBABILITY-DISTRIBUTION FUNCTIONS; LOW-ORBIT MICROWAVE; SOUTHERN OSCILLATION; MONTHLY RAINFALL; GAUGE OBSERVATIONS; GEOSYNCHRONOUS IR; UNITED-STATES; SATELLITE; DATASET AB The Global Precipitation Climatology Project (GPCP) Version-2 Monthly Precipitation Analysis is described. This globally complete, monthly analysis of surface precipitation at 2.5degrees latitude x 2.5degrees longitude resolution is available from January 1979 to the present. It is a merged analysis that incorporates precipitation estimates from low-orbit satellite microwave data, geosynchronous-orbit satellite infrared data, and surface rain gauge observations. The merging approach utilizes the higher accuracy of the low-orbit microwave observations to calibrate, or adjust, the more frequent geosynchronous infrared observations. The dataset is extended back into the premicrowave era (before mid-1987) by using infrared-only observations calibrated to the microwave-based analysis of the later years. The combined satellite-based product is adjusted by the rain gauge analysis. The dataset archive also contains the individual input fields, a combined satellite estimate, and error estimates for each field. This monthly analysis is the foundation for the GPCP suite of products, including those at finer temporal resolution. The 23-yr GPCP climatology is characterized, along with time and space variations of precipitation. C1 NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Lab Hydrospher Proc, Greenbelt, MD 20771 USA. NOAA, NESDIS, Off Res & Applicat, Camp Springs, MD USA. NOAA, NWS, Natl Ctr Environm Predict, Camp Springs, MD USA. Deutsch Wetterdienst, Global Precipitat Climatol Ctr, Offenbach, Germany. Univ Maryland, Baltimore, MD 21201 USA. Atmospheres Lab, Baltimore, MD USA. Univ Maryland, College Pk, MD 20742 USA. RP Adler, RF (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 912, Greenbelt, MD 20771 USA. RI Arkin, Phillip/F-5808-2010; Curtis, Scott/C-1115-2013; Huffman, George/F-4494-2014; Ferraro, Ralph/F-5587-2010; OI Huffman, George/0000-0003-3858-8308; Ferraro, Ralph/0000-0002-8393-7135; Curtis, Scott/0000-0001-9065-8639 NR 57 TC 2101 Z9 2181 U1 27 U2 172 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 DEC PY 2003 VL 4 IS 6 BP 1147 EP 1167 DI 10.1175/1525-7541(2003)004<1147:TVGPCP>2.0.CO;2 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 757EB UT WOS:000187534900011 ER PT J AU Reichle, RH Koster, RD AF Reichle, RH Koster, RD TI Assessing the impact of horizontal error correlations in background fields on soil moisture estimation SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID ENSEMBLE KALMAN FILTER; GENERAL-CIRCULATION MODEL; ATMOSPHERIC DATA ASSIMILATION; SEQUENTIAL DATA ASSIMILATION; CATCHMENT-BASED APPROACH; LAND DATA ASSIMILATION; SURFACE PROCESSES; ANALYSIS SCHEME; PRECIPITATION; METHODOLOGY AB The importance of horizontal error correlations in background (i.e., model forecast) fields for large-scale soil moisture estimation is assessed by comparing the performance of one- and three-dimensional ensemble Kalman filters (EnKF) in a twin experiment. Over a domain centered on the U. S. Great Plains, gauge-based precipitation data is used to force the "true'' model solution, and reanalysis data for the prior (or background) fields. The difference between the two precipitation datasets is thought to be representative of errors that might be encountered in a global land assimilation system. To ensure realistic conditions the synthetic observations of surface soil moisture match the spatiotemporal pattern and expected errors of retrievals from the Scanning Multichannel Microwave Radiometer (SMMR) on the Nimbus-7 satellite. After filter calibration, average actual estimation errors in the (volumetric) root zone moisture content are 0.015 m(3) m(-3) for the 3D-EnKF, 0.019 m(3) m(-3) for the 1D-EnKF, and 0.036 m(3) m(-3) without assimilation. Clearly, taking horizontal error correlations into account improves estimation accuracy. Soil moisture estimation errors in the 3D-EnKF are smallest for a correlation scale of 28 in model parameter and forcing errors, which coincides with the horizontal scale of difference fields between gauge-based and reanalysis precipitation. In this case the 3D-EnKF requires 1.6 times the computational effort of the 1D-EnKF, but this factor depends on the experiment setup. C1 NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. RP Reichle, RH (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Code 900-3,Bldg 33,Rm A-110, Greenbelt, MD 20771 USA. RI Reichle, Rolf/E-1419-2012; Koster, Randal/F-5881-2012 OI Koster, Randal/0000-0001-6418-6383 NR 30 TC 74 Z9 76 U1 0 U2 7 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 DEC PY 2003 VL 4 IS 6 BP 1229 EP 1242 DI 10.1175/1525-7541(2003)004<1229:ATIOHE>2.0.CO;2 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 757EB UT WOS:000187534900017 ER PT J AU Schultz, MR Hyer, MW AF Schultz, MR Hyer, MW TI Snap-through of unsymmetric cross-ply laminates using piezoceramic actuators SO JOURNAL OF INTELLIGENT MATERIAL SYSTEMS AND STRUCTURES LA English DT Article DE MFC (TM) actuator; morphing; Rayleigh-Ritz technique; bistable composites ID ROOM-TEMPERATURE SHAPES; CURED SHAPE AB The paper discusses the concept of using a piezoceramic actuator bonded to one side of a two-layer unsymmetric cross ply [0/90](T) laminate to provide the moments necessary to snap the laminate from one stable equilibrium shape to another. The results presented are considered an alternative to existing morphing concepts wherein actuators are used to elastically warp structures into a shape other than their natural and unique equilibrium shape. These existing concepts require the continuous application of power to maintain the warped shape. With the concept discussed here, the actuators are used only to change from one equilibrium shape to another, so continuous power is not needed. The paper discusses several phases of modeling, including bonding the actuator to the laminate and applying voltage to the actuator to effect the shape change, and experimental work. Two models are developed, a simple model and a more refined one. Both are based on the Rayleigh-Ritz technique and the use of energy and variational methods. The experimental phase of the study is discussed, particularly the measurement of the voltage level needed to snap the laminate. The voltage measurements are compared with predictions and the agreement between measurements and the predictions of the refined model are reasonable, both qualitatively and quantitatively. Suggestions for future activities are presented. C1 NASA, Struct Dynam Branch, Langley Res Ctr, Hampton, VA 23681 USA. Virginia Polytech Inst & State Univ, Dept Engn Sci & Mech, Blacksburg, VA 24061 USA. RP Schultz, MR (reprint author), NASA, Struct Dynam Branch, Langley Res Ctr, Mail Stop 230,Bldg 1293B,Room 235,4B W Taylor St, Hampton, VA 23681 USA. NR 23 TC 59 Z9 59 U1 2 U2 10 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1045-389X J9 J INTEL MAT SYST STR JI J. Intell. Mater. Syst. Struct. PD DEC PY 2003 VL 14 IS 12 BP 795 EP 814 DI 10.1177/s104538903039261 PG 20 WC Materials Science, Multidisciplinary SC Materials Science GA 758UT UT WOS:000187669300004 ER PT J AU Strekalov, D Aveline, D Yu, N Thompson, R Matsko, AB Maleki, L AF Strekalov, D Aveline, D Yu, N Thompson, R Matsko, AB Maleki, L TI Stabilizing an optoelectronic microwave oscillator with photonic filters SO JOURNAL OF LIGHTWAVE TECHNOLOGY LA English DT Article DE atomic clocks; electromagnetically induced transparency; optoelectronic oscillator; photonic filter ID ELECTROMAGNETICALLY INDUCED TRANSPARENCY; GROUP-VELOCITY; SPECTROSCOPY; SLOW; PERFORMANCE; ULTRASLOW; VAPOR; LIGHT AB This paper compares methods of active stabilization of an optoelectronic microwave oscillator (OEO) based on insertion of a source of optical group delay into an OEO loop. The performance of an OEO stabilized with either a high-Q optical cavity or an atomic cell is analyzed. We show that the elements play a role of narrow-band microwave filters improving an OEO stability. An atomic cell also allows for locking the oscillation frequency to particular atomic clock transitions. This reports a proof-of-principle experiment on an OEO stabilization using the effect of electromagnetically induced transparency in a hot rubidium atomic vapor cell. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Strekalov, D (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM Andrey.Matsko@jpl.nasa.gov RI Matsko, Andrey/A-1272-2007 NR 22 TC 52 Z9 53 U1 2 U2 13 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0733-8724 EI 1558-2213 J9 J LIGHTWAVE TECHNOL JI J. Lightwave Technol. PD DEC PY 2003 VL 21 IS 12 BP 3052 EP 3061 DI 10.1109/JLT.2003.821724 PG 10 WC Engineering, Electrical & Electronic; Optics; Telecommunications SC Engineering; Optics; Telecommunications GA 772PW UT WOS:000188851300014 ER PT J AU Tucker, DS Nettles, AT Cagle, H AF Tucker, DS Nettles, AT Cagle, H TI Lifetime predictions of a titanium silicate glass with machined flaws SO JOURNAL OF MATERIALS SCIENCE LETTERS LA English DT Article ID DYNAMIC FATIGUE C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Tucker, DS (reprint author), NASA, George C Marshall Space Flight Ctr, SD 71, Huntsville, AL 35812 USA. NR 17 TC 0 Z9 0 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0261-8028 J9 J MATER SCI LETT JI J. Mater. Sci. Lett. PD DEC 1 PY 2003 VL 22 IS 23 BP 1723 EP 1725 DI 10.1023/B:JMSL.0000004658.13148.4b PG 3 WC Materials Science, Multidisciplinary SC Materials Science GA 744YZ UT WOS:000186661600020 ER PT J AU Paden, B Groom, N Antaki, JF AF Paden, B Groom, N Antaki, JF TI Design formulas for permanent-magnet bearings SO JOURNAL OF MECHANICAL DESIGN LA English DT Article DE permanent magnet bearings; machine elements; design formulas AB As the energy densities in permanent magnet materials increases, permanent magnet (PM) bearings are becoming increasingly attractive machine elements for applications ranging from turbo machinery to energy storage flywheels. Desirable qualities include high speed, low wear energy savings, and freedom from lubricants that can degrade or contaminate other system components. In this paper we develop analytical expressions for stiffness and peak load in stacked-structure radial magnetic bearings that extend the seminal work of Backers, and Yonnet and co-workers. In addition to the derivation of simple design rules, the axial peak force and negative axial stiffness are calculated. C1 Univ Calif Santa Barbara, Dept Mech & Environm Engn, Santa Barbara, CA 93106 USA. NASA, LARC ret, White Marsh, VA 23183 USA. Carnegie Mellon Univ, Pittsburgh, PA 15213 USA. RP Paden, B (reprint author), Univ Calif Santa Barbara, Dept Mech & Environm Engn, Santa Barbara, CA 93106 USA. EM paden@engineering.ucsb.edu; njgroom@visi.net; antaki@andrew.cmu.edu RI Antaki, James/S-3051-2016 OI Antaki, James/0000-0002-5430-7353 NR 8 TC 25 Z9 26 U1 1 U2 5 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA SN 1050-0472 J9 J MECH DESIGN JI J. Mech. Des. PD DEC PY 2003 VL 125 IS 4 BP 734 EP 738 DI 10.1115/1.1625402 PG 5 WC Engineering, Mechanical SC Engineering GA 771LX UT WOS:000188788300009 ER PT J AU Yang, EH Wiberg, DV AF Yang, EH Wiberg, DV TI A wafer-scale membrane transfer process for the fabrication of optical quality, large continuous membranes SO JOURNAL OF MICROELECTROMECHANICAL SYSTEMS LA English DT Article DE adaptive optics; conitnuous membrane; deformable mirror; electrostatic actuator; membrane transfer; single crystal silicon; surface quality; wafer-scale AB This paper describes a new fabrication technique developed for the construction of large area mirror membranes via the transfer of wafer-scale continuous membranes from one substrate to another. Using this technique, wafer-scale silicon mirror membranes have been successfully transferred without the use of sacrificial layers such as adhesives or polymers. This transfer technique has also been applied to the fabrication and transfer of 1 mum thick corrugated membrane actuators. These membrane actuators consist of several concentric-ring-type corrugations constructed within a polysilicon membrane. A typical polysilicon actuator membrane with an electrode gap of 1.5 mum, fabricated using the wafer-scale transfer technique, shows a vertical deflection of 0.4 mum at 55 V. The mirror membranes are constructed from single-crystal silicon, 10 cm in diameter, and have been successfully transferred in their entirety. Using a white-light interferometer, the measured average peak-to-valley surface figure error for the transferred single-crystal silicon mirror membranes is approximately 9 nm as measured over a 1 mm(2) membrane area. The wafer-scale membrane transfer technique demonstrated in this paper has the following benefits over previously reported transfer techniques: 1) No postassembly release process to remove sacrificial polymers is required. 2) The bonded interface is completely isolated from any acid, etchant, or solvent during the transfer process, ensuring a clean and uniform membrane surface. 3) Our technique is capable of transferring large, continuous membranes onto substrates. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Eui-Hyeok.Yang@jpl.nasa.gov OI Yang, Eui-Hyeok/0000-0003-4893-1691 NR 15 TC 16 Z9 17 U1 0 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1057-7157 EI 1941-0158 J9 J MICROELECTROMECH S JI J. Microelectromech. Syst. PD DEC PY 2003 VL 12 IS 6 BP 804 EP 815 DI 10.1109/JMEMS.2003.818454 PG 12 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology; Instruments & Instrumentation; Physics, Applied SC Engineering; Science & Technology - Other Topics; Instruments & Instrumentation; Physics GA 761VP UT WOS:000187936400005 ER PT J AU Brault, JW Brown, LR Chackerian, C Freedman, R Predoi-Cross, A Pine, AS AF Brault, JW Brown, LR Chackerian, C Freedman, R Predoi-Cross, A Pine, AS TI Self-broadened (CO)-C-12-O-16 line shapes in the nu=2 <- 0 band SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE CO; self broadening and shifts; Dicke narrowing; line mixing; speed dependence; line intensities ID MULTISPECTRUM FITTING PROCEDURE; DEPENDENT COLLISIONAL WIDTH; FUNDAMENTAL-BAND; LINESHAPE MODELS; CARBON-MONOXIDE; SHIFT COEFFICIENTS; SPECTRAL PROFILES; CO; PARAMETERS; AR AB Precise intensities, self-broadenings and shifts have been obtained for the (CO)-C-12-O-16 nu = 2 <-- 0 band from simultaneous fits of low-noise, high-resolution Fourier-transform spectra at pressures from 27 to 80 kPa (200-600 Torr). Observed line shapes exhibit deviations on the order of 1% from the conventional Voigt profile, primarily due to speed-dependent broadening and secondarily to line mixing. Dicke narrowing is reduced by over an order-of-magnitude from the diffusion value, presumably because of correlations between velocity- and phase-changing collisions. (C) 2003 Elsevier Inc. All rights reserved. C1 Alpine Technol, Germantown, MD 20874 USA. Univ Ottawa, Dept Phys, Ottawa, ON K1N 6N5, Canada. NASA, Ames Res Ctr, Stanford, CA 94305 USA. SETI Inst, Stanford, CA 94305 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Kitt Peak Natl Observ, Tucson, AZ 85726 USA. RP Pine, AS (reprint author), Alpine Technol, 14401 Poplar Hill Rd, Germantown, MD 20874 USA. EM alanpine@erols.com NR 56 TC 43 Z9 43 U1 0 U2 13 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD DEC PY 2003 VL 222 IS 2 BP 220 EP 239 DI 10.1016/j.jms.2003.07.002 PG 20 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA 750JY UT WOS:000186988600010 ER PT J AU Isachsen, PE LaCasce, JH Mauritzen, C Hakkinen, S AF Isachsen, PE LaCasce, JH Mauritzen, C Hakkinen, S TI Wind-driven variability of the large-scale recirculating flow in the Nordic seas and Arctic Ocean SO JOURNAL OF PHYSICAL OCEANOGRAPHY LA English DT Article ID NEAR-SURFACE CIRCULATION; NORTHERN NORTH-ATLANTIC; STATISTICAL-MECHANICS; LAGRANGIAN DRIFTERS; BOTTOM TOPOGRAPHY; MODEL; GREENLAND; DYNAMICS; WATER; JEBAR AB The varying depth-integrated currents in the Nordic seas and Arctic Ocean are modeled using an integral equation derived from the shallow-water equations. This equation assumes that mass divergence in the surface Ekman layer is balanced by convergence in the bottom Ekman layer. The primary flow component follows contours of f/H. The model employs observed winds and realistic bottom topography and has one free parameter, the coefficient of the ( linear) bottom drag. The data used for comparison are derived from in situ current meters, satellite altimetry, and a primitive equation model. The current-meter data come from a 4-yr record at 75degreesN in the Greenland Sea. The currents here are primarily barotropic, and the model does well at simulating the variability. The "best'' bottom friction parameter corresponds to a spindown time of 30 - 60 days. A further comparison with bottom currents from a mooring on the Norwegian continental slope, deployed over one winter period, also shows reasonable correspondence. The principal empirical orthogonal function obtained from satellite altimetry data in the Nordic seas has a spatial structure that closely resembles f/H. A direct comparison of this mode's fluctuations with those predicted by the theoretical model yields linear correlation coefficients in the range 0.75 - 0.85. The primitive equation model is a coupled ocean - ice version of the Princeton Ocean Model for the North Atlantic and Arctic. Monthly mean depth-averaged velocities are calculated from a 42-yr integration and then compared with velocities predicted from an idealized model driven by the same reanalyzed atmospheric winds. In the largely ice-free Norwegian Sea, the coherences between the primitive equation and idealized model velocities are as high as 0.9 on timescales of a few months to a few years. They are lower in the remaining partially or fully ice-covered basins of the Greenland Sea and the Arctic Ocean, presumably because ice alters the momentum transferred to the ocean by the wind. The coherence in the Canadian Basin of the Arctic can be increased substantially by forcing the idealized model with ice velocities rather than the wind. Estimates of the depth-integrated vorticity budget in the primitive equation model suggest that bottom friction is important but that lateral diffusion is of equal or greater importance in compensating surface Ekman pumping. C1 Norwegian Meteorol Inst, N-0313 Oslo, Norway. Norwegian Polar Res Inst, Tromso, Norway. Univ Bergen, Inst Geophys, Bergen, Norway. Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP LaCasce, JH (reprint author), Norwegian Meteorol Inst, POB 43, N-0313 Oslo, Norway. RI Hakkinen, Sirpa/E-1461-2012; OI LaCasce, Joseph Henry/0000-0001-7655-5596 NR 34 TC 37 Z9 37 U1 1 U2 7 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 DEC PY 2003 VL 33 IS 12 BP 2534 EP 2550 DI 10.1175/1520-0485(2003)033<2534:WVOTLR>2.0.CO;2 PG 17 WC Oceanography SC Oceanography GA 754PX UT WOS:000187327400005 ER PT J AU Thakoor, S Cabrol, N Lay, N Chahl, J Soccol, D Hine, B Zornetzer, S AF Thakoor, S Cabrol, N Lay, N Chahl, J Soccol, D Hine, B Zornetzer, S TI Review: The benefits and applications of bioinspired flight capabilities SO JOURNAL OF ROBOTIC SYSTEMS LA English DT Review ID EXPLORATION SYSTEMS; MARS; HONEYBEES; EVOLUTION AB This paper addresses the challenges of flight on Mars that at this time have the same element of novelty as flight on Earth itself was a novelty in the Kitty Hawk era almost 100 years ago, details the scientific need for such flyers, highlights the bioinspired engineering of exploration systems (BEES) flyer development and finally describes a few viable mission architecture options that allow reliable data return from the BEES flyers using the limited telecom infrastructure that can be made available with a lander base to orbiter combination on Mars. Our recent developments using inspiration from biology that are enabling the pathway to demonstrate flight capability for Mars exploration are described. These developments hold substantial spin-offs for a variety of applications both for NASA and DoD. Unmanned exploration to date suggests that Mars once had abundant liquid water (considered essential for life as we know it). It is not clear what transpired on the Martian climate to have turned the planet into the desert that it is today. Developing a comprehensive understanding of the past and present climatic events for Mars may provide important information relevant to the future of our own planet. Such exploration missions are enabled using the BEES technology. (C) 2003 Wiley Periodicals, Inc. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Def Sci & Technol Org, Canberra, ACT, Australia. Australian Natl Univ, Canberra, ACT, Australia. RP Thakoor, S (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM sarita.thakoor@jpl.nasa.gov OI Chahl, Javaan/0000-0001-6496-0543 NR 37 TC 7 Z9 7 U1 0 U2 5 PU JOHN WILEY & SONS INC PI HOBOKEN PA 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0741-2223 J9 J ROBOTIC SYST JI J. Robot. Syst. PD DEC PY 2003 VL 20 IS 12 BP 687 EP 706 DI 10.1002/rob.10116 PG 20 WC Robotics SC Robotics GA 760PV UT WOS:000187843600001 ER PT J AU West, WC Whitacre, JF Ratnakumar, BV AF West, WC Whitacre, JF Ratnakumar, BV TI Radio frequency magnetron-sputtered LiCoPO4 cathodes for 4.8 V thin-film batteries SO JOURNAL OF THE ELECTROCHEMICAL SOCIETY LA English DT Article ID RECHARGEABLE LITHIUM BATTERIES; ELECTROCHEMICAL PERFORMANCE; PHOSPHO-OLIVINES; ELECTROLYTE; IMPROVEMENT; DEPOSITION; BEHAVIOR; LIFEPO4; LIMN2O4 AB Thin-film batteries employing sputtered LiCoPO4 cathode layers, Li3.3PO3.8N0.22 (LiPON) electrolyte, and Li anode films have been successfully fabricated and tested. The cells exhibit a high-voltage charge/ discharge plateau of 4.8 V, with a lower plateau at 2.5 V corresponding to a much higher conductivity phase. Cells fabricated with as-deposited cathode layers are highly resistive and cannot be charged or discharged to appreciable capacities, even at very low rates of approximately C/100. Upon annealing, the films sputtered from the LiCoPO4 target become discontinuous and take on a granular morphology. X-ray diffraction results show that these grains consist of untextured crystalline LiCoPO4 on a Pt current collector layer, a finding further supported by the results from subsequent electrochemical analyses. Thin-film batteries fabricated with crystalline LiCoPO4 cathodes are among the highest voltage thin-film batteries yet reported. (C) 2003 The Electrochemical Society. C1 CALTECH, Jet Prop Lab, Electrochem Technol Grp, Pasadena, CA 91109 USA. RP West, WC (reprint author), CALTECH, Jet Prop Lab, Electrochem Technol Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 24 TC 36 Z9 37 U1 3 U2 31 PU ELECTROCHEMICAL SOC INC PI PENNINGTON PA 65 SOUTH MAIN STREET, PENNINGTON, NJ 08534 USA SN 0013-4651 J9 J ELECTROCHEM SOC JI J. Electrochem. Soc. PD DEC PY 2003 VL 150 IS 12 BP A1660 EP A1666 DI 10.1149/1.1619987 PG 7 WC Electrochemistry; Materials Science, Coatings & Films SC Electrochemistry; Materials Science GA 749DB UT WOS:000186902400015 ER PT J AU Whitacre, JF West, WC Ratnakumar, BV AF Whitacre, JF West, WC Ratnakumar, BV TI A combinatorial study of LiyMnxNi2-xO4 cathode materials using microfabricated solid-state electrochemical cells SO JOURNAL OF THE ELECTROCHEMICAL SOCIETY LA English DT Article ID SECONDARY LITHIUM BATTERIES; LICOO2 THIN-FILMS; SPINEL LIMN2O4; ENERGY DENSITY; ION BATTERIES; DEPOSITION; FABRICATION; IMPROVEMENT; LIBRARIES; STRESS AB A methodology for batch-fabricating hundreds of submillimeter thin-film solid-state batteries was used in conjunction with a combinatorial materials synthesis technique. This approach allowed for the simultaneous creation of many solid-state microbatteries that had LiyMnxNi2-xO4 cathodes, where x varied continuously from 0.2 to 1.8 and y varied from 2.7 to 3.7 in the as-deposited films. Sputtered lithium phosphorous oxynitride (LiPON) was used as an electrolyte, while evaporated, micropatterned Li metal served as the anode layer. The composition, thickness, and microstructure of the cathodes were examined using X-ray energy-dispersive spectroscopy, synchrotron-based X-ray diffraction, Rutherford backscattering spectroscopy, stylus profilometry, inductively coupled plasma mass spectroscopy, and scanning electron microscopy. Electrochemical cycling data allowed for cell performance to be correlated to cathode composition and structure. Cathodes with a composition of LiMn1.4Ni0.6O4 had both the highest specific capacity as well as the longest high-potential (4.7 V) discharge plateau, while cells with higher Mn content had a longer 4 V discharge plateau, a result that qualitatively agrees with similar studies on conventional bulk-fabricated cathodes of the same material. (C) 2003 The Electrochemical Society. C1 CALTECH, Jet Prop Lab, Electrochem Technol Grp, Pasadena, CA 91109 USA. RP Whitacre, JF (reprint author), CALTECH, Jet Prop Lab, Electrochem Technol Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 33 TC 19 Z9 19 U1 2 U2 26 PU ELECTROCHEMICAL SOC INC PI PENNINGTON PA 65 SOUTH MAIN STREET, PENNINGTON, NJ 08534 USA SN 0013-4651 J9 J ELECTROCHEM SOC JI J. Electrochem. Soc. PD DEC PY 2003 VL 150 IS 12 BP A1676 EP A1683 DI 10.1149/1.1622957 PG 8 WC Electrochemistry; Materials Science, Coatings & Films SC Electrochemistry; Materials Science GA 749DB UT WOS:000186902400018 ER PT J AU Eisele, TP Keating, J Swalm, C Mbogo, CM Githeko, AK Regens, JL Githure, JI Andrews, L Beier, JC AF Eisele, TP Keating, J Swalm, C Mbogo, CM Githeko, AK Regens, JL Githure, JI Andrews, L Beier, JC TI Linking field-based ecological data with remotely sensed data using a geographic information system in two malaria endemic urban areas of Kenya SO MALARIA JOURNAL LA English DT Article ID SUB-SAHARAN AFRICA; INOCULATION RATES; EARTH-OBSERVATION; WESTERN KENYA; TRANSMISSION; URBANIZATION; RISK AB Background: Remote sensing technology provides detailed spectral and thermal images of the earth's surface from which surrogate ecological indicators of complex processes can be measured. Methods: Remote sensing data were overlaid onto georeferenced entomological and human ecological data randomly sampled during April and May 2001 in the cities of Kisumu (population approximate to 320,000) and Malindi (population approximate to 81,000), Kenya. Grid cells of 270 meters x 270 meters were used to generate spatial sampling units for each city for the collection of entomological and human ecological field-based data. Multispectral Thermal Imager (MTI) satellite data in the visible spectrum at five meter resolution were acquired for Kisumu and Malindi during February and March 2001, respectively. The MTI data were fit and aggregated to the 270 meter x 270 meter grid cells used in field-based sampling using a geographic information system. The normalized difference vegetation index (NDVI) was calculated and scaled from MTI data for selected grid cells. Regression analysis was used to assess associations between NDVI values and entomological and human ecological variables at the grid cell level. Results: Multivariate linear regression showed that as household density increased, mean grid cell NDVI decreased (global F-test=9.81, df 3,72, P-value=<0.01; adjusted R-2=0.26). Given household density, the number of potential anopheline larval habitats per grid cell also increased with increasing values of mean grid cell NDVI (global F-test=14.29, df 3,36, P-value=<0.01; adjusted R-2=0.51). Conclusions: NDVI values obtained from MTI data were successfully overlaid onto georeferenced entomological and human ecological data spatially sampled at a scale of 270 meters x 270 meters. Results demonstrate that NDVI at such a scale was sufficient to describe variations in entomological and human ecological parameters across both cities. C1 Tulane Univ, Sch Publ Hlth & Trop Med, Dept Int Hlth & Dev, New Orleans, LA 70118 USA. Tulane Univ, Sch Publ Hlth & Trop Med, Dept Pharmacol, New Orleans, LA USA. Kenya Govt Med Res Ctr, Ctr Geog Med Res, Kilifi, Kenya. Kenya Govt Med Res Ctr, Ctr Vector Biol & Control Res, Kisumu, Kenya. Univ Oklahoma, Sarkeys Energy Ctr, Inst Sci & Publ Policy, Norman, OK 73019 USA. Int Ctr Insect Physiol & Ecol, Human Hlth Div, Nairobi, Kenya. NASA, Ames Res Ctr, USRA, Moffett Field, CA 94035 USA. Univ Miami, Global Publ Hlth Program, Miami, FL 33152 USA. RP Eisele, TP (reprint author), Tulane Univ, Sch Publ Hlth & Trop Med, Dept Int Hlth & Dev, New Orleans, LA 70118 USA. EM teisele@tulane.edu; jkeating@tulane.edu; cswalm@tulane.edu; cmbogo@kilifi.mimcom.net; AGitheko@kisian.mimcom.net; regens@ou.edu; jgithure@icipe.org; landrews@mail.arc.nasa.gov; jbeier@med.miami.edu NR 27 TC 22 Z9 25 U1 0 U2 4 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1475-2875 J9 MALARIA J JI Malar. J. PD DEC PY 2003 VL 2 AR 44 DI 10.1186/1475-2875-2-44 PG 17 WC Infectious Diseases; Parasitology; Tropical Medicine SC Infectious Diseases; Parasitology; Tropical Medicine GA 767YX UT WOS:000188502400001 ER PT J AU Haan, SI Charalambides, PG Kuhn, JL Patterson, MCL AF Haan, SI Charalambides, PG Kuhn, JL Patterson, MCL TI Supercritical matrix microcracking in brittle matrix plain weave composites under uniaxial tension SO MECHANICS OF MATERIALS LA English DT Article DE ceramic; woven; composites; microcracking; damage; non-linear; stress-induced; degradation ID WOVEN FABRIC COMPOSITES; ELASTIC RESPONSE; DAMAGE ANALYSIS; BEHAVIOR; STRESS; MODULI; CRACK; TIP; MECHANICS; SOLIDS AB A stress induced supercritical non-linear microcracking model is employed as part of an incremental and iterative hierarchical modeling scheme aimed at investigating the evolution of damage in brittle matrix plain weave fabric composites subjected to uniaxial tension. The study focuses exclusively on matrix micro-damage and its effect on the macroscopic non-linear composite response. For a given load increment, the requisite micro-stresses and associated state of matrix microcracking are updated through an iterative converging scheme that employs the semi-analytical approximate model to compute micro-stresses and the discrete microcracking model to evaluate micro-damages. A wide range of non-linear stress-strain curves were obtained through parametric studies. Degradation of the in-plane effective properties of the unit-cell and evolution of the volumetric matrix damage were monitored throughout the simulations. The simulated predictions were then used to develop empirical in-plane effective property degradation laws in terms of the applied loading. Damage-induced macroscopic elastic anisotropies were predicted as was the formation of macroscopic damage zones consistent with discrete micro-fracture events such as inter-bundle matrix cracking, bundle mode-I cracking, and transverse bundle matrix cracking. Stress-strain curves obtained from the model were compared favorably with their experimental counterparts obtained from literature and commercial sources. (C) 2003 Elsevier Ltd. All rights reserved. C1 Univ Maryland Baltimore Cty, Dept Mech Engn, Baltimore, MD 21250 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Ceram Composites Inc, Millersville, MD 21108 USA. RP Charalambides, PG (reprint author), Univ Maryland Baltimore Cty, Dept Mech Engn, 1000 Hilltop Circle, Baltimore, MD 21250 USA. NR 36 TC 2 Z9 3 U1 1 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0167-6636 J9 MECH MATER JI Mech. Mater. PD DEC PY 2003 VL 35 IS 12 BP 1107 EP 1126 DI 10.1016/S0167-6636(03)00006-1 PG 20 WC Materials Science, Multidisciplinary; Mechanics SC Materials Science; Mechanics GA 733QC UT WOS:000186011300001 ER PT J AU Chen, J Tewari, SN Magadi, G De Groh, HC AF Chen, J Tewari, SN Magadi, G De Groh, HC TI Effect of crucible diameter reduction on the convection, macrosegregation, and dendritic morphology during directional solidification of Pb-2.2 wt pct Sb alloy SO METALLURGICAL AND MATERIALS TRANSACTIONS A-PHYSICAL METALLURGY AND MATERIALS SCIENCE LA English DT Article ID PB-SN ALLOYS; STABILITY; GROWTH; FLOW AB The Pb-2.2 wt pct Sb alloy has been directionally solidified in 1, 2-, 3-, and 7-mm-diameter crucibles with planar and dendritic liquid-solid interface morphology. For plane front solidification, the experimentally observed macrosegregation along the solidified length follows the relationship proposed by Favier.([17,18]) Application of a 0.4 T transverse magnetic field has no effect on the extent of convection. Reducing the ampoule diameter appears to decrease the extent of convection. However, extensive convection is still present even in the 1-mm-diameter crucible. An extrapolation of the observed behavior indicates that nearly diffusive transport conditions require ampoules that are about 40 mum in diameter. Reduction of the crucible diameter does not appear to have any significant effect on the primary dendrite spacing. However, it results in considerable distortion of the dendrite morphology and ordering. This is especially true for the 1-mm-diameter samples. C1 Cleveland State Univ, Dept Chem Engn, Cleveland, OH 44115 USA. Amer Bur Shipping, Dept Mat, Houston, TX 77060 USA. NASA, Glenn Res Ctr, Adv Metall Branch, Cleveland, OH 44135 USA. RP Chen, J (reprint author), Cleveland State Univ, Dept Chem Engn, Cleveland, OH 44115 USA. NR 18 TC 10 Z9 10 U1 0 U2 7 PU MINERALS METALS MATERIALS SOC PI WARRENDALE PA 184 THORN HILL RD, WARRENDALE, PA 15086 USA SN 1073-5623 J9 METALL MATER TRANS A JI Metall. Mater. Trans. A-Phys. Metall. Mater. Sci. PD DEC PY 2003 VL 34A IS 12 BP 2985 EP 2990 DI 10.1007/s11661-003-0197-7 PG 6 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA 753QC UT WOS:000187241200027 ER PT J AU Jones, JH AF Jones, JH TI Constraints on the structure of the martian interior determined from the chemical and isotopic systematics of SNC meteorites SO METEORITICS & PLANETARY SCIENCE LA English DT Article; Proceedings Paper CT Workshop on Unmixing the SNCs CY OCT 11-13, 2002 CL LUNAR & PLANETARY INST, HOUSTON, TEXAS HO LUNAR & PLANETARY INST ID MANTLE-CRUST SYSTEM; TERRESTRIAL PLANETS; OXYGEN FUGACITY; MARS; EVOLUTION; BASALTS; STATE; DIFFERENTIATION; GEOCHEMISTRY; NEODYMIUM AB The crystallization ages of martian (SNC) meteorites give evidence that martian volcanism has continued until recent times-perhaps until the present. These meteorites also indicate that the mantle source regions of this volcanism are modestly to extremely depleted by terrestrial standards. These 2 observations produce a conundrum. How is it that such depleted source regions have produced basaltic magma for such a long time? This contribution attempts to quantify the radiogenic heat production in 2 distinct martian mantle source regions: those of the shergottites and nalchlites. Compared to the depleted upper mantle of the Earth (MORB), the nakhlite source region is depleted by about a factor of 2, and the shergottite source region is depleted by a factor of 6. According to current geophysical models, the nakhlite source contains the minimum amount of radioactive heat production to sustain whole-mantle convection and basalt generation over geologic time. A corollary of this conclusion is that the shergottite source contains much too little radioactivity to produce recent (<200 Ma) basalts. A model martian interior with a deep nakhlite mantle that is insulated by a shallow shergottite mantle may allow basalt production from both source regions if the divide between the nakhtite-shergottite mantles acts as a thermal boundary layer. Similarities between lunar and martian isotopic reservoirs indicate that the Moon and Mars may have experienced similar styles of differentiation. C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Jones, JH (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM jjones2@ems.jsc.nasa.gov NR 38 TC 35 Z9 35 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 DEC PY 2003 VL 38 IS 12 BP 1807 EP 1814 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 771TQ UT WOS:000188802500007 ER PT J AU Jonker, PG van der Klis, M Kouveliotou, C Mendez, M Lewin, WHG Belloni, T AF Jonker, PG van der Klis, M Kouveliotou, C Mendez, M Lewin, WHG Belloni, T TI MS 1603.6+2600: an accretion disc corona source? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; stars : individual : MS 1603.6+2600; stars : neutron; X-rays : stars ID X-RAY BINARY; PERSISTENT EMISSION; QUIESCENCE; 4U-2129+47; CHANDRA; SYSTEM; TRANSIENTS; DISCOVERY; BURSTERS; FLARES AB We have observed the eclipsing low-mass X-ray binary MS 1603.6 + 2600 with Chandra for 7 ks. The X-ray spectrum is well fit with a single absorbed power law with an index of similar to2. We find a clear sinusoidal modulation in the X-ray light curve with a period of 1.7 +/- 0.2 h, consistent with the period of 1.85 h found before. However, no (partial) eclipses were found. We argue that if the X-ray flare observed in earlier X-ray observations was a type I X-ray burst, then the source can only be an accretion disc corona source at a distance of similar to11-24 kpc (implying a height above the Galactic disc of similar to8-17 kpc). It has also been proposed in the literature that MS 1603.76 + 2600 is a dipper at similar to75 kpc. We argue that, in this dipper scenario, the observed optical properties of MS 1603.6 + 2600 are difficult to reconcile with the optical properties one would expect on the basis of comparisons with other high-inclination, low-mass X-ray binaries, unless the X-ray flare was not a type I X-ray burst. In that case, the source can be a nearby soft X-ray transient accreting at a quiescent rate, as was proposed by Hakala et al., or a high-inclination source at similar to15-20 kpc. C1 Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Natl Space Sci & Technol Ctr, Space Sci Res Ctr, Huntsville, AL 35805 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. SRON, Natl Inst Space Res, NL-3584 CA Utrecht, Netherlands. MIT, Dept Phys, Cambridge, MA 02138 USA. MIT, Space Res Ctr, Cambridge, MA 02138 USA. Osserv Astron Brera, INAF, I-23807 Merate, Italy. RP Jonker, PG (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. RI Mendez, Mariano/C-8011-2012 OI Mendez, Mariano/0000-0003-2187-2708 NR 30 TC 8 Z9 8 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 1 PY 2003 VL 346 IS 2 BP 684 EP 688 DI 10.1046/j.1365-2966.2003.07123.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745QE UT WOS:000186698700033 ER PT J AU Mingo, N Yang, L Li, D Majumdar, A AF Mingo, N Yang, L Li, D Majumdar, A TI Predicting the thermal conductivity of Si and Ge nanowires SO NANO LETTERS LA English DT Article ID SILICON NANOWIRES; QUANTUM-WELL; PHONON; SUPERLATTICES AB theoretically predict the thermal conductivity versus temperature dependence of Si and Ge nanowires. Three methods are compared: the traditional Callaway and Holland approaches, and our "real dispersions" approach. Calculations with the former two show large disagreements with experimental data. On the contrary, the real dispersions approach yields good agreement with experiments for Si nanowires; between 37 and 115 nm wide, approximately. In all cases, only bulk data are used as inputs for the calculation. Predictions for Ge nanowires of varying diameters are given, enabling future experimental verification. C1 NASA, Ames Res Ctr, Eloret Corp, Moffett Field, CA 94035 USA. Univ Calif Berkeley, Dept Mech Engn, Berkeley, CA 94720 USA. RP Mingo, N (reprint author), NASA, Ames Res Ctr, Eloret Corp, Moffett Field, CA 94035 USA. RI Li, Deyu/D-2938-2012 OI Li, Deyu/0000-0001-8364-0924 NR 30 TC 183 Z9 185 U1 2 U2 30 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 DEC PY 2003 VL 3 IS 12 BP 1713 EP 1716 DI 10.1021/nl034721i PG 4 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 753BF UT WOS:000187211000018 ER PT J AU Koehne, J Chen, H Li, J Cassell, AM Ye, Q Ng, HT Han, J Meyyappan, M AF Koehne, J Chen, H Li, J Cassell, AM Ye, Q Ng, HT Han, J Meyyappan, M TI Ultrasensitive label-free DNA analysis using an electronic chip based on carbon nanotube nanoelectrode arrays SO NANOTECHNOLOGY LA English DT Article ID NUCLEIC-ACIDS; ELECTROCATALYSIS; FABRICATION AB We report the detection of DNA PCR amplicons using an ultrasensitive label-free electronic technique based on multiwalled carbon nanotube (MWNT) nanoelectrode arrays embedded in an SiO2 matrix. Specific PCR amplicons are reliably detected using electrochemical (EC) methods through allele-specific oligonucleotide hybridization. The inherent guanine bases in the DNA amplicon target of similar to300 bases serve as signal moieties with the aid of Ru(bpy)(3)(2+) mediators, providing an amplified anodic current associated with the oxidation of guanine groups at the nanoelectrode surface. The reduced size and density of the nanoelectrode array provided by MWNTs dramatically improves the sensitivity of EC detection. In addition, the abundant guanine bases in target DNA produce a large signal. Less than similar to 1000 target amplicons can be detected on a microspot, approaching the sensitivity limit of conventional laser-based fluorescence techniques. This method also eliminates the labelling requirement and makes the measurements much simpler. This platform can be employed for developing highly automated electronic chips with multiplex nanoelectrode arrays for quick DNA analysis. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Li, J (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM jli@mail.arc.nasa.gov RI Li, Jun/H-7771-2013 OI Li, Jun/0000-0002-3689-8946 NR 21 TC 109 Z9 111 U1 1 U2 19 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0957-4484 EI 1361-6528 J9 NANOTECHNOLOGY JI Nanotechnology PD DEC PY 2003 VL 14 IS 12 BP 1239 EP 1245 AR PII S0957-4484(03)66806-6 DI 10.1088/0957-4484/14/12/001 PG 7 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Science & Technology - Other Topics; Materials Science; Physics GA 761ZC UT WOS:000187944500003 PM 21444977 ER PT J AU Runyan, MC Ade, PAR Bock, JJ Bond, JR Cantalupo, C Contaldi, CR Daub, MD Goldstein, JH Gomez, PL Holzapfel, WL Kuo, CL Lange, AE Lueker, M Newcomb, M Peterson, JB Pogosyan, D Romer, AK Ruhl, J Torbet, E Woolsey, D AF Runyan, MC Ade, PAR Bock, JJ Bond, JR Cantalupo, C Contaldi, CR Daub, MD Goldstein, JH Gomez, PL Holzapfel, WL Kuo, CL Lange, AE Lueker, M Newcomb, M Peterson, JB Pogosyan, D Romer, AK Ruhl, J Torbet, E Woolsey, D TI First results from the arcminute cosmology bolometer array receiver SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT Workshop on the Cosmic Microwave Background Radiation and its Polarization CY MAR 19-22, 2003 CL MINNEAPOLIS, MINNESOTA DE cosmic microwave background - instrumentation; observations ID PROBE WMAP OBSERVATIONS; ANGULAR POWER SPECTRUM; MICROWAVE BACKGROUND ANISOTROPY; PARAMETERS; SIMULATIONS AB We review the first science results from the Arcminute Cosmology Bolometer Array Receiver (ACBAR); a multi-frequency millimeter-wave receiver optimized for observations of the Cosmic Microwave Background (CMB) and the Sunyaev-Zel'dovich (SZ) effect in clusters of galaxies. ACBAR was installed on the 2 m Viper telescope at the South Pole in January 2001 and the results presented here incorporate data through July 2002. We present the power spectrum of the CMB at 150 GHz over the range l = 150-3000 measured by ACBAR as well as estimates for the values of the cosmological parameters within the context of ACDM models. We find that the inclusion of Omega(Lambda) greatly improves the fit to the power spectrum. We also observe a slight excess of small-scale anisotropy at 150 GHz; if interpreted as power from the SZ effect of unresolved clusters, the measured signal is consistent with CBI and BIMA within the context of the SZ power spectrum models tested. (C) 2003 Elsevier B.V. All rights reserved. C1 CALTECH, Dept Phys Math & Astron, Pasadena, CA 91125 USA. Univ Wales Coll Cardiff, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 1A1, Canada. Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA. Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RI Peterson, Jeffrey/O-4794-2014; Holzapfel, William/I-4836-2015 OI Peterson, Jeffrey/0000-0003-1340-818X; NR 24 TC 7 Z9 7 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD DEC PY 2003 VL 47 IS 11-12 BP 915 EP 923 DI 10.1016/j.newar.2003.09.001 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 758TG UT WOS:000187665800007 ER PT J AU Kogut, A AF Kogut, A TI Reionization and structure formation with ARCADE SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT Workshop on the Cosmic Microwave Background Radiation and its Polarization CY MAR 19-22, 2003 CL MINNEAPOLIS, MINNESOTA ID UNIVERSE; Z-SIMILAR-TO-6; SIGNATURES; EVOLUTION; OBJECTS; GHZ AB Structure formation in the early universe is expected to produce a cosmological background of free-free emission. The Absolute Radiometer for Cosmology, Astrophysics, and Diffuse Emission (ARCADE) will measure the spectrum of the cosmic microwave background at centimeter wavelengths to detect this signature of structure formation. I describe the ARCADE instrument and the cryogenic engineering required to achieve millikelvin accuracy at such long wavelengths. Published by Elsevier B.V. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kogut, A (reprint author), NASA, Goddard Space Flight Ctr, Code 685, Greenbelt, MD 20771 USA. RI Kogut, Alan/D-6293-2012 NR 16 TC 4 Z9 4 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD DEC PY 2003 VL 47 IS 11-12 BP 945 EP 951 DI 10.1016/j.newar.2003.09.005 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 758TG UT WOS:000187665800011 ER PT J AU Kogut, A AF Kogut, A TI WMAP polarization results SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT Workshop on the Cosmic Microwave Background Radiation and its Polarization CY MAR 19-22, 2003 CL MINNEAPOLIS, MINNESOTA ID MICROWAVE-ANISOTROPY-PROBE; BACKGROUND POLARIZATION; COSMOLOGICAL OBJECTS; REIONIZATION; UNIVERSE; Z-SIMILAR-TO-6; HISTORY; SPECTRA; QUASARS; STARS AB The Wilkinson Microwave Anisotropy Probe (WMAP) has mapped the full sky in Stokes I, Q, and U parameters at frequencies 23, 33, 41, 61, and 94 GHz. We detect correlations between the temperature and polarization maps significant at more than 10 standard deviations. The correlations are inconsistent with instrument noise and are significantly larger than the upper limits established for potential systematic errors. Correlations on small angular scales are consistent with the the signal expected from adiabatic initial conditions. We detect excess power on large angular scales consistent with an early epoch of reionization. A model-independent fit to reionization optical depth yields results consistent with the best-fit LambdaCDM model, with best-fit value tau = 0.17 +/- 0.04 at 68% confidence, including systematic and foreground uncertainties. Published by Elsevier B.V. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kogut, A (reprint author), NASA, Goddard Space Flight Ctr, Code 685, Greenbelt, MD 20771 USA. RI Kogut, Alan/D-6293-2012 NR 34 TC 4 Z9 4 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD DEC PY 2003 VL 47 IS 11-12 BP 977 EP 986 DI 10.1016/j.newar.2003.09.029 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 758TG UT WOS:000187665800014 ER PT J AU Lamarre, JM Puget, JL Bouchet, F Ade, PAR Benoit, A Bernard, JP Bock, J De Bernardis, P Charra, J Couchot, F Delabrouille, J Efstathiou, G Giard, M Guyot, G Lange, A Maffei, B Murphy, A Pajot, F Piat, M Ristorcelli, I Santos, D Sudiwala, R Sygnet, JF Torre, JP Yurchenko, V Yvon, D AF Lamarre, JM Puget, JL Bouchet, F Ade, PAR Benoit, A Bernard, JP Bock, J De Bernardis, P Charra, J Couchot, F Delabrouille, J Efstathiou, G Giard, M Guyot, G Lange, A Maffei, B Murphy, A Pajot, F Piat, M Ristorcelli, I Santos, D Sudiwala, R Sygnet, JF Torre, JP Yurchenko, V Yvon, D TI The Planck High Frequency Instrument, a third generation CMB experiment, and a full sky submillimeter survey SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT Workshop on the Cosmic Microwave Background Radiation and its Polarization CY MAR 19-22, 2003 CL MINNEAPOLIS, MINNESOTA AB The High Frequency Instrument (HFI) of Planck is the most sensitive CMB experiment ever planned. Statistical fluctuations (photon noise) of the CMB itself will be the major limitation to the sensitivity of the CMB channels. Higher frequency channels will measure galactic foregrounds. Together with the Low Frequency Instrument, this will make a unique tool to measure the full sky and to separate the various components of its spectrum. Measurement of the polarization of these various components will give a new picture of the CMB. In addition, HFI will provide the scientific community with new full sky maps of intensity and polarization at six frequencies, with unprecedented angular resolution and sensitivity. This paper describes the logics that prevailed to define the HFI and the performances expected from this instrument. It details several features of the HFI design that has not been published up to now. (C) 2003 Published by Elsevier B.V. C1 Observ Paris, LERMA, F-75014 Paris, France. Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. Inst Astrophys, F-75014 Paris, France. Univ Wales Coll Cardiff, Cardiff, S Glam, Wales. CNRS, CRTBT, F-38026 Grenoble, France. CESR, F-31018 Toulouse, France. CALTECH, Jet Prop Lab, Pasadena, CA USA. Univ Roma La Sapienza, Rome, Italy. UPX, IN2P3, Lab Accelerateur Lineaire, F-91405 Orsay, France. Coll France, PCC, F-75231 Paris, France. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. CALTECH, Pasadena, CA 91125 USA. State Univ Maynooth, Dept Phys, Maynooth, Kildare, Ireland. ISN, IN2P3, F-38026 Grenoble, France. CEA, SPP, DAPNIA, Gif Sur Yvette, France. RP Lamarre, JM (reprint author), Observ Paris, LERMA, 61 Bd Observ, F-75014 Paris, France. RI Bouchet, Francois/B-5202-2014; Yvon, Dominique/D-2280-2015; OI de Bernardis, Paolo/0000-0001-6547-6446; Bouchet, Francois/0000-0002-8051-2924 NR 12 TC 64 Z9 65 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD DEC PY 2003 VL 47 IS 11-12 BP 1017 EP 1024 DI 10.1016/j.newar.2003.09.006 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 758TG UT WOS:000187665800019 ER PT J AU Lawrence, CR AF Lawrence, CR TI The low frequency instrument on Planck SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT Workshop on the Cosmic Microwave Background Radiation and its Polarization CY MAR 19-22, 2003 CL MINNEAPOLIS, MINNESOTA C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lawrence, CR (reprint author), CALTECH, Jet Prop Lab, Mailcode 169-327,4800 Oak Grove Dr, Pasadena, CA 91109 USA. OI Villa, Fabrizio/0000-0003-1798-861X NR 0 TC 1 Z9 1 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD DEC PY 2003 VL 47 IS 11-12 BP 1025 EP 1032 DI 10.1016/j.newar.2003.09.009 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 758TG UT WOS:000187665800020 ER PT J AU Montroy, T Ade, PAR Balbi, A 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 Ganga, K Hivon, E Hristov, VV Iacoangeli, A Jaffe, AH Kisner, TS Jones, WC Lange, AE Masi, S Mauskopf, PD MacTavish, C Melchiorri, A Nati, F Natoli, P Netterfield, CB Pascale, E Piacentini, F Pogosyan, D Polenta, G Prunet, S Ricciardi, S Romeo, G Ruhl, JE Torbet, E Tegmark, M Vittorio, N AF Montroy, T Ade, PAR Balbi, A 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 Ganga, K Hivon, E Hristov, VV Iacoangeli, A Jaffe, AH Kisner, TS Jones, WC Lange, AE Masi, S Mauskopf, PD MacTavish, C Melchiorri, A Nati, F Natoli, P Netterfield, CB Pascale, E Piacentini, F Pogosyan, D Polenta, G Prunet, S Ricciardi, S Romeo, G Ruhl, JE Torbet, E Tegmark, M Vittorio, N TI Measuring CMB polarization with BOOMERANG SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT Workshop on the Cosmic Microwave Background Radiation and its Polarization CY MAR 19-22, 2003 CL MINNEAPOLIS, MINNESOTA ID ANISOTROPY AB BOOMERANG is a balloon-borne telescope designed for long duration (LDB) flights around Antarctica. The second LDB flight of BOOMERANG took place in January 2003. The primary goal of this flight was to measure the polarization of the CMB. The receiver uses polarization sensitive bolometers at 145 GHz. Polarizing grids provide polarization sensitivity at 245 and 345 GHz. We describe the BOOMERANG telescope noting changes made for 2003 LDB flight, and discuss some of the issues involved in the measurement of polarization with bolometers. Lastly, we report on the 2003 flight and provide an estimate of the expected results. (C) 2003 Elsevier B.V. All rights reserved. C1 Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA. Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. Jet Prop Lab, Pasadena, CA USA. Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 1A1, Canada. LBNL, Natl Energy Res Sci Comp Ctr, Berkeley, CA USA. CNR, IFAC, I-50127 Florence, Italy. CSU Dominguez Hills, Carson, CA USA. CALTECH, IPAC, Pasadena, CA 91125 USA. Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. Univ Alberta, Dept Phys, Edmonton, AB, Canada. Inst Astrophys, F-75014 Paris, France. Ist Nazl Geofis, I-00161 Rome, Italy. Univ Penn, Dept Phys, Philadelphia, PA 19104 USA. Univ Toronto, Dept Phys, Toronto, ON, Canada. Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, London SW7 2AZ, England. Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy. Univ Calif Berkeley, Ctr Particle Astrophys, Berkeley, CA 94720 USA. RP Montroy, T (reprint author), Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA. RI Jaffe, Andrew/D-3526-2009; de Gasperis, Giancarlo/C-8534-2012; Nati, Federico/I-4469-2016; Piacentini, Francesco/E-7234-2010; OI Hivon, Eric/0000-0003-1880-2733; Ricciardi, Sara/0000-0002-3807-4043; Melchiorri, Alessandro/0000-0001-5326-6003; de Gasperis, Giancarlo/0000-0003-2899-2171; Nati, Federico/0000-0002-8307-5088; 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 NR 10 TC 15 Z9 15 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD DEC PY 2003 VL 47 IS 11-12 BP 1057 EP 1065 DI 10.1016/j.newar.2003.09.011 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 758TG UT WOS:000187665800023 ER PT J AU Johnson, BR Abroe, ME Ade, P Bock, J Borrill, J Collins, JS Ferreira, P Hanany, S Jaffe, AH Jones, T Lee, AT Levinson, L Matsumura, T Rabii, B Renbarger, T Richards, PL Smoot, GF Stompor, R Tran, HT Winant, CD AF Johnson, BR Abroe, ME Ade, P Bock, J Borrill, J Collins, JS Ferreira, P Hanany, S Jaffe, AH Jones, T Lee, AT Levinson, L Matsumura, T Rabii, B Renbarger, T Richards, PL Smoot, GF Stompor, R Tran, HT Winant, CD TI MAXIPOL: a balloon-borne experiment for measuring the polarization anisotropy of the cosmic microwave background radiation SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT Workshop on the Cosmic Microwave Background Radiation and its Polarization CY MAR 19-22, 2003 CL MINNEAPOLIS, MINNESOTA ID MAXIMA-1 AB We discuss MAXIPOL, a bolometric balloon-borne experiment designed to measure the E-mode polarization anisotropy of the cosmic microwave background radiation (CMB) on angular scales of 10' to 2degrees. MAXIPOL is the first CMB experiment to collect data with a polarimeter that utilizes a rotating half-wave plate and fixed wire-grid polarizer. We present the instrument design, elaborate on the polarimeter strategy and show the instrument performance during flight with some time domain data. Our primary dataset was collected during a 26 h turnaround flight that was launched from the National Scientific Ballooning Facility in Ft. Sumner, New Mexico in May 2003. During this flight five regions of the sky were mapped. Data analysis is in progress. (C) 2003 Elsevier B.V. All rights reserved. C1 Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. Univ Wales Coll Cardiff, Dept Phys & Astron, Cardiff CF1 3NS, S Glam, Wales. Jet Prop Lab, Pasadena, CA USA. Lawrence Berkeley Natl Lab, Computat Res Div, Berkeley, CA USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. Univ Oxford, Oxford OX1 2JD, England. Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA USA. Weizmann Inst Sci, Dept Particle Phys, IL-76100 Rehovot, Israel. RP Johnson, BR (reprint author), Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. RI Jaffe, Andrew/D-3526-2009 NR 12 TC 19 Z9 19 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD DEC PY 2003 VL 47 IS 11-12 BP 1067 EP 1075 DI 10.1016/j.newar.2003.09.034 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 758TG UT WOS:000187665800024 ER PT J AU Church, S Ade, P Bock, J Bowden, M Carlstrom, J Ganga, K Gear, W Hinderks, J Hu, W Keating, B Kovac, J Lange, A Leitch, E Mallie, O Melhuish, S Murphy, A Rusholme, B O'Sullivan, C Piccirillo, L Pryke, C Taylor, A Thompson, K AF Church, S Ade, P Bock, J Bowden, M Carlstrom, J Ganga, K Gear, W Hinderks, J Hu, W Keating, B Kovac, J Lange, A Leitch, E Mallie, O Melhuish, S Murphy, A Rusholme, B O'Sullivan, C Piccirillo, L Pryke, C Taylor, A Thompson, K TI QUEST on DASI: a South Pole CMB polarization experiment SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT Workshop on the Cosmic Microwave Background Radiation and its Polarization CY MAR 19-22, 2003 CL MINNEAPOLIS, MINNESOTA AB QUEST on DASI is a ground-based, high-sensitivity, high-resolution (l(max) similar to 2500) experiment designed to map CMB polarization at 100 and 150 GHz and to measure the power spectra from E-modes, B-modes from lensing of the CMB, and B-modes from primordial gravitational waves. The experiment comprises a 2.6 m Cassegrain optical system, equipped with an array of 62 polarization-sensitive bolometers (PSBs), located at the South Pole. The instrument is designed to minimize systematic effects; features include differencing of pairs of orthogonal PSBs within a single feed, a rotatable achromatic waveplate, and axisymmetric rotatable optics. In addition the South Pole location allows both repeatable and highly controlled observations. QUEST on DASI will commence operation in early 2005. (C) 2003 Elsevier B.V. All rights reserved. C1 Stanford Univ, Dept Phys, Stanford, CA 94305 USA. Univ Wales Coll Cardiff, Dept Phys & Astron, Cardiff, S Glam, Wales. Jet Prop Lab, Pasadena, CA USA. Univ Chicago, Dept Phys, Chicago, IL 60637 USA. CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. CALTECH, Dept Phys Math & Astron, Pasadena, CA 91125 USA. Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland. Univ Edinburgh, Inst Astron, Edinburgh, Midlothian, Scotland. RP Church, S (reprint author), Stanford Univ, Dept Phys, Stanford, CA 94305 USA. RI Melhuish, Simon/B-1299-2016 OI Melhuish, Simon/0000-0001-8725-4991 NR 7 TC 32 Z9 33 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD DEC PY 2003 VL 47 IS 11-12 BP 1083 EP 1089 DI 10.1016/j.newar.2003.09.033 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 758TG UT WOS:000187665800026 ER PT J AU Gaier, T Lawrence, CR Seiffert, MD Wells, MM Kangaslahti, P Dawson, D AF Gaier, T Lawrence, CR Seiffert, MD Wells, MM Kangaslahti, P Dawson, D TI Amplifier arrays for CMB polarization SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT Workshop on the Cosmic Microwave Background Radiation and its Polarization CY MAR 19-22, 2003 CL MINNEAPOLIS, MINNESOTA ID DESIGN AB Cryogenic low noise amplifier technology has been successfully used in the study of the cosmic microwave background (CMB). Monolithic millimeter wave integrated circuit (MMIC) technology makes the mass production of coherent detection receivers feasible. We have produced large numbers of MMIC amplifiers for CMB measurements. We have also demonstrated the viability of multi-function multi-chip modules as sensitive receiver front-ends. MMIC integration makes it possible to realize massive arrays of receivers suitable for measurements of the polarization of the CMB. We describe the development of the unit cell of such an array and the development plans for implementation. Published by Elsevier B.V. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Gaier, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 12 TC 7 Z9 7 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD DEC PY 2003 VL 47 IS 11-12 BP 1167 EP 1171 DI 10.1016/j.newar.2003.09.010 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 758TG UT WOS:000187665800037 ER PT J AU Bindschadler, R AF Bindschadler, R TI Landsat coverage of the earth at high latitudes SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING LA English DT Article AB Overlapping coverage of Landsat imagery at high latitudes is examined systematically and quantitatively. The Earth is separated into "row strips" aligned with the Landsat World Reference System (WRS), and the multi-scene coverage of Landsat imagery is divided into three types of areas: extended, missing and overlap. Varying image orientation and narrowing row-strip width with increasing latitude are shown to have major impacts on these three areas. The dependencies of these coverage areas on skipping image collections from adjacent paths are calculated, This forms the basis for sampling strategies that can significantly reduce the number of images required to obtain full ground coverage at high latitudes. The calculations show that Antarctica can be covered with approximately one-third the total number of scene opportunities. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Bindschadler, R (reprint author), NASA, Goddard Space Flight Ctr, Code 916, Greenbelt, MD 20771 USA. EM Robert.A.Bindschadler@nasa.gov NR 1 TC 8 Z9 8 U1 0 U2 1 PU AMER SOC PHOTOGRAMMETRY PI BETHESDA PA 5410 GROSVENOR LANE SUITE 210, BETHESDA, MD 20814-2160 USA SN 0099-1112 J9 PHOTOGRAMM ENG REM S JI Photogramm. Eng. Remote Sens. PD DEC PY 2003 VL 69 IS 12 BP 1333 EP 1339 PG 7 WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Geology; Remote Sensing; Imaging Science & Photographic Technology GA 817RL UT WOS:000221194500003 ER PT J AU Boulatov, A Smelyanskiy, VN AF Boulatov, A Smelyanskiy, VN TI Quantum adiabatic algorithms and large spin tunnelling SO PHYSICAL REVIEW A LA English DT Article AB We study the quantum adiabatic evolution algorithm with different evolution paths that correspond to different control Hamiltonians H(tau) sampled from a random ensemble. The algorithm is applied to a random binary optimization problem where the cost function is symmetric with respect to the permutation of individual bits. We investigate the method proposed by Farhi when different evolution paths preserve the bit symmetry of the control Hamiltonians H(tau) and are generated by an ensemble of random 8x8 matrices. In this case, the algorithm dynamics is completely described in terms of the motion of a spin-n/2 system. We show that different evolution paths can be parametrized by a small number of independent parameters that are expansion coefficients of H(tau) in a certain universal set of operators. One of these operators is responsible for avoiding the tunnelling for the spin-n/2 system and the corresponding coefficient determines the algorithm complexity for a given problem instance. We show that any problem instance can be solved in polynomial time by applying one of the two universal path modifications (due to the possible reflection symmetry of the problem). We show that a successful evolution path of the algorithm always corresponds to the trajectory of a classical spin n/2 and provide a complete characterization of such paths. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Boulatov, A (reprint author), NASA, Ames Res Ctr, MS 269-3, Moffett Field, CA 94035 USA. EM boulatov@email.arc.nasa.gov; vadim.N.smelyanskiy@nasa.gov RI Boulatov, Alexei/A-7096-2014 NR 23 TC 9 Z9 9 U1 0 U2 0 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 DEC PY 2003 VL 68 IS 6 AR 062321 DI 10.1103/PhysRevA.68.062321 PG 12 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 761DP UT WOS:000187885000039 ER PT J AU Shresta, S Hu, BL Phillips, NG AF Shresta, S Hu, BL Phillips, NG TI Moving atom-field interaction: Correction to the Casimir-Polder effect from coherent backaction SO PHYSICAL REVIEW A LA English DT Article ID ENERGY-MOMENTUM TENSOR; QUANTUM ELECTRODYNAMICS; ADIABATIC REGULARIZATION; FORCES AB The Casimir-Polder force is an attractive force between a polarizable atom and a conducting or dielectric boundary. Its original computation was in terms of the Lamb shift of the atomic ground state in an electromagnetic field modified by boundary conditions along the wall and assuming a stationary atom. We calculate the corrections to this force due to a moving atom, demanding maximal preservation of entanglement generated by the moving atom-conducting wall system. We do this by using nonperturbative path integral techniques which allow for coherent backaction and thus can treat non-Markovian processes. We recompute the atom-wall force for a conducting boundary by allowing the bare atom-EMF ground state to evolve (or self-dress) into the interacting ground state. We find a clear distinction between the cases of stationary and adiabatic motions. Our result for the retardation correction for adiabatic motion is up to twice as much as that computed for stationary atoms. We give physical interpretations of both the stationary and adiabatic atom-wall forces in terms of alteration of the virtual photon cloud surrounding the atom by the wall and the Doppler effect. C1 Univ Maryland, Dept Phys, College Pk, MD 20742 USA. NASA, SSAI, Astron & Solar Phys Lab, GSFC, Greenbelt, MD 20771 USA. RP Shresta, S (reprint author), Univ Maryland, Dept Phys, College Pk, MD 20742 USA. EM sanjiv@physics.umd.edu; hub@physics.umd.edu; Nicholas.G.Phillips@gsfc.nasa.gov NR 28 TC 19 Z9 19 U1 1 U2 4 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 DEC PY 2003 VL 68 IS 6 AR 062101 DI 10.1103/PhysRevA.68.062101 PG 13 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 761DP UT WOS:000187885000007 ER PT J AU Smith, SJ Lozano, JA Tayal, SS Chutjian, A AF Smith, SJ Lozano, JA Tayal, SS Chutjian, A TI Electron excitation cross sections for the 2s(2)2p P-2(o)-> 2s2p(2) P-4 and 2s2p(2) D-2 transitions in O3+ SO PHYSICAL REVIEW A LA English DT Article ID B-LIKE IONS; O-IV; IMPACT EXCITATION; ATOMIC DATA; C-II; S-IV; LINES; INTERCOMBINATION; EMISSION AB Experimental and theoretical electron-excitation cross sections are reported for the 2s(2)2p P-2(o)-->2s2p(2) P-4 and -->2s2p(2) D-2 transitions in O3+. The transition energies are centered at 8.85 and 15.7 eV, respectively. Measurements are made using the energy-loss merged-beams method. The center-of-mass energy range covered is 6.1 (below threshold) to 19.3 eV. Comparison is made with results of new calculations in a 25-state R-matrix theory and with results in a previous eight-state R-matrix calculation. The presence of rich resonance structure is confirmed in both experiment and theory. In most cases there is good agreement in the magnitude of cross section, and energy location of the resonances. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Clark Atlanta Univ, Dept Phys, Atlanta, GA 30314 USA. RP Smith, SJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 17 TC 8 Z9 8 U1 0 U2 0 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 DEC PY 2003 VL 68 IS 6 AR 062708 DI 10.1103/PhysRevA.68.062708 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 761DP UT WOS:000187885000056 ER PT J AU Cartoixa, X Ting, DZY McGill, TC AF Cartoixa, X Ting, DZY McGill, TC TI Description of bulk inversion asymmetry in the effective-bond-orbital model SO PHYSICAL REVIEW B LA English DT Article ID BAND-STRUCTURE; ELECTRONIC-STRUCTURE; SEMICONDUCTORS; SUPERLATTICES; PARAMETERS AB We have extended the effective-bond-orbital model (EBOM) method [Y. C. Chang, Phys. Rev. B 37, 8215 (1988)] to include the effects of the bulk inversion asymmetry (BIA) present in zinc blendes. This is accomplished without adding to the number of basis states or extending the range of interaction. We have also investigated a variant form of the EBOM proposed in the original formulation that offers improved zone-center behavior, but may also generate spurious solutions in heterostructure calculations due to poor description of bulk zone-boundary band structure. We offer suggestions for avoiding this problem so that this variant form of EBOM may be used safely. In general, we find that the addition of BIA effects in EBOM results in improved descriptions of zone-center band structure, but also in a loss of accuracy far from the Brillouin-zone center. We illustrate the use of the BIA extension with band-structure calculations for bulk GaSb. We show that the spin splitting predicted by the extended EBOM method for an AlSb/GaSb superlattice is in good agreement with k.p calculations that include BIA effects. C1 CALTECH, TJ Watson Sr Labs Appl Phys 128 95, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Cartoixa, X (reprint author), CALTECH, TJ Watson Sr Labs Appl Phys 128 95, Pasadena, CA 91125 USA. EM tcm@ssdp.caltech.edu NR 31 TC 26 Z9 26 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 DEC PY 2003 VL 68 IS 23 AR 235319 DI 10.1103/PhysRevB.68.235319 PG 7 WC Physics, Condensed Matter SC Physics GA 764DL UT WOS:000188186400076 ER PT J AU Mingo, N Yang, L AF Mingo, N Yang, L TI Phonon transport in nanowires coated with an amorphous material: An atomistic Green's function approach SO PHYSICAL REVIEW B LA English DT Article ID LATTICE THERMAL-CONDUCTIVITY; DIELECTRIC QUANTUM WIRES; SILICON NANOWIRES; CONDUCTANCE; GERMANIUM; SURFACES; MODEL; FLOW AB An approach is presented for the atomistic study of phonon transport in real dielectric nanowires via Green's functions. The formalism is applied to investigate the phonon flow through nanowires coated by an amorphous material. Examples for a simple model system and for real Si nanowires coated by silica are given. New physical results emerge for these systems, regarding the character of the transition from ballistic to diffusive transport, the low-temperature thermal conductance, and the influence of the wire-coating interface on the thermal transport. An efficient treatment of phonon scattering by the amorphous coating is also developed, representing a valuable tool for the investigation of thermal conduction through amorphous-coated nanowires. C1 NASA, Ames Res Ctr, Eloret Corp, Moffett Field, CA 94035 USA. RP NASA, Ames Res Ctr, Eloret Corp, Mail Stop N229-1, Moffett Field, CA 94035 USA. NR 45 TC 196 Z9 196 U1 6 U2 28 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 DEC PY 2003 VL 68 IS 24 AR 245406 DI 10.1103/PhysRevB.68.245406 PG 12 WC Physics, Condensed Matter SC Physics GA 766TP UT WOS:000188391900079 ER PT J AU Ting, DZY Cartoixa, X AF Ting, DZY Cartoixa, X TI Bulk inversion asymmetry enhancement of polarization efficiency in nonmagnetic resonant-tunneling spin filters SO PHYSICAL REVIEW B LA English DT Article ID SEMICONDUCTOR HETEROSTRUCTURE; RELAXATION ANISOTROPY; QUANTUM-WELLS; INJECTION AB We analyze the effect of bulk inversion asymmetry (BIA) on the efficiency of nonmagnetic heterostructure resonant tunneling spin filters grown along [001]. We show that when only structural inversion asymmetry (SIA) is taken into account, the theoretical upper limit of current spin polarization for the Rashba effect resonant tunneling spin filter with a one-sided collector geometry is 2/pi(approximate to63.7%), independent of the direction of the one-sided collector. When both SIA and BIA effects are included, we can significantly enhance or degrade current spin polarization from the SIA-only value by varying the collection angle, with the best and worst directions, respectively, being [110] and [1 (1) over bar0] (or vice versa, depending on the relative sign between the SIA and BIA coefficients). We can similarly improve the spin filtering efficiency of Rashba effect resonant tunneling spin filters that rely on the use of a lateral electric field in the emitter region to induce spin polarization, simply by applying the field along [110] (or [1 (1) over bar0]). C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Illinois, Dept Phys, Urbana, IL 61801 USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 30 TC 28 Z9 28 U1 0 U2 3 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 DEC PY 2003 VL 68 IS 23 AR 235320 DI 10.1103/PhysRevB.68.235320 PG 8 WC Physics, Condensed Matter SC Physics GA 764DL UT WOS:000188186400077 ER PT J AU Carmel, Y Shkvarunets, A Nusinovich, GS Rodgers, J Bliokh, YP Goebel, DM AF Carmel, Y Shkvarunets, A Nusinovich, GS Rodgers, J Bliokh, YP Goebel, DM TI Electron beam dynamics in Pasotron microwave sources SO PHYSICS OF PLASMAS LA English DT Article ID BACKWARD-WAVE OSCILLATOR; EFFICIENCY AB The Pasotron is a high efficiency (similar to50%), plasma-assisted microwave generator in which the beam electrons exhibit two-dimensional motion in the slow wave structure. The electron beam propagates in the ion-focusing regime (Bennett pinch regime) because there is no applied magnetic field. Since initially only the neutral gas is present in the vacuum system and the ions in the neutralizing plasma channel are produced only due to the beam impact ionization, the beam dynamics in Pasotrons is inherently a nonstationary process, and important for efficient operation. The present paper contains results of experimental studies of stationary and nonstationary effects in the beam dynamics in Pasotrons and their theoretical interpretation. (C) 2003 American Institute of Physics. C1 Univ Maryland, Inst Res Elect & Appl Phys, College Pk, MD 20742 USA. Technion Israel Inst Technol, Haifa, Israel. Jet Propuls Lab, Pasadena, CA USA. RP Carmel, Y (reprint author), Univ Maryland, Inst Res Elect & Appl Phys, College Pk, MD 20742 USA. RI Bliokh, Yury/A-3743-2013; Nusinovich, Gregory/C-1314-2017 OI Nusinovich, Gregory/0000-0002-8641-5156 NR 11 TC 11 Z9 11 U1 0 U2 4 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-664X J9 PHYS PLASMAS JI Phys. Plasmas PD DEC PY 2003 VL 10 IS 12 BP 4865 EP 4873 DI 10.1063/1.1624248 PG 9 WC Physics, Fluids & Plasmas SC Physics GA 746PP UT WOS:000186755000033 ER PT J AU Spilker, L Ferrari, C Cuzzi, JN Showalter, A Pearl, J Wallis, B AF Spilker, L Ferrari, C Cuzzi, JN Showalter, A Pearl, J Wallis, B TI Saturn's rings in the thermal infrared SO PLANETARY AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT 27th General Assembly of the European-Geophysical-Society CY APR 21-26, 2002 CL NICE, FRANCE SP European Geophys Soc DE infrared; planetary rings; rings; Saturn's rings; thermal ID PLANETARY RINGS; BRIGHTNESS TEMPERATURE; PARTICLE SIZES; WATER FROST; VOYAGER-1; EVOLUTION; SYSTEM; ICE; OCCULTATION; SIMULATIONS AB This paper reviews our current knowledge of Saturn's rings' physical properties as derived from thermal infrared observations. Ring particle composition, surface structure and spin as well as the vertical structure of the main rings can be determined. These properties are the key to understand the origin and evolution of Saturn's rings. Ring composition is mainly constrained by observations in the near-infrared but the signature of some probable contaminants present in water ice may also be found at mid-infrared wavelengths. The absence of the silicate signature limits nowadays their mass fraction to 10(-7+/-1). Recent measurements on the thermal inertia of the ring particle surface show it is very low, of the order of 5+/-2 J m(-2) K-1 s(-1/2). New models and observations of the complete crossing of the planetary shadow are needed to attribute this low value either to compact regoliths covered by cracks due to collisions and thermal stresses or to large fluffy and irregular surfaces. Studies of the energy balance of ring particles show a preference for slowly spinning particles in the main rings. Supplementary observations at different phase angles, showing the temperature contrast between night and day sides of particles, and new models including finite spin and thermal inertia, are needed to constrain the actual spin distribution of ring particles. These results can then be compared to numerical simulations of ring dynamics. Many thermal models have been proposed to reproduce observations of the main rings, including alternative mono- or many-particles-thick layers or vertical heterogeneity, with no definitive answer. Observations on the lit and dark faces of rings as a function of longitude, at many incidence and emission angles, would provide prime information on the vertical thermal gradient due to interparticle shadowing from which constraints on the local vertical structure and dynamics can be produced. Future missions such as Cassini will provide new information to further constrain the ring thermal models. (C) 2003 Elsevier Ltd. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Paris 07, F-91191 Gif Sur Yvette, France. CEA Saclay, DSM, DAPNIA, SAp, F-91191 Gif Sur Yvette, France. NASA, Ames Res Ctr 245 3, Moffett Field, CA 94035 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Spilker, L (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 230-205, Pasadena, CA 91109 USA. RI Ferrari, Cecile/P-9735-2016 OI Ferrari, Cecile/0000-0001-5962-7439 NR 61 TC 23 Z9 23 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 DEC PY 2003 VL 51 IS 14-15 BP 929 EP 935 DI 10.1016/j.pss.2003.05.004 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 757NL UT WOS:000187568300003 ER PT J AU Rannou, P McKay, CP Lorenz, RD AF Rannou, P McKay, CP Lorenz, RD TI A model of Titan's haze of fractal aerosols constrained by multiple observations SO PLANETARY AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT 27th General Assembly of the European-Geophysical-Society CY APR 21-26, 2002 CL NICE, FRANCE SP European Geophys Soc DE Titan; atmosphere structure; photometry; haze ID AGGREGATE PARTICLES; PHYSICAL MODEL; ATMOSPHERE; SURFACE; SCATTERING; CLOUDS; SPECTROPHOTOMETRY; WAVELENGTH; TELESCOPE; SPHERES AB We use Titan's geometric albedo to constrain the vertical distribution of the haze. Microphysical models incorporating fractal aggregates do not readily fit the methane features at 0.62 mum band and the dark 0.88 mum of the albedo spectrum simultaneously. We take advantage of this apparent discrepancy to constrain the haze vertical profile. We used the geometric albedo and several results and constraints from other works to better constrain the vertical haze extinction profile, especially in the low stratosphere. The objective of this model is to give a solution that simultaneously fits the main constraints known to apply to the haze. We find that the haze extinction increases with decreasing altitude with a scale height about equal to the atmospheric scale height down to 100 km. Below this altitude, extinction must decrease down to 30 km. This is necessary in order to have enough haze to sustain a relatively high albedo (0.076) in the dark 0.88 mum methane band and to show the 0.62 mum band in the haze continuum. We set the haze production rate around 7 x 10(-14) kg m(-2) s(-1), and the aerosols production altitude around 400 km (or at pressure 1.5 Pa). The physical processes which generate such a profile are not clear. However, purely one-dimensional effects such as condensation, sedimentation, and rainout can be ruled out, and we believe that this relative clearing in Titan's troposphere and lower stratosphere is due to particle horizontal transport by the mean circulation. (C) 2003 Elsevier Ltd. All rights reserved. C1 Univ Paris 06, Serv Aeron, F-75252 Paris, France. NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. RP Rannou, P (reprint author), Univ Paris 06, Serv Aeron, 4 Pl Jussieu,B102, F-75252 Paris, France. RI RANNOU, Pascal/I-9059-2012; Lorenz, Ralph/B-8759-2016 OI Lorenz, Ralph/0000-0001-8528-4644 NR 38 TC 53 Z9 53 U1 0 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD DEC PY 2003 VL 51 IS 14-15 BP 963 EP 976 DI 10.1016/j.pss.2003.05.008 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 757NL UT WOS:000187568300007 ER PT J AU Encrenaz, T Drossart, P Orton, G Feuchtgruber, H Lellouch, E Atreya, SK AF Encrenaz, T Drossart, P Orton, G Feuchtgruber, H Lellouch, E Atreya, SK TI The rotational temperature and column density of H-3(+) in Uranus SO PLANETARY AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT 27th General Assembly of the European-Geophysical-Society CY APR 21-26, 2002 CL NICE, FRANCE SP European Geophys Soc DE infrared spectroscopy; planetary atmospheres; Uranus ID EMISSION; JUPITER; H-3+ AB H-3(+) emission from Uranus has been observed repeatedly for over a decade. However, the details of the emission mechanisms are still 3 poorly understood. In this paper, we discuss our findings from the observations we made in September 2000 and September 2001. The spectrum of Uranus was recorded at the NASA Infrared Telescope Facility using the SpeX instrument between 3 and 5 mum, with a resolving power of 1000. The 3.4-4.1 mum range permits a determination of both the H-3(+) column density and its rotational temperature. The H-3(+) emission, measured at 3.986 mum in the 0.8 x 3.7 arcsec aperture, was 0.031 Jy in September 2000 and 0.053 Jy in September 2001. The rotational temperature was found to be 560 +/- 40 K and 640 +/- 40 K in 2000 and 2001 respectively, with corresponding column densities of 5.1 (+3.2, -1.4) 10(11) and 4.0 (+1.8, -1.0) 10(11) cm(-2). These results extend the baseline for the variability study of the H-3(+) emission (Astrophys. J. 524 (1999) 1059). Previous observations between 1992 and 1998 seemed to indicate a correlation between the H-3(+) intensity and the solar cycle. The current data for 2000 and 2001 appear to be consistent with this general tendency. (C) 2003 Elsevier Ltd. All rights reserved. C1 Observ Paris, LESIA, F-92190 Meudon, France. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. RP Encrenaz, T (reprint author), Observ Paris, LESIA, F-92190 Meudon, France. NR 17 TC 3 Z9 3 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD DEC PY 2003 VL 51 IS 14-15 BP 1013 EP 1016 DI 10.1016/j.pss.2003.05.010 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 757NL UT WOS:000187568300011 ER PT J AU Wilson, EH Atreya, SK AF Wilson, EH Atreya, SK TI Chemical sources of haze formation in Titan's atmosphere SO PLANETARY AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT 27th General Assembly of the European-Geophysical-Society CY APR 21-26, 2002 CL NICE, FRANCE SP European Geophys Soc DE Titan; atmospheric composition; photochemistry; organic chemistry ID POLYCYCLIC AROMATIC-HYDROCARBONS; VOYAGER INFRARED OBSERVATIONS; ABSOLUTE RATE-CONSTANT; ULTRAVIOLET PHOTOCHEMISTRY; RATE COEFFICIENTS; HYDROGEN-CYANIDE; VERTICAL DISTRIBUTIONS; OPTICAL-PROPERTIES; ORGANIC-CHEMISTRY; LOW-TEMPERATURE AB A prominent feature of Titan's atmosphere is a thick haze region that acts as the end product of hydrocarbon and nitrile chemistry. Using a one-dimensional photochemical model, an investigation into the chemical mechanisms responsible for the formation of this haze region is conducted. The model derives profiles for Titan's atmospheric constituents that are consistent with observations. Included is an updated benzene profile that matches more closely with-recent ISO observations (Icarus 161 (2003) 383), replacing the profile given in the benzene study of Wilson et al. (J. Geophys. Res. 108 (2003) 5014). Using these profiles, pathways from polyynes, aromatics, and nitriles are considered, as well as possible copolymerization among the pathways. The model demonstrates that the growth of polycyclic aromatic hydrocarbons throughout the lower stratosphere plays an important role in furnishing the main haze layer, with nitriles playing a secondary role. The peak chemical production of haze layer ranges from 140 to 300 km peaking at an altitude of 220 km, with a production rate of 3.2 x 10(-14) g cm(-2) s(-1). Possible mechanisms for polymerization and copolymerization and suggestions for further kinetic study are discussed, along with the implications for the distribution of haze in Titan's atmosphere. (C) 2003 Elsevier Ltd. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. RP Wilson, EH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 169-237, Pasadena, CA 91109 USA. NR 95 TC 129 Z9 132 U1 1 U2 17 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 DEC PY 2003 VL 51 IS 14-15 BP 1017 EP 1033 DI 10.1016/j.pss.2003.06.003 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 757NL UT WOS:000187568300012 ER PT J AU Velli, M AF Velli, M TI MHD turbulence and the heating of astrophysical plasmas SO PLASMA PHYSICS AND CONTROLLED FUSION LA English DT Article; Proceedings Paper CT 30th EPS Conference on Controlled Fusion and Plasma Physics CY JUL 07-11, 2003 CL ST PETERSBURG, RUSSIA ID INTERPLANETARY ALFVENIC FLUCTUATIONS; QUIET SOLAR CORONA; WAVES; WIND; DISSIPATION; NANOFLARES; SPECTRUM; REGIONS; MODEL; FLOW AB Magnetohydrodynamic (MHD) turbulence plays a major role in the dynamics and thermodynamics of astrophysical plasmas in many environments and over a wide range of scales and parameters: primary examples are the heating of stellar and accretion disk coronae, acceleration of stellar winds, and star formation in molecular clouds. In the case of the solar wind and corona in situ measurements and remote-sensing observations have given the most detailed experimental knowledge of the interplay between large-scale driving forces, the development of a turbulent cascade, and the collisionless kinetics of dissipation, than in any other natural magnetized plasma environment (with the possible exception of the earth's magnetosphere). The questions of coronal and solar wind acceleration will be reviewed here within the general context of MHD turbulence and nonlinear interactions, from the large-scale energy sources and driving to the dissipation scales dominated by wave-particle interactions, from the special role of Alfven waves to the naturally intermittent nature of coronal energy release and solar flares. C1 Univ Florence, Dipartimento Astron & Sci Spazio, I-50121 Florence, Italy. Jet Propuls Lab, Pasadena, CA USA. RP Velli, M (reprint author), Univ Florence, Dipartimento Astron & Sci Spazio, I-50121 Florence, Italy. EM velli@arcetri.astro.it NR 51 TC 11 Z9 11 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0741-3335 J9 PLASMA PHYS CONTR F JI Plasma Phys. Control. Fusion PD DEC PY 2003 VL 45 SU 12A BP A205 EP A216 AR PII S0741-3335(03)70577-6 DI 10.1088/0741-3335/45/12A/014 PG 12 WC Physics, Fluids & Plasmas SC Physics GA 763JD UT WOS:000188080900016 ER PT J AU Seagroves, S Harker, J Laughlin, G Lacy, J Castellano, T AF Seagroves, S Harker, J Laughlin, G Lacy, J Castellano, T TI Detection of intermediate-period transiting planets with a network of small telescopes: transitsearch.org SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID EXTRASOLAR GIANT PLANETS; ATMOSPHERE; PHOTOMETRY; HD-209458; RADII; STAR AB We describe a project (transitsearch. org) currently attempting to discover transiting intermediate-period planets orbiting bright parent stars, and we simulate that project's performance. The discovery of such a transit would be an important astronomical advance, bridging the critical gap in understanding between HD 209458b and Jupiter. However, the task is made difficult by intrinsically low transit probabilities and small transit duty cycles. This project's efficient and economical strategy is to photometrically monitor stars that are known (from radial velocity surveys) to bear planets, using a network of widely spaced observers with small telescopes. These observers, each individually capable of precision (1%) differential photometry, monitor candidates during the time windows in which the radial velocity solution predicts a transit if the orbital inclination is close to 90degrees. We use Monte Carlo techniques to simulate the performance of this network, performing simulations with different configurations of observers in order to optimize coordination of an actual campaign. Our results indicate that transitsearch. org can reliably rule out or detect planetary transits within the current catalog of known planet-bearing stars. A distributed network of skilled amateur astronomers and small college observatories is a cost-effective method for discovering the small number of transiting planets with periods in the range 10 days < P < 200 days that orbit bright (V < 11) stars. C1 Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO, Lick Observ, Santa Cruz, CA 95064 USA. NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Seagroves, S (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO, Lick Observ, Santa Cruz, CA 95064 USA. NR 22 TC 30 Z9 30 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 DEC PY 2003 VL 115 IS 814 BP 1355 EP 1362 DI 10.1086/380421 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745GT UT WOS:000186681500001 ER PT J AU Shukla, S Seal, S Nguyen, P Ng, HT Meyyappan, M AF Shukla, S Seal, S Nguyen, P Ng, HT Meyyappan, M TI Transmission electron microscopy sample preparation of tin oxide nanowire sensor using focused ion-beam milling technique SO SENSOR LETTERS LA English DT Article ID GAS-SENSING PROPERTIES; THIN-FILMS; NO2 AB Transmission electron microscopy (TEM) sample preparation using a focused ion-beam (FIB) milling technique, utilizing a Ga+ ion beam at 30 kV, is systematically demonstrated, for the first time, for a nanocrystalline, highly porous indium oxide-doped tin oxide (In-SnO2) nanowire thin-film gas sensor. The In-SnO2 nanowires are deposited on a sapphire (Al2O3) Substrate by a catalyst-assisted heteroepitaxy technique. The subsequent FIB and TEM characterization of the present nanowire thin-film gas sensor show that, under the given processing conditions, an In-SnO2 nanowire thin film with a thickness of 5-6 mu m contains a highly entangled and porous network of nanowires, with a diameter of 100 nm and a nanocrystallite size less than 5 nm. These characteristics of the present In-SnO2 nanowire thin film are highly suitable for typical gas-sensing applications. C1 Univ Cent Florida, Mech Mat Aerosp Engn Dept, Orlando, FL 32816 USA. Univ Cent Florida, Adv Mat Proc & Anal Ctr, Orlando, FL 32816 USA. NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Seal, S (reprint author), Univ Cent Florida, Mech Mat Aerosp Engn Dept, Orlando, FL 32816 USA. EM sseal@pegasus.cc.ucf.edu NR 12 TC 2 Z9 2 U1 1 U2 4 PU AMER SCIENTIFIC PUBLISHERS PI STEVENSON RANCH PA 25650 NORTH LEWIS WAY, STEVENSON RANCH, CA 91381-1439 USA SN 1546-198X J9 SENS LETT JI Sens. Lett. PD DEC PY 2003 VL 1 IS 1 BP 75 EP 78 DI 10.1166/sl.2003.005 PG 4 WC Chemistry, Analytical; Electrochemistry; Instruments & Instrumentation; Physics, Applied SC Chemistry; Electrochemistry; Instruments & Instrumentation; Physics GA 004PT UT WOS:000234765400014 ER PT J AU Artho, C Havelund, K Biere, A AF Artho, C Havelund, K Biere, A TI High-level data races SO SOFTWARE TESTING VERIFICATION & RELIABILITY LA English DT Article; Proceedings Paper CT 1st International Workshop on Verification and Validation of Enterprise Information Systems (VVEIS 2003) CY APR, 2003 CL ANGERS, FRANCE DE Java; multi-threading; data races; software verification; consistency ID MODEL-CHECKING; JAVA PROGRAMS AB Data races are a common problem in concurrent and multi-threaded programming. Experience shows that the classical notion of a data race is not powerful enough to capture certain types of inconsistencies occurring in practice. This paper investigates data races on a higher abstraction layer. This enables detection of inconsistent uses of shared variables, even if no classical race condition occurs. For example, a data structure representing a coordinate pair may have to be treated atomically. By lifting the meaning of a data race to a higher level, such problems can now be covered. The paper defines the concepts 'view' and 'view consistency' to give a notation for this novel kind of property. It describes what kinds of errors can be detected with this new definition, and where its limitations are. It also gives a formal guideline for using data structures in a multi-threaded environment. (C) US Government copyright. C1 ETH Zentrum, Inst Comp Syst, CH-8092 Zurich, Switzerland. NASA, Ames Res Ctr, Kestrel Technol, Moffett Field, CA 94035 USA. RP ETH Zentrum, Inst Comp Syst, CH-8092 Zurich, Switzerland. EM artho@inf.ethz.ch NR 38 TC 19 Z9 20 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0960-0833 EI 1099-1689 J9 SOFTW TEST VERIF REL JI Softw. Test. Verif. Reliab. PD DEC PY 2003 VL 13 IS 4 BP 207 EP 227 DI 10.1002/stvr.281 PG 21 WC Computer Science, Software Engineering SC Computer Science GA 765HC UT WOS:000188260200002 ER PT J AU Jones, HP AF Jones, HP TI Data calibration and analysis for He I 1083 nm imaging spectroscopy SO SOLAR PHYSICS LA English DT Article ID CORONAL HOLES; QUIET-SUN; HELIUM; FILAMENT; SPECTRUM; REGION AB Imaging spectroscopy in the He I 1083 nm lines is a powerful tool for probing the top of the chromosphere and bottom of the transition region, but simple techniques for spectral calibration and analysis often fail for this line. A method for spectral flat-fielding using a uniform solar exposure with spectral lines in place is presented and illustrated with 1083 nm data obtained at the National Solar Observatory (NSO) Kitt Peak Vacuum Telescope with the NASA/NSO Spectromagnetograph. An efficient method for analysis of the data producing images in continuum intensity, line-of-sight velocity, equivalent width, central line depth, Doppler width, and line asymmetry is also presented and illustrated. C1 NASA, Goddard Space Flight Ctr, SW Solar Stn, Tucson, AZ 85726 USA. RP Jones, HP (reprint author), NASA, Goddard Space Flight Ctr, SW Solar Stn, POB 23732, Tucson, AZ 85726 USA. EM hjones@noao.edu NR 19 TC 7 Z9 7 U1 0 U2 1 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD DEC PY 2003 VL 218 IS 1-2 BP 1 EP 16 DI 10.1023/B:SOLA.0000013031.13781.66 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 766DM UT WOS:000188330200001 ER PT J AU Kodibagkar, VD Browning, CD Tang, XP Wu, Y Bowman, RC Conradi, MS AF Kodibagkar, VD Browning, CD Tang, XP Wu, Y Bowman, RC Conradi, MS TI Magnetic alignment in nominally non-magnetic hexagonal metal hydrides: NMR SO SOLID STATE NUCLEAR MAGNETIC RESONANCE LA English DT Article DE metal-hydrides; orientation; magnetic alignment; texture; powder lineshapes; preferred orientation ID ELECTRIC-FIELD GRADIENTS; HYDROGEN DIFFUSION; KNIGHT-SHIFT; ZRBE2H1.4; YD3; DYNAMICS AB Powders of three hexagonal metal-hydrides or -deuterides are found to align in 4.4-8.3 T magnetic fields used for NMR. The field-alignment is unexpected, since all three systems have very small susceptibilities, as demonstrated by sharp NMR lines. The extent of alignment runs from nearly complete to barely detectable in ZrBe2(H,D)(x), LuD3, and YD3, respectively. The preferred alignment direction in ZrBe2(H, D)(x) is with the crystallites' c-axis perpendicular to B, while the c-axis and B tend to be parallel in LuD3 and YD3. The susceptibilities chi(\\) and chi(perpendicular to) are determined from bulk magnetization measurements in aligned ZrBe2H1.4 powder. The alignment must be considered for proper analysis of NMR spectra in these and related materials. (C) 2003 Elsevier Inc. All rights reserved. C1 Washington Univ, Dept Phys, St Louis, MO 63130 USA. Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Conradi, MS (reprint author), Washington Univ, Dept Phys, 1 Brookings Dr,Campus Box 1105, St Louis, MO 63130 USA. OI Bowman, Robert/0000-0002-2114-1713 NR 20 TC 4 Z9 4 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 0926-2040 J9 SOLID STATE NUCL MAG JI Solid State Nucl. Magn. Reson. PD DEC PY 2003 VL 24 IS 4 BP 254 EP 262 DI 10.1016/j.ssnmr.2003.08.003 PG 9 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical; Physics, Condensed Matter; Spectroscopy SC Chemistry; Physics; Spectroscopy GA 751QQ UT WOS:000187078800004 PM 14642420 ER PT J AU Weigel, RS Klimas, AJ Vassiliadis, D AF Weigel, R. S. Klimas, A. J. Vassiliadis, D. TI Precursor analysis and prediction of large-amplitude relativistic electron fluxes SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article C1 [Weigel, R. S.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA. [Klimas, A. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Vassiliadis, D.] NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Greenbelt, MD 20771 USA. RP Weigel, RS (reprint author), Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA. EM robert.weigel@lasp.colorado.edu NR 19 TC 5 Z9 5 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 DEC PY 2003 VL 1 IS 3 PG 7 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA V31CR UT WOS:000208862200003 ER PT J AU Zheng, YH Fok, MC Khazanov, GV AF Zheng, Yihua Fok, Mei-Ching Khazanov, George V. TI A radiation belt-ring current forecasting model SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article C1 [Zheng, Yihua] NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Greenbelt, MD 20771 USA. [Fok, Mei-Ching] NASA, Goddard Space Flight Ctr, Interplanetary Phys Branch, Greenbelt, MD 20771 USA. [Khazanov, George V.] NASA, Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. RP Zheng, YH (reprint author), NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Greenbelt, MD 20771 USA. EM yzheng@lepvax.gsfc.nasa.gov RI feggans, john/F-5370-2012 FU University Partnering for Operational Support (UPOS) Program FX We are grateful for the useful discussions with Richard Wolf. We thank Peggy Sloan for developing the visualization software. The LANL SOPA data are provided by Geoff Reeves. This work is supported by the University Partnering for Operational Support (UPOS) Program. NR 35 TC 0 Z9 0 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 DEC PY 2003 VL 1 IS 3 PG 10 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA V31CR UT WOS:000208862200001 ER PT J AU Silver, A Kleinsasser, A Kerber, G Herr, Q Dorojevets, M Bunyk, P Abelson, L AF Silver, A Kleinsasser, A Kerber, G Herr, Q Dorojevets, M Bunyk, P Abelson, L TI Development of superconductor electronics technology for high-end computing SO SUPERCONDUCTOR SCIENCE & TECHNOLOGY LA English DT Article; Proceedings Paper CT International Superconducting Electronics Conference (ISEC 2003) CY JUL 07-11, 2003 CL SYDNEY, AUSTRALIA ID INTEGRATED-CIRCUIT PROCESS; DESIGN; CHIP AB This paper describes our programme to develop and demonstrate ultra-high performance single flux quantum (SFQ) VLSI technology that will enable superconducting digital processors for petaFLOPS-scale computing. In the hybrid technology, multi-threaded architecture, the computational engine to power a petaFLOPS machine at affordable power will consist of 4096 SFQ multi-chip processors, with 50 to 100 GHz clock frequency and associated cryogenic RAM. We present the superconducting technology requirements, progress to date and our plan to meet these requirements. We improved SFQ 2 Nb VLSI by two generations, to a 8 kA cm(-2), 1.25 mum junction process, incorporated new CAD tools into our methodology, demonstrated methods for recycling the bias current and data communication at speeds up to 60 Gb s(-1), both on and between chips through passive transmission lines. FLUX-1 is the most ambitious project implemented in SFQ technology to date, a prototype general-purpose 8 bit microprocessor chip. We are testing the FLUX-1 chip (5K gates, 20 GHz clock) and designing a 32 bit floating-point SFQ multiplier with vector-register memory. We report correct operation of the complete stripline-connected gate library with large bias margins, as well as several larger functional units used in FLUX-1. The next stage will be an SFQ multi-processor machine. Important challenges include further reducing chip supply current and on-chip power dissipation, developing at least 64 kbit, sub-nanosecond cryogenic RAM chips, developing thermally and electrically efficient high data rate cryogenic-to-ambient input/output technology and improving Nb VLSI to increase gate density. C1 Jet Prop Lab, Pasadena, CA 91109 USA. Northrop Grumman Space Technol, Redondo Beach, CA 90278 USA. SUNY Stony Brook, Dept Elect & Comp Engn, Stony Brook, NY 11794 USA. RP Silver, A (reprint author), Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Arnold.H.Silver@JPL.nasa.gov; Alan.W.Kleinsasser@JPL.nasa.gov; George.Kerber@NGC.com; Quentin.Herr@NGC.com; Paul.Bunyk@NGC.com; Lynn.Abelson@NGC.com NR 14 TC 11 Z9 11 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0953-2048 J9 SUPERCOND SCI TECH JI Supercond. Sci. Technol. PD DEC PY 2003 VL 16 IS 12 BP 1368 EP 1374 AR PII S0953-2048(03)67570-6 DI 10.1088/0953-2048/16/12/010 PG 7 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 760DN UT WOS:000187796500010 ER PT J AU DellaCorte, C AF DellaCorte, C TI Keep your feedback rolling! 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. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOC TRIBOLOGISTS & LUBRICATION ENGINEERS PI PARK RIDGE PA 840 BUSSE HIGHWAY, PARK RIDGE, IL 60068 USA SN 0024-7154 J9 TRIBOL LUBR TECHNOL JI Tribol. Lubr. Technol. PD DEC PY 2003 VL 59 IS 12 BP 8 EP 8 PG 1 WC Engineering, Mechanical SC Engineering GA 755DM UT WOS:000187388500002 ER PT J AU Zanoni, VM Goward, SN AF Zanoni, VM Goward, SN TI A new direction in Earth observations from space: IKONOS - Preface SO REMOTE SENSING OF ENVIRONMENT LA English DT Editorial Material C1 NASA, Earth Sci Applicat Directorate, Stennis Space Ctr, MS 39529 USA. Univ Maryland, Dept Geog, College Pk, MD 20742 USA. RP Zanoni, VM (reprint author), NASA, Earth Sci Applicat Directorate, Mail Code MA20, Stennis Space Ctr, MS 39529 USA. NR 16 TC 4 Z9 5 U1 0 U2 0 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 NOV 30 PY 2003 VL 88 IS 1-2 BP 1 EP 2 DI 10.1016/j.rse.2003.08.011 PG 2 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 751QM UT WOS:000187078500001 ER PT J AU Birk, RJ Stanley, T Snyder, GI Hennig, TA Fladeland, MM Policelli, F AF Birk, RJ Stanley, T Snyder, GI Hennig, TA Fladeland, MM Policelli, F TI Government programs for research and operational uses of commercial remote sensing data SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Earth science; commercial remote sensing; multispectral; imagery; digital elevation model; mapping; monitoring; IKONOS; QuickBird; OrbView-3; LIDAR; radar; hyperspectral ID IKONOS AB sThe private sector is delivering products and services derived from an expanding array of airborne and spaceborne remote sensing systems. The successful commercial launches of the IKONOS, QuickBird, and OrbView-3 satellites in 1999, 2001, and 2003, respectively, combined with commercial airborne sensors such as the Positive Systems ADAR 5500 (multi spectral), the Intermap STAR-3i (interferometric synthetic aperture radar), and TerraPoint, LLC, LIDAR System have ushered in an era of expanded capability and capacity for the field of remote sensing of our Earth. Remote sensing data from commercial sensors offer the public and private geospatial information communities important new sources of timely and accurate spatial information that can augment data provided by public-sector remote sensing systems. Several Federal agencies, including the National Aeronautics and Space Administration (NASA), the U.S. Geological Survey, and the National Imagery and Mapping Agency (NIMA), have established data purchase programs and related activities to access, evaluate, and assimilate new commercial remote sensing products to serve research and operational requirements. Plans for future commercial systems and data products indicate an expanding set of data types using hyperspectral, radar, LIDAR, and microwave technologies. The availability of new data sources has established the basis for Federal programs to provide for systematic characterization of the products, consistent with the characterization of data products enabled by traditional sources that include Landsat, SPOT, and the Advanced Very High Resolution Radiometer (AVHRR), An overview of commercial remote sensing initiatives within the National Aeronautics and Space Administration, the U.S. Department of the Interior, and the U.S. Department of Defense (DoD), and of their Joint Agency Commercial Imagery Evaluation (JACIE) team, illustrates these points, highlights lessons learned from these activities, and outlines recommendations for the future. (C) 2003 Elsevier Inc. All rights reserved. C1 NASA, Off Earth Sci, Washington, DC 20546 USA. NASA, Earth Sci Applicat Directorate, Stennis Space Ctr, MS USA. US Geol Survey, Natl Ctr, Reston, VA 22092 USA. Natl Imagery & Mapping Agcy, Bethesda, MD USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Birk, RJ (reprint author), NASA, Off Earth Sci, 300 E St SW, Washington, DC 20546 USA. NR 28 TC 24 Z9 27 U1 1 U2 7 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 NOV 30 PY 2003 VL 88 IS 1-2 BP 3 EP 16 DI 10.1016/j.rse.2003.07.007 PG 14 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 751QM UT WOS:000187078500002 ER PT J AU Zanoni, V Stanley, T Ryan, R Pagnutti, M Baldridge, B Roylance, S Snyder, G Lee, G AF Zanoni, V Stanley, T Ryan, R Pagnutti, M Baldridge, B Roylance, S Snyder, G Lee, G TI The Joint Agency Commercial Imagery Evaluation team: overview and IKONOS joint characterization approach SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Joint Agency Commercial Imagery Evaluation team; IKONOS; remote sensing AB The Joint Agency Commercial Imagery Evaluation (JACIE) team was formed to leverage government agencies' capabilities for the characterization of commercial remote sensing data. The team is composed of staff from the National Aeronautics and Space Administration (NASA), the National Imagery and Mapping Agency (NIMA), and the U.S. Geological Survey (USGS). Each JACIE agency has a vested interest in the purchase and use of commercial imagery to support its research and applications. It is critical that this imagery be assessed for its accuracy and utility. Through JACIE, NASA, NIMA, and USGS jointly characterized image products from Space Imaging's IKONOS satellite. The JACIE team acquired IKONOS imagery of several study sites to perform the assessments. Each JACIE agency performed an aspect of the characterization according to its area of expertise. NASA and its university partners performed a system characterization focusing on radiometric calibration, geopositional accuracy, and spatial resolution assessment; NIMA performed image interpretability and feature extraction evaluations; and the USGS assessed the geopositional accuracy of several IKONOS products. The results of the JACIE team's IKONOS effort, which were discussed with Space Imaging and then presented at an industry - government workshop, ensured and improved overall product quality and benefited both the commercial industry and the government. Additional JACIE activities include the characterization of other commercial products such as those from the DigitalGlobe QuickBird and the Orbital Imaging (Orbimage) OrbView-3 satellites. (C) 2003 Published by Elsevier Inc. C1 NASA, Earth Sci Applicat Directorate MA20, Stennis Space Ctr, MS 39529 USA. Lockheed Martin Space Operat Stennis Program, Stennis Space Ctr, MS 39529 USA. Booz Allen & Hamilton Inc, NIMA Commercial Imagery Program, Mclean, VA 22102 USA. US Geol Survey, Washington, DC 20242 USA. RP Zanoni, V (reprint author), NASA, Earth Sci Applicat Directorate MA20, Stennis Space Ctr, MS 39529 USA. NR 25 TC 8 Z9 8 U1 0 U2 6 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD NOV 30 PY 2003 VL 88 IS 1-2 BP 17 EP 22 DI 10.1016/j.rse.2003.07.005 PG 6 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 751QM UT WOS:000187078500003 ER PT J AU Pagnutti, M Ryan, RE Kelly, M Holekamp, K Zanoni, V Thome, K Schiller, S AF Pagnutti, M Ryan, RE Kelly, M Holekamp, K Zanoni, V Thome, K Schiller, S TI Radiometric characterization of IKONOS multispectral imagery SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE IKONOS; space Imaging; multispectral imagery ID CALIBRATION; SENSORS; SCATTERING AB A radiometric characterization of Space Imaging's IKONOS 4-m multispectral imagery has been performed by a National Aeronautics and Space Administration (NASA) funded team from NASA Stennis Space Center, the University of Arizona Remote Sensing Group (U of A RSG), and South Dakota State University (SDSU). Both intrinsic radiometry and the effects of Space Imaging processing on radiometry were investigated. Relative radiometry was examined with uniform Antarctic and Saharan sites. Absolute radiometric calibration was performed using reflectance-based vicarious calibration methods on several uniform sites imaged by IKONOS coincident with ground-based surface and atmospheric measurements. Ground-based data and the IKONOS spectral response function served as input to radiative transfer codes to generate a top-of-atmosphere (TOA) radiance estimate. Calibration coefficients derived from each vicarious calibration were combined to generate an IKONOS radiometric gain coefficient for each multispectral band assuming a linear response over the full dynamic range of the instrument. These calibration coefficients were made available to Space Imaging, which subsequently adopted them by updating its initial set of calibration coefficients. IKONOS imagery procured through the NASA Scientific Data Purchase was processed with or without a Modulation Transfer Function Compensation (MTFC) kernel. The radiometric effects of this kernel on various scene types were also investigated. (C) 2003 Elsevier Inc. All rights reserved. C1 Remote Sensing Direcotrate, Lockheed Martin Space Operat Stennis Program, Stennis Space Ctr, MS 39529 USA. NASA, Earth Sci Applicat Directorate, Stennis Space Ctr, MS USA. Univ Arizona, Ctr Opt Sci, Remote Sensing Grp, Tucson, AZ 85721 USA. S Dakota State Univ, Dept Phys, Brookings, SD USA. RP Pagnutti, M (reprint author), Remote Sensing Direcotrate, Lockheed Martin Space Operat Stennis Program, Bldg 1105, Stennis Space Ctr, MS 39529 USA. EM Mary.Pagnutti@ssc.nasa.gov RI Thome, Kurtis/D-7251-2012 NR 30 TC 31 Z9 32 U1 0 U2 11 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 NOV 30 PY 2003 VL 88 IS 1-2 BP 53 EP 68 DI 10.1016/j.rse.2003.07.008 PG 16 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 751QM UT WOS:000187078500006 ER PT J AU Morisette, JT Nickeson, JE Davis, P Wang, YJ Tian, YH Woodcock, CE Shabanov, N Hansen, M Cohen, WB Oetter, DR Kennedy, RE AF Morisette, JT Nickeson, JE Davis, P Wang, YJ Tian, YH Woodcock, CE Shabanov, N Hansen, M Cohen, WB Oetter, DR Kennedy, RE TI High spatial resolution satellite observations for validation of MODIS land products: IKONOS observations acquired under the NASA Scientific Data Purchase SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE MODIS; IKONOS; NASA ID LEAF-AREA INDEX; PHOTOSYNTHETICALLY ACTIVE RADIATION; KM AVHRR DATA; LAI PRODUCT; MISR DATA; ALGORITHM; FRACTION; SURFACE; MODELS AB Phase II of the Scientific Data Purchase (SDP) has provided NASA investigators access to data from four different satellite and airborne data sources. the Moderate Resolution Imaging Spectrometer (MODIS) land discipline team (MODLAND) sought to utilize these data in support of land product validation activities with a focus on the EOS Land Validation Core Sites. These sites provide a globally distributed network of sites where field, aircraft, and satellite data are being collected. As much as possible, uniform data sets useful for validation are being made available for the core sites. The globally consistent, high-resolution imagery available from IKONOS are being used for their geolocation accuracy and ability to characterize the landscape at the 1- to 4-m spatial resolution. This paper provides an overview of the MODIS Land Team's validation strategy to incorporate high-resolution imagery and presents three case studies as examples of the use of IKONOS data for MODIS land validation activities. We conclude that the globally consistent data from IKONOS, available through NASA's SDP, have supplied critical validation data sets at a reasonable cost. (C) 2003 Published by Elsevier Inc. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Sci Syst & Applicat Inc, Greenbelt, MD USA. Univ Maryland, Dept Geog, College Pk, MD 20742 USA. Boston Univ, Dept Geog, Boston, MA 02215 USA. US Forest Serv, USDA, Washington, DC USA. Oregon State Univ, Dept Forest Sci, Corvallis, OR 97331 USA. RP Morisette, JT (reprint author), NASA, Goddard Space Flight Ctr, Code 923, Greenbelt, MD 20771 USA. NR 35 TC 25 Z9 26 U1 1 U2 6 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD NOV 30 PY 2003 VL 88 IS 1-2 BP 100 EP 110 DI 10.1016/j.rse.2003.04.003 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 751QM UT WOS:000187078500009 ER PT J AU Hurtt, G Xiao, XM Keller, M Palace, M Asner, GP Braswell, R Brondizio, ES Cardoso, M Carvalho, CJR Fearon, MG Guild, L Hagen, S Hetrick, S Moore, B Nobre, C Read, JM Sa, T Schloss, A Vourlitis, G Wickel, AJ AF Hurtt, G Xiao, XM Keller, M Palace, M Asner, GP Braswell, R Brondizio, ES Cardoso, M Carvalho, CJR Fearon, MG Guild, L Hagen, S Hetrick, S Moore, B Nobre, C Read, JM Sa, T Schloss, A Vourlitis, G Wickel, AJ TI IKONOS imagery for the Large Scale Biosphere-Atmosphere Experiment in Amazonia (LBA) SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE IKONOS; remote sensing; spatial heterogeneity; land use; land cover; LBA ID LARGE-FOOTPRINT LIDAR; CANOPY STRUCTURE; RAIN-FOREST; AVHRR DATA; BIOMASS; VEGETATION; DEFORESTATION; ESTUARY; LANDSAT; BRAZIL AB The LBA-ECO program is one of several international research components under the Brazilian-led Large Scale Biosphere-Atmosphere Experiment in Amazonia (LBA). The field-oriented research activities of this study are organized along transects and include a set of primary field sites, where the major objective is to study land-use change and ecosystem dynamics, and a smaller set of 15 operational eddy flux tower sites, where the major objective is to quantify net exchange Of CO2 with the atmosphere. To supplement these studies and help to address issues of fine-scale spatial heterogeneity and scaling, high-resolution satellite imagery (IKONOS, 1-4 m) have been acquired over some of these study sites. This paper begins with a description of the acquisition strategy and IKONOS holdings for LBA. This section is followed with a review of some of the most promising new applications of these data in LBA. (C) 2003 Elsevier Inc. All rights reserved. C1 Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. Univ New Hampshire, Dept Nat Resources, Durham, NH 03824 USA. US Forest Serv, USDA, Int Inst Trop Forestry, Rio Piedras, PR USA. Stanford Univ, Carnegie Inst Washington, Dept Global Ecol, Stanford, CA 94305 USA. Indiana Univ, Dept Anthropol, Bloomington, IN 47405 USA. EMBRAPA Amazonia Oriental, BR-66095100 Belem, Para, Brazil. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Indiana Univ, Anthropol Ctr Training & Res Global Environm Chan, Bloomington, IN 47405 USA. CPTEC, INPE, BR-12630000 Cachoeira Paulista, SP, Brazil. Syracuse Univ, Maxwell Sch, Dept Geog, Syracuse, NY 13244 USA. Calif State Univ, Dept Sci Biol, San Marcos, CA 92096 USA. Univ Bonn, Dept Ecol & Resource Management, Ctr Dev Res, D-53113 Bonn, Germany. RP Hurtt, G (reprint author), Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. RI Hurtt, George/A-8450-2012; Keller, Michael/A-8976-2012; Asner, Gregory/G-9268-2013; Braswell, Bobby/D-6411-2016; OI Keller, Michael/0000-0002-0253-3359; Asner, Gregory/0000-0001-7893-6421; Braswell, Bobby/0000-0002-4061-9516; Cardoso, Manoel/0000-0003-2447-6882 NR 54 TC 38 Z9 41 U1 2 U2 7 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 NOV 30 PY 2003 VL 88 IS 1-2 BP 111 EP 127 DI 10.1016/j.rse.2003.04.004 PG 17 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 751QM UT WOS:000187078500010 ER PT J AU Masuoka, PM Claborn, DM Andre, RG Nigro, J Gordon, SW Klein, TA Kim, HC AF Masuoka, PM Claborn, DM Andre, RG Nigro, J Gordon, SW Klein, TA Kim, HC TI Use of IKONOS and Landsat for malaria control in the Republic of Korea SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE IKONOS; Landsat; malaria control ID KYUNGGI PROVINCE; LARVAL HABITATS; VILLAGES AB Malaria reemerged in the Republic of Korea (ROK) in 1993. While limited numbers of U.S. soldiers in high-risk areas use chloroquine/primaquine chemoprophylaxis to prevent malaria, control of mosquito larvae through larviciding also can be used to reduce the risk of malaria transmission. In order to estimate the cost of larviciding, accurate estimates of the spatial extent of mosquito larval habitats are necessary. The purpose of this study was to determine whether an accurate estimate of the area covered by mosquito larval habitats can be obtained using Landsat 7 Enhanced Thematic Mapper+ (ETM+) and/or IKONOS data for the Korean test site. To estimate the area covered by larval habitats near Camp Greaves [Paekyeon-Ri, near Tongil-Chon (village)] in the ROK, an IKONOS and a Landsat 7 ETM+ image were classified using a parallelepiped classification. In a comparison with rice paddy field sites, 24 (92%) of the sites were classified correctly on the IKONOS image and 17 (65%) were classified correctly on the Landsat image. Comparing the classifications on a pixel-by-pixel basis, the agreement between the two classifications was 79%. Part of the disagreement was due to the difference in resolution of the two images. In spite of local differences, the two classifications produced similar area estimates. Although either Landsat or IKONOS could be used in Korea for a reasonable estimate of habitat area, only IKONOS can resolve small irrigation ponds. While ponds represent a small portion of the total larval habitat, they are an important source for mosquito breeding during the late rice-growing season in the ROK since they contain higher larval densities. High-resolution imagery, such as IKONOS, would be necessary for planning and implementing treatment of these smaller habitats. (C) 2003 Elsevier Inc. All rights reserved. C1 Uniformed Serv Univ Hlth Sci, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Navy Dis Vector Ecol & Control Ctr, Naval Air Stn, Jacksonville, FL 32212 USA. Uniformed Serv Univ Hlth Sci, Dept Prevent Med & Biometr, Bethesda, MD 20814 USA. USA, Ctr Hlth Promot & Prevent Med, Ft Mcpherson, GA 30330 USA. Prevent Serv Directorate, Med Command 18, Unit 15281, APO, AP 96205 USA. RP Masuoka, PM (reprint author), Uniformed Serv Univ Hlth Sci, Goddard Space Flight Ctr, Code 920, Greenbelt, MD 20771 USA. RI Gordon, Scott/B-8875-2011; Valle, Ruben/A-7512-2013 NR 17 TC 18 Z9 23 U1 0 U2 3 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 NOV 30 PY 2003 VL 88 IS 1-2 BP 187 EP 194 DI 10.1016/j.rse.2003.04.009 PG 8 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 751QM UT WOS:000187078500015 ER PT J AU Goward, SN Townshend, JRG Zanoni, V Policelli, F Stanley, T Ryan, R Holekamp, K Underwood, L Pagnutti, M Fletcher, R AF Goward, SN Townshend, JRG Zanoni, V Policelli, F Stanley, T Ryan, R Holekamp, K Underwood, L Pagnutti, M Fletcher, R TI Acquisition of earth science remote sensing observations from commercial sources: lessons learned from the Space Imaging IKONOS example SO REMOTE SENSING OF ENVIRONMENT LA English DT Article ID LAND-COVER AB Over the last decade, NASA and other federal agencies have been increasingly encouraged to explore commercial sources of land remote sensing data rather than pursuing government-funded sources of these measurements (prior to U.S. Commercial Executive, 2003. U.S. Commercial Remote Sensing Policy. White House, Washington, DC). The science and applications users have been skeptical of this move to commercial sources of observations both because of uncertainty over the capabilities of the private sector and the unsatisfactory outcomes of previous efforts to commercialize satellite-acquired land remote sensing observations. In an effort to more fully explore the potential of commercial remotely sensed land data sources, the NASA Earth Science Enterprise (ESE) implemented an experimental Scientific Data Purchase (SDP) that solicited bids from the private sector to meet ESE-user data needs. The SDP activity spanned nearly 5 years and supplied many US and international researchers with sources of land remote sensing observations that had not been previously available. The images from the Space Imaging IKONOS system provided a particularly good match to the current ESE missions such as Terra and Landsat 7 and therefore serve as focal point in this analysis. Throughout the SDP process, there have been many lessons learned concerning interactions between US industry, government agencies and the science user community. The specifies of the Space Imaging IKONOS experience under the NASA SDP are most valuable with respect to possible future uses of commercial vendors to supply NASA ESE user needs for space-acquired land observations. Areas where valuable lessons were learned included the technical, scientific, proprietary and management aspects of the interactions. As this activity has evolved, user confidence in the technical and scientific qualities of the IKONOS measurements has increased substantially. There are still areas where further progress could be achieved, with respect to proprietary and management aspects of scientific commercial data buys. To date, the NASA scientific and applications users who have examined the IKONOS imagery have found the data to be of high quality, providing substantial value to their specific pursuits. They have found that the novel attributes of IKONOS, particularly in the spatiotemporal domain have introduced new analysis challenges not previously experienced with EOS sensors such as Landsat and MODIS. The technical qualities of the observations have been substantially improved during the SDP activity as a result of independent validation and verification by the Joint Agency Commercial Imagery Evaluation (JACIE) of the IKONOS observations. The experience gained from the Space Imaging IKONOS SDP activity, suggests that US private sector is technically capable of meeting the needs of NASA ESE science and application users. The future success of such interactions between industry, government and users appears to be far more dependent on the organizational and legal aspects of such arrangements than technical capabilities of the data providers. (C) 2003 Elsevier Inc. All rights reserved. C1 Univ Maryland, Dept Geog, Washington, DC 20242 USA. NASA, Earth Sci Applciat Div, Stennis Space Ctr, MS 39529 USA. Remote Sensing Directorate, Lockheed Martin Space Operat Stennis Program, Stennis Space Ctr, MS 39529 USA. RP Goward, SN (reprint author), Univ Maryland, Dept Geog, 2181 LeFrak Hall, Washington, DC 20242 USA. EM sgoward@umd.edu NR 34 TC 3 Z9 3 U1 0 U2 4 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 NOV 30 PY 2003 VL 88 IS 1-2 BP 209 EP 219 DI 10.1016/j.rse.2003.06.007 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 751QM UT WOS:000187078500017 ER PT J AU Mahesh, A Eager, R Campbell, JR Spinhirne, JD AF Mahesh, A Eager, R Campbell, JR Spinhirne, JD TI Observations of blowing snow at the South Pole SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE blowing snow; Antarctica; polar climate ID THRESHOLD WIND-SPEEDS; KATABATIC WINDS; MICROPULSE LIDAR; PART II; ANTARCTICA; MODEL; TRANSPORT; ALTIMETRY; CLOUD AB [ 1] Observations of blowing snow from visual observers' records as well as ground- based infrared and lidar measurements at South Pole Station are analyzed to obtain the first climatology of blowing snow over the Antarctic Plateau. Occurrence frequencies of blowing snow, wind direction and speed during blowing snow events, typical snow layer heights, as well as optical depths are determined. Blowing snow is recorded in roughly one third of the visual observations and occurs under a narrow range of wind directions. Blowing snow layers are usually less than 400 m in thickness but can exceed 1000 m. During blowing snow conditions, these near- surface layers are apparent in lidar backscatter profiles. These layers emit radiances similar to those from optically thin clouds frequently seen over the Antarctic Plateau. Because the near- surface blowing snow layers are frequently present, they are a factor in space- borne laser altimetry and other satellite remote sensing. C1 NASA, Goddard Earth Sci & Technol Ctr, Greenbelt, MD 20771 USA. Valparaiso Univ, Dept Geog & Meteorol, Valparaiso, IN 46383 USA. Sci Syst & Applicat Inc, Lanham, MD 20706 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Mahesh, A (reprint author), NASA, Goddard Earth Sci & Technol Ctr, Code 912, Greenbelt, MD 20771 USA. EM ashwin.mahesh@gsfc.nasa.gov RI Campbell, James/C-4884-2012 OI Campbell, James/0000-0003-0251-4550 NR 36 TC 26 Z9 26 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 29 PY 2003 VL 108 IS D22 AR 4707 DI 10.1029/2002JD003327 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 749QW UT WOS:000186941200002 ER PT J AU Varnai, T Marshak, A AF Varnai, T Marshak, A TI A method for analyzing how various parts of clouds influence each other's brightness SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE clouds; solar radiation; three-dimensional ID INDEPENDENT PIXEL APPROXIMATION; RADIATIVE-TRANSFER; INHOMOGENEOUS CLOUDS; OPTICAL DEPTH; SOLAR-RADIATION; FLUXES; ALBEDO; ATMOSPHERES; FIELDS; MODEL AB [ 1] This paper proposes a method for obtaining new information on three- dimensional ( 3- D) radiative effects that arise from horizontal radiative interactions in heterogeneous clouds. Unlike current radiative transfer models, it can not only calculate how 3- D effects change radiative quantities at any given point but can also determine which areas contribute to these 3- D effects, to what degree, and through what mechanisms. The new method uses Monte Carlo radiative transfer simulations to generate numerous photon trajectories through the cloud field, and then it examines the radiative processes along each trajectory. After describing the proposed method, the paper illustrates its new capabilities both for detailed case studies and for the statistical processing of large data sets. Because the proposed method makes it possible, for the first time, to link a particular change in cloud properties to the resulting 3- D effect, it can be used to develop new types of radiative transfer parameterizations. Encouraging initial results suggest that such parameterizations will be able to incorporate 3- D effects in practical applications currently limited to 1- D theory, such as remote sensing of cloud properties and dynamical cloud modeling. C1 NASA, Goddard Space Flight Ctr, Climate & Radiat Branch, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. RP Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 20771 USA. EM varnai@climate.gsfc.nasa.gov RI Marshak, Alexander/D-5671-2012 NR 35 TC 14 Z9 15 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 29 PY 2003 VL 108 IS D22 AR 4706 DI 10.1029/2003JD003561 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 749QW UT WOS:000186941200004 ER PT J AU Bell, JF Squyres, SW Herkenhoff, KE Maki, JN Arneson, HM Brown, D Collins, SA Dingizian, A Elliot, ST Hagerott, EC Hayes, AG Johnson, MJ Johnson, JR Joseph, J Kinch, K Lemmon, MT Morris, RV Scherr, L Schwochert, M Shepard, MK Smith, GH Sohl-Dickstein, JN Sullivan, RJ Sullivan, WT Wadsworth, M AF Bell, JF Squyres, SW Herkenhoff, KE Maki, JN Arneson, HM Brown, D Collins, SA Dingizian, A Elliot, ST Hagerott, EC Hayes, AG Johnson, MJ Johnson, JR Joseph, J Kinch, K Lemmon, MT Morris, RV Scherr, L Schwochert, M Shepard, MK Smith, GH Sohl-Dickstein, JN Sullivan, RJ Sullivan, WT Wadsworth, M TI Mars Exploration Rover Athena Panoramic Camera (Pancam) investigation SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; multispectral imaging; space missions; Mars; Exploration Rover ID PATHFINDER LANDING SITE; BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; MARTIAN ATMOSPHERE; IRON-OXIDES; VIKING LANDERS; IMAGER; DUST; SOILS; SURFACE; ROCKS AB The Panoramic Camera (Pancam) investigation is part of the Athena science payload launched to Mars in 2003 on NASA's twin Mars Exploration Rover ( MER) missions. The scientific goals of the Pancam investigation are to assess the high-resolution morphology, topography, and geologic context of each MER landing site, to obtain color images to constrain the mineralogic, photometric, and physical properties of surface materials, and to determine dust and aerosol opacity and physical properties from direct imaging of the Sun and sky. Pancam also provides mission support measurements for the rovers, including Sun-finding for rover navigation, hazard identification and digital terrain modeling to help guide long-term rover traverse decisions, high-resolution imaging to help guide the selection of in situ sampling targets, and acquisition of education and public outreach products. The Pancam optical, mechanical, and electronics design were optimized to achieve these science and mission support goals. Pancam is a multispectral, stereoscopic, panoramic imaging system consisting of two digital cameras mounted on a mast 1.5 m above the Martian surface. The mast allows Pancam to image the full 360degrees in azimuth and +/- 90degrees in elevation. Each Pancam camera utilizes a 1024 x 1024 active imaging area frame transfer CCD detector array. The Pancam optics have an effective focal length of 43 mm and a focal ratio of f/20, yielding an instantaneous field of view of 0.27 mrad/pixel and a field of view of 16degrees x 16degrees. Each rover's two Pancam "eyes'' are separated by 30 cm and have a 1degrees toe-in to provide adequate stereo parallax. Each eye also includes a small eight position filter wheel to allow surface mineralogic studies, multispectral sky imaging, and direct Sun imaging in the 400 - 1100 nm wavelength region. Pancam was designed and calibrated to operate within specifications on Mars at temperatures from - 55degrees to + 5degreesC. An onboard calibration target and fiducial marks provide the capability to validate the radiometric and geometric calibration on Mars. C1 Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Univ Washington, Dept Astron, Seattle, WA 98195 USA. GHS Opt, Pasadena, CA 91101 USA. Bloomsburg Univ Penn, Dept Geog & Geosci, Bloomsburg, PA 17817 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. Univ Aarhus, Inst Phys & Astron, DK-8000 Aarhus, Denmark. US Geol Survey, Branch Astrogeol, Flagstaff, AZ 86001 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Cornell Univ, Dept Astron, 402 Space Sci Bldg, Ithaca, NY 14853 USA. EM jfb8@cornell.edu; squyres@astrosun.tn.cornell.edu; kherkenhoff@usgs.gov; justin.n.maki@jpl.nasa.gov; hma6@cornell.edu; dbrown@mail1.jpl.nasa.gov; stewart.a.collins@jpl.nasa.gov; arsham.dingizian@jpl.nasa.gov; stythe.t.elliot@jpl.nasa.gov; edward.c.hagerott@jpl.nasa.gov; agh4@cornell.edu; mjj8@cornell.edu; jrjohnson@usgs.gov; jj21@cornell.edu; kjartan@ifa.au.dk; lemmon@physics.tamu.edu; richard.v.morris1@jsc.nasa.gov; lawrence.m.scherr@jpl.nasa.gov; mark.a.schwochert@jpl.nasa.gov; mshepard@bloomu.edu; raybender@att.net; jns9@cornell.edu; sullivan@cuspif.tn.cornell.edu; woody@astro.washington.edu; mark.v.wadsworth@jpl.nasa.gov RI Johnson, Jeffrey/F-3972-2015; Lemmon, Mark/E-9983-2010; Hayes, Alexander/P-2024-2014; Kinch, Kjartan/C-5742-2015 OI Lemmon, Mark/0000-0002-4504-5136; Hayes, Alexander/0000-0001-6397-2630; Kinch, Kjartan/0000-0002-4629-8880 NR 71 TC 133 Z9 135 U1 2 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 NOV 29 PY 2003 VL 108 IS E12 AR 8063 DI 10.1029/2003JE002070 PG 30 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 749RG UT WOS:000186942200001 ER PT J AU Pan, M Sheffield, J Wood, EF Mitchell, KE Houser, PR Schaake, JC Robock, A Lohmann, D Cosgrove, B Duan, QY Luo, L Higgins, RW Pinker, RT Tarpley, JD AF Pan, M Sheffield, J Wood, EF Mitchell, KE Houser, PR Schaake, JC Robock, A Lohmann, D Cosgrove, B Duan, QY Luo, L Higgins, RW Pinker, RT Tarpley, JD TI Snow process modeling in the North American Land Data Assimilation System (NLDAS): 2. Evaluation of model simulated snow water equivalent SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE snow water equivalent; land surface modeling ID HEAT-BALANCE; ETA-MODEL; COVER; PRECIPITATION; SURFACE; HYDROLOGY; VARIABILITY; TEMPERATURE; HEMISPHERE; AIRBORNE AB [1] This is the second part of a study on the cold season process modeling in the North American Land Data Assimilation System ( NLDAS). The first part concentrates on the assessment of model simulated snow cover extent. In this second part, the focus is on the evaluation of simulated snow water equivalent ( SWE) from the four land surface models ( Noah, MOSAIC, SAC and VIC) in the NLDAS. Comparisons are made with observational data from the Natural Resources Conservation Service's Snowpack Telemetry ( SNOTEL) network for a 3- year retrospective period at selected sites in the mountainous regions of the western United States. All models show systematic low bias in the maximum annual simulated SWE that is most notable in the Cascade and Sierra Nevada regions where differences can approach 1000 mm. Comparison of NLDAS precipitation forcing with SNOTEL measurements revealed a large bias in the NLDAS annual precipitation which may be lower than the SNOTEL record by up to 2000 mm at certain stations. Experiments with the VIC model indicated that most of the bias in SWE is removed by scaling the precipitation by a regional factor based on the regression of the NLDAS and SNOTEL precipitation. Individual station errors may be reduced further still using precipitation scaled to the local station SNOTEL record. Furthermore, the NLDAS air temperature is shown to be generally colder in winter months and biased warmer in spring and summer when compared to the SNOTEL record, although the level of bias is regionally dependent. Detailed analysis at a selected station indicate that errors in the air temperature forcing may cause the partitioning of precipitation into snowfall and rainfall by the models to be incorrect and thus may explain some of the remaining errors in the simulated SWE. C1 Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. NOAA, Natl Weather Serv, Off Hydrol Dev, Silver Spring, MD 20910 USA. NOAA, NWS, NCEP, Climate Predict Ctr, Camp Springs, MD USA. NOAA, NWS, NCEP, Environm Modeling Ctr, Camp Springs, MD 20746 USA. Univ Maryland, Dept Meteorol, College Pk, MD 20742 USA. Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ 08901 USA. NOAA, NESDIS, Off Res & Applicat, Camp Springs, MD 20746 USA. RP Pan, M (reprint author), Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. EM justin@princeton.edu RI Sheffield, Justin/A-6388-2008; Luo, Lifeng/C-8734-2009; Pinker, Rachel/F-6565-2010; Pan, Ming/B-6841-2011; Houser, Paul/J-9515-2013; Duan, Qingyun/C-7652-2011; Robock, Alan/B-6385-2016 OI Pan, Ming/0000-0003-3350-8719; Houser, Paul/0000-0002-2991-0441; Duan, Qingyun/0000-0001-9955-1512; NR 44 TC 88 Z9 90 U1 1 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 NOV 26 PY 2003 VL 108 IS D22 AR 8850 DI 10.1029/2003JD003994 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 749QV UT WOS:000186941100003 ER PT J AU Vogel, B Muller, R Deshler, T Grooss, JU Karhu, J McKenna, DS Muller, M Toohey, D Toon, GC Stroh, F AF Vogel, B Muller, R Deshler, T Grooss, JU Karhu, J McKenna, DS Muller, M Toohey, D Toon, GC Stroh, F TI Vertical profiles of activated ClO and ozone loss in the Arctic vortex in January and March 2000: In situ observations and model simulations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE chlorine monoxide (ClO); chlorine activation; ozone loss; TRIPLE; CLaMS; THESEO 2000 ID POLAR STRATOSPHERIC CLOUDS; CHEMICAL LAGRANGIAN MODEL; NITRIC-ACID TRIHYDRATE; SOLAR PROTON EVENTS; WINTER STRATOSPHERE; HETEROGENEOUS INTERACTIONS; SULFURIC-ACID; COSMIC-RAYS; LOSS RATES; DEPLETION AB [ 1] In situ observations of ClO mixing ratios obtained from a balloonborne instrument launched in Kiruna on 27 January 2000 and on 1 March 2000 are presented. ClO mixing ratios and quasi- simultaneously observed ozone loss are compared to model simulations performed with the Chemical Lagrangian Model of the Stratosphere ( CLaMS). ClO mixing ratios are simulated initializing the model simulations for early winter conditions. Sensitivity studies are performed to explore the impact of the surface area of the background aerosol, of denitrification, and of the recently reported kinetics of the ClO self- reaction [ Bloss et al., 2001] on simulated ClO. For 27 January 2000, model simulations agree with rate constants reported by Bloss et al. [ 2001], whereas for 1 March 2000 simulations employing rate constants reported by Bloss et al. [ 2001] and by Sander et al. [ 2000] reproduce the ClO measurements. The impact of uncertainties arising from accumulated errors along the calculated backward trajectories and uncertainties within temperatures derived from the UK Met Office are also studied. For both flights, simulated ClO show a good overall agreement with measured ClO within uncertainties arising from accumulated errors along air parcel histories. We find a layer of low ClO mixing ratios < 100 pptv between 600 and 620 K for the flight on 27 January 2000 and between 525 and 550 K on 1 March 2000. For this layer, measured ClO is substantially lower than simulated ClO. Potential causes are discussed, but the discrepancy remains unexplained at present. Furthermore, for 1 March 2000, an overall agreement is found between model simulations and measurements by the HALOE instrument of HCl and NOx (= NO + NO2) for all altitudes considered. We conclude that denitrification occurred up to a potential temperature of approximate to 550 K ( approximate to 24 km altitude) on 1 March 2000. Finally, model simulations show that between late January and 1 March, a significant ozone loss of about 0.8 - 1.8 ppmv is derived between 425 and 490 K of potential temperature in agreement with measured ozone loss and correlated with the enhanced ClO. For 1 March 2000, 77 +/- 10 DU is obtained as an estimate of the loss in column ozone. C1 Forschungszentrum Julich, Inst Stratosphar Chem ICG 1, D-52425 Julich, Germany. Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82071 USA. Finnish Meteorol Inst, FIN-99600 Sodankyla, Finland. Natl Ctr Atmospher Res, Boulder, CO 80307 USA. Goethe Univ Frankfurt, Inst Meteorol & Geophys, D-60325 Frankfurt, Germany. Univ Colorado, Program Atmospher & Ocean Sci, Boulder, CO 80309 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Vogel, B (reprint author), Forschungszentrum Julich, Inst Stratosphar Chem ICG 1, Postfach 1913, D-52425 Julich, Germany. EM b.vogel@fz-juelich.de; ro.mueller@fz-juelich.de; deshler@uwyo.edu; j.-u.grooss@fz-juelich.de; juha.karhu@fmi.fi; danny@acd.ucar.edu; m.mueller@meteor.uni-frankfurt.de; toohey@colorado.edu; geoffrey.c.toon@jpl.nasa.gov; f.stroh@fz-juelich.de RI Stroh, Fred/A-6505-2009; Toohey, Darin/A-4267-2008; Muller, Rolf/A-6669-2013; GrooSS, Jens-Uwe/A-7315-2013; Vogel, Barbel/A-9988-2013; McKenna, Daniel/E-7806-2014 OI Stroh, Fred/0000-0002-4492-2977; Toohey, Darin/0000-0003-2853-1068; Muller, Rolf/0000-0002-5024-9977; GrooSS, Jens-Uwe/0000-0002-9485-866X; McKenna, Daniel/0000-0002-4360-4782 NR 75 TC 17 Z9 17 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 26 PY 2003 VL 108 IS D22 AR 8334 DI 10.1029/2002JD002564 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 749QV UT WOS:000186941100001 ER PT J AU Kwok, R Cunningham, GF Nghiem, SV AF Kwok, R Cunningham, GF Nghiem, SV TI A study of the onset of melt over the Arctic Ocean in RADARSAT synthetic aperture radar data SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article DE melt onset; Arctic ice cover; radar remote sensing; Lagrangian ice motion ID MULTICHANNEL MICROWAVE RADIOMETER; SEA-ICE; PASSIVE-MICROWAVE; SNOWMELT ONSET; SIGMA-DEGREES; REGIONS AB [ 1] The regional melt onset signal of Lagrangian elements of Arctic sea ice in RADARSAT synthetic aperture radar ( SAR) data during the spring of 1998 is examined. The melt signal is clearly detectable not only in backscatter changes over multiyear ice but also first- year ice and mixtures of these ice types. This allows a more complete mapping of the progression of melt over the sea ice cover. For the spring of 1998 the onset dates range between 10 May and 29 June. The spatial pattern of melt onset is characterized by sharp boundaries delineating distinct regions with relatively uniform onset dates. This pattern appears to be associated with moisture and warm air brought in by a lowpressure trough and the timing of a rain event reported at the Surface Heat Budget of the Arctic Ocean ( SHEBA) camp. Measurements from the SHEBA camp show good correspondence between the timing of melt in SAR imagery and the onset of albedo drop off associated with the beginning of summer. Onset dates are compared with the timing of the zero crossing of the temperature records from drifting buoys and the onset dates derived from satellite passive microwave brightness temperature fields. The timing of our estimates is within 1 - 2 days of the zero crossing of the buoy temperature records. Onset dates derived from passive microwave observations appear to be biased toward a later stage of melt. Comparison with results derived from a SAR data set from the spring of 1992 show that the onset of melt in 1998, derived from RADARSAT, in the Beaufort Sea occurred 2 weeks earlier. 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. RI Kwok, Ron/A-9762-2008 OI Kwok, Ron/0000-0003-4051-5896 NR 19 TC 12 Z9 12 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD NOV 26 PY 2003 VL 108 IS C11 AR 3363 DI 10.1029/2002JC001363 PG 13 WC Oceanography SC Oceanography GA 749RA UT WOS:000186941600002 ER PT J AU Buckley, SM Rosen, PA Hensley, S Tapley, BD AF Buckley, SM Rosen, PA Hensley, S Tapley, BD TI Land subsidence in Houston, Texas, measured by radar interferometry and constrained by extensometers SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article DE radar interferometry; subsidence; synthetic aperture radar; extensometer; Houston; SAR ID SYNTHETIC-APERTURE RADAR; LOS-ANGELES; HECTOR MINE; MW 7.1; EARTHQUAKE; CALIFORNIA; GROUNDWATER; VALLEY; FIELD; FAULT AB We present results from a radar interferometry study over the Houston-Galveston, Texas Gulf Coast region. From the nearly 60 potential interferograms considered, an atmospheric artifact assessment is performed and a tractable set of interferograms selected for detailed processing and error analysis. The subsequent interferogram time series spanning 1996 - 1998 is constrained by coincident extensometer data with root-mean-square error less than 2.5 mm. The interferogram time series confirms that historic subsidence in east Houston has stopped. Consistent with current groundwater use patterns, broad-scale subsidence bowls are observed in west and northwest Houston, where maximum subsidence rates are in excess of 2 and 4 cm yr(-1), respectively. Linear interferogram phase signatures associated with approximately 1 cm of differential subsidence across faults, including the Long Point fault in northwest Houston, are observed. Near the Seabrook extensometer, a hereto-unidentified subsidence bowl with a maximum subsidence rate in excess of 3 cm yr(-1) is revealed. This study demonstrates that when used in conjunction with a set of traditional geodetic measurements, radar interferometry can measure the spatial and temporal evolution of urban land subsidence within even the most challenging of environments. C1 Univ Texas, Ctr Space Res, Austin, TX 78759 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Buckley, SM (reprint author), Univ Texas, Ctr Space Res, 3925 W Braker Ln,Suite 200, Austin, TX 78759 USA. EM buckley@csr.utexas.edu NR 31 TC 39 Z9 39 U1 1 U2 16 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 NOV 26 PY 2003 VL 108 IS B11 AR 2542 DI 10.1029/2002JB001848 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 749RJ UT WOS:000186942400002 ER PT J AU Creilson, JK Fishman, J Wozniak, AE AF Creilson, JK Fishman, J Wozniak, AE TI Intercontinental transport of tropospheric ozone: a study of its seasonal variability across the North Atlantic utilizing tropospheric ozone residuals and its relationship to the North Atlantic Oscillation SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID AIR-POLLUTION TRANSPORT; SURFACE OZONE; NONMETHANE HYDROCARBONS; MAPPING SPECTROMETER; TOMS MEASUREMENTS; CARBON-MONOXIDE; UNITED-STATES; COLUMN OZONE; CLIMATOLOGY; AMERICA AB Using the empirically-corrected tropospheric ozone residual (TOR) technique, which utilizes coincident observations of total ozone from the Total Ozone Mapping Spectrometer (TOMS) and stratospheric ozone profiles from the Solar Backscattered Ultraviolet (SBUV) instruments, the seasonal and regional distribution of tropospheric ozone across the North Atlantic from 1979-2000 is examined. Its relationship to the North Atlantic Oscillation (NAO) is also analyzed as a possible transport mechanism across the North Atlantic. Monthly climatologies of tropospheric ozone for five different regions across the North Atlantic exhibit strong seasonality. The correlation between these monthly climatologies of the TOR and ozonesonde profiles at nearby sites in both eastern North America and western Europe are highly significant (R values of +0.98 and +0.96 respectively) and help to validate the use of satellite retrievals of tropospheric ozone. Distinct springtime interannual variability over North Atlantic Region 5 (eastern North Atlantic-western Europe) is particularly evident and exhibits similar variability to the positive phase of the NAO (R=+0.61, rho=<0.01). Positive phases of the NAO are indicative of a stronger Bermuda-Azores high and a stronger Icelandic low and thus faster more zonal flow across the North Atlantic from west to east. This flow regime appears to be causing the transport of tropospheric ozone across the North Atlantic and onto Europe. The consequence of such transport is the impact on a downwind region's ability to meet their ozone attainment goals. This link between the positive phase of the NAO and increased tropospheric ozone over Region 5 could be an important tool for prediction of such pollution outbreaks. C1 NASA, Langley Res Ctr, Hampton, VA 23665 USA. Sci Applicat Int Corp, Hampton, VA USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Creilson, JK (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. EM J.K.Creilson@larc.nasa.gov NR 54 TC 54 Z9 56 U1 0 U2 7 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 NOV 25 PY 2003 VL 3 BP 2053 EP 2066 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 747CV UT WOS:000186788400002 ER PT J AU Meng, CJ Pinker, RT Tarpley, JD Laszlo, I AF Meng, CJ Pinker, RT Tarpley, JD Laszlo, I TI A satellite approach for estimating regional land surface energy budget for GCIP/GAPP SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE surface energy budget ID GENERAL-CIRCULATION MODELS; MULTISCALE GEM MODEL; ETA-MODEL; GLOBAL-SCALE; VEGETATION; TEMPERATURE; PARAMETERIZATION; RADIATION; HYDROLOGY; PROJECT AB Conventional observations cannot provide information on land surface energy fluxes, or information for land surface parameterizations, on a global or regional scale. In this paper, a satellite approach for estimating regional land surface energy budget is developed and implemented to the Mississippi River Basin, which serves as the focus of the World Climate Research Program Global Energy and Water cycles Experiment ( GEWEX) Continental Scale International Project ( GCIP) and GEWEX Americas Prediction Project (GAPP). The objective of this study is to evaluate the potential of using recently available satellite information to advance current capabilities in determining regional land surface energy budget. The primary forcing parameters in this approach, namely, surface shortwave radiation and skin temperature, are derived from the Geostationary Operational Environmental Satellite ( GOES) observations, using inference schemes that are operationally executed at the National Oceanic and Atmospheric Administration National Environmental Satellite Data and Information Service (NESDIS). Shortwave radiation is used to define the absorbed energy at the surface. Diurnal variation of skin temperature is used to define the surface energy partitioning. The real-time NESDIS GOES product covers the continental United States (25degrees - 53 degrees N, 67degrees - 125 degreesW), at a 0.5degrees spatial resolution and an hourly temporal resolution. Atmospheric conditions of near-surface air temperature, humidity, and wind speed are obtained from the NOAA National Centers for Environmental Prediction (NCEP) Eta model output. A 1-year simulation ( May 1997 to May 1998) of the Mississippi River Basin surface energy budget is performed. Model inputs of shortwave radiation and skin temperature, and resulting latent and sensible heat fluxes, are evaluated on various spatial and temporal scales. On a local scale, over the 1-year study period, the RMS difference between estimated and observed monthly shortwave fluxes and latent and sensible heat fluxes are 32, 21, and 20 Wm(-2), respectively. On a regional scale the estimated summertime energy fluxes are of similar pattern and same order of magnitude as the corresponding reanalysis results from NCEP and National Center for Atmospheric Research. C1 Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. Natl Environm Satellite Data & Informat Serv, NOAA, Camp Springs, MD 20746 USA. RP Natl Ctr Environm Predict, 5200 Auth Rd,Room 207, Camp Springs, MD 20746 USA. EM jesse.meng@noaa.gov RI Laszlo, Istvan/F-5603-2010; Pinker, Rachel/F-6565-2010 OI Laszlo, Istvan/0000-0002-5747-9708; NR 58 TC 6 Z9 6 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 NOV 25 PY 2003 VL 108 IS D22 AR 8861 DI 10.1029/2002JD003088 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 749QU UT WOS:000186941000001 ER PT J AU Kanik, I Noren, C Makarov, OP Vattipalle, P Ajello, JM Shemansky, DE AF Kanik, I Noren, C Makarov, OP Vattipalle, P Ajello, JM Shemansky, DE TI Electron impact dissociative excitation of O-2: 2. Absolute emission cross sections of the OI(130.4 nm) and OI(135.6 nm) lines SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID EXTREME-ULTRAVIOLET EMISSION; COMPLETE UV SPECTRUM; IO PLASMA TORUS; VACUUM ULTRAVIOLET; ANGULAR-DISTRIBUTIONS; MEDIUM-RESOLUTION; OXYGEN MOLECULES; O2; STATE; N-2 AB [ 1] In this work, we report the OI( 135.6 nm) absolute emission cross section resulting from the long- lived ( 180 mus) OI(S-5 --> P-3) transition from dissociative excitation of O-2. From the ratio of the integrated intensities of the OI( 135.6 nm) and OI( 130.4 nm) features and from the absolute emission cross section for the OI( 130.4 nm) emission feature from electron impact dissociative excitation of O-2 at 100 eV, the absolute emission cross section for the OI( 135.6 nm) feature was determined to be 6.4 x 10(-18) cm(2) at 100 eV. Electron impact-induced optical excitation functions for optically allowed transitions at 115.2 nm and 130.4 nm and for an optically forbidden transition at 135.6 nm were also obtained over the electron impact energy range 0 - 600 eV. The OI( 135.6 nm) emission cross section was measured in the laboratory utilizing a large collision chamber ( 1.5 m in diameter). Electrons were produced with an electrostatically focusing gun with a large focal length ( 50 cm). The OI( 130.4 nm, 135.6 nm) excitation functions were put on an absolute scale as described in the text, and the OI( 135.6 nm)/ OI( 130.4 nm) ratio was determined for the entire energy range ( 0 - 600 eV). The atomic O UVemission cross sections from dissociative excitation of O2 can be used to model the recent Hubble Space Telescope observations of OI( 130.4 nm) and OI( 135.6 nm) intensities from Ganymede [ Feldman et al., 2000] and Europa [ Hall et al., 1995, 1998]. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91019 USA. Univ So Calif, Dept Aerosp & Mech Engn, Los Angeles, CA 90089 USA. RP CALTECH, Jet Prop Lab, Pasadena, CA 91019 USA. EM ikanik@pop.jpl.nasa.gov; cnoren@jpl.nasa.gov; oleg.makarov@uconn.edu; vattipal@mail.jpl.nasa.gov; jajello@pop.jpl.nasa.gov; dans@hippolyta.usc.edu NR 43 TC 22 Z9 22 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD NOV 25 PY 2003 VL 108 IS E11 AR 5126 DI 10.1029/2000JE001423 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 749RE UT WOS:000186942000002 ER PT J AU Makarov, OP Kanik, I Ajello, JM AF Makarov, OP Kanik, I Ajello, JM TI Electron impact dissociative excitation of O-2: 1. Kinetic energy distributions of fast oxygen atoms SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE atmospheres of Jovian satellites; analysis of Hubble Space Telescope UV observations; particle precipitation; electron impact dissociation cross sections; high-resolution UV spectroscopy; aurora and airglow of the Earth ID COMPLETE UV SPECTRUM; ULTRAVIOLET-SPECTRUM; VACUUM ULTRAVIOLET; LINE-PROFILE; LYMAN-ALPHA; EMISSION; H-2; GANYMEDE; HYDROGEN; ATMOSPHERE AB [ 1] The kinetic energy distribution of oxygen atoms resulting from electron impact dissociation of O-2 has been measured. A high- resolution vacuum ultraviolet spectrometer was employed for the measurement of the OI( 115.2 nm, 130.4 nm, 135.6 nm) fine-structure emission line profiles at 35 eV and 100 eV electron impact energies. The deconvolved line profiles of atomic oxygen reveal the existence of a broad line profile (similar to 30 - 40 mAngstrom full width at half maximum) produced from a combination of dissociative excitation and dissociative ionization excitation processes. The atomic oxygen kinetic energy distributions at 100 eV electron impact energy spans the energy range from 1 to 10 eV, with a peak value near 1 eV. The excitation functions of OI( 115.2 nm, 130.4 nm, 135.6 nm) were measured in the vicinity of threshold, from 14 to 50 eV. The PACS classification is 34.80. Gs ( electron scattering- molecular dissociation) and 33.50Dq ( molecular spectra- fluorescence). C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Makarov, OP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 31 TC 4 Z9 4 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD NOV 25 PY 2003 VL 108 IS E11 AR 5125 DI 10.1029/2000JE001422,2003 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 749RE UT WOS:000186942000001 ER PT J AU Huang, CS Foster, JC Reeves, GD Le, G Frey, HU Pollock, CJ Jahn, JM AF Huang, CS Foster, JC Reeves, GD Le, G Frey, HU Pollock, CJ Jahn, JM TI Periodic magnetospheric substorms: Multiple space-based and ground-based instrumental observations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE storm; substorm; periodic substorms; sawtooth injections ID TRAVELING COMPRESSION REGIONS; GEOTAIL OBSERVATIONS; CURRENT DISRUPTION; GEOSYNCHRONOUS ORBIT; MAGNETIC-FIELD; MAGNETOTAIL; PLASMA; RECONNECTION; MODELS; ONSET AB Quasi-periodic, sawtooth-like variations of energetic plasma particle fluxes are often measured at geosynchronous orbit during magnetic storms. The outstanding problems are whether the sawtooth flux variations represent particle injections from the tail to the inner magnetosphere, whether the sawtooth variations correspond to substorm onsets, and what mechanism is responsible for the generation of periodic particle injections ( or periodic substorms). In this paper, we present the measurements of multiple space-based and ground-based instruments in the magnetosphere and ionosphere during two magnetic storms. The Geotail satellite was located in the near tail between X-GSM = - 20 and - 30 R-E and detected periodic southward turnings of the magnetospheric magnetic field. The southward turnings of B-z are interpreted as the signature of periodic near-tail reconnection and plasmoid formations. Geosynchronous satellites measured periodic gradual dropouts and rapid increases of energetic charged fluxes and magnetic field dipolarization. The IMAGE satellite measured enhanced emissions of energetic neutral atoms in the ring current and auroral brightenings. The Canadian Auroral Network for the OPEN Program Unified Study's photometers measured intensifications and latitudinal motion of auroral emissions. The auroral electrojet index showed periodic increases. These magnetospheric and ionospheric phenomena have the same periodicity and indicate the occurrence of periodic substorms. There is an excellent correspondence among the substorm signatures from all the measurements. The results show that periodic magnetospheric substorms can indeed occur during continuous southward interplanetary magnetic field, and the mean period in these two cases is similar to 2.7 hours. The sawtooth variations of energetic plasma fluxes at geosynchronous orbit represent true particle injections from the tail to the inner magnetosphere. The sawtooth injections are related to the near-tail reconnection and correspond to the onsets of periodic substorms. C1 MIT, Haystack Observ, Westford, MA 01886 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. NASA, Goddard Space Flight Ctr, Extraterr Phys Lab, Greenbelt, MD 20771 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. SW Res Inst, Dept Space Sci, San Antonio, TX 78228 USA. RP Huang, CS (reprint author), MIT, Haystack Observ, Route 40, Westford, MA 01886 USA. RI Le, Guan/C-9524-2012; Reeves, Geoffrey/E-8101-2011 OI Le, Guan/0000-0002-9504-5214; Reeves, Geoffrey/0000-0002-7985-8098 NR 43 TC 47 Z9 47 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-SPACE JI J. Geophys. Res-Space Phys. PD NOV 25 PY 2003 VL 108 IS A11 AR 1411 DI 10.1029/2003JA009992 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 749RN UT WOS:000186942800001 ER PT J AU Dunn, W Chou, C Li, H Hai, R Patterson, D Stolc, V Zhu, H Liu, FY AF Dunn, W Chou, C Li, H Hai, R Patterson, D Stolc, V Zhu, H Liu, FY TI Functional profiling of a human cytomegalovirus genome SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article ID BACTERIAL ARTIFICIAL CHROMOSOME; ESCHERICHIA-COLI; IMMUNE EVASION; MUTAGENESIS; GENES; CLONING; CONSTRUCTION; STRAINS; TROPISM; CELLS AB Human cytomegalovirus (HCMV), a ubiquitous herpesvirus, causes a lifelong subclinical infection in healthy adults but leads to significant morbidity and mortality in neonates and immunocompromised individuals. Its ability to grow in different cell types is responsible for HCMV-associated diseases, including mental retardation and retinitis, and vascular disorders. To globally assess viral gene function for replication in cells, we determined the genomic sequence of a bacterial artificial chromosome (BAC)-based clone of HCMV Towne strain and used this information to delete each of its 162 unique ORFs and generate a collection of viral mutants. The growth of these mutants in different cultured cells was examined to systematically investigate the necessity of each ORF for replication. Our results showed that 45 ORFs are essential for viral replication in fibroblasts and 117 are nonessential. Some genes were found to be required for viral replication in retinal pigment epithelial cells and microvascular endothelial cells, but not in fibroblasts, indicating their role as tropism factors. Interestingly, several viral mutants grew 10- to 500-fold better than the parental strain in different cell types, suggesting that the deleted ORFs encode replication temperance or repressing functions. Thus, HCMV encodes supportive and suppressive growth regulators for optimizing its replication in human fibroblasts, epithelial, and endothelial cells. Suppression of viral replication by virus-encoded temperance factors represents a novel mechanism for regulating the growth of an animal virus, and may contribute to HCMV's optimal infection of different tissues and successful proliferation among the human population. C1 Univ Calif Berkeley, Sch Publ Hlth, Div Infect Dis, Berkeley, CA 94720 USA. Univ Med & Dent New Jersey, Sch Med, Dept Microbiol & Mol Genet, Newark, NJ 07101 USA. NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Liu, FY (reprint author), Univ Calif Berkeley, Sch Publ Hlth, Div Infect Dis, 140 Warren Hall, Berkeley, CA 94720 USA. NR 35 TC 372 Z9 393 U1 2 U2 16 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 NOV 25 PY 2003 VL 100 IS 24 BP 14223 EP 14228 DI 10.1073/pnas.2334032100 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 747KN UT WOS:000186803800085 PM 14623981 ER PT J AU Choi, DI Wu, B AF Choi, DI Wu, B TI To detect the looped Bloch bands of Bose-Einstein condensates in optical lattices SO PHYSICS LETTERS A LA English DT Article ID ATOMS; SUPERFLUID AB A loop structure was predicted to exist in the Bloch bands of Bose-Einstein condensates in optical lattices recently in [Phys. Rev. A 61 (2000) 023402]. We discuss how to detect experimentally the looped band with an accelerating optical lattice through extensive and realistic numerical simulations. We find that the loop can be detected through observing either nonlinear Landau-Zener tunneling or destruction of Bloch oscillations. (C) 2003 Elsevier B.V. All rights reserved. C1 Univ Space Res Assoc, Seabrook, MD 20706 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Univ Texas, Dept Phys, Austin, TX 78712 USA. Oak Ridge Natl Lab, Div Solid State, Oak Ridge, TN 37831 USA. RP Choi, DI (reprint author), Univ Space Res Assoc, 7501 Forbes Blvd 206, Seabrook, MD 20706 USA. RI Wu, Biao/B-3329-2008 OI Wu, Biao/0000-0001-9229-5894 NR 22 TC 8 Z9 8 U1 0 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0375-9601 J9 PHYS LETT A JI Phys. Lett. A PD NOV 24 PY 2003 VL 318 IS 6 BP 558 EP 563 DI 10.1016/j.physleta.2003.09.066 PG 6 WC Physics, Multidisciplinary SC Physics GA 747PH UT WOS:000186812900011 ER PT J AU Zhou, XY Tsurutani, BT Reeves, G Rostoker, G Sun, W Ruohoniemi, JM Kamide, Y Lui, ATY Parks, GK Gonzalez, WD Arballo, JK AF Zhou, XY Tsurutani, BT Reeves, G Rostoker, G Sun, W Ruohoniemi, JM Kamide, Y Lui, ATY Parks, GK Gonzalez, WD Arballo, JK TI Ring current intensification and convection-driven negative bays: Multisatellite studies SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE ring current intensification; magnetic storm; storm-substorm relationship; auroras during storm and substorms; solar wind-magnetosphere coupling ID UV AURORAL DISTRIBUTION; FIELD-ALIGNED CURRENT; BURSTY BULK FLOWS; MAGNETOSPHERIC SUBSTORMS; MAGNETIC STORMS; PLASMA SHEET; GEOMAGNETIC STORMS; MAGNETOTAIL; DST; ONSET AB [1] The original view on the cause of ring current intensifications was a frequent occurrence of intense substorm expansion phases. Results from many studies have supported this view. However, whether this is the only mechanism of ring current buildup has been a controversy. Kamide [ 1992] asserted that ring current intensification is due to "sustained, southward IMF, not because of frequent occurrence of intense substorms.'' Lui et al. [ 2001] have shown that the ring current can be intensified during enhanced convection without substorm occurrence. Tsurutani et al. [ 2003] have found that there was a lack of substorm expansion phases for long periods of time ( up to 7 hours) in 5 out of 11 storm main phases ( in 1997) that were induced by the smoothly varying B-z component of the interplanetary magnetic field ( IMF) within interplanetary magnetic clouds. In this paper, a relatively weak magnetic storm event ( with minimum SYM-H at - 47 nT) that occurred on 15 July 1997 is studied using ground-based magnetograms, polar cap potentials from Super Dual Auroral Radar Network, and Los Alamos National Laboratory (LANL) geosynchronous energetic particle data as well as the Polar UV imaging ( for aurorae) and Wind ( for the solar wind) data. It is shown that during the storm main phase, there was a lack of substorm expansion phase activity ( from imaging and the ground-based data) and a lack of energetic particle injections at the geostationary orbit. The most prominent auroral forms were north-south aligned auroral patches and torches. Dawn and dusk aurorae were more intense than the aurorae near midnight, where auroral gaps occurred. In addition, this paper shows that there was a significant directly driven activity during the storm main phase when the IMF was continually southward. We argue that during this event the ring current intensification was more strongly associated with enhanced magnetospheric convection than with impulsive energy unloading. Three scenarios are suggested to explain the relatively low intensity of the magnetic storm induced by a magnetic cloud. They are ( 1) weak nightside auroral zone ionospheric ion outflows ( due to lack of substorms), ( 2) choked penetration of the tail plasma flow ( due to lack of substorms), and ( 3) retarded magnetospheric convection ( due to reduced solar wind-magnetosphere reconnection). The observed saturation of the polar cap potential drop is in support of this latter mechanism. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Univ Alberta, Fac Sci, Avadh Bhatia Phys Lab 412, Dept Phys, Edmonton, AB T6G 2J1, Canada. Univ Alaska, Inst Geophys, Fairbanks, AK 99775 USA. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. Nagoya Univ, Solar Terr Environm Lab, Aichi 442, Japan. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Inst Nacl Pesquisas Espaciais, BR-12201970 Sao Paulo, Brazil. RP Zhou, XY (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Reeves, Geoffrey/E-8101-2011 OI Reeves, Geoffrey/0000-0002-7985-8098 NR 75 TC 7 Z9 8 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 NOV 22 PY 2003 VL 108 IS A11 AR 1407 DI 10.1029/2003JA009881 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 749CD UT WOS:000186900300004 ER PT J AU Cosgrove, BA Lohmann, D Mitchell, KE Houser, PR Wood, EF Schaake, JC Robock, A Sheffield, J Duan, QY Luo, LF Higgins, RW Pinker, RT Tarpley, JD AF Cosgrove, BA Lohmann, D Mitchell, KE Houser, PR Wood, EF Schaake, JC Robock, A Sheffield, J Duan, QY Luo, LF Higgins, RW Pinker, RT Tarpley, JD TI Land surface model spin-up behavior in the North American Land Data Assimilation System (NLDAS) SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE LDAS; LSM; spin-up ID SOIL-MOISTURE SIMULATIONS; PARAMETERIZATION SCHEMES; CLIMATE; PROJECT; TRANSPIRATION; SENSITIVITY AB The process of a model adjusting to its forcing (model spin-up) can severely bias land surface simulations, and result in questionable land surface model (LSM) output during the spin-up process. To gain a better understanding of how spin-up processes affect complex spatial and temporal land surface modeling situations in general, and the Retrospective North American Land Data Assimilation System (NLDAS) simulations in particular, a two-phase study was conducted. The first phase examined results from Control, Wet, and Dry 11 year-long Mosaic simulations, while the second phase attempted to explain spin-up behavior in NLDAS Retrospective simulations from the Mosaic, Noah, VIC and Sacramento LSMs based in part on the results from phase 1. Total column and root zone soil moisture spin up slowly, while evaporation and deep soil temperature spin up more quickly. Mosaic soil moisture initialization with NCEP/DOE Global Reanalysis 2 (NCEP/DOE R-2) data (Control run) leads to a faster spin-up time than saturated (Wet run) or dry (Dry run) initialization, with the Control run reaching equilibrium 1 to 2 years sooner than the Wet run and 3 to 4 years more quickly than the Dry run. Overall, practical drift of land surface stores and output ceased in the Control run within approximately 1 year, and fine-scale equilibrium was reached within 5.5 years. Spin-up times exhibited large spatial variability, and although no single causal factor could be determined, they were correlated most strongly with precipitation and temperature forcing. In general, NLDAS models reach a state of rough equilibrium within the first 1 to 2 years of the 3-year Retrospective simulation. The Sacramento LSM has the shortest spin-up phase, followed by the Mosaic, VIC, and Noah LSMs. Initial NCEP/DOE R-2 conditions were too dry in general for the VIC and Noah LSMs, and too moist for the Mosaic and Sacramento LSMs. These results indicate that in most cases, the 1-year spin-up time used in the Retrospective NLDAS simulations eliminated spin-up problems from the subsequent period that was used for analysis. C1 NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Sci Applicat Int Corp, Greenbelt, MD 20771 USA. Natl Ctr Environm Predict, Environm Modeling Ctr, Camp Springs, MD 20746 USA. Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. NOAA, Off Hydrol Dev, Silver Spring, MD 20910 USA. Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ 08901 USA. Natl Ctr Environm Predict, Climate Predict Ctr, Camp Springs, MD 20746 USA. Univ Maryland, Dept Meteorol, College Pk, MD 20742 USA. NOAA, Off Res & Applicat, Natl Environm Satellite Data & Informat Serv, Camp Springs, MD 20746 USA. RP Cosgrove, BA (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Sci Applicat Int Corp, Mail Code 974-1, Greenbelt, MD 20771 USA. EM cosgrove@gsfc.nasa.gov RI Sheffield, Justin/A-6388-2008; Luo, Lifeng/C-8734-2009; Pinker, Rachel/F-6565-2010; Houser, Paul/J-9515-2013; Duan, Qingyun/C-7652-2011; Robock, Alan/B-6385-2016 OI Houser, Paul/0000-0002-2991-0441; Duan, Qingyun/0000-0001-9955-1512; NR 26 TC 11 Z9 11 U1 1 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 NOV 21 PY 2003 VL 108 IS D22 AR 8845 DI 10.1029/2002JD003316 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 749BL UT WOS:000186898700003 ER PT J AU Sheffield, J Pan, M Wood, EF Mitchell, KE Houser, PR Schaake, JC Robock, A Lohmann, D Cosgrove, B Duan, QY Luo, LF Higgins, RW Pinker, RT Tarpley, JD Ramsay, BH AF Sheffield, J Pan, M Wood, EF Mitchell, KE Houser, PR Schaake, JC Robock, A Lohmann, D Cosgrove, B Duan, QY Luo, LF Higgins, RW Pinker, RT Tarpley, JD Ramsay, BH TI Snow process modeling in the North American Land Data Assimilation System (NLDAS): 1. Evaluation of model-simulated snow cover extent SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE land surface models; NLDAS; snow cover extent ID LATITUDE HYDROLOGICAL PROCESSES; TORNE-KALIX BASIN; CLIMATE VARIABILITY; PILPS PHASE-2(E); ETA-MODEL; SURFACE; REPRESENTATION; HEMISPHERE; SCHEMES; INTERCOMPARISONS AB This study evaluates the cold season process modeling in the North American Land Data Assimilation System (NLDAS) and consists of two parts: (1) assessment of land surface model simulations of snow cover extent and (2) evaluation of snow water equivalent. In this first part, simulations of snow cover extent from the four land surface models (Noah, MOSAIC, Sacramento land surface model (SAC), and Variable Infiltration Capacity land surface model (VIC)) in the NLDAS were compared with observational data from the Interactive Multisensor Snow and Ice Mapping System for a 3 year retrospective period over the conterminous United States. In general, all models simulate reasonably well the regional-scale spatial and seasonal dynamics of snow cover. Systematic biases are seen in the model simulations, with consistent underestimation of snow cover extent by MOSAIC (-19.8% average bias) and Noah (-22.5%), and overestimation by VIC (22.3%), with SAC being essentially unbiased on average. However, the level of bias at the regional scale varies with geographic location and elevation variability. Larger discrepancies are seen over higher elevation regions of the northwest of the United States that may be due, in part, to errors in the meteorological forcings and also at the snow line boundary, where most temporal and spatial variability in snow cover extent is likely to occur. The spread between model simulations is fairly low and generally envelopes the observed data at the mean regional scale, indicating that the models are quite capable of simulating the general behavior of snow processes at these scales. Intermodel differences can be explained to some extent by differences in the model representations of subgrid variability and parameterizations of snow cover extent. C1 Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. NOAA, NCEP, Environm Modeling Ctr, Sci Ctr,Natl Weather Serv, Camp Springs, MD 20746 USA. NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. NOAA, Natl Weather Serv, Off Hydrol Dev, Silver Spring, MD 20910 USA. Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ 08901 USA. NOAA, Climate Predict Ctr, Natl Ctr Environm Predict, NWS, Camp Springs, MD 20746 USA. Univ Maryland, Dept Meteorol, College Pk, MD 20742 USA. NOAA, NESDIS, Off Res & Applicat, Camp Springs, MD 20746 USA. RP Mitchell, KE (reprint author), Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. EM justin@princeton.edu; mpan@princeton.edu; efwood@runoff.princeton.edu; kenneth.mitchell@noaa.gov; houser@dao.gsfc.nasa.gov; john.schaake@noaa.gov; robock@envsci.rutgers.edu; dlohmann@ncep.noaa.gov; brian.cosgrove@gsfc.nasa.gov; qingyun.duan@noaa.gov; lluo@princeton.edu; wayne.higgins@noaa.gov; pinker@metosrv2.umd.edu; dan.tarpley@noaa.gov; bruce.r.ramsay@noaa.gov RI Sheffield, Justin/A-6388-2008; Luo, Lifeng/C-8734-2009; Pinker, Rachel/F-6565-2010; Pan, Ming/B-6841-2011; Houser, Paul/J-9515-2013; Duan, Qingyun/C-7652-2011; Robock, Alan/B-6385-2016 OI Pan, Ming/0000-0003-3350-8719; Houser, Paul/0000-0002-2991-0441; Duan, Qingyun/0000-0001-9955-1512; NR 31 TC 57 Z9 58 U1 0 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 NOV 21 PY 2003 VL 108 IS D22 AR 8849 DI 10.1029/2002JD003274 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 749BL UT WOS:000186898700002 ER PT J AU Gingrich, RM Kok, P Lee, H Vatan, F Dowling, JP AF Gingrich, RM Kok, P Lee, H Vatan, F Dowling, JP TI All linear optical quantum memory based on quantum error correction SO PHYSICAL REVIEW LETTERS LA English DT Article ID LIGHT; STORAGE AB When photons are sent through a fiber as part of a quantum communication protocol, the error that is most difficult to correct is photon loss. Here we propose and analyze a two-to-four qubit encoding scheme, which can recover the loss of one qubit in the transmission. This device acts as a repeater, when it is placed in series to cover a distance larger than the attenuation length of the fiber, and it acts as an optical quantum memory, when it is inserted in a fiber loop. We call this dual-purpose device a "quantum transponder." C1 CALTECH, Jet Prop Lab, Quantum Comp Technol Grp, Sect 367, Pasadena, CA 91109 USA. RP Gingrich, RM (reprint author), CALTECH, Jet Prop Lab, Quantum Comp Technol Grp, Sect 367, MS 126-347,4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI DOWLING, JONATHAN/L-2749-2013; Kok, Pieter/B-1658-2010 NR 15 TC 29 Z9 29 U1 0 U2 2 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 NOV 21 PY 2003 VL 91 IS 21 AR 217901 DI 10.1103/PhysRevLett.91.217901 PG 4 WC Physics, Multidisciplinary SC Physics GA 746QL UT WOS:000186757000055 PM 14683335 ER PT J AU Menzies, RT Tratt, DM AF Menzies, RT Tratt, DM TI Differential laser absorption spectrometry for global profiling of tropospheric carbon dioxide: selection of optimum sounding frequencies for high-precision measurements SO APPLIED OPTICS LA English DT Article AB We discuss the spectroscopic requirements for a laser absorption spectrometer (LAS) approach to high-precision carbon dioxide (CO2) measurements in the troposphere. Global-scale, high-precision CO2 measurements are highly desirable in an effort to improve understanding and quantification of the CO2 sources and sinks and their impact on global climate. We present differential absorption sounding characteristics for selected LAS transmitter laser wavelengths, emphasizing the effects of atmospheric temperature profile uncertainties. Candidate wavelengths for lower-troposphere measurements are identified in the CO2 bands centered near 1.57, 1.60, and 2.06 mum. (C) 2003 Optical Society of America. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Menzies, RT (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM rmenzies@jpl.nasa.gov RI Tratt, David/A-7884-2009 OI Tratt, David/0000-0002-3942-6848 NR 21 TC 66 Z9 66 U1 2 U2 8 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 NOV 20 PY 2003 VL 42 IS 33 BP 6569 EP 6577 DI 10.1364/AO.42.006569 PG 9 WC Optics SC Optics GA 744DJ UT WOS:000186612400003 PM 14658457 ER PT J AU De Propris, R Stanford, SA Eisenhardt, PR Dickinson, M AF De Propris, R Stanford, SA Eisenhardt, PR Dickinson, M TI The K-selected Butcher-Oemler effect SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : evolution; galaxies : formation; galaxies : high-redshift ID DISTANT CLUSTER GALAXIES; FRANCE REDSHIFT SURVEY; LUMINOSITY FUNCTION; HST OBSERVATIONS; FIELD GALAXIES; STAR-FORMATION; RICH CLUSTERS; DISK GALAXIES; EVOLUTION; POPULATIONS AB We investigate the Butcher-Oemler effect using samples of galaxies brighter than observed-frame K* + 1.5 in 33 clusters at 0.1 less than or similar to z less than or similar to 0.9. We attempt to duplicate as closely as possible the methodology of Butcher & Oemler. Apart from selecting in the K band, the most important difference is that we use a brightness limit fixed at 1.5 mag below an observed-frame K* rather than the nominal limit of rest-frame M-V = -20 used by Butcher & Oemler. For an early-type galaxy at z = 0.1, our sample cutoff is 0.2 mag brighter than rest-frame M-V = -20, while at z = 0.9, our cuto. is 0.9 mag brighter. If the blue galaxies tend to be faint, then the difference in magnitude limits should result in our measuring lower blue fractions. A more minor difference from the Butcher & Oemler methodology is that the area covered by our galaxy samples has a radius of 0.5 or 0.7 Mpc at all redshifts, rather than R-30, the radius containing 30% of the cluster population. In practice our field sizes are generally similar to those used by Butcher & Oemler. We find that the fraction of blue galaxies in our K-selected samples is lower on average than that derived from several optically selected samples and that it shows little trend with redshift. However, at the redshifts z < 0.6, at which our sample overlaps with that of Butcher & Oemler, the difference in f(B) as determined from our K-selected samples and those of Butcher & Oemler is much reduced. The large scatter in the measured f(B), even in small redshift ranges, in our study indicates that determining the f(B) for a much larger sample of clusters from K-selected galaxy samples is important. As a test of our methods, our data allow us to construct optically selected samples down to rest-frame M-V = -20, as used by Butcher & Oemler, for four clusters that are common between our sample and theirs. For these rest-frame V-selected samples, we find similar fractions of blue galaxies to Butcher & Oemler, while the K-selected samples for the same four clusters yield blue fractions that are typically half as large. This comparison indicates that selecting in the K band is the primary difference between our study and previous optically based studies of the Butcher & Oemler effect. Selecting in the observed K band is more nearly a process of selecting galaxies by their mass than is the case for optically selected samples. Our results suggest that the Butcher-Oemler effect is at least partly due to low-mass galaxies whose optical luminosities are boosted. These lower mass galaxies could evolve into the rich dwarf population observed in nearby clusters. C1 Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. RP De Propris, R (reprint author), Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. NR 43 TC 36 Z9 36 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 NOV 20 PY 2003 VL 598 IS 1 BP 20 EP 35 DI 10.1086/378697 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745KW UT WOS:000186688700003 ER PT J AU Shrader, CR Titarchuk, L AF Shrader, CR Titarchuk, L TI A method for black hole mass determination in accretion-powered X-ray sources SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies : active; quasars : general; radiation mechanisms : nonthermal; relativity ID QUASI-PERIODIC OSCILLATION; SEYFERT 1 GALAXIES; MONTE-CARLO SIMULATIONS; ACTIVE GALACTIC NUCLEI; HIGH-ENERGY SPECTRA; GRO J1655-40; INTRINSIC SIGNATURE; NEUTRON-STAR; WHITE-DWARF; BINARIES AB We describe a method for the determination of black hole masses based on information inferred from high-energy spectra. It is required that the spectral energy distribution consist of thermal and Comptonized components. One can then, in principle, infer the depth of the gravitational potential well for sources of known distance. The thermal component is inferred by the integration of a blackbody spectral form over the disk. We assume that the color temperature distribution in the disk has a specific shape given by the Shakura-Sunyaev disk model that goes to zero at the inner disk radius and at infinity and has a maximum at 4.2 R-S. In this formulation there is only one parameter, the so-called color correction factor, relating the apparent temperature to effective temperature, which characterizes the thermal emission component. We have made use of improved Galactic black hole binary dynamical mass determinations to derive, in effect, an empirical calibration of this factor. We then present our analysis of observational data for representative objects of several classes: Galactic black hole X-ray binaries, narrow-line Seyfert galaxies (NLS1s), and "ultraluminous" extragalactic X-ray sources (ULXs). We then apply our mass determination calculation and present our results. We argue that this approach can potentially fill a void in the current knowledge of NLS1 and ULX properties and discuss how a deeper understanding of both classes has relevance to the broader issues of how cosmic black holes, beyond the stellar-mass realm, are formed and what is their overall mass distribution. C1 NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Univ Space Res Assoc, Lanham, MD USA. USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA. George Mason Univ, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. RP Shrader, CR (reprint author), NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. NR 47 TC 23 Z9 23 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2003 VL 598 IS 1 BP 168 EP 177 DI 10.1086/378801 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745KW UT WOS:000186688700012 ER PT J AU Donahue, M Gaskin, JA Patel, SK Joy, M Clowe, D Hughes, JP AF Donahue, M Gaskin, JA Patel, SK Joy, M Clowe, D Hughes, JP TI The mass, baryonic fraction, and X-ray temperature of the luminous, high-redshift cluster of galaxies MS 0451.6-0305 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : clusters : individual (MS 0451.6-0305); intergalactic medium; X-rays : galaxies : clusters ID MEDIUM-SENSITIVITY SURVEY; PROBE WMAP OBSERVATIONS; COMA CLUSTER; COSMOLOGICAL PARAMETERS; HUBBLE CONSTANT; NEARBY CLUSTERS; CHANDRA OBSERVATIONS; DISTANT CLUSTERS; DYNAMICAL STATE; SURVEY CATALOGS AB We present new Chandra X-ray observations of the luminous and cosmologically signicant X-ray cluster of galaxies, MS 0451.6-0305, at z = 0.5386. Spectral imaging data for the cluster are consistent with an isothermal cluster of (10.0-10.6) +/- 1.6 keV, with an intracluster Fe abundance of (0.32-0.40) +/- 0.13 solar. The systematic uncertainties, arising from calibration and model uncertainties, of the temperature determination are nearly the same size as the statistical uncertainties, since the time-dependent correction for absorption on the detector is uncertain for these data. We discuss the effects of this correction on the spectral fitting. The effects of statistics and fitting assumptions of two-dimensional models for the X-ray surface brightness are thoroughly explored. This cluster appears to be elongated, and so we quantify the effects of assuming an ellipsoidal gas distribution on the gas mass and the total gravitating mass estimates. These data are also jointly fitted with previous Sunyaev-Zeldovich observations to obtain an estimate of the cluster's distance (D-A = 1219(-288)(+340) +/- 387 Mpc, statistical followed by systematic uncertainties) assuming spherical symmetry. If, instead, we assume a Hubble constant, the X-ray and Sunyaev-Zeldovich data are used together to test the consistency of an ellipsoidal gas distribution and to weakly constrain the intrinsic axis ratio. The mass derived from the X-ray data is consistent with the weak-lensing mass and is only marginally less than the mass determined from the optical velocities. We confirm that this cluster is very hot and massive, further supporting the conclusion of previous analyses that the universe has a low matter density and that cluster properties have not evolved much since z similar to 0.5. Furthermore, the presence of iron in this high-redshift cluster at an abundance that is the same as that of low-redshift clusters implies that there has been very little evolution of the cluster iron abundance since z similar to 0.5. We discuss the possible detection of a faint, soft, extended component that may be the by-product of hierarchical structure formation. C1 Space Telescope Sci Inst, Baltimore, MD 21218 USA. NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35805 USA. Univ Bonn, Inst Astrophys & Extraterr Forsch, D-53121 Bonn, Germany. Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. RP Donahue, M (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. RI Donahue, Megan/B-5361-2012 NR 81 TC 28 Z9 28 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2003 VL 598 IS 1 BP 190 EP 209 DI 10.1086/378688 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745KW UT WOS:000186688700014 ER PT J AU Fabbiano, G Krauss, M Zezas, A Rots, A Neff, S AF Fabbiano, G Krauss, M Zezas, A Rots, A Neff, S TI The multicolored hot interstellar medium of ''the antennae'' galaxies (NGC 4038/4039) SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 4038; NGC 4039, Antennae); galaxies : interactions; galaxies : peculiar; X-rays : galaxies ID YOUNG STAR-CLUSTERS; X-RAY-EMISSION; CHANDRA OBSERVATIONS; LUMINOSITY FUNCTION; METAL ABUNDANCE; NGC 4038/39; ASCA; MULTIWAVELENGTH; REGIONS; GAS AB We report the results of the analysis of the extended soft emission discovered in the Chandra ACIS pointing at the merging system NGC 4038/4039 ("the Antennae''). We present a multicolor X-ray image that suggests both extensive absorption by the dust in this system, peaking in the contact region, as well as variations in the temperature of different emitting regions of the hot interstellar medium (ISM). Spectral fits to multicomponent thermal emission models confirm this picture and give a first evaluation of the parameters of the hot plasma. We compare the diffuse X-ray emission with radio continuum (6 cm), H I, CO, and Halpha images to take a first look at the multiphase ISM of "the Antennae'' galaxies. We find that the hot (X-ray) and cold (CO) gas have comparable thermal pressures in the two nuclear regions. We also conclude that the displacement between the peak of the diffuse X-ray emission in the north of the galaxy system, toward the inner regions of the northern spiral arm (as defined by Halpha, radio continuum, and H I), could result from ram pressure of infalling H I clouds. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. RP Fabbiano, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Zezas, Andreas/C-7543-2011 OI Zezas, Andreas/0000-0001-8952-676X NR 43 TC 29 Z9 29 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2003 VL 598 IS 1 BP 272 EP 287 DI 10.1086/378791 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745KW UT WOS:000186688700021 ER PT J AU Ling, JC Wheaton, WA AF Ling, JC Wheaton, WA TI Gamma-ray spectra and variability of the Crab Nebula emission observed by BATSE SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : observations; ISM : individual (Crab Nebula); supernova remnants ID HARD X-RAY; CYGNUS X-1; SYNCHROTRON NEBULA; LINE FEATURES; GRANAT-SIGMA; FIGARO-II; PULSAR; RANGE; SPECTROMETER; RESOLUTION AB We report similar to 600 days of BATSE earth occultation observations of the total gamma-ray (30 keV to 1.7 MeV) emission from the Crab Nebula between 1991 May 24 (TJD 8400) and 1994 October 3 ( TJD 9628). Light curves from 35 - 100, 100 - 200, 200 - 300, 300 - 400, 400 - 700, and 700 - 1000 keV show that positive fluxes were detected by BATSE in each of these six energy bands at significances of approximately 31, 20, 9.2, 4.5, 2.6, and 1.3 sigma, respectively, per day. We also observed significant flux and spectral variations in the 35 - 300 keV energy region, with timescales of days to weeks. The spectra below 300 keV, averaged over typical Compton Gamma Ray Observatory viewing periods of 6 - 13 days, can be well described by a broken power law with average indices of similar to 2.1 and similar to 2.4, varying around a spectral break at similar to 100 keV. Above 300 keV, the long-term averaged spectra, averaged over three 400 day periods ( TJD 8400 - 8800, 8800 - 9200, and 9200 9628, respectively), are well represented by the same power law with index of similar to 2.34 up to similar to 670 keV, plus a hard spectral component extending from similar to 670 keV to similar to 1.7 MeV, with a spectral index of similar to 1.75. The latter component could be related to a complex structure observed by COMPTEL in the 0.7 - 3 MeV range. Above 3 MeV, the extrapolation of the power-law continuum determined by the low-energy BATSE spectrum is consistent with fluxes measured by COMPTEL in the 3 - 25 MeV range and by EGRET from 30 - 50 MeV. We interpret these results as synchrotron emission produced by the interaction of particles ejected from the pulsar with the field in different dynamical regions of the nebula system, as observed recently by the Hubble Space Telescope, XMM-Newton, and Chandra. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. RP Ling, JC (reprint author), CALTECH, Jet Prop Lab, MS 169-327,4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 57 TC 13 Z9 13 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2003 VL 598 IS 1 BP 334 EP 348 DI 10.1086/378700 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745KW UT WOS:000186688700026 ER PT J AU Titarchuk, L Kazanas, D Becker, PA AF Titarchuk, L Kazanas, D Becker, PA TI Broad redshifted line as a signature of outflow SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; radiation mechanisms : nonthermal stars : neutron ID CONVERGING FLUID-FLOW; BLACK-HOLE ACCRETION; X-RAY REFLECTION; DYNAMICAL COMPTONIZATION; SPHERICAL FLOWS; FLUORESCENCE; SCATTERING; RADIATION; SPECTRA; DISKS AB We formulate and solve the diffusion problem of line photon propagation in a bulk outflow from a compact object ( black hole or neutron star) using a generic assumption regarding the distribution of line photons within the outflow. Thomson scattering of the line photons within the expanding flow leads to a decrease of their energy which is of first order in v/c, where v is the outflow velocity and c is the speed of light. We demonstrate that the emergent line pro. le is closely related to the time distribution of photons diffusing through the flow ( the light curve) and consists of a broad redshifted feature. We analyzed the line profiles for the general case of outflow density distribution. We emphasize that the redshifted lines are intrinsic properties of the powerful outflow that are supposed to be in many compact objects. C1 George Mason Univ, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. USN, Res Lab, Washington, DC 20375 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Titarchuk, L (reprint author), George Mason Univ, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. NR 27 TC 23 Z9 23 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2003 VL 598 IS 1 BP 411 EP 418 DI 10.1086/378701 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745KW UT WOS:000186688700033 ER PT J AU Moran, TG AF Moran, TG TI Test for Alfven wave signatures in a solar coronal hole SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; Sun : corona; Sun : UV radiation; waves ID ION TEMPERATURES; ULTRAVIOLET MEASUREMENTS; MAGNETIC-FIELD; SOHO MISSION; SUMER; LIMB; WIND; VELOCITY; ATMOSPHERE; SPECTROMETER AB Using spectral line observations to study minor ion motions in a solar coronal hole, a test was made for the presence of Alfven waves. From this we conclude that the Alfven wave flux into the upper portion of the hole is not significant. The SOHO/SUMER ultraviolet spectrograph was used to observe 22 coronal ions with masses ranging from 14m(H) to 56m(H) and charge states ranging from + 4 to + 11. The line widths of 33 vacuum ultraviolet (VUV) lines radiated by these ions were measured off-limb in a coronal hole at heights between 1.02 and 1.3 solar radii (R-.), and the height dependencies of sufficiently intense lines were measured to test for the increase of width with height expected for undamped Alfven wave propagation. Line widths from ions formed at coronal hole temperatures were found to increase with height to 1.1 R-. and were constant for greater heights. If this line broadening is a manifestation of Alfven wave propagation, the waves are strongly damped above 1.1 R-.. Consequently, another mechanism must transport energy to the solar wind acceleration region. In addition, the observed dependence of line-of-sight ion speed squared on the reciprocal of the mass indicates that there is not a common nonthermal velocity if there is a common ion temperature. This suggests that Alfven waves do not cause the anomalously large effective temperatures measured. C1 Catholic Univ Amer, Washington, DC 20064 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. RP Moran, TG (reprint author), Catholic Univ Amer, Washington, DC 20064 USA. NR 46 TC 26 Z9 26 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2003 VL 598 IS 1 BP 657 EP 666 DI 10.1086/378795 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745KW UT WOS:000186688700055 ER PT J AU Gopalswamy, N Lara, A Yashiro, S Howard, RA AF Gopalswamy, N Lara, A Yashiro, S Howard, RA TI Coronal mass ejections and solar polarity reversal SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : activity; Sun : coronal mass ejections (CMEs); Sun : magnetic fields; Sun : prominences ID HOLES; FIELD; CYCLE-23 AB We report on a close relationship between the solar polarity reversal and the cessation of high-latitude coronal mass ejections (CMEs). This result holds good for individual poles of the Sun for cycles 21 and 23, for which CME data are available. The high-latitude CMEs provide a natural explanation for the disappearance of the polar crown filaments (PCFs) that rush the poles. The PCFs, which are closed field structures, need to be removed before the poles could acquire open field structure of the opposite polarity. Inclusion of CMEs along with the photospheric and subphotospheric processes completes the full set of phenomena to be explained by any solar dynamo theory. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. USN, Res Lab, Washington, DC 20375 USA. RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Gopalswamy, Nat/D-3659-2012 NR 17 TC 94 Z9 94 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 NOV 20 PY 2003 VL 598 IS 1 BP L63 EP L66 DI 10.1086/380430 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745KX UT WOS:000186688800016 ER PT J AU Kaufmann, RK Zhou, L Myneni, RB Tucker, CJ Slayback, D Shabanov, NV Pinzon, J AF Kaufmann, RK Zhou, L Myneni, RB Tucker, CJ Slayback, D Shabanov, NV Pinzon, J TI The effect of vegetation on surface temperature: A statistical analysis of NDVI and climate data SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB [1] We use statistical techniques to quantify the effect of interannual variations in vegetation within land covers on surface temperature in North America and Eurasia from satellite measures of surface greenness and ground based meteorological observations. During the winter, reductions in the extent of snow cover cause (in a statistical sense) temperature to rise. During the summer, increases in terrestrial vegetation within land covers cause (in a statistical sense) temperature to fall. Temperature-induced increases in vegetation have slowed increases in surface temperature, but this feedback may be limited by the range over which temperature has a positive effect on vegetation. C1 Boston Univ, Dept Geog, Boston, MA 02215 USA. Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA. RP Kaufmann, RK (reprint author), Boston Univ, Dept Geog, 675 Commonwealth Ave, Boston, MA 02215 USA. RI Slayback, Daniel/E-7465-2011; Zhou, Liming/A-2688-2012; Myneni, Ranga/F-5129-2012 NR 15 TC 49 Z9 54 U1 1 U2 23 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 NOV 20 PY 2003 VL 30 IS 22 AR 2147 DI 10.1029/2003GL018251 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 749BD UT WOS:000186898000004 ER PT J AU Sahai, R Morris, M Knapp, GR Young, K Barnbaum, C AF Sahai, R Morris, M Knapp, GR Young, K Barnbaum, C TI A collimated, high-speed outflow from the dying star V Hydrae SO NATURE LA English DT Article ID BIPOLAR PLANETARY-NEBULAE; ASYMPTOTIC GIANT BRANCH; CARBON STAR; BOW SHOCK; JET; BUBBLES; WIND AB Stars with masses in the range 1-8 solar masses (M.) live ordinary lives for similar to10(9)-10(10) years, but die extraordinary deaths. First, during their death throes as asymptotic giant branch (AGB) stars they eject, over 10(4)-10(5) years, half or more of their mass in slowly expanding, spherical winds, and then, in a short (a few 100-1,000 years) and poorly understood phase, they are transformed into aspherical planetary nebula. Recent studies support the idea that high-speed, jet-like flows play a crucial role in this transformation(1). Evidence for such outflows is indirect, however; this phase is so short that few nearby stars are likely to be caught in the act. Here we report the discovery of a newly launched, high-speed jet-like outflow in the nearby AGB star, V Hydrae. We have detected both proper motions and ongoing evolution in the jet. These results support a model in which the jet is driven by an accretion disk around an unseen, compact companion. We also find a central, dense equatorial disk-like structure which may enable and/or enhance the formation of the accretion disk. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Calif Los Angeles, Div Astron, Dept Phys & Astrophys, Los Angeles, CA 90095 USA. Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Valdosta State Univ, Dept Phys Astron & Geosci, Valdosta, GA 31698 USA. RP Sahai, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 24 TC 38 Z9 38 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 NOV 20 PY 2003 VL 426 IS 6964 BP 261 EP 264 DI 10.1038/nature02086 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 744YQ UT WOS:000186660800036 PM 14628044 ER PT J AU Pinker, RT Tarpley, JD Laszlo, I Mitchell, KE Houser, PR Wood, EF Schaake, JC Robock, A Lohmann, D Cosgrove, BA Sheffield, J Duan, QY Luo, LF Higgins, RW AF Pinker, RT Tarpley, JD Laszlo, I Mitchell, KE Houser, PR Wood, EF Schaake, JC Robock, A Lohmann, D Cosgrove, BA Sheffield, J Duan, QY Luo, LF Higgins, RW TI Surface radiation budgets in support of the GEWEX Continental-Scale International Project (GCIP) and the GEWEX Americas Prediction Project (GAPP), including the North American Land Data Assimilation System (NLDAS) Project SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE surface radiation budget; GCIP/GAPP; satellite radiation budgets ID PHOTOSYNTHETICALLY ACTIVE RADIATION; DIFFERENCE VEGETATION INDEX; SATELLITE-OBSERVATIONS; CLIMATE RESEARCH; SOLAR-RADIATION; ENERGY BALANCE; DATA SET; MODEL; PARAMETERIZATION; IRRADIANCE AB In support of the World Climate Research Program GEWEX Continental-Scale International Project (GCIP) and the GEWEX Americas Prediction Project (GAPP), real-time estimates of shortwave radiative fluxes, both at the surface and at the top of the atmosphere, are being produced operationally by the National Oceanic and Atmospheric Administration (NOAA)/National Environmental Satellite Data and Information Service using observations from GOES images. The inference scheme has been developed at the Department of Meteorology, University of Maryland, and the atmospheric and surface model input parameters are produced and provided by the NOAA/National Centers for Environmental Prediction. The radiative fluxes are being evaluated on hourly, daily, and monthly timescales using observations at about 50 stations. The satellite estimates have been found to be within acceptable limits during snow-free periods, but the difficulty in detecting clouds over snow affects the accuracy during the winter season. In what follows, this activity is discussed, and evaluation results of the derived fluxes against ground observations for time periods of 1-2 years are presented. C1 Univ Maryland, Dept Meteorol, College Pk, MD 20742 USA. Natl Environm Satellite Data & Informat Serv, Off Res & Applicat, Satellite Res Lab, NOAA, Camp Springs, MD 20746 USA. NOAA, Environm Modeling Ctr, Natl Ctr Environm Predict, Washington, DC USA. NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. Natl Weather Serv, Off Hydrol Dev, NOAA, Silver Spring, MD 20910 USA. Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ 08901 USA. NASA, Data Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Natl Weather Serv, Climate Predict Ctr, Natl Ctr Environm Predict, NOAA, Washington, DC USA. RP Pinker, RT (reprint author), Univ Maryland, Dept Meteorol, 2213 Comp & Space Sci Bldg, College Pk, MD 20742 USA. EM pinker@atmos.umd.edu; dan.tarpley@noaa.gov; istvan.laszlo@noaa.gov; kenneth.mitchell@noaa.gov; houser@dao.gsfc.nasa.gov; efwood@princeton.edu; john.schaake@noaa.gov; robock@envsci.rutgers.edu; dlohmann@ncep.noaa.gov; brian.cosgrove@gsfc.nasa.gov; justin@princeton.edu; qingyun.duan@noaa.gov; lluo@rutgers.edu; wayne.higgins@noaa.gov RI Sheffield, Justin/A-6388-2008; Laszlo, Istvan/F-5603-2010; Luo, Lifeng/C-8734-2009; Pinker, Rachel/F-6565-2010; Houser, Paul/J-9515-2013; Duan, Qingyun/C-7652-2011; Robock, Alan/B-6385-2016 OI Laszlo, Istvan/0000-0002-5747-9708; Houser, Paul/0000-0002-2991-0441; Duan, Qingyun/0000-0001-9955-1512; NR 67 TC 112 Z9 115 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 19 PY 2003 VL 108 IS D22 AR 8844 DI 10.1029/2002JD003301 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 749BK UT WOS:000186898600002 ER PT J AU Manning, W Wang, JR AF Manning, W Wang, JR TI Retrieval of precipitable water using Special Sensor Microwave/Temperature-2 (SSM/T-2) millimeter-wave radiometric measurements SO RADIO SCIENCE LA English DT Article DE millimeter-wave; radiometry; remote sensing; precipitable water; water vapor; polar meteorology ID VAPOR; MIR; GHZ AB [1] Four years of Special Sensor Microwave/Temperature-2 (SSM/T-2) measurements over the high-latitude regions of both the Northern and Southern Hemispheres are used to retrieve precipitable water W < 0.8 cm. The retrieved W values compare well with several thousand near-concurrent radiosonde-derived estimates of W. Additionally, very good agreement is found between the retrieved SSM/T-2 W values and continuous ground-based radiometer-derived estimates of W during a couple of extended time periods. A bias (0.03 - 0.06 cm) exists between the W values retrieved from the SSM/T-2 and the values derived from the radiosonde/radiometer observations. This bias is caused primarily by the assumption of equivalent surface emissivity across the 150 - 183 GHz frequency range that is made during the development of the retrieval algorithm. The spatial distribution of the SSM/T-2-retrieved winter mean W values is examined together with digital elevation models for both the Greenland and Antarctic ice sheets. This detailed comparison conveys expected climatological characteristics that are quite sensible when the combined effects of the surface elevation and the general atmospheric circulation patterns near and over the ice sheets are considered in unison. The SSM/T-2 W retrieval presented provides accurate W information with a high sampling rate for the potentially climate change-sensitive polar regions of the Northern and Southern Hemispheres. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. RP Manning, W (reprint author), Night Vis & Elect Sensors Directorate, 10221 Burbeck Rd, Ft Belvoir, VA 22060 USA. NR 28 TC 3 Z9 3 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0048-6604 J9 RADIO SCI JI Radio Sci. PD NOV 19 PY 2003 VL 38 IS 6 AR 1097 DI 10.1029/2002RS002735 PG 15 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications GA 749CE UT WOS:000186900400002 ER PT J AU Tsurutani, BT Clay, DR Zhang, LD Dasgupta, B Brinza, D Henry, M Mendis, A Moses, S Glassmeier, KH Musmann, G Richter, I AF Tsurutani, BT Clay, DR Zhang, LD Dasgupta, B Brinza, D Henry, M Mendis, A Moses, S Glassmeier, KH Musmann, G Richter, I TI Dust impacts at Comet P/Borrelly SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID PLASMA-WAVE INSTRUMENT; HALLEY; VEGA-2; FIELD AB [1] The NASA DS1 spacecraft flew past comet P/Borrelly on September 22, 2001, on the sunward side of the comet. Dust impacts were detected by sharp increases (or decreases) in electric fields measured by the plasma wave dipole antennae. Electric pulses from as small as 0.014 Vm(-1) to saturation (similar to+/-0.8 Vm(-1)) were detected. Pulse overshoots were noted in the largest electric pulses. No simultaneous dc magnetic signatures >1 nT were detected in the magnetometer data. Assuming that cometary dust grains propagating in the sunward direction were decelerated by solar radiation pressure, arguments are made that the size of the earliest dust particles detected were probably similar to0.4 mum in radius. Elaboration of the characteristics of these electric pulses and pulse overshoots and their interpretations will be reserved for a subsequent work. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Calif San Diego, Dept Elect Engn, La Jolla, CA 92093 USA. Northrop Grumman Space Technol, Redondo Beach, CA USA. Tech Univ Carolo Wilhelmina Braunschweig, D-3300 Braunschweig, Germany. RP Tsurutani, BT (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 19 TC 6 Z9 6 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD NOV 18 PY 2003 VL 30 IS 22 AR 2134 DI 10.1029/2003GL017580 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 749BB UT WOS:000186897800001 ER PT J AU Djikaev, YS Tabazadeh, A AF Djikaev, YS Tabazadeh, A TI Effect of adsorption on the uptake of organic trace gas by cloud droplets SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE uptake of organics; adsorption effect; cloud droplets ID AIR-WATER-INTERFACE; ATMOSPHERIC AEROSOL; FOG DROPLETS; SURFACE; FILMS; ACID; CRYSTALLIZATION; NUCLEATION; PARTICLES AB [1] Adsorption can greatly influence the partitioning of organic trace species between the gas and liquid phases. Here we investigate how adsorption of organic species at the air-water interface in clouds can increase the amount of trace gas found in cloud water. For atmospherically relevant cloud surface areas and realistic ranges of adsorption parameters, we show that a significant amount of organic molecules can reside at the cloud droplet surface. Two different physical situations are considered corresponding to the cases where the surfactant is water-soluble and where it is water-insoluble. For both cases, numerical calculations were carried out for a wide range of adsorption parameters, effective Henry's law constants ( the former case only), and cloud surface areas. For a soluble surfactant, our calculations show that the "overall'' Henry's law constant, which takes into account for both adsorption at the droplet surface and partitioning into the droplet interior, can significantly differ from the standard Henry's law constant. For a moderately soluble species the overall uptake can strongly depend on the surface coverage if the species has a strong affinity for partitioning into the surface layer. Our results also suggest that even insoluble and/or scarcely soluble species can be scavenged by clouds if they are surface-active. C1 NASA, Ames Res Ctr, NRC Assoc, Natl Res Council Res Associateship Program, Moffett Field, CA 94035 USA. NASA, Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA. RP Djikaev, YS (reprint author), NASA, Ames Res Ctr, NRC Assoc, Natl Res Council Res Associateship Program, MS 245-4, Moffett Field, CA 94035 USA. EM djikaev@venus.arc.nasa.gov; azadeh.tabazadeh-1@nasa.gov NR 33 TC 23 Z9 23 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 18 PY 2003 VL 108 IS D22 AR 4689 DI 10.1029/2003JD003741 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 749BJ UT WOS:000186898500005 ER PT J AU He, GW Rubinstein, R AF He, GW Rubinstein, R TI The mapping closure approximation to the conditional dissipation rate for turbulent scalar mixing SO JOURNAL OF TURBULENCE LA English DT Article ID LARGE-EDDY SIMULATION; PASSIVE SCALAR; REACTING FLOWS; FIELD; STATISTICS; DIFFUSION; BINARY AB A novel mapping closure approximation (MCA) technique is developed to construct a model for the conditional dissipation rate (CDR) of a scalar in homogeneous turbulence. It is shown that the CDR model from amplitude mapping closure is incorrect in asymptotic behaviour for unsymmetric binary mixing. The correct asymptotic behaviour can be described by the CDR model formulated by the MCA technique. The MCA approach is outlined for constructing a successive approximation to the probability density function and conditional moment. C1 Chinese Acad Sci, Inst Mech, LNM, Beijing 100080, Peoples R China. NASA, Langley Res Ctr, Computat Modeling & Simulat Branch, Hampton, VA 23681 USA. RP He, GW (reprint author), Chinese Acad Sci, Inst Mech, LNM, Beijing 100080, Peoples R China. NR 19 TC 2 Z9 2 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1468-5248 J9 J TURBUL JI J. Turbul. PD NOV 18 PY 2003 VL 4 AR 029 PG 7 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA 745DG UT WOS:000186673200001 ER PT J AU Pinto, NJ Johnson, AT MacDiarmid, AG Mueller, CH Theofylaktos, N Robinson, DC Miranda, FA AF Pinto, NJ Johnson, AT MacDiarmid, AG Mueller, CH Theofylaktos, N Robinson, DC Miranda, FA TI Electrospun polyaniline/polyethylene oxide nanofiber field-effect transistor SO APPLIED PHYSICS LETTERS LA English DT Article ID THIN-FILM; DOPED POLYACETYLENE; CARBON NANOTUBE; POLYMER; SEMICONDUCTOR; CIRCUITS; FIBERS; SINGLE; DEVICE AB We report on the observation of field-effect transistor (FET) behavior in electrospun camphorsulfonic-acid-doped polyaniline/polyethylene oxide (PEO) nanofibers. Saturation channel currents are observed at surprisingly low source-drain voltages. The hole mobility in the depletion regime is 1.4x10(-4) cm(2)/V s, while the one-dimensional (1-D) charge density (at zero gate bias) is calculated to be approximately 1 hole per 50 two-ring repeat units of polyaniline, consistent with the rather high channel conductivity (similar to10(-3) S/cm). Reducing or eliminating the PEO content in the fiber is expected to enhance device parameters. Electrospinning is thus proposed as a simple method of fabricating one-dimensional polymer FETs. (C) 2003 American Institute of Physics. C1 Univ Puerto Rico, Dept Phys & Elect, Humacao, PR 00791 USA. Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. Univ Penn, Dept Chem, Philadelphia, PA 19104 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. Univ Texas, Dept Chem, Richardson, TX 75083 USA. Univ Texas, Dept Phys, Richardson, TX 75083 USA. RP Pinto, NJ (reprint author), Univ Puerto Rico, Dept Phys & Elect, Humacao, PR 00791 USA. RI 李, 府中/H-4357-2011 NR 23 TC 232 Z9 235 U1 8 U2 102 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 NOV 17 PY 2003 VL 83 IS 20 BP 4244 EP 4246 DI 10.1063/1.1627484 PG 3 WC Physics, Applied SC Physics GA 742NF UT WOS:000186523400055 ER PT J AU Rosenberg, B AF Rosenberg, B TI NASA research park plans bio-nano-it convergence SO AVIATION WEEK & SPACE TECHNOLOGY LA English DT Article C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Rosenberg, B (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU MCGRAW HILL INC PI NEW YORK PA 1221 AVENUE OF THE AMERICAS, NEW YORK, NY 10020 USA SN 0005-2175 J9 AVIAT WEEK SPACE TEC JI Aviat. Week Space Technol. PD NOV 17 PY 2003 VL 159 IS 20 BP 80 EP 80 PG 1 WC Engineering, Aerospace SC Engineering GA 744ZY UT WOS:000186663800040 ER PT J AU Li, L Roden, J Shapiro, BE Wold, BJ Forman, SJ Bhatia, R AF Li, L Roden, J Shapiro, BE Wold, BJ Forman, SJ Bhatia, R TI Reproducibility, fidelity and discriminant validity of mRNA amplification for microarray analysis of disordered gene expression in hematological malignancies. SO BLOOD LA English DT Meeting Abstract CT 45th Annual Meeting of the American-Society-of-Hematology CY DEC 06-09, 2003 CL SAN DIEGO, CALIFORNIA SP Amer Soc Hematol C1 City Hope Natl Med Ctr, Div Hematol BMT, Duarte, CA USA. NASA Jet Prop Lab, Machine Learning Syst Grp, Pasadena, CA USA. CALTECH, Div Biol, Pasadena, CA 91125 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC HEMATOLOGY PI WASHINGTON PA 1900 M STREET. NW SUITE 200, WASHINGTON, DC 20036 USA SN 0006-4971 J9 BLOOD JI Blood PD NOV 16 PY 2003 VL 102 IS 11 MA 3168 BP 852A EP 852A PN 1 PG 1 WC Hematology SC Hematology GA 742UP UT WOS:000186536703168 ER PT J AU Dasgupta, B Tsurutani, BT Janaki, MS AF Dasgupta, B Tsurutani, BT Janaki, MS TI A kinetic approach to the Ponderomotive Force SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MAGNETIC HOLES; SOLAR-WIND; ACCELERATION; CYCLOTRON; WAVES; FREQUENCY; PLASMA; IONS AB [1] It has been suggested that Magnetic Holes ( MHs) are caused by perpendicular proton energization due to the Ponderomotive Force ( PF) associated with phase steepened Alfven waves. Here we include particle finite Larmor radius ( FLR) effects and the effects of ion gyroharmonics in the PF expression. The general expression for the PF is derived by using the hot plasma dielectric tensor from kinetic theory. The fully kinetic expression has a multiple resonance character which is not revealed in the fluid picture. It will be shown that by including such effects, the expression for the PF will be significantly altered, both at the low frequency and high frequency limit. Also, an explicit analytic expression for the PF keeping only the first order FLR terms is given for conceptual purposes for the readers. C1 CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. Saha Inst Nucl Phys, Kolkata 700064, W Bengal, India. RP CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM brahmananda.dasgupta@jpl.nasa.gov NR 21 TC 20 Z9 22 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 NOV 15 PY 2003 VL 30 IS 21 AR 2128 DI 10.1029/2003GL017385 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 744UV UT WOS:000186652000001 ER PT J AU Davies, AG AF Davies, AG TI Temperature, age and crust thickness distributions of Loki Patera on Io from Galileo NIMS data: Implications for resurfacing mechanism SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID THERMAL EMISSION; LAVA LAKES; HEAT-FLOW; VOLCANISM AB [1] A high- spatial- resolution, multi- wavelength observation by the Galileo NIMS instrument has been analysed to determine the temperature and area distribution of a large portion of the ionian volcano Loki Patera. The temperatures of the cooler components from a two- temperature fit to the data can be used to determine ages of the surface. The age of the floor along a profile across the floor of the caldera ranges from similar to 10 to similar to 80 days. This puts the start of the resurfacing in July/ early August 2001, yielding a resurfacing rate of approximately 1 km/ day, with the new lava spreading from the SW corner of the caldera in a NE direction. This rate is consistent with resurfacing by foundering of the crust on a lava lake. However, the temperature distribution may also result from the emplacement of flows. Implied crust thicknesses ( derived using a lava cooling model) range from 2.6 to 0.9 m. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Davies, AG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 20 TC 18 Z9 18 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 NOV 15 PY 2003 VL 30 IS 21 AR 2133 DI 10.1029/2003GL018371 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 744UV UT WOS:000186652000006 ER PT J AU Carmichael, GR Tang, Y Kurata, G Uno, I Streets, DG Thongboonchoo, N Woo, JH Guttikunda, S White, A Wang, T Blake, DR Atlas, E Fried, A Potter, B Avery, MA Sachse, GW Sandholm, ST Kondo, Y Talbot, RW Bandy, A Thorton, D Clarke, AD AF Carmichael, GR Tang, Y Kurata, G Uno, I Streets, DG Thongboonchoo, N Woo, JH Guttikunda, S White, A Wang, T Blake, DR Atlas, E Fried, A Potter, B Avery, MA Sachse, GW Sandholm, ST Kondo, Y Talbot, RW Bandy, A Thorton, D Clarke, AD TI Evaluating regional emission estimates using the TRACE-P observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE emission evaluation; chemical transport model; TRACE-P; biomass burning ID CHEMICAL-TRANSPORT MODEL; CARBON-MONOXIDE; ASIA; BIOMASS; PACIFIC; SYSTEM; CO AB Measurements obtained during the NASA Transport and Chemical Evolution over the Pacific (TRACE-P) experiment are used in conjunction with regional modeling analysis to evaluate emission estimates for Asia. A comparison between the modeled values and the observations is one method to evaluate emissions. Based on such analysis it is concluded that the inventory performs well for the light alkanes, CO, ethyne, SO2, and NOx. Furthermore, based on model skill in predicting important photochemical species such as O-3, HCHO, OH, HO2, and HNO3, it is found that the emissions inventories are of sufficient quality to support preliminary studies of ozone production. These are important finding in light of the fact that emission estimates for many species (such as speciated NMHCs and BC) for this region have only recently been estimated and are highly uncertain. Using a classification of the measurements built upon trajectory analysis, we compare observed species distributions and ratios of species to those modeled and to ratios estimated from the emissions inventory. It is shown that this technique can reconstruct a spatial distribution of propane/benzene that looks remarkably similar to that calculated from the emissions inventory. A major discrepancy between modeled and observed behavior is found in the Yellow Sea, where modeled values are systematically underpredicted. The integrated analysis suggests that this may be related to an underestimation of emissions from the domestic sector. The emission is further tested by comparing observed and measured species ratios in identified megacity plumes. Many of the model derived ratios (e.g., BC/CO, SOx/C2H2) fall within similar to25% of those observed and all fall outside of a factor of 2.5. C1 Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA 52242 USA. Toyohashi Univ Technol, Dept Ecol Engn, Toyohashi, Aichi 4418580, Japan. Kyushu Univ, Appl Mech Res Inst, Fukuoka 8168580, Japan. Argonne Natl Lab, Decis & Informat Sci Div, Argonne, IL 60439 USA. Univ Calif Davis, Dept Chem Engn, Davis, CA 95616 USA. Hong Kong Polytech Univ, Dept Civil & Struct Engn, Hong Kong, Hong Kong, Peoples R China. Univ Calif Irvine, Dept Chem, Irvine, CA 92697 USA. Natl Ctr Atmospher Res, Boulder, CO 80305 USA. Univ Tulsa, Tulsa, OK 74104 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Georgia Inst Technol, Atlanta, GA 30332 USA. Univ Tokyo, Adv Sci & Technol Res Ctr, Meguro Ku, Tokyo 1538904, Japan. Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. Drexel Univ, Dept Chem, Philadelphia, PA 19104 USA. Univ Hawaii, Sch Ocean & Earth Sci & Technol, Honolulu, HI 96822 USA. RP Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA 52242 USA. EM gcarmich@engineering.uiowa.edu; ytang@cgrer.uiowa.edu; kurata@eco.tut.ac.jp; iuno@riam.kyushu-u.ac.jp; dstreets@anl.gov; nthongbo@cgrer.uiowa.edu; woojh21@cgrer.uiowa.edu; sguttiku@cgrer.uiowa.edu; adwhite@ucdavis.edu; cetwang@polyu.edu.hk; drblake@uci.edu; atlas@ucar.edu; fried@ucar.edu; william-potter@utulsa.edu; m.a.avery@larc.nasa.gov; g.w.sachse@larc.nasa.gov; scott.sandholm@eas.gatech.edu; kondo@atmos.rcast.u-tokyo.ac.jp; robert.talbot@unh.edu; bandyar@drexel.edu; dct@drexel.edu; tclarke@soest.hawaii.edu RI Uno, Itsushi/B-5952-2011; Kondo, Yutaka/D-1459-2012; WANG, Tao/B-9919-2014; Kyushu, RIAM/F-4018-2015; Atlas, Elliot/J-8171-2015; U-ID, Kyushu/C-5291-2016; Tang, Youhua/D-5205-2016 OI WANG, Tao/0000-0002-4765-9377; Tang, Youhua/0000-0001-7089-7915 NR 18 TC 125 Z9 131 U1 2 U2 24 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 NOV 15 PY 2003 VL 108 IS D21 AR 8820 DI 10.1029/2002JD003116 PG 27 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 744VM UT WOS:000186653600002 ER PT J AU Davis, DD Chen, G Crawford, JH Liu, S Tan, D Sandholm, ST Jing, P Cunnold, DM DiNunno, B Browell, EV Grant, WB Fenn, MA Anderson, BE Barrick, JD Sachse, GW Vay, SA Hudgins, CH Avery, MA Lefer, B Shetter, RE Heikes, BG Blake, DR Blake, N Kondo, Y Oltmans, S AF Davis, DD Chen, G Crawford, JH Liu, S Tan, D Sandholm, ST Jing, P Cunnold, DM DiNunno, B Browell, EV Grant, WB Fenn, MA Anderson, BE Barrick, JD Sachse, GW Vay, SA Hudgins, CH Avery, MA Lefer, B Shetter, RE Heikes, BG Blake, DR Blake, N Kondo, Y Oltmans, S TI An assessment of western North Pacific ozone photochemistry based on springtime observations from NASA's PEM-West B (1994) and TRACE-P (2001) field studies SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE TRACE-P; ozone; Pacific Rim ID TROPOSPHERIC OZONE; TROPICAL PACIFIC; POTENTIAL VORTICITY; SEASONAL-VARIATION; CHEMISTRY; TRANSPORT; MODEL; DISTRIBUTIONS; AIR; STRATOSPHERE AB The current study provides a comparison of the photochemical environments for two NASA field studies focused on the western North Pacific (PEM-West-B (PWB) and TRACE-P (TP)). These two studies were separated in calendar time by approximately 7 years. Both studies were carried out under springtime conditions, with PWB being launched in 1994 and TP being deployed in 2001 (i.e., 23 February-15 March 1994 and 10 March-15 April 2001, respectively). Because of the 7-year time separation, these two studies presented a unique scientific opportunity to assess whether evidence could be found to support the Department of Energy's projections in 1997 that increases in anthropogenic emissions from East Asia could reach 5%/yr. Such projections would lead one to the conclusion that a significant shift in the atmospheric photochemical properties of the western North Pacific would occur. To the contrary, the findings from this study support the most recent emission inventory data [Streets et al., 2003] in that they show no significant systematic trend involving increases in any O-3 precursor species and no evidence for a significant shift in the level of photochemical activity over the western North Pacific. This conclusion was reached in spite of there being real differences in the concentration levels of some species as well as differences in photochemical activity between PWB and TP. However, nearly all of these differences were shown to be a result of a near 3-week shift in TP's sampling window relative to PWB, thus placing it later in the spring season. The photochemical enhancements seen during TP were most noticeable for latitudes in the range of 25-45degreesN. Most important among these were increases in J((OD)-D-1), OH, and HO2 and values for photochemical ozone formation and destruction, all of which were typically two times larger than those calculated for PWB. A comparison of these airborne results with ozonesonde data from four Japanese stations provided further evidence showing that the 3-week shift in the respective sampling windows of PWB and TP was a likely cause for the differences seen in O-3 levels and in photochemical activity between the two airborne studies. C1 Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Acad Sinica, Inst Earth Sci, Taipei 11529, Taiwan. Natl Ctr Atmospher Res, Boulder, CO 80303 USA. Univ Rhode Isl, Grad Sch Oceanog, Narragansett, RI 02882 USA. Univ Calif Irvine, Dept Chem, Irvine, CA 92697 USA. Univ Tokyo, Adv Sci & Technol Res Ctr, Tokyo, Japan. NOAA, Boulder, CO 80303 USA. RP Davis, DD (reprint author), Georgia Inst Technol, Sch Earth & Atmospher Sci, ES&T Bldg, Atlanta, GA 30332 USA. EM douglas.davis@eas.gatech.edu; gao.chen@eas.gatech.edu; j.h.crawford@larc.nasa.gov; shawliu@earth.sinica.edu.tw; scott.sandholm@eas.gatech.edu; pjing@eas.gatech.edu; cunnold@eas.gatech.edu; bdinunno@eas.gatech.edu; e.v.browell@larc.nasa.gov; w.b.grant@larc.nasa.gov; m.a.fenn@larc.nasa.gov; b.e.anderson@larc.nasa.gov; j.d.barrick@larc.nasa.gov; g.w.sachse@larc.nasa.gov; c.h.hudgins@larc.nasa.gov; m.a.avery@larc.nasa.gov; lefer@ucar.edu; shetter@ucar.edu; drblake@uci.edu; nblake@uci.edu; soltmans@cmdl.noaa.gov RI Kondo, Yutaka/D-1459-2012; Grant, William/B-8311-2009; Crawford, James/L-6632-2013; Lefer, Barry/B-5417-2012 OI Grant, William/0000-0002-1439-3285; Crawford, James/0000-0002-6982-0934; Lefer, Barry/0000-0001-9520-5495 NR 44 TC 26 Z9 26 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 NOV 15 PY 2003 VL 108 IS D21 AR 8829 DI 10.1029/2002JD003232 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 744VM UT WOS:000186653600005 ER PT J AU Jordan, CE Anderson, BE Talbot, RW Dibb, JE Fuelberg, HE Hudgins, CH Kiley, CM Russo, R Scheuer, E Seid, G Thornhill, KL Winstead, E AF Jordan, CE Anderson, BE Talbot, RW Dibb, JE Fuelberg, HE Hudgins, CH Kiley, CM Russo, R Scheuer, E Seid, G Thornhill, KL Winstead, E TI Chemical and physical properties of bulk aerosols within four sectors observed during TRACE-P SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE aerosols; TRACE-P; Asia ID PACIFIC EXPLORATORY MISSION; ASIAN CONTINENTAL OUTFLOW; SUBSONIC ASSESSMENT OZONE; OCEAN EXPERIMENT INDOEX; OXIDE EXPERIMENT SONEX; OPTICAL-PROPERTIES; INDIAN-OCEAN; PEM-TROPICS; TRANSPORT PATHWAYS; WESTERN PACIFIC AB Chemical and physical aerosol data collected on the DC-8 during TRACE-P were grouped into four sectors based on back trajectories. The four sectors represent long-range transport from the west (WSW), regional circulation over the western Pacific and Southeast Asia (SE Asia), polluted transport from northern Asia with substantial sea salt at low altitudes (NNW) and a substantial amount of dust (Channel). WSW has generally low mixing ratios at both middle and high altitudes, with the bulk of the aerosol mass due to non-sea-salt water-soluble inorganic species. Low altitude SE Asia also has low mean mixing ratios in general, with the majority of the aerosol mass comprised of non-sea-salts, however, soot is also relatively important in this region. NNW had the highest mean sea salt mixing ratios, with the aerosol mass at low altitudes (<2 km) evenly divided between sea salts, non-sea-salts, and dust. The highest mean mixing ratios of water-soluble ions and soot were observed at the lowest altitudes (<2 km) in the Channel sector. The bulk of the aerosol mass exported from Asia emanates from Channel at both low and midaltitudes, due to the prevalence of dust compared to other sectors. Number densities show enhanced fine particles for Channel and NNW, while their volume distributions are enhanced due to sea salt and dust. Low-altitude Channel exhibits the highest condensation nuclei (CN) number densities along with enhanced scattering coefficients, compared to the other sectors. At midaltitudes (2-7 km), low mean CN number densities coupled with a high proportion of nonvolatile particles (greater than or equal to65%) observed in polluted sectors (Channel and NNW) are attributed to wet scavenging which removes hygroscopic CN particles. Low single scatter albedo in SE Asia reflects enhanced soot. C1 NASA, Langley Res Ctr, Natl Res Council, Hampton, VA 23681 USA. Univ New Hampshire, Inst Study Earth Oceans & Space, Complex Syst Res Ctr, Durham, NH 03824 USA. Univ New Hampshire, Inst Study Earth Oceans & Space, Climate Change Res Ctr, Durham, NH 03824 USA. Florida State Univ, Dept Meteorol, Tallahassee, FL 32306 USA. NASA, Langley Res Ctr, SAIC, Hampton, VA 23681 USA. NASA, Langley Res Ctr, GATS, Hampton, VA 23681 USA. RP NASA, Langley Res Ctr, Natl Res Council, MS 483, Hampton, VA 23681 USA. EM c.e.jordan@larc.nasa.gov; b.e.anderson@larc.nasa.gov NR 45 TC 20 Z9 20 U1 1 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 NOV 15 PY 2003 VL 108 IS D21 AR 8813 DI 10.1029/2002JD003337 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 744VM UT WOS:000186653600006 ER PT J AU Kiley, CM Fuelberg, HE Palmer, PI Allen, DJ Carmichael, GR Jacob, DJ Mari, C Pierce, RB Pickering, KE Tang, YH Wild, O Fairlie, TD Logan, JA Sachse, GW Shaack, TK Streets, DG AF Kiley, CM Fuelberg, HE Palmer, PI Allen, DJ Carmichael, GR Jacob, DJ Mari, C Pierce, RB Pickering, KE Tang, YH Wild, O Fairlie, TD Logan, JA Sachse, GW Shaack, TK Streets, DG TI An intercomparison and evaluation of aircraft-derived and simulated CO from seven chemical transport models during the TRACE-P experiment SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID GENERAL-CIRCULATION MODEL; TROPICAL SOUTH ATLANTIC; ISENTROPIC-SIGMA MODEL; ATMOSPHERIC CHEMISTRY; DEPOSITION; OZONE; ASIA; EMISSIONS; AEROSOLS; BIOMASS AB Four global scale and three regional scale chemical transport models are intercompared and evaluated during NASA's Transport and Chemical Evolution over the Pacific (TRACE-P) experiment. Model simulated and measured CO are statistically analyzed along aircraft flight tracks. Results for the combination of 11 flights show an overall negative bias in simulated CO. Biases are most pronounced during large CO events. Statistical agreements vary greatly among the individual flights. Those flights with the greatest range of CO values tend to be the worst simulated. However, for each given flight, the models generally provide similar relative results. The models exhibit difficulties simulating intense CO plumes. CO error is found to be greatest in the lower troposphere. Convective mass flux is shown to be very important, particularly near emissions source regions. Occasionally meteorological lift associated with excessive model-calculated mass fluxes leads to an overestimation of middle and upper tropospheric mixing ratios. Planetary Boundary Layer (PBL) depth is found to play an important role in simulating intense CO plumes. PBL depth is shown to cap plumes, confining heavy pollution to the very lowest levels. C1 Florida State Univ, Dept Meteorol, Tallahassee, FL 32306 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02318 USA. Univ Maryland, Dept Meteorol, College Pk, MD 20742 USA. Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA 52242 USA. Univ Iowa, Dept Chem & Biochem Engn, Iowa City, IA 52242 USA. Univ Toulouse 3, UMR CNRS, Lab Aerol, F-31400 Toulouse, France. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Frontier Res Syst Global Change, Kanazawa Ku, Yokohama, Kanagawa 2360001, Japan. Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI USA. Argonne Natl Lab, Argonne, IL 60439 USA. RP Florida State Univ, Dept Meteorol, 404 Love Bldg, Tallahassee, FL 32306 USA. EM ckiley@huey.met.fsu.edu; fuelberg@huey.met.fsu.edu; pip@io.harvard.edu; allen@atmos.umd.edu; gcarmich@icaen.uiowa.edu; djacob@fas.harvard.edu; marc@aero.obs-mip.fr; r.b.pierce@larc.nasa.gov; pickerin@atmos.umd.edu; ytang@cgrer.uiowa.edu; oliver@jamstec.go.jp; tdf@io.harvard.edu; jal@io.harvard.edu; g.w.sachse@larc.nasa.gov; dstreets@anl.gov RI Wild, Oliver/A-4909-2009; Palmer, Paul/F-7008-2010; Allen, Dale/F-7168-2010; Pierce, Robert Bradley/F-5609-2010; Pickering, Kenneth/E-6274-2012 OI Wild, Oliver/0000-0002-6227-7035; Allen, Dale/0000-0003-3305-9669; Pierce, Robert Bradley/0000-0002-2767-1643; NR 51 TC 56 Z9 57 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 NOV 15 PY 2003 VL 108 IS D21 AR 8819 DI 10.1029/2002JD003089 PG 35 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 744VM UT WOS:000186653600001 ER PT J AU Lefer, BL Shetter, RE Hall, SR Crawford, JH Olson, JR AF Lefer, BL Shetter, RE Hall, SR Crawford, JH Olson, JR TI Impact of clouds and aerosols on photolysis frequencies and photochemistry during TRACE-P: 1. Analysis using radiative transfer and photochemical box models SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE photolysis frequencies; radiative transfer modeling; actinic flux spectroradiometer; photochemical box model; j-value impact factor; ozone production ID PEM-TROPICS-B; INTERCOMPARISON IPMMI; ACTINIC FLUX; ULTRAVIOLET-RADIATION; RATE COEFFICIENTS; BOUNDARY-LAYER; UV-RADIATION; PHOTODISSOCIATION; TROPOSPHERE; PACIFIC AB This study examines the agreement between photolysis frequency measurements by the NCAR scanning actinic flux spectroradiometer (SAFS) and calculations from a cloud-free model (CFM) and investigates the impact of these differences on ozone photochemistry. Overall, the mean jNO(2)measurement to model ratio for all flights of TRACE-P was 0.943 +/- 0.271. The sky conditions during the Transport and Chemical Evolution over the Pacific (TRACE-P) experiment were determined to be "cloud-free" 40% of the time; hence a CFM is frequently not representative of the local atmospheric conditions. Our analysis indicates that clouds have a larger impact on photolysis frequencies (from -90 to +200%) than do aerosols (maximum of +/-20%). The CFM and SAFS jNO(2) and jO(D-1) values differed by 9% and 0-7%, respectively, during a vertical profile through a cloud-free and low AOD atmosphere. This suggests that measurement/model agreement to less than 10% may be difficult without better aerosol optical parameter inputs even under low-AOD conditions. For the TRACE-P chemical environment, OH, NO, and HO2 were more sensitive than other compounds (e.g., CH3C(O)O-2, CH3OOH) to changes (or errors) in photolysis frequency inputs to a photochemical box model. Compounds including NO2, PAN, and HCHO exhibited different relationships to j-value changes below and above the boundary layer. Ozone production and loss rates increased linearly with changes (or errors) in the photolysis frequency with the resulting net O-3 tendency increasing with a linear slope near unity. During the TRACE-P mission the net photochemical effect of clouds and aerosols was a large decrease in photochemical O-3 production in the boundary layer. C1 Natl Ctr Atmospher Res, Boulder, CO 80305 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Lefer, BL (reprint author), Natl Ctr Atmospher Res, Boulder, CO 80305 USA. EM lefer@ucar.edu; shetter@ucar.edu; halls@ucar.edu; j.h.crawford@larc.nasa.gov; j.r.olson@larc.nasa.gov RI Crawford, James/L-6632-2013; Lefer, Barry/B-5417-2012 OI Crawford, James/0000-0002-6982-0934; Lefer, Barry/0000-0001-9520-5495 NR 51 TC 34 Z9 35 U1 0 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 NOV 15 PY 2003 VL 108 IS D21 AR 8821 DI 10.1029/2002JD003171 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 744VM UT WOS:000186653600003 ER PT J AU Woo, JH Streets, DG Carmichael, GR Tang, YH Yoo, B Lee, WC Thongboonchoo, N Pinnock, S Kurata, G Uno, I Fu, QY Vay, S Sachse, GW Blake, DR Fried, A Thornton, DC AF Woo, JH Streets, DG Carmichael, GR Tang, YH Yoo, B Lee, WC Thongboonchoo, N Pinnock, S Kurata, G Uno, I Fu, QY Vay, S Sachse, GW Blake, DR Fried, A Thornton, DC TI Contribution of biomass and biofuel emissions to trace gas distributions in Asia during the TRACE-P experiment SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE bioemissions; chemical mass balance; Asian outflow ID RECEPTOR MODEL; BLACK CARBON; INDIAN-OCEAN; POLLUTION; IDENTIFICATION AB A comprehensive emission inventory with enhanced spatial and temporal resolution is used to help quantify the contribution from three source categories (fossil, biofuel, and biomass burning) during the NASA TRACE-P experiment. Daily biomass burning emissions are developed to support this analysis. Emissions of 27 species and their ratios, by sector, region, and source category are presented. The emission distributions and chemical composition are further analyzed using various statistical techniques. Using cluster analysis, the 27 chemical species are combined into 8 groups that have similar regional distribution, and 52 regions are assembled into 11 regional groups that have similar chemical composition. These groups are used in Chemical Mass Balance analysis to characterize air masses and to quantify the contribution of the three source categories to the observed species distributions. Five DC8 flights with 16 flight segments associated with outflow events are analyzed. In general, Asian outflow is a complex mixture of biofuel, biomass, and fossil sources. Flights in the post frontal regions at high latitudes and low altitudes have a high contribution of fossil fuel emissions. Flights in the warm sector of cold fronts are dominated by biomass burning contributions (about 70%). Biofuel contributions are high (about 70%) when air masses come from central China. The receptor model results are shown to be consistent with other 3-D chemical model sensitivity studies and analysis using ratios of indicator species (e. g., dK(+)/dSO(4)(2-), CH3CN/(SOy), SOy/CO, and C2Cl4/CO). C1 Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA 52242 USA. Argonne Natl Lab, Decis & Informat Sci Div, Argonne, IL 60439 USA. Univ Iowa, Dept Biostat, Iowa City, IA 52242 USA. ACT Inc, Iowa City, IA 52243 USA. European Commiss, Joint Res Ctr, Ispra, Italy. Toyohashi Univ Technol, Dept Ecol Engn, Toyohashi, Aichi 4418580, Japan. Kyushu Univ, Appl Mech Res Inst, Fukuoka 8168580, Japan. Shanghai Acad Environm Sci, Shanghai, Peoples R China. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Univ Calif Irvine, Dept Chem, Irvine, CA 92697 USA. Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80303 USA. Drexel Univ, Dept Chem, Philadelphia, PA 19104 USA. RP Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA 52242 USA. EM woojh21@cgrer.uiowa.edu RI Uno, Itsushi/B-5952-2011; Kyushu, RIAM/F-4018-2015; U-ID, Kyushu/C-5291-2016; Tang, Youhua/D-5205-2016 OI Tang, Youhua/0000-0001-7089-7915 NR 35 TC 53 Z9 54 U1 0 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 NOV 15 PY 2003 VL 108 IS D21 AR 8812 DI 10.1029/2002JD003200 PG 36 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 744VM UT WOS:000186653600004 ER PT J AU Cody, RJ Romani, PN Nesbitt, FL Iannone, MA Tardy, DC Stief, LJ AF Cody, RJ Romani, PN Nesbitt, FL Iannone, MA Tardy, DC Stief, LJ TI Rate constant for the reaction CH3+CH3 -> C2H6 at T=155 K and model calculation of the CH3 abundance in the atmospheres of Saturn and Neptune SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE methyl radical combination; low temperature rate constant; Lindemann expression; Saturn; Neptune; atmospheric photochemical models ID THERMAL UNIMOLECULAR REACTIONS; SPECTROMETER SOLAR OCCULTATIONS; METHYL RADICAL RECOMBINATION; COLLISION RATE CONSTANTS; GENERAL EXPRESSION; MASS-SPECTROMETRY; RATE COEFFICIENTS; ISO OBSERVATIONS; MASTER EQUATION; ENERGY-TRANSFER AB [1] The column abundances of CH3 observed by the Infrared Space Observatory (ISO) satellite on Saturn and Neptune were lower than predicted by atmospheric photochemical models, especially for Saturn. It has been suggested that the models underestimated the loss of CH3 due to poor knowledge of the rate constant k of the CH3 + CH3 self-reaction at the low temperatures and pressures of these atmospheres. Motivated by this suggestion, we undertook a combined experimental and photochemical modeling study of the CH3 + CH3 reaction and its role in determining planetary CH3 abundances. In a discharge flow-mass spectrometer system, k was measured at T = 155 K and three pressures of He. The results in units of cm(3) molecule(-1) s(-1) are k(0.6 Torr) = 6.82 x 10(-11), k(1.0 Torr) = 6.98 x 10(-11), and k(1.5 Torr) = 6.91 x 10(-11). Analytical expressions for k were derived that ( 1) are consistent with the present laboratory data at T = 155 K, our previous data at T = 202 K and 298 K, and those of other studies in He at T = 296 - 298 K and (2) have some theoretical basis to provide justification for extrapolation. The derived analytical expressions were then used in atmospheric photochemical models for both Saturn and Neptune. These model results reduced the disparity with observations of Saturn, but not with observations of Neptune. However, the disparity for Neptune is much smaller. The solution to the remaining excess CH3 prediction in the models relative to the ISO observations lies, to a large extent, elsewhere in the CH3 photochemistry or transport, not in the CH3 + CH3 rate. C1 NASA, Extraterr Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Catholic Univ Amer, Dept Chem, Washington, DC 20064 USA. Millersville Univ Pennsylvania, Dept Chem, Millersville, PA 17551 USA. Univ Iowa, Dept Chem, Iowa City, IA 52242 USA. RP Cody, RJ (reprint author), NASA, Extraterr Phys Lab, Goddard Space Flight Ctr, Code 691, Greenbelt, MD 20771 USA. EM regina.cody@nasa.gov RI Romani, Paul/D-2729-2012; Cody, Regina/D-5996-2013 NR 52 TC 15 Z9 15 U1 2 U2 5 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 NOV 15 PY 2003 VL 108 IS E11 AR 5119 DI 10.1029/2002JE002037 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 744XA UT WOS:000186657100001 ER PT J AU Johnson, JR Horz, F AF Johnson, JR Horz, F TI Visible/near-infrared spectra of experimentally shocked plagioclase feldspars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE feldspars; spectroscopy; visible/near-infrared; pressure; shock; maskelynite ID METAMORPHISM; SPECTROSCOPY; ANORTHOSITE; REFLECTANCE; CONSTRAINTS; ROCKS; GLASS AB [1] High shock pressures cause structural changes in plagioclase feldspars such as mechanical fracturing and disaggregation of the crystal lattice at submicron scales, the formation of diaplectic glass (maskelynite), and genuine melting. Past studies of visible/ near-infrared spectra of shocked feldspars demonstrated few spectral variations with pressure except for a decrease in the depth of the absorption feature near 1250 - 1300 nm and an overall decrease in reflectance. New visible/ near - infrared spectra ( 400 - 2500 nm) of experimentally shocked (17 - 56 GPa) albite- and anorthite-rich rock powders demonstrate similar trends, including the loss of minor hydrated mineral bands near 1410, 1930, 2250, and 2350 nm. However, the most interesting new observations are increases in reflectance at intermediate pressures, followed by subsequent decreases in reflectance at higher pressures. The amount of internal scattering and overall sample reflectance is controlled by the relative proportions of micro-fractures, submicron grains, diaplectic glass, and melts formed during shock metamorphism. We interpret the observed reflectance increases at intermediate pressures to result from progressively larger proportions of submicron feldspar grains and diaplectic glass. The ensuing decreases in reflectance occur after diaplectic glass formation is complete and the proportion of genuine melt inclusions increases. The pressure regimes over which these reflectance variations occur differ between albite and anorthite, consistent with thermal infrared spectra of these samples and previous studies of shocked feldspars. These types of spectral variations associated with different peak shock pressures should be considered during interpretation and modeling of visible/ near-infrared remotely sensed spectra of planetary and asteroidal surfaces. C1 US Geol Survey, Flagstaff, AZ 86001 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP US Geol Survey, 2255 N Gemini Dr, Flagstaff, AZ 86001 USA. EM jrjohnson@usgs.gov RI Johnson, Jeffrey/F-3972-2015 NR 39 TC 31 Z9 31 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD NOV 15 PY 2003 VL 108 IS E11 AR 5120 DI 10.1029/2003JE002127 PG 6 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 744XA UT WOS:000186657100004 ER PT J AU Siqueira, P Chapman, B McGarragh, G AF Siqueira, P Chapman, B McGarragh, G TI The coregistration, calibration, and interpretation of multiseason JERS-1 SAR data over South America SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE JERS-1 SAR; South America; Large-Scale Biosphere-Atmosphere ID SYNTHETIC-APERTURE RADAR; SIR-C/X-SAR; AMAZON BASIN; SATELLITE DATA; DEFORESTATION; VALIDATION; VEGETATION; MICHIGAN; MOSAICS; CARBON AB The Large-Scale Biosphere-Atmosphere(LBA) experiment in Amazonia represents a unique opportunity to make a comprehensive study of the Amazon region and its component ecosystems. To make sense of the field studies and to generalize the results from them, remote sensing techniques and comprehensive mapping are critical elements for producing region-wide science results. In this paper, we present the processing work done for one such mapping campaign, that of the JERS-1 L-band two season (low and high-flood) SAR data collected in 1995 and 1996. Specifically, to make a useable resource for other LBA researchers to explore, the datasets from the two seasons had to be coregistered (to a sub-pixel level), radiometrically calibrated, and interpreted to verify the quality of the data. This paper describes the techniques used to achieve these goals and an estimate of the land cover based on a simple classification of the data. (C) 2003 Elsevier Inc. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Siqueira, P (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Siqueira, Paul/D-9760-2016 OI Siqueira, Paul/0000-0001-5781-8282 NR 30 TC 10 Z9 11 U1 1 U2 2 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 NOV 15 PY 2003 VL 87 IS 4 BP 389 EP 403 DI 10.1016/j.rse.2002.12.002 PG 15 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 747WA UT WOS:000186827400002 ER PT J AU Shukla, S Patil, S Kuiry, SC Rahman, Z Du, T Ludwig, L Parish, C Seal, S AF Shukla, S Patil, S Kuiry, SC Rahman, Z Du, T Ludwig, L Parish, C Seal, S TI Synthesis and characterization of sol-gel derived nanocrystalline tin oxide thin film as hydrogen sensor SO SENSORS AND ACTUATORS B-CHEMICAL LA English DT Article DE alkoxide; hydrogen; nanocrystalline; sensor; sol-gel; tin oxide ID GAS-SENSING CHARACTERISTICS; ION-ASSISTED DEPOSITION; H-2 SENSOR; SNO2; THICKNESS; SENSITIVITY; PALLADIUM; CARBON AB Tin oxide (SnOx) semiconductor thin film is coated on Pyrex glass (silica) substrates using the sol-gel dip-coating technique utilizing alkoxide precursor. The thin film is extensively characterized for its surface morphology, chemistry, thickness, and nanocrystallite size using different analytical techniques such as scanning electron microscopy (SEM), X-ray photoelectron spectroscopy (XPS), atomic force microscopy (AFM), and high-resolution transmission electron microscopy (HRTEM). The HRTEM sample preparation is done for the first time using focused ion-beam (FIB) milling technique. Under the given processing conditions, SnOx, semiconductor thin film having thickness 100-150 nm and nanocrystallite size 6-8 nm is obtained. In view of the reported literature and the present experimental data, it is demonstrated that the film is suitable for sensing H-2 gas at room temperature. Sensitivity value as high as 394% is observed at room temperature for 4 vol.% H-2, which is an explosive limit at room temperature for the space-based applications as set by NASA. (C) 2003 Elsevier B.V. All rights reserved. C1 Univ Cent Florida, AMPAC, MMAE, Mech Mat Aerosp Engn Dept, Orlando, FL 32816 USA. NASA, John F Kennedy Space Ctr, Kennedy Space Ctr, FL 32899 USA. RP Seal, S (reprint author), Univ Cent Florida, AMPAC, MMAE, Mech Mat Aerosp Engn Dept, Engn 381,4000 Cent Florida Blvd, Orlando, FL 32816 USA. OI Shukla, Satyajit/0000-0002-7947-8095 NR 33 TC 81 Z9 83 U1 2 U2 23 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0925-4005 J9 SENSOR ACTUAT B-CHEM JI Sens. Actuator B-Chem. PD NOV 15 PY 2003 VL 96 IS 1-2 BP 343 EP 353 DI 10.1016/S0925-4005(03)00568-9 PG 11 WC Chemistry, Analytical; Electrochemistry; Instruments & Instrumentation SC Chemistry; Electrochemistry; Instruments & Instrumentation GA 748TZ UT WOS:000186878300043 ER PT J AU Chao, BF Au, AY Boy, JP Cox, CM AF Chao, BF Au, AY Boy, JP Cox, CM TI Time-variable gravity signal of an anomalous redistribution of water mass in the extratropic Pacific during 1998-2002 SO GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS LA English DT Article DE time-variable gravity; J(2) anomaly; extratropic Pacific; water mass distribution; geodesy and gravity : ocean/earth/atmosphere interactions; oceanography : general : climate and interannual variability ID INTERDECADAL VARIABILITY; EARTH ROTATION; EL-NINO; OCEAN; CLIMATE; FIELD; OSCILLATION; CIRCULATION; LAGEOS; MODEL AB Cox and Chao [2002] reported the detection of a large anomaly in the time series of Earth's dynamic oblateness J(2), the lowest-degree gravity spatial harmonic, in the form of a positive jump since 1998 overshadowing the decreasing secular trend in J(2) caused primarily by the postglacial rebound (PGR). Here we report that recent data show that J(2) has been rapidly returning toward "normal'' (with PGR considered) since early 2001. In search of the geophysical and climatic causes for this "1998-2002 J(2) anomaly,'' we report an oceanographic event that took place in the extratropic north and south Pacific basins that was found to match remarkably well with the time evolution of the anomaly. We examine the leading (nonseasonal, extratropic Pacific) Empirical Orthogonal Function/Principal Component modes in the sea-surface height (SSH) data from TOPEX/Poseidon, sea surface temperature (SST) data from the National Center for Environmental Predictions, and output fields of the Estimating the Circulation and the Climate of the Ocean (ECCO) ocean general circulation model (OGCM), including ocean bottom pressure (OBP) and temperature and salinity profiles. The phenomenon appears to be part of the Pacific Decadal Oscillation, and temporal correlations are made. However, quantitatively, the OBP field of the ECCO model predicts a J(2) anomaly that is smaller in magnitude than the observed by a factor of about 3. We discuss various possibilities for reconciling this discrepancy in terms of inadequacies of present OGCMs and considering other geophysical contributions; a complete resolution of the J(2) enigma awaits further studies. C1 NASA, Goddard Space Flight Ctr, Space Geodesy Branch, Greenbelt, MD 20771 USA. NASA, Raytheon ITSS, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Chao, BF (reprint author), NASA, Goddard Space Flight Ctr, Space Geodesy Branch, Greenbelt, MD 20771 USA. RI Chao, Benjamin Fong/N-6156-2013; Boy, Jean-Paul/E-6677-2017 OI Boy, Jean-Paul/0000-0003-0259-209X NR 33 TC 23 Z9 23 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1525-2027 J9 GEOCHEM GEOPHY GEOSY JI Geochem. Geophys. Geosyst. PD NOV 14 PY 2003 VL 4 AR 1096 DI 10.1029/2003GC000589 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 744UJ UT WOS:000186651000003 ER PT J AU Black, RA Heymsfield, GM Hallett, J AF Black, RA Heymsfield, GM Hallett, J TI Extra large particle images at 12 km in a hurricane eyewall: Evidence of high-altitude supercooled water? SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ICE AB The conventional wisdom about hurricanes suggests that updrafts are weak and supercooled water is scarce in the eyewall, and almost non-existent at temperatures colder than about -5degreesC [Black and Hallett, 1986]. However, there is evidence that some hurricanes are different. Questions about the existence of high-altitude supercooled cloud water cannot be answered with only the instruments aboard the typical propeller-driven aircraft. During the summer of 1998, the NASA DC-8 aircraft made penetrations of the intensifying eyewall of Hurricane Bonnie at 12 km MSL, collecting the first truly high-altitude 2-D particle imagery in a hurricane. The similarity of the splash images in Hurricane Bonnie to those from raindrops obtained at higher temperatures in other hurricanes suggests that the large images obtained by the DC-8 were soft, low density graupel, rather than hard, high-density graupel particles or frozen raindrops. This implies that these particles grew to several millimeters in diameter at altitude, rather than simply advecting from lower, warmer altitudes. This growth in turn requires the presence of deeply supercooled cloud droplets. Thermal emission from supercooled water aloft increases the microwave brightness temperatures, giving a misleading impression that there is much less ice aloft than actually exists. The extra attenuation from the occasional presence of large graupel at these altitudes reduces the ability of microwave sensors to see precipitation at lower altitudes. Both of these effects impede efforts to accurately quantify condensate mass remotely from radiometric data such as that provided by the TRMM satellite. C1 NOAA, Atlantic Oceanog & Meteorol Lab, Hurricane Res Div, Miami, FL 33149 USA. NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Branch, Greenbelt, MD 20771 USA. Univ Nevada, Desert Res Inst, Reno, NV 89512 USA. RP Black, RA (reprint author), NOAA, Atlantic Oceanog & Meteorol Lab, Hurricane Res Div, Miami, FL 33149 USA. RI Black, Robert/C-9617-2009 OI Black, Robert/0000-0001-6938-125X NR 11 TC 7 Z9 7 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD NOV 14 PY 2003 VL 30 IS 21 AR 2124 DI 10.1029/2003GL017864 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 744UU UT WOS:000186651900001 ER PT J AU Huebert, BJ Bates, T Russell, PB Shi, GY Kim, YJ Kawamura, K Carmichael, G Nakajima, T AF Huebert, BJ Bates, T Russell, PB Shi, GY Kim, YJ Kawamura, K Carmichael, G Nakajima, T TI An overview of ACE-Asia: Strategies for quantifying the relationships between Asian aerosols and their climatic impacts SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE Asia; aerosols; radiative forcing ID WESTERN NORTH PACIFIC; SOIL DUST AEROSOL; SINGLE-SCATTERING ALBEDO; INDIAN-OCEAN EXPERIMENT; SEA-SALT AEROSOLS; EAST CHINA SEA; OPTICAL-PROPERTIES; IN-SITU; TROPOSPHERIC AEROSOLS; ELEMENTAL CARBON AB The International Global Atmospheric Chemistry Program (IGAC) has conducted a series of Aerosol Characterization Experiments (ACE) that integrate in situ measurements, satellite observations, and models to reduce the uncertainty in calculations of the climate forcing due to aerosol particles. ACE-Asia, the fourth in this series of experiments, consisted of two focused components: (1) An intensive field study that sought to quantify the spatial and vertical distribution of aerosol concentrations and properties, the processes controlling their formation, evolution, and fate, and the column-integrated radiative effect of the aerosol (late March through May 2001). (2) A longer-term network of ground stations that used in situ and column-integrated measurements to quantify the chemical, physical, and optical properties of aerosols in the ACE-Asia study area and to assess their spatial and temporal (seasonal and interannual) variability (2000-2003). The approach of the ACE-Asia science team was to make simultaneous measurements of aerosol chemical, physical, and optical properties and their radiative impacts in a variety of air masses, often coordinated with satellite overpasses. Three aircraft, two research ships, a network of lidars, and many surface sites gathered data on Asian aerosols. Chemical transport models (CTMs) were integrated into the program from the start, being used in a forecast mode during the intensive observation period to identify promising areas for airborne and ship observations and then later as tools for integrating observations. The testing and improvement of a wide range of aerosol models (including microphysical, radiative transfer, CTM, and global climate models) was one important way in which we assessed our understanding of the properties and controlling processes of Asian aerosols. We describe here the scientific goals and objectives of the ACE-Asia experiment, its observational strategies, the types of observations made by the mobile platforms and stationary sites, the models that will integrate our understanding of the climatic effect of aerosol particles, and the types of data that have been generated. Eight scientific questions focus the discussion. The intensive observations took place during a season of unusually heavy dust, so we have a large suite of observations of dust and its interaction with air pollutants. Further information about ACE-Asia can be found on the project Web site at http://saga.pmel.noaa.gov/aceasia/. C1 Univ Hawaii, Dept Oceanog, Honolulu, HI 96822 USA. NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Chinese Acad Sci, Inst Atmospher Phys, Beijing 100029, Peoples R China. Kwangju Inst Sci & Technol, Dept Environm Sci & Engn, Adv Environm Monitoring Res Ctr, Kwangju 500712, South Korea. Hokkaido Univ, Inst Low Temp Sci, Kita Ku, Sapporo, Hokkaido 0600819, Japan. Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA 52240 USA. Univ Tokyo, Ctr Climate Syst Res, Meguro Ku, Tokyo 1538904, Japan. RP Univ Hawaii, Dept Oceanog, Honolulu, HI 96822 USA. EM huebert@hawaii.edu; bates@pmel.noaa.gov; prussell@mail.arc.nasa.gov; shigy@mail.iap.ac.cn; yjkim@kjist.ac.kr; kawamura@lowtem.hokudai.ac.jp; gcarmich@icaen.uiowa.edu; teruyuki@ccsr.u-tokyo.ac.jp RI Kawamura, Kimitaka/B-3839-2011; Nakajima, Teruyuki/H-2370-2013; Bates, Timothy/L-6080-2016 OI Nakajima, Teruyuki/0000-0002-9042-504X; NR 100 TC 507 Z9 534 U1 11 U2 54 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 NOV 14 PY 2003 VL 108 IS D23 AR 8633 DI 10.1029/2003JD003550 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 744VW UT WOS:000186654400001 ER PT J AU Johnson, PV Kanik, I Khakoo, MA McConkey, JW Tayal, SS AF Johnson, PV Kanik, I Khakoo, MA McConkey, JW Tayal, SS TI Low energy differential and integral electron-impact cross sections for the 2s(2)2p(4) P-3 -> 2p(3)3s S-3(o) excitation in atomic oxygen SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID MOLECULAR-OXYGEN; TRANSITION 1304; VALUES AB 0Differential and integral cross sections (ICSs) for 2s(2)2p(4) P-3 --> 2p(3)3s S-3(o) excitation in atomic oxygen have been measured at electron-impact energies of 15, 17.5, 20, 22.5 and 27.5 eV. Differential measurements were conducted with a conventional electron energy-loss spectrometer and a microwave discharge source of atomic oxygen. Relative differential cross sections (DCSs) were determined between 15 and 30 eV impact energy. With the help of theoretical predictions of the shape of the DCS at large angles, measured results were extrapolated to 1800 scattering angle and relative ICSs were deduced. The relative excitation function was normalized to the 30 eV impact energy ICS given by Kanik et al (2001 J. Phys. B: At. MoL Opt. Phys. 34 2647). Normalization of the ICS values allowed the measured DCSs to be put on the absolute scale. Theoretical calculations of the DCSs were carried out using the R-matrix with the pseudostates approach. A total of 22 spectroscopic bound and autoionizing states, together with 19 pseudostates, were included in the close-coupling expansion. The pseudostates were chosen to simulate continuum target states. Theoretical results, along with other available experimental data, have been compared with the current experimental results. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Calif State Univ Fullerton, Dept Phys, Fullerton, CA 92634 USA. Univ Windsor, Dept Phys, Windsor, ON N9B 3P4, Canada. Clark Atlanta Univ, Dept Phys, Atlanta, GA 30314 USA. RP Johnson, PV (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Johnson, Paul/D-4001-2009 OI Johnson, Paul/0000-0002-0186-8456 NR 17 TC 14 Z9 14 U1 0 U2 3 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 NOV 14 PY 2003 VL 36 IS 21 BP 4289 EP 4299 AR PII S0953-4075(03)65286-7 DI 10.1088/0953-4075/36/21/008 PG 11 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 750KG UT WOS:000186989400014 ER PT J AU Li, ZQ Ackerman, TP Wiscombe, W Stephens, GL AF Li, ZQ Ackerman, TP Wiscombe, W Stephens, GL TI Have clouds darkened since 1995? SO SCIENCE LA English DT Letter ID SHORTWAVE EXPERIMENT ARESE; SOLAR-RADIATION; ATMOSPHERIC ABSORPTION; SATELLITE C1 Univ Maryland, Dept Meteorol, College Pk, MD 20742 USA. Univ Maryland, ESSIC, College Pk, MD 20742 USA. Chinese Acad Sci, Inst Atmospher Phys, Beijing 100864, Peoples R China. Pacific NW Natl Lab, Atmospher Radiat Measurement Program, Richland, WA 99352 USA. NASA, Climate & Radiat Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. RP Li, ZQ (reprint author), Univ Maryland, Dept Meteorol, 2207 CSS Bldg, College Pk, MD 20742 USA. RI Wiscombe, Warren/D-4665-2012; Li, Zhanqing/F-4424-2010 OI Wiscombe, Warren/0000-0001-6844-9849; Li, Zhanqing/0000-0001-6737-382X NR 15 TC 2 Z9 2 U1 0 U2 8 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 NOV 14 PY 2003 VL 302 IS 5648 BP 1150 EP 1151 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 742XW UT WOS:000186544300022 ER PT J AU Smith, EJ Marsden, RG Balogh, A Gloeckler, G Geiss, J McComas, DJ McKibben, RB MacDowall, RJ Lanzerotti, LJ Krupp, N Krueger, H Landgraf, M AF Smith, EJ Marsden, RG Balogh, A Gloeckler, G Geiss, J McComas, DJ McKibben, RB MacDowall, RJ Lanzerotti, LJ Krupp, N Krueger, H Landgraf, M TI The Sun and heliosphere at solar maximum SO SCIENCE LA English DT Review ID ULYSSES OBSERVATIONS; MAGNETIC-FIELD; MODULATION; LATITUDE; POLE AB Recent Ulysses observations from the Sun's equator to the poles reveal fundamental properties of the three-dimensional heliosphere at the maximum in solar activity. The heliospheric magnetic field originates from a magnetic dipole oriented nearly perpendicular to, instead of nearly parallel to, the Sun's rotation axis. Magnetic fields, solar wind, and energetic charged particles from low-latitude sources reach all latitudes, including the polar caps. The very fast high-latitude wind and polar coronal holes disappear and reappear together. Solar wind speed continues to be inversely correlated with coronal temperature. The cosmic ray flux is reduced symmetrically at all latitudes. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. European Space Agcy, European Space Technol Ctr, Dept Space Sci, NL-2200 AG Noordwijk, Netherlands. Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BZ, England. Univ Maryland, Dept Phys, College Pk, MD 20742 USA. Int Space Sci Inst, CH-3012 Bern, Switzerland. SW Res Inst, San Antonio, TX 78238 USA. Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Lucent Technol, Bell Labs, Murray Hill, NJ 07974 USA. New Jersey Inst Technol, Ctr Solar Terr Res, Newark, NJ 07021 USA. Max Planck Inst Aeron, D-37191 Katlenburg Lindau, Germany. Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. RP Smith, EJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI MacDowall, Robert/D-2773-2012 NR 35 TC 51 Z9 51 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 NOV 14 PY 2003 VL 302 IS 5648 BP 1165 EP 1169 DI 10.1126/science.1086295 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 742XW UT WOS:000186544300040 PM 14615526 ER PT J AU Newburn, RL Duxbury, TC Hanner, M Semenov, BV Hirst, EE Bhat, RS Bhaskaran, S Wang, TCM Tsou, P Brownlee, DE Cheuvront, AR Gingerich, DE Bollendonk, GR Vellinga, JM Parham, KA Mumaw, SJ AF Newburn, RL Duxbury, TC Hanner, M Semenov, BV Hirst, EE Bhat, RS Bhaskaran, S Wang, TCM Tsou, P Brownlee, DE Cheuvront, AR Gingerich, DE Bollendonk, GR Vellinga, JM Parham, KA Mumaw, SJ TI Phase curve and albedo of asteroid 5535 Annefrank SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE 5535 Annefrank; asteroid photometry; asteroid phase curves; asteroid imaging; asteroid albedos ID GALILEO PHOTOMETRY AB Seventy-two images of the S-class asteroid 5535 Annefrank, acquired on 2 November 2002 at target ranges of 11,415-3078.5 km, were transmitted to Earth as a part of an engineering readiness test of the Stardust mission. Forty-four of these were used to create a phase curve extending to 134degrees, the largest angle yet achieved for any S-class asteroid. Flux fell by more than six magnitudes between the extrapolated 0degrees and 134degrees. A maximum illuminated cross section of 16 km(2) was seen at a phase angle of 47.2degrees. Assuming a camera efficiency of 75%, a broadband (470-940 nm) geometric albedo of 0.24 was derived for Annefrank. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Washington, Dept Astron, Seattle, WA 98195 USA. Lockheed Martin Astronaut, Denver, CO 80201 USA. RP Newburn, RL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 6 TC 12 Z9 13 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD NOV 12 PY 2003 VL 108 IS E11 AR 5117 DI 10.1029/2003JE002106 PG 7 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 744WW UT WOS:000186656700001 ER PT J AU Pan, FF Peters-Lidard, CD Sale, MJ AF Pan, FF Peters-Lidard, CD Sale, MJ TI An analytical method for predicting surface soil moisture from rainfall observations SO WATER RESOURCES RESEARCH LA English DT Article DE soil moisture; precipitation; Antecedent Precipitation Index (API); loss coefficient ID PLANETARY BOUNDARY-LAYER; CATCHMENT-BASED APPROACH; MESOSCALE CIRCULATIONS; MODEL; VARIABILITY; SENSITIVITY; IMPACT; WATER; SIMULATION; VEGETATION AB [1] A simple analytical method for estimating surface soil moisture directly from rainfall data is proposed and studied. Soil moisture dynamics are represented by a linear stochastic partial differential equation [Entekhabi and Rodriguez-Iturbe, 1994]. A diagnostic equation is derived from the soil moisture dynamics equation by eliminating the diffusion term. The derived daily soil moisture function is a time-weighted average of previous cumulative rainfall over a given period (e.g., > 14 days). The advantage of this method is that information on the initial condition of soil moisture, which is often not available at all times and locations, is not needed. The loss coefficient in the diagnostic equation for soil moisture can be estimated from land surface characteristics and soil properties. The method for determining the averaging window size, the loss coefficient, and the infiltration coefficient are described and demonstrated. The soil moisture data observed during three field experiments, i.e., Monsoon' 90, Washita' 92, and SGP' 97, are compared to the calculated soil moisture. The results indicate that the proposed method is robust and has the potential for useful soil moisture predictions. C1 Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA. NASA, Hydrol Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20071 USA. RP Pan, FF (reprint author), Oak Ridge Natl Lab, Div Environm Sci, MS 6335, Oak Ridge, TN 37831 USA. RI Pan, Feifei/D-3370-2015; Peters-Lidard, Christa/E-1429-2012 OI Pan, Feifei/0000-0003-4373-7566; Peters-Lidard, Christa/0000-0003-1255-2876 NR 41 TC 29 Z9 30 U1 1 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 J9 WATER RESOUR RES JI Water Resour. Res. PD NOV 12 PY 2003 VL 39 IS 11 AR 1314 DI 10.1029/2003WR002142 PG 20 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 744XR UT WOS:000186658600002 ER PT J AU Carmichael, GR Tang, Y Kurata, G Uno, I Streets, D Woo, JH Huang, H Yienger, J Lefer, B Shetter, R Blake, D Atlas, E Fried, A Apel, E Eisele, F Cantrell, C Avery, M Barrick, J Sachse, G Brune, W Sandholm, S Kondo, Y Singh, H Talbot, R Bandy, A Thorton, D Clarke, A Heikes, B AF Carmichael, GR Tang, Y Kurata, G Uno, I Streets, D Woo, JH Huang, H Yienger, J Lefer, B Shetter, R Blake, D Atlas, E Fried, A Apel, E Eisele, F Cantrell, C Avery, M Barrick, J Sachse, G Brune, W Sandholm, S Kondo, Y Singh, H Talbot, R Bandy, A Thorton, D Clarke, A Heikes, B TI Regional-scale chemical transport modeling in support of the analysis of observations obtained during the TRACE-P experiment SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID AEROSOL DISTRIBUTIONS; ASIA; EMISSIONS; SEA; ASSIMILATION; METHODOLOGY; EVOLUTION; INDOEX; SYSTEM; OCEAN AB Data obtained during the TRACE-P experiment is used to evaluate how well the CFORS/STEM-2K1 regional-scale chemical transport model is able to represent the aircraft observations. Thirty-one calculated trace gas and aerosol parameters are presented and compared to the in situ data. The regional model is shown to accurately predict many of the important features observed. The mean values of all the model parameters in the lowest 1 km are predicted within +/-30% of the observed values. The correlation coefficients (R) for the meteorological parameters are found to be higher than those for the trace species. For example, for temperature, R>0.98. Among the trace species, ethane, propane, and ozone show the highest values (0.8100 cm(-3)) were observed both within and along the upper outer edges of plumes that were identified by enhanced carbon monoxide and fine particulate sulfate concentrations. The results from two research flights are investigated in detail. Three to four-nm particle concentrations are generally correlated with gas phase sulfuric acid and found in regions of low surface areas relative to the immediate surroundings or where there are steep transitions to lower surface areas. Sulfuric acid and surface area concentrations in the most polluted plume reached 6x10(7) cm(-3) and 750 mum(2) cm(-3), respectively, in regions of particle formation. In contrast to these anthropogenic plumes, few 3 to 4 nm particles were observed in the clean background and few were detected within a volcanic plume where the studies highest H2SO4 concentrations (>10(8) cm(-3)) were recorded. Enhanced SO2 concentrations in the range of approximately 2 to 7 ppb, in conjunction with other unidentified, possibly coemitted species, appear to be the driving factor for nucleation. C1 Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. NASA, Langley Res Ctr, Hampton, VA 23665 USA. Univ Hawaii Manoa, Dept Oceanog, Honolulu, HI 96822 USA. Natl Ctr Atmospher Res, Boulder, CO 80307 USA. Drexel Univ, Dept Chem, Philadelphia, PA 19104 USA. Florida State Univ, Dept Meteorol, Tallahassee, FL 32306 USA. RP Georgia Inst Technol, Sch Earth & Atmospher Sci, 311 Ferst Dr, Atlanta, GA 30332 USA. EM rweber@eas.gatech.edu; gte822w@prism.gatech.edu; g.chen@express.larc.nasa.gov; pwang@quadramed.com; kapustin@soest.hawaii.edu; kmoore@soest.hawaii.edu; tclarke@soest.hawaii.edu; mauldin@ucar.edu; kosciuch@ucar.edu; cantrell@ucar.edu; eisele@ucar.edu; dct@drexel.edu; bandyar@drexel.edu; g.w.sachse@larc.nasa.gov; fuelberg@huey.met.fsu.edu NR 45 TC 38 Z9 38 U1 1 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 11 PY 2003 VL 108 IS D21 AR 8814 DI 10.1029/2002JD003112 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 744VC UT WOS:000186652700005 ER PT J AU Wild, O Sundet, JK Prather, MJ Isaksen, ISA Akimoto, H Browell, EV Oltmans, SJ AF Wild, O Sundet, JK Prather, MJ Isaksen, ISA Akimoto, H Browell, EV Oltmans, SJ TI Chemical transport model ozone simulations for spring 2001 over the western Pacific: Comparisons with TRACE-P lidar, ozonesondes, and Total Ozone Mapping Spectrometer columns SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE tropospheric ozone; tropopause; stratospheric intrusions; Western Pacific ID CHEMISTRY; EMISSIONS; SYSTEM; TROPOSPHERE; SCHEMES; ASIA AB Two closely related chemical transport models (CTMs) employing the same high-resolution meteorological data (similar to180 km x similar to180 km x similar to600 m) from the European Centre for Medium-Range Weather Forecasts are used to simulate the ozone total column and tropospheric distribution over the western Pacific region that was explored by the NASA Transport and Chemical Evolution over the Pacific (TRACE-P) measurement campaign in February-April 2001. We make extensive comparisons with ozone measurements from the lidar instrument on the NASA DC-8, with ozonesondes taken during the period around the Pacific Rim, and with TOMS total column ozone. These demonstrate that within the uncertainties of the meteorological data and the constraints of model resolution, the two CTMs (FRSGC/UCI and Oslo CTM2) can simulate the observed tropospheric ozone and do particularly well when realistic stratospheric ozone photochemistry is included. The greatest differences between the models and observations occur in the polluted boundary layer, where problems related to the simplified chemical mechanism and inadequate horizontal resolution are likely to have caused the net overestimation of about 10 ppb mole fraction. In the upper troposphere, the large variability driven by stratospheric intrusions makes agreement very sensitive to the timing of meteorological features. C1 Frontier Res Syst Global Change, Kanazawa Ku, Yokohama, Kanagawa 2360001, Japan. Univ Oslo, Dept Geophys, Oslo, Norway. Univ Calif Irvine, Irvine, CA USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. NOAA, Climate Monitoring & Diagnost Lab, Boulder, CO 80303 USA. RP Wild, O (reprint author), Frontier Res Syst Global Change, Kanazawa Ku, 3172-25 Showa Machi, Yokohama, Kanagawa 2360001, Japan. EM oliver@jamstec.go.jp; j.k.sundet@geofysikk.uio.no; mprather@uci.edu; i.s.a.isaksen@geofysikk.uio.no; akimoto@jamstec.go.jp; e.v.browell@larc.nasa.gov; soltmans@cmdl.noaa.gov RI Wild, Oliver/A-4909-2009 OI Wild, Oliver/0000-0002-6227-7035 NR 32 TC 58 Z9 58 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 11 PY 2003 VL 108 IS D21 AR 8826 DI 10.1029/2002JD003283 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 744VC UT WOS:000186652700008 ER PT J AU Herkenhoff, KE Squyres, SW Bell, JF Maki, JN Arneson, HM Bertelsen, P Brown, DI Collins, SA Dingizian, A Elliott, ST Goetz, W Hagerott, EC Hayes, AG Johnson, MJ Kirk, RL McLennan, S Morris, RV Scherr, LM Schwochert, MA Shiraishi, LR Smith, GH Soderblom, LA Sohl-Dickstein, JN Wadsworth, MV AF Herkenhoff, KE Squyres, SW Bell, JF Maki, JN Arneson, HM Bertelsen, P Brown, DI Collins, SA Dingizian, A Elliott, ST Goetz, W Hagerott, EC Hayes, AG Johnson, MJ Kirk, RL McLennan, S Morris, RV Scherr, LM Schwochert, MA Shiraishi, LR Smith, GH Soderblom, LA Sohl-Dickstein, JN Wadsworth, MV TI Athena Microscopic Imager investigation SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars Exploration Rover; Microscopic Imager; Athena; NASA; camera ID PATHFINDER LANDING SITE; MARS PATHFINDER; SURFACE; CAMERA; INFORMATION; THRESHOLD; QUALITY; DESIGN; DUNES; ROVER AB [1] The Athena science payload on the Mars Exploration Rovers ( MER) includes the Microscopic Imager ( MI). The MI is a fixed- focus camera mounted on the end of an extendable instrument arm, the Instrument Deployment Device ( IDD). The MI was designed to acquire images at a spatial resolution of 30 microns/ pixel over a broad spectral range ( 400 - 700 nm). The MI uses the same electronics design as the other MER cameras but has optics that yield a field of view of 31 x 31 mm across a 1024 x 1024 pixel CCD image. The MI acquires images using only solar or skylight illumination of the target surface. A contact sensor is used to place the MI slightly closer to the target surface than its best focus distance ( about 66 mm), allowing concave surfaces to be imaged in good focus. Coarse focusing ( similar to 2 mm precision) is achieved by moving the IDD away from a rock target after the contact sensor has been activated. The MI optics are protected from the Martian environment by a retractable dust cover. The dust cover includes a Kapton window that is tinted orange to restrict the spectral bandpass to 500 - 700 nm, allowing color information to be obtained by taking images with the dust cover open and closed. MI data will be used to place other MER instrument data in context and to aid in petrologic and geologic interpretations of rocks and soils on Mars. C1 US Geol Survey, Astrogeol Team, Flagstaff, AZ 86001 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Copenhagen, Niels Bohr Inst Astron Phys & Geophys, DK-2100 Copenhagen, Denmark. SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. GHS Opt, Pasadena, CA 91101 USA. RP US Geol Survey, Astrogeol Team, 2255 N Gemini Dr, Flagstaff, AZ 86001 USA. EM kherkenhoff@usgs.gov RI Hayes, Alexander/P-2024-2014 OI Hayes, Alexander/0000-0001-6397-2630 NR 39 TC 81 Z9 81 U1 1 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD NOV 11 PY 2003 VL 108 IS E12 AR 8065 DI 10.1029/2003JE002076 PG 23 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 744XD UT WOS:000186657400001 ER PT J AU Rieder, R Gellert, R Bruckner, J Klingelhofer, G Dreibus, G Yen, A Squyres, SW AF Rieder, R Gellert, R Bruckner, J Klingelhofer, G Dreibus, G Yen, A Squyres, SW TI The new Athena alpha particle X-ray spectrometer for the Mars Exploration Rovers SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; surface composition; in situ measurements; alpha particle X-ray spectrometer; Mars Exploration Rovers ID CHEMICAL-COMPOSITION; MARTIAN SOIL; ROCKS AB [1] The new alpha particle X- ray spectrometer ( APXS) is part of the Athena payload of the two Mars Exploration Rovers ( MER). The APXS sensor head is attached to the turret of the instrument deployment device ( IDD) of the rover. The APXS is a very light- weight instrument for determining the major and minor elemental composition of Martian soils, rocks, and other geological materials at the MER landing sites. The sensor head has simply to be docked by the IDD on the surface of the selected sample. X- ray radiation, excited by alpha particles and X rays of the radioactive sources, is recorded by a high- resolution X- ray detector. The X- ray spectra show elements starting from sodium up to yttrium, depending on their concentrations. The backscattered alpha spectra, measured by a ring of detectors, provide additional data on carbon and oxygen. By means of a proper calibration, the elemental concentrations are derived. Together with data from the two other Athena instruments mounted on the IDD, the samples under investigation can be fully characterized. Key APXS objectives are the determination of the chemistry of crustal rocks and soils and the examination of water- related deposits, sediments, or evaporates. Using the rock abrasion tool attached to the IDD, issues of weathering can be addressed by measuring natural and abraded surfaces of rocks. C1 Max Planck Inst Chem, D-55020 Mainz, Germany. Johannes Gutenberg Univ Mainz, Inst Anorgan Chem & Analyt Chem, D-55099 Mainz, Germany. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Rieder, R (reprint author), Max Planck Inst Chem, Postfach 3060, D-55020 Mainz, Germany. EM rieder@mpch-mainz.mpg.de; gellert@mpch-mainz.mpg.de; brueckner@mpch-mainz.mpg.de; klingel@mail.uni-mainz.de; dreibus@mpch-mainz.mpg.de; albert.yen@jpl.nasa.gov; squyres@astrosun.tn.cornell.edu NR 15 TC 123 Z9 123 U1 2 U2 19 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 NOV 11 PY 2003 VL 108 IS E12 AR 8066 DI 10.1029/2003JE002150 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 744XD UT WOS:000186657400002 ER PT J AU Tratt, DM Hecht, MH Catling, DC Samulon, EC Smith, PH AF Tratt, DM Hecht, MH Catling, DC Samulon, EC Smith, PH TI In situ measurement of dust devil dynamics: Toward a strategy for Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE dust devils; vortex structure; vortex dynamics; Rankine vortex model; in situ measurements ID DOPPLER RADAR; VORTICES AB [1] An intensive 3-day dust devil investigation was conducted near Eloy, Arizona, during June of 2001. The goal was to evaluate strategies for observing dust devils on Mars by studying the physics of terrestrial dust devils. As part of this campaign, an instrumented vehicle outfitted with wind, temperature, and pressure sensors was used to intercept and penetrate numerous dust devils. Defined analysis of meteorological fields was only possible with knowledge of the whole body motion of a dust devil. One such data set analyzed revealed a dust devil structure characterized by a tangential wind proportional to radius, r, inside the warm, low-pressure core of a dust devil, and proportional to r(-1/2) outside the core. We discuss the implications for optimum measurement strategies. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. RP Tratt, DM (reprint author), NASA, Goddard Space Flight Ctr, Earth Sci Technol Off, Code 407, Greenbelt, MD 20771 USA. RI Tratt, David/A-7884-2009 OI Tratt, David/0000-0002-3942-6848 NR 19 TC 28 Z9 28 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD NOV 11 PY 2003 VL 108 IS E11 AR 5116 DI 10.1029/2003JE002161 PG 7 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 744WR UT WOS:000186656300001 ER PT J AU Black, JK Deines-Jones, P Ready, SE Street, RA AF Black, JK Deines-Jones, P Ready, SE Street, RA TI X-ray polarimetry with an active-matrix pixel proportional counter SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article DE X-ray polarimetry; particle tracking; proportional counter; GEM; pixel readout ID MICRO-WELL DETECTORS; PATTERN GAS DETECTOR AB We report the first results from an X-ray polarimeter with a micropattern gas proportional counter using an amorphous silicon active matrix readout. With 100% polarized X-rays at 4.5 keV, we obtain a modulation factor of 0.33+/-0.03, confirming previous reports of the high polarization sensitivity of a finely segmented pixel proportional counter. The detector described here has a geometry suitable for the focal plane of an astronomical X-ray telescope. Amorphous silicon readout technology will enable additional extensions and improvements. (C) 2003 Elsevier B.V. All rights reserved. C1 NASA, Goddard Space Flight Ctr, Forbin Sci, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Greenbelt, MD 20771 USA. Palo Alto Res Ctr, Palo Alto, CA 94304 USA. RP Black, JK (reprint author), NASA, Goddard Space Flight Ctr, Forbin Sci, Code 662, Greenbelt, MD 20771 USA. NR 14 TC 25 Z9 26 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD NOV 11 PY 2003 VL 513 IS 3 BP 639 EP 643 DI 10.1016/j.nima.2003.07.015 PG 5 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 742ED UT WOS:000186502800021 ER PT J AU Cassell, AM Ng, HT Delzeit, L Ye, Q Li, J Han, J Meyyappan, M AF Cassell, AM Ng, HT Delzeit, L Ye, Q Li, J Han, J Meyyappan, M TI High throughput methodology for carbon nanomaterials discovery and optimization SO APPLIED CATALYSIS A-GENERAL LA English DT Article DE carbon nanotubes; heterogeneous catalysis; CVD; combinatorial materials; microarrays ID MULTILAYERED METAL-CATALYSTS; CHEMICAL-VAPOR-DEPOSITION; RAMAN-SCATTERING; NANOTUBES; COMBINATORIAL; GROWTH; ARRAYS; DIAMETER AB The application of high throughput methodology in the discovery of catalyst formulations and novel nanomaterials is expected to impact a wide range of applications. Carbon nanomaterials such as nanotubes, nanofibers, and diamond-like carbon are promising candidate materials for use in a wide variety of electrical, optical and mechanical applications. Therefore, the application of combinatorial methodologies to the discovery and optimization of carbon nanomaterials and catalyst formulations to produce them will accelerate the advancement of nanoscale science and technology. Here, we present an overview of the various combinatorial methodologies employed in the search for carbon nanotubes and related structures. It is hoped that continued innovations in high throughput methodology, especially for nanomaterials development, would be adapted to the many challenges facing nanotechnology. (C) 2003 Elsevier Science B.V. All rights reserved. C1 NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. ELORET Corp, Sunnyvale, CA 94087 USA. RP Cassell, AM (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, MS 229-1, Moffett Field, CA 94035 USA. EM acassell@mail.arc.nasa.gov RI Li, Jun/H-7771-2013 OI Li, Jun/0000-0002-3689-8946 NR 28 TC 9 Z9 9 U1 1 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0926-860X J9 APPL CATAL A-GEN JI Appl. Catal. A-Gen. PD NOV 10 PY 2003 VL 254 IS 1 BP 85 EP 96 DI 10.1016/S0926-860X(03)00279-5 PG 12 WC Chemistry, Physical; Environmental Sciences SC Chemistry; Environmental Sciences & Ecology GA 746KM UT WOS:000186745600010 ER PT J AU Larrabee, DC Khodaparast, GA Kono, J Ueda, K Nakajima, Y Nakai, M Sasa, S Inoue, M Kolokolov, KI Li, J Ning, CZ AF Larrabee, DC Khodaparast, GA Kono, J Ueda, K Nakajima, Y Nakai, M Sasa, S Inoue, M Kolokolov, KI Li, J Ning, CZ TI Temperature dependence of intersubband transitions in InAs/AlSb quantum wells SO APPLIED PHYSICS LETTERS LA English DT Article ID MU-M; CASCADE LASERS; ABSORPTION; LAYER; SUPERLATTICES; GAAS; INAS AB We have carried out a systematic temperature-dependent study of intersubband absorption in InAs/AlSb quantum wells from 5 to 10 nm well width. The resonance energy redshifts with increasing temperature from 10 to 300 K, and the amount of redshift increases with decreasing well width. We have modeled the transitions using eight-band k.p theory combined with semiconductor Bloch equations, including the main many-body effects. Temperature is incorporated via band filling and nonparabolicity, and good agreement with experiment is achieved for the temperature dependence of the resonance. (C) 2003 American Institute of Physics. C1 Rice Univ, Rice Quantum Inst, Dept Elect & Comp Engn, Houston, TX 77005 USA. Rice Univ, Ctr Nanoscale Sci & Technol, Houston, TX 77005 USA. Osaka Inst Technol, New Mat Res Ctr, Osaka 5358585, Japan. NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Kono, J (reprint author), Rice Univ, Rice Quantum Inst, Dept Elect & Comp Engn, Houston, TX 77005 USA. RI Ning, C. Z./D-4699-2009 OI Ning, C. Z./0000-0003-4583-8889 NR 23 TC 26 Z9 26 U1 1 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 0003-6951 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD NOV 10 PY 2003 VL 83 IS 19 BP 3936 EP 3938 DI 10.1063/1.1626264 PG 3 WC Physics, Applied SC Physics GA 739RP UT WOS:000186360500028 ER PT J AU Brandon, EJ West, W Wesseling, E AF Brandon, EJ West, W Wesseling, E TI Carbon-based printed contacts for organic thin-film transistors SO APPLIED PHYSICS LETTERS LA English DT Article ID FIELD-EFFECT TRANSISTORS; RESISTANCE; CIRCUITS AB Organic thin-film transistors (OTFTs) employing a flexible, conductive carbon particle-polymer composite material for the drain-source ohmic contacts are reported herein. The contacts can be deposited using standard stencil printing techniques and are processed at low temperature, thereby facilitating their integration with heat sensitive substrates. The carbon contacts were stencil printed on a silicon dioxide gate dielectric layer, and the poly(3-hexylthiophene) semiconductor was deposited via solution casting from toluene. The OTFTs exhibited field-effect behavior over a range of drain-source and gate voltages, similar to devices employing deposited gold contacts. (C) 2003 American Institute of Physics. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Brandon, EJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 13 TC 13 Z9 13 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD NOV 10 PY 2003 VL 83 IS 19 BP 3945 EP 3947 DI 10.1063/1.1625794 PG 3 WC Physics, Applied SC Physics GA 739RP UT WOS:000186360500031 ER PT J AU Hjorth, J Moller, P Gorosabel, J Fynbo, JPU Toft, S Jaunsen, AO Kaas, AA Pursimo, T Torii, K Kato, T Yamaoka, H Yoshida, A Thomsen, B Andersen, MI Burud, I Ceron, JMC Castro-Tirado, AJ Fruchter, AS Kaper, L Kouveliotou, C Masetti, N Palazzi, E Pedersen, H Pian, E Rhoads, J Rol, E Tanvir, NR Vreeswijk, PM Wijers, RAMJ van den Heuvel, EPJ AF Hjorth, J Moller, P Gorosabel, J Fynbo, JPU Toft, S Jaunsen, AO Kaas, AA Pursimo, T Torii, K Kato, T Yamaoka, H Yoshida, A Thomsen, B Andersen, MI Burud, I Ceron, JMC Castro-Tirado, AJ Fruchter, AS Kaper, L Kouveliotou, C Masetti, N Palazzi, E Pedersen, H Pian, E Rhoads, J Rol, E Tanvir, NR Vreeswijk, PM Wijers, RAMJ van den Heuvel, EPJ TI Very high column density and small reddening toward GRB 020124 at z=3.20 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; dust, extinction; galaxies : abundances; galaxies : ISM; gamma rays : bursts ID GAMMA-RAY BURSTS; LY-ALPHA GALAXIES; TIME-DEPENDENT PHOTOIONIZATION; INFRARED EXTINCTION LAW; HUBBLE-SPACE-TELESCOPE; HIGH-REDSHIFT GALAXIES; LYMAN-BREAK GALAXIES; OPTICAL AFTERGLOW; HOST GALAXY; MAGELLANIC CLOUD AB We present optical and near-infrared observations of the dim afterglow of GRB 020124, obtained between 2 and 68 hr after the gamma-ray burst. The burst occurred in a very faint (Rgreater than or similar to29.5) damped Lyalpha absorber (DLA) at a redshift of z=3.198+/-0.004. The derived column density of neutral hydrogen is log(N-Hi)=21.7+/-0.2, and the rest-frame reddening is constrained to be E(B-V)<0.065, i.e., A(V)<0.20 for standard extinction laws with R-V&AP;3. The resulting dust-to-gas ratio is less than 11% of that found in the Milky Way but consistent with the SMC and high-redshift QSO DLAs, indicating a low metallicity and/or a low dust-to-metal ratio in the burst environment. A gray extinction law (large R-V), produced through preferential destruction of small dust grains by the gamma-ray burst, could increase the derived A(V) and dust-to-gas ratio. The dimness of the afterglow is, however, fully accounted for by the high redshift: if GRB 020124 had been at z=1, it would have been approximately 1.8 mag brighter-in the range of typical bright afterglows. C1 Univ Copenhagen, Astron Observ, DK-2100 Copenhagen O, Denmark. European So Observ, D-85748 Garching, Germany. Danish Space Res Inst, DK-2100 Copenhagen O, Denmark. CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. European So Observ, Santiago 19, Chile. Nord Opt Telescope, E-38700 Santa Cruz De La Palma, Canary Islands, Spain. RIKEN, Cosm Radiat Lab, Wako, Saitama 3510198, Japan. Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. Kyushu Univ, Fac Sci, Dept Phys, Chuo Ku, Fukuoka 8108560, Japan. Aoyama Gakuin Univ, Dept Phys, Tokyo 1578572, Japan. Astrophys Inst Potsdam, D-14482 Potsdam, Germany. Real Inst, Cadiz 11110, Spain. Observ Armada, Secc Astron, Cadiz 11110, Spain. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. NASA, Univ Res Assoc, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. CNR, IASF, Sez Bologna, I-40129 Bologna, Italy. Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. Univ Hertfordshire, Dept Phys Sci, Hatfield AL10 9AB, Herts, England. RP Hjorth, J (reprint author), Univ Copenhagen, Astron Observ, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark. EM jens@astro.ku.dk RI Hjorth, Jens/M-5787-2014; Palazzi, Eliana/N-4746-2015; OI Hjorth, Jens/0000-0002-4571-2306; Palazzi, Eliana/0000-0002-8691-7666; Castro-Tirado, A. J./0000-0003-2999-3563; Masetti, Nicola/0000-0001-9487-7740; Pian, Elena/0000-0001-8646-4858 NR 48 TC 92 Z9 92 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 NOV 10 PY 2003 VL 597 IS 2 BP 699 EP 705 DI 10.1086/378493 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 740ZG UT WOS:000186432700006 ER PT J AU Schmitt, HR Donley, JL Antonucci, RRJ Hutchings, JB Kinney, AL Pringle, JE AF Schmitt, HR Donley, JL Antonucci, RRJ Hutchings, JB Kinney, AL Pringle, JE TI A Hubble Space Telescope survey of extended [O III] lambda 5007 angstrom emission in a far-infrared-selected sample of Seyfert galaxies: Results SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : nuclei; galaxies : Seyfert; galaxies : structure; surveys ID NARROW-LINE REGION; ACTIVE GALACTIC NUCLEI; ANISOTROPIC IONIZING-RADIATION; POINT-SOURCE CATALOG; WARM IRAS SOURCES; UNIFIED SCHEMES; STELLAR POPULATIONS; SPECTRAL SIGNATURES; VLA OBSERVATIONS; RADIO STRUCTURES AB We present the results of a Hubble Space Telescope (HST) survey of extended [O III] emission in a sample of 60 nearby Seyfert galaxies (22 Seyfert 1's and 38 Seyfert 2's), selected by mostly isotropic properties. The comparison between the semimajor axis size of their [O III] emitting regions (R-maj) shows that Seyfert 1's and Seyfert 2's have similar distributions, which seems to contradict unified model predictions. We discuss possible ways to explain this result, which could be due to either observational limitations or the models used for the comparison with our data. We show that Seyfert 1 narrow-line regions (NLRs) are more circular and concentrated than Seyfert 2's, which can be attributed to foreshortening in the former. We find a good correlation between the NLR size and luminosity, following the relation R-maj proportional to L([O III])(0.33+/-0.04), which is flatter than a previous one found for QSOs and Seyfert 2's. We discuss possible reasons for the different results, and their implications to photoionization models. We confirm previous results that show that the [O III] and radio emission are well aligned and also find no correlation between the orientation of the extended [O III] emission and the host galaxy major axis. This agrees with results showing that the torus axis and radio jet are not aligned with the host galaxy rotation axis, indicating that the orientation of the gas in the torus, and not the spin of the black hole, determines the orientation of the accretion disk, and consequently, the orientation of the radio jet. C1 Natl Radio Astron Observ, Charlottesville, VA 22903 USA. Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. Natl Res Council Canada, Herzberg Inst Astrophys, Dominion Astrophys Observ, Victoria, BC V9E 2E7, Canada. NASA Headquarters, Washington, DC 20546 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Schmitt, HR (reprint author), Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. NR 84 TC 93 Z9 93 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 NOV 10 PY 2003 VL 597 IS 2 BP 768 EP 779 DI 10.1086/381224 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 740ZG UT WOS:000186432700011 ER PT J AU Ebisawa, K Zycki, P Kubota, A Mizuno, T Watarai, K AF Ebisawa, K Zycki, P Kubota, A Mizuno, T Watarai, K TI Accretion disk spectra of ultraluminous X-ray sources in nearby spiral galaxies and Galactic superluminal jet sources SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; X-rays : galaxies ID MICROQUASAR GRO J1655-40; SUPERMASSIVE BLACK-HOLES; ASCA OBSERVATION; OBSERVATIONAL APPEARANCE; LMC X-1; MASS; MODEL; IC-342; NUCLEI; BINARIES AB Ultraluminous compact X-ray sources (ULXs) in nearby spiral galaxies and Galactic superluminal jet sources share the common spectral characteristic that they have unusually high disk temperatures that cannot be explained in the framework of the standard optically thick accretion disk in the Schwarzschild metric. On the other hand, the standard accretion disk around the Kerr black hole might explain the observed high disk temperature, since the inner radius of the Kerr disk becomes smaller and the disk temperature can consequently be higher. However, we point out that the observable Kerr disk spectra become significantly harder than Schwarzschild disk spectra only when the disk is highly inclined. This is because the emission from the innermost part of the accretion disk is Doppler boosted for an edge-on Kerr disk while hardly seen for a face-on disk. The Galactic superluminal jet sources are known to be highly inclined systems; thus, their energy spectra may be explained with the standard Kerr disk with known black hole masses. For ULXs, on the other hand, the standard Kerr disk model seems implausible, since it is highly unlikely that their accretion disks are preferentially inclined, and if the edge-on Kerr disk model is applied, the black hole mass becomes unreasonably large (greater than or similar to300 M-circle dot). Instead, the slim-disk (advection-dominated optically thick disk) model is likely to explain the observed super-Eddington luminosities, hard energy spectra, and spectral variations of ULXs. We suggest that ULXs are accreting black holes with a few tens of solar masses, which is not unexpected from the standard stellar evolution scenario, and that their X-ray emission is from the slim disk shining at super-Eddington luminosities. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. Inst Space & Astronaut Sci, Kanagawa 2298510, Japan. Stanford Linear Accelerator Ctr, Menlo Pk, CA 94025 USA. Kyoto Univ, Yukawa Inst Theoret Phys, Sakyo Ku, Kyoto 6068502, Japan. RP Ebisawa, K (reprint author), Univ Space Res Assoc, Columbia, MD USA. NR 69 TC 69 Z9 69 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 NOV 10 PY 2003 VL 597 IS 2 BP 780 EP 797 DI 10.1086/378586 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 740ZG UT WOS:000186432700012 ER PT J AU Konopelko, A Mastichiadis, A Kirk, J de Jager, OC Stecker, FW AF Konopelko, A Mastichiadis, A Kirk, J de Jager, OC Stecker, FW TI Modeling the TeV gamma-ray spectra of two low-Redshift active Galactic nuclei: Markarian 501 and Markarian 421 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects : individual (Markarian 421, Markarian 501); galaxies : active; gamma rays : observations ID AIR CERENKOV TELESCOPES; HIGH-ENERGY PHOTONS; BL-LAC OBJECTS; X-RAY; MULTIWAVELENGTH OBSERVATIONS; GALAXY MARKARIAN-421; HEGRA SYSTEM; BLAZAR; ABSORPTION; EVOLUTION AB We discuss the results of modeling the TeV gamma-ray spectra of two active galactic nuclei, Mrk 501 and Mrk 421, that have almost the same redshifts: z=0.031 and 0.034, respectively. The effect of intergalactic gamma-ray absorption is treated as an uncertainty in the measurement of the intrinsic spectrum. Although the objects differ, we obtain satisfactory fits for both of them in a synchrotron self-Compton scenario. Compared to previous models, our fits are characterized by higher values of the Doppler factor (deltagreater than or equal to50) and an electron injection spectrum extending to higher energies (gamma(max)greater than or equal to1.5x10(5)). In the case of Mrk 421, the observed difference in spectral slope in X-rays and TeV gamma-rays between the high and low states can be explained as a variation of a single parameter-the maximum energy gamma(max)mc(2) at which electrons are injected. C1 Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. Univ Athens, Dept Phys, GR-15783 Zografos, Greece. Potchefstroom Univ Christian Higher Educ, Unit Space Phys, ZA-2520 Potchefstroom, South Africa. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Konopelko, A (reprint author), Max Planck Inst Kernphys, Postfach 10 39 80, D-69029 Heidelberg, Germany. RI Stecker, Floyd/D-3169-2012; Kirk, John/A-8901-2013 OI Kirk, John/0000-0002-9859-0496 NR 79 TC 99 Z9 99 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2003 VL 597 IS 2 BP 851 EP 859 DI 10.1086/374593 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 740ZG UT WOS:000186432700017 ER PT J AU Feng, YX Tennant, AF Zhang, SN AF Feng, YX Tennant, AF Zhang, SN TI Probing the inflow/outflow and accretion disk of Cygnus X-1 in the high state with the Chandra high energy transmission grating SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries : general; black hole physics; stars : individual (Cygnus X-1); X-rays : binaries ID X-RAY BINARIES; BLACK-HOLE; HDE 226868; TRANSITIONS; LINE; SPECTRUM; WINDS; ASCA; DIPS AB Cygnus X-1 was observed in the high state at the conjunction orbital phase (0) with the Chandra High Energy Transmission Grating (HETG). Strong and asymmetric absorption lines of highly ionized species were detected, such as Fe XXV, Fe XXIV, Fe XXIII, Si XIV, S XVI, Ne X, etc. In the high state the pro. le of the absorption lines is composed of an extended red wing and a less extended blue wing. The red wings of higher ionized species are more extended than those of lower ionized species. The detection of these lines provides a way to probe the properties of the flow around the companion and the black hole in Cyg X-1 during the high state. A broad emission feature around 6.5 keV was significantly detected from the spectra of both the Chandra/HETG and the RXTE/Proportional Counter Array. This feature appears to be symmetric and can be fitted with a Gaussian function rather than the Laor disk line model of the fluorescent Fe Kalpha line from an accretion disk. The implications of these results on the structure of the accretion flow of Cyg X-1 in the high state are discussed. C1 Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. NASA, Natl Space Sci & Technol Ctr, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Zhang, SN (reprint author), Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. NR 35 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 NOV 10 PY 2003 VL 597 IS 2 BP 1017 EP 1022 DI 10.1086/378495 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 740ZG UT WOS:000186432700032 ER PT J AU Still, M Hussain, G AF Still, M Hussain, G TI Coronal element abundances of the post-common-envelope binary V471 Tauri with ASCA SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; stars : individual (V471 Tauri); stars : magnetic fields; white dwarfs; X-rays : binaries ID V471 TAURI; X-RAY; ECLIPSING BINARY; WHITE-DWARF; ENERGETIC PARTICLES; CLOSE BINARIES; RADIO-EMISSION; HYADES CLUSTER; STARS; MASS AB We report on ASCA observations of the coronally active companion star in the post-common-envelope binary V471 Tau. Evolutionary calculations indicate that there should be no peculiar abundances on the companion star resulting from the common-envelope epoch. Indeed, we find no evidence for peculiar abundances, although uncertainties are high. We find that a single-temperature plasma model does not fit the data. Two-temperature models with decoupled elemental abundances suggest that Fe is underabundant compared to the Hyades photospheric mean. In the absence of a measurement of photospheric Ne abundance in the cluster, we find that Ne is overabundant compared to the solar photospheric value. This is indicative of the inverse first ionization potential effect. Differences between coronal and photospheric abundances are believed to result from the fractionation of ionized and neutral material in the upper atmosphere of the star. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Still, M (reprint author), Univ Space Res Assoc, Columbia, MD USA. NR 49 TC 7 Z9 8 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2003 VL 597 IS 2 BP 1059 EP 1064 DI 10.1086/378507 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 740ZG UT WOS:000186432700036 ER PT J AU Lawrence, JK Cadavid, AC Miccolis, D Berger, TE Ruzmaikin, A AF Lawrence, JK Cadavid, AC Miccolis, D Berger, TE Ruzmaikin, A TI Influence of photospheric magnetic fields and dynamics on chromospheric K-line emission SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : chromosphere; Sun : magnetic fields ID BAND BRIGHT POINTS; CELL-NETWORK DISTINCTIONS; SOLAR ATMOSPHERE; MAGNETOATMOSPHERIC WAVES; OSCILLATIONS; INTERNETWORK; SUN; PROPAGATION; TURBULENCE; FLOWS AB We analyze a 9 hr sequence of simultaneous, high-resolution, high-cadence G-band and K-line solar filtergrams plus magnetograms of lower cadence and resolution. Images include both network and inter-network. The magnetic and filtergram intensities, their fluctuations, and relative phases change with progressive strengthening of local magnetic field. At increased flux levels, sudden photospheric downflows create long-lived magnetic elements. For weak magnetic fields the K-line and G-band intensities include an oscillatory component with period 4 minutes. For stronger fields, the K-line period shifts to 5 minutes, while the G-band fluctuations fade due to dissociation of their source, the CH radical. These K-line and G-band fluctuations, whose periods are longer than the acoustic cutoff, are coherent and in phase. They also are coherent with fluctuations of the magnetic field. Weak-field magnetic fluctuations lead the intensity fluctuations by a phase shift of 90degrees. Strong-field magnetic fluctuations trail the intensities by 100degrees. These are interpreted as standing waves in the photosphere and low chromosphere. Another class of G-band fluctuations, with periods shorter than the acoustic cutoff, is associated both with stronger magnetic fields and with enhanced K-line emission with fluctuations longer than the cutoff period. This suggests waves excited by rapid photospheric perturbations and propagating up along magnetic flux tubes. C1 Calif State Univ Northridge, Dept Phys & Astron, Northridge, CA 91330 USA. Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Calif State Univ Northridge, Dept Phys & Astron, Northridge, CA 91330 USA. NR 38 TC 5 Z9 5 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 NOV 10 PY 2003 VL 597 IS 2 BP 1178 EP 1189 DI 10.1086/378559 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 740ZG UT WOS:000186432700047 ER PT J AU Holmes, EK Dermott, SF Gustafson, BAS Grogan, K AF Holmes, EK Dermott, SF Gustafson, BAS Grogan, K TI Resonant structure in the Kuiper disk: An asymmetric plutino disk SO ASTROPHYSICAL JOURNAL LA English DT Article DE Kuiper Belt; solar system : general ID SOLAR-SYSTEM DUST; BACKGROUND EXPERIMENT SEARCH; NEAR-SHOEMAKER SPACECRAFT; BELT OBJECTS; INFRARED-EMISSION; ASTEROID FAMILIES; INTERSTELLAR DUST; PARTICLES; GRAINS; DYNAMICS AB In order to develop a dynamical model of the Kuiper disk, we run numerical integrations of particles originating from source bodies trapped in the 3:2 external mean motion resonance with Neptune to determine what percentage of particles remain in the resonance for a variety of particle and source body sizes. The dynamical evolution of the particles is followed from source to sink with Poynting-Robertson light drag, solar wind drag, radiation pressure, the Lorentz force, neutral interstellar gas drag, and the effects of planetary gravitational perturbations included. We find that the number of particles in the 3:2 resonance increases with decreasing beta (i.e., increasing particle size) for the cases in which the initial source bodies are small (less than or equal to10 km in diameter) and that the percentage of particles in resonance is not significantly changed by either the addition of the Lorentz force, as long as the potential of the particles is small (approximate to5 V), or the effect of neutral interstellar gas drag. The brightness of the entire Kuiper disk is calculated using a model composed of 500 mum diameter particles and fits well with upper limits to the Kuiper disk brightness and previous estimates. A disk with a size-frequency distribution weighted toward large particles, which are more likely to remain in resonance, may have a stronger, more easily identifiable resonant signature than a disk composed of small particles. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA. RP CALTECH, Jet Prop Lab, MS 169-506,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM elizabeth.holmes@jpl.nasa.gov; dermott@astro.ufl.edu; gustaf@astro.ufl.edu; keith.grogan@jpl.nasa.gov RI Gustafson, Bo/B-9526-2011 NR 72 TC 15 Z9 16 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 NOV 10 PY 2003 VL 597 IS 2 BP 1211 EP 1236 DI 10.1086/378509 PN 1 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 740ZG UT WOS:000186432700050 ER PT J AU Sekanina, Z AF Sekanina, Z TI Erosion model for the sungrazing comets observed with the solar and Heliospheric Observatory SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets : general; methods : data analysis ID HALLEY DUST PARTICLES; HALE-BOPP; SODIUM; FRAGMENTATION; SPECTROMETER; WAVELENGTH; NUCLEUS; GIOTTO; TAILS; RATES AB The objectives of this study are to model and interpret quantitatively the brightness variations of 27 Solar and Heliospheric Observatory (SOHO) sungrazers. The light curves, published by Uzzo et al. and by Biesecker et al., are shown to provide information on a proposed erosion process, which consists of continuous, progressive bulk fragmentation and sublimation of these minicomets on their approach to the Sun. The erosion rate and the time of peak signal are determined primarily by an effective latent energy of erosion (analogous to a sublimation heat), which is found to have a bimodal distribution with sharp peaks near 34,000-35,000 and 40,000-41,000 cal mol(-1) for the main components of the 27 objects. Their derived initial diameters are between 17 and 200 m. With the given range of erosion energies, a sungrazer that is to survive its return to the Sun needs to be more than 1-1.4 km in diameter, depending on its perihelion distance. The shape of the light curves at heliocentric distances smaller than 7 R-circle dot is interpreted to indicate the existence of fairly sizable, but unresolved, close companions, which appear to have split off from their parent bodies shortly before, if not during, observation. All subfragments that survived longer than the main components had erosion energies significantly higher than the average, between 45,000 and nearly 90,000 cal mol(-1). There is also evidence for subfragments with erosion energies lower than 34,000 cal mol(-1). Because the erosion process is believed to be dominated by continual fragmentation, the existence of such subfragments should not be surprising. The brightness of the SOHO sungrazers at peak signal is mass diagnostic, and their cumulative distribution varies inversely as the initial mass to a power of 0.56-0.68. Thus, much of the total mass is still locked in the most massive fragments, and the Kreutz system is apparently in an early phase of its evolution. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM zs@sek.jpl.nasa.gov NR 47 TC 26 Z9 26 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2003 VL 597 IS 2 BP 1237 EP 1265 DI 10.1086/378192 PN 1 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 740ZG UT WOS:000186432700051 ER PT J AU Choudhary, DP Moore, RL AF Choudhary, DP Moore, RL TI Filament eruption without coronal mass ejection SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID GEOMAGNETIC-ACTIVITY; SOLAR-ACTIVITY; ACTIVE-REGION; FLARES; EIT AB We report characteristics of quiescent filament eruptions that were not associated with coronal mass ejections (CMEs). We examined 12 quiescent filament eruptions, each of which was located far from disk center (greater than or equal to0.7 R-Sun) in diffuse remnant magnetic fields of decayed active regions, was well observed in full-disk movies in Ha and Fe XII, and had good coronagraph coverage. Of the 12 events, 9 were associated with CMEs and 3 were not. Even though the two kinds of eruption were indistinguishable in their magnetic setting and in the eruptive motion of the filament in the Ha movies, each of the CME-producing eruptions produced a two-ribbon flare in Ha and a coronal arcade and/or two-ribbon flare in Fe XII, and each of the non-CME-producing eruptions did not. From this result, and the appearance of the eruptive motion in the Fe XII movies, we conclude that the non-CME-associated filament eruptions are confined eruptions like the confined filament eruptions in active regions. C1 NASA, George C Marshall Space Flight Ctr, Space Sci Dept SD50, Huntsville, AL 35812 USA. RP NASA, George C Marshall Space Flight Ctr, Space Sci Dept SD50, Huntsville, AL 35812 USA. EM debi.choudhary@msfc.nasa.gov NR 25 TC 8 Z9 8 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 NOV 8 PY 2003 VL 30 IS 21 AR 2107 DI 10.1029/2003GL018332 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 742FW UT WOS:000186507600004 ER PT J AU Bian, HS Zender, CS AF Bian, HS Zender, CS TI Mineral dust and global tropospheric chemistry: Relative roles of photolysis and heterogeneous uptake SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE tropospheric chemistry; mineral dust; photolysis impact; heterogeneous reaction ID MARINE BOUNDARY-LAYER; REMOTE-SENSING OBSERVATIONS; CHEMICAL-TRANSPORT MODEL; IN-SITU; ULTRAVIOLET-RADIATION; AEROSOL DISTRIBUTIONS; ATMOSPHERIC CHEMISTRY; ACCURATE SIMULATION; OPTICAL-PROPERTIES; SULFUR CYCLE AB We investigate the influence of mineral dust on tropospheric chemistry in the present climate at the global scale. The analysis examines the effects of dust on photolysis and heterogeneous uptake, operating independently and together. In numerical experiments the size-resolved, time-varying mineral dust distribution predicted by the global Dust Entrainment and Deposition (DEAD) model perturbs the gas phase species in a global chemical transport model (University of California at Irvine (UCI) CTM). We find that the photolysis perturbation dominates limited regions in the low to middle troposphere, while heterogeneous uptake dominates the rest of atmosphere. Coupling of the photochemical and heterogeneous effects of dust is weak in the global mean but moderate in dusty regions, where coupling is sometimes responsible for more than 20% of local O-3 changes. Ozone and odd-nitrogen concentrations are perturbed in opposite directions by photolysis and heterogeneous chemistry, resulting in a weak net change. However, both processes decrease the concentrations of OH and HO2. The global mean change due to dust is -0.7% for tropospheric O-3, -11.1% for OH, -5.2% for HO2, and -3.5% for HNO3. Large seasonal signals are present near dust source regions. Over the North African region and tropical Atlantic Ocean downwind, OH decreases by -66.8%, six times more than the global mean reduction. Interestingly, net photolysis-induced annual mean O-3 changes are greater in the Southern Hemisphere than in the Northern Hemisphere, where significantly more dust and O-3 precursors reside. In polar regions, O-3 change is dominated by transported O-3 and is not sensitive to local dust concentration. O-3 change due to photolysis depends not only on dust vertical structure but also on the availability of O-3 precursors. O-3 change due to heterogeneous reactions on dust is sensitive to dust vertical structure, mainly through the influence of temperature on uptake rates. C1 Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. RP Univ Maryland Baltimore Cty, NASA, Goddard Space Flight Ctr, Goddard Earth Sci & Technol Ctr, Mail Code 916, Greenbelt, MD 20771 USA. EM bian@rondo.gsfc.nasa.gov; zender@uci.edu RI Zender, Charles/D-4485-2012 OI Zender, Charles/0000-0003-0129-8024 NR 74 TC 83 Z9 85 U1 2 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 NOV 8 PY 2003 VL 108 IS D21 AR 4672 DI 10.1029/2002JD003143 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 742GG UT WOS:000186508600002 ER PT J AU Martin, TZ Bridges, NT Murphy, JR AF Martin, TZ Bridges, NT Murphy, JR TI Near-surface temperatures at proposed Mars Exploration Rover landing sites SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; atmosphere; temperature; MER; surface; model ID THERMAL EMISSION SPECTROMETER; GENERAL-CIRCULATION; MARTIAN ATMOSPHERE; SIMULATIONS; MODEL AB [1] Minimum nighttime temperatures at the Mars Exploration Rover ( MER) landing sites may limit power available for science activities and thus mission lifetime. Here, 1 m air temperatures at the end of the nominal 90 sol primary mission are derived for the four primary and three previously considered MER landing sites based on Mars Global Surveyor Thermal Emission Spectrometer thermal inertia and albedo, estimated opacity, and predictions of air temperatures from a one-dimensional atmospheric model. Taking these results and mapping them onto the probability density distribution of the landing ellipses shows that of the air temperatures of the primary sites, Sinus Meridiani ("Hematite'') is the coldest, with an 8% chance of encountering minimum nighttime temperatures below the 176 K value considered a practical limit for operations. Elysium and Gusev are at 7% and 3%, respectively, whereas Isidis has no computed temperatures below 191 K. For the Hematite site, preliminary observations and interpretations are also made using high-resolution Odyssey Thermal Imaging System predawn images. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. RP Martin, TZ (reprint author), CALTECH, Jet Prop Lab, MS 169-237,4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Bridges, Nathan/D-6341-2016 NR 9 TC 8 Z9 8 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD NOV 8 PY 2003 VL 108 IS E12 AR 8089 DI 10.1029/2003JE002063 PG 7 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 742HC UT WOS:000186510500001 ER PT J AU Kruger, H Geissler, P Horanyi, M Graps, AL Kempf, S Srama, R Moragas-Klostermeyer, G Moissl, R Johnson, TV Grun, E AF Kruger, H Geissler, P Horanyi, M Graps, AL Kempf, S Srama, R Moragas-Klostermeyer, G Moissl, R Johnson, TV Grun, E TI Jovian dust streams: A monitor of Io's volcanic plume activity SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID JUPITERS MAGNETOSPHERE; GALILEO; DETECTOR; GRAINS AB Streams of high speed dust particles originate from Jupiter's moon Io. After release from Io, the particles collect electric charges in the Io plasma torus, gain energy from the co-rotating electric field of Jupiter's magnetosphere, and leave the Jovian system into interplanetary space with escape speeds over 200 km s(-1). The Galileo spacecraft has continuously monitored the dust streams during 34 revolutions about Jupiter between 1996 and 2002. The observed dust fluxes exhibit large orbit-to-orbit variability due to systematic and stochastic changes. After removal of the systematic variations, the total dust emission rate of Io has been calculated. It varies between 10(-3) and 10 kg s(-1), and is typically in the range of 0.1 to 1 kg s(-1). We compare the dust emission rate with other markers of volcanic activity on Io like large-area surface changes caused by volcanic deposits and sightings of volcanic plumes. C1 Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. US Geol Survey, Flagstaff, AZ 86001 USA. Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. Univ Colorado, Dept Phys, Boulder, CO 80309 USA. INAF, IFSI, I-00133 Rome, Italy. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. RP Kruger, H (reprint author), Max Planck Inst Kernphys, Postfach 103980, D-69029 Heidelberg, Germany. NR 26 TC 24 Z9 24 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 NOV 7 PY 2003 VL 30 IS 21 AR 2101 DI 10.1029/2003GL017827 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 742FV UT WOS:000186507400003 ER PT J AU Mlynczak, M Martin-Torres, FJ Russell, J Beaumont, K Jacobson, S Kozyra, J Lopez-Puertas, M Funke, B Mertens, C Gordley, L Picard, R Winick, J Wintersteiner, P Paxton, L AF Mlynczak, M Martin-Torres, FJ Russell, J Beaumont, K Jacobson, S Kozyra, J Lopez-Puertas, M Funke, B Mertens, C Gordley, L Picard, R Winick, J Wintersteiner, P Paxton, L TI The natural thermostat of nitric oxide emission at 5.3 mu m in the thermosphere observed during the solar storms of April 2002 SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID TERRESTRIAL THERMOSPHERE; MESOSPHERE; ENERGETICS AB The Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) experiment on the Thermosphere-Ionosphere Mesosphere Energetics and Dynamics (TIMED) satellite observed the infrared radiative response of the thermosphere to the solar storm events of April 2002. Large radiance enhancements were observed at 5.3 mum, which are due to emission from the vibration-rotation bands of nitric oxide (NO). The emission by NO is indicative of the conversion of solar energy to infrared radiation within the atmosphere and represents a "natural thermostat" by which heat and energy are efficiently lost from the thermosphere to space and to the lower atmosphere. We describe the SABER observations at 5.3 mum and their interpretation in terms of energy loss. The infrared enhancements remain only for a few days, indicating that such perturbations to the thermospheric state, while dramatic, are short-lived. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. Analyt Serv & Mat Inc, Hampton, VA 23666 USA. Hampton Univ, Hampton, VA 23668 USA. G&A Tech Software, Newport News, VA USA. Univ Michigan, Ann Arbor, MI 48109 USA. Inst Astrofis Andalucia, E-18080 Granada, Spain. USAF, Res Lab, Hanscom AFB, MA USA. ARCON Corp, Waltham, MA USA. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. RP Mlynczak, M (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA. EM m.g.mlynczak@nasa.gov RI Mlynczak, Martin/K-3396-2012; Lopez Puertas, Manuel/M-8219-2013; Funke, Bernd/C-2162-2008; Paxton, Larry/D-1934-2015; Martin-Torres, Francisco Javier/G-6329-2015 OI Lopez Puertas, Manuel/0000-0003-2941-7734; Funke, Bernd/0000-0003-0462-4702; Paxton, Larry/0000-0002-2597-347X; Martin-Torres, Francisco Javier/0000-0001-6479-2236 NR 11 TC 50 Z9 51 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD NOV 7 PY 2003 VL 30 IS 21 AR 2100 DI 10.1029/2003GL017693 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 742FV UT WOS:000186507400002 ER PT J AU Salem, JA Manderscheid, JM AF Salem, JA Manderscheid, JM TI Stresses in a thin, circular aeolotropic plate subjected to uniform lateral load SO JOURNAL OF PHYSICS D-APPLIED PHYSICS LA English DT Article AB Closed form, approximate stress solutions for simply supported cubic and orthotropic plates subjected to a lateral pressure are presented and compared with a series solution. The accuracy of the approximate solutions depends on the degree of anisotropy. For cubic plates exhibiting significant anisotropy, the approximate solution is within similar to10% of the series solution. For a graphite-epoxy composite plate of orthotropic symmetry, the approximate solution is within 10% of the series solution for the maximum stress at the plate centre and within 23% for the minimum stress at the plate centre. Single crystal plates tend to exhibit a large tangential stress where the stiff directions intersect the plate edges, implying that the edges of brittle single crystal test specimens must either be prepared better than those of isotropic specimens or have more of the plate overhanging the support. C1 NASA, Glenn Res Ctr, Life Predict Branch, Cleveland, OH 44135 USA. RP Salem, JA (reprint author), NASA, Glenn Res Ctr, Life Predict Branch, MS 49-7, Cleveland, OH 44135 USA. NR 7 TC 2 Z9 2 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0022-3727 J9 J PHYS D APPL PHYS JI J. Phys. D-Appl. Phys. PD NOV 7 PY 2003 VL 36 IS 21 BP 2730 EP 2737 AR PII S0022-3727(03)58791-5 DI 10.1088/0022-3727/36/21/022 PG 8 WC Physics, Applied SC Physics GA 748DA UT WOS:000186845900024 ER PT J AU Navarro-Gonzalez, R Rainey, FA Molina, P Bagaley, DR Hollen, BJ de la Rosa, J' Small, AM Quinn, RC Grunthaner, FJ Caceres, L Gomez-Silva, B McKay, CP AF Navarro-Gonzalez, R Rainey, FA Molina, P Bagaley, DR Hollen, BJ de la Rosa, J' Small, AM Quinn, RC Grunthaner, FJ Caceres, L Gomez-Silva, B McKay, CP TI Mars-like soils in the Atacama Desert, Chile, and the dry limit of microbial life SO SCIENCE LA English DT Article AB The Viking missions showed the martian soil to be lifeless and depleted in organic material and indicated the presence of one or more reactive oxidants. Here we report the presence of Mars-like soils in the extreme arid region of the Atacama Desert. Samples from this region had organic species only at trace levels and extremely low levels of culturable bacteria. Two samples from the extreme arid region were tested for DNA and none was recovered. Incubation experiments, patterned after the Viking labeled-release experiment but with separate biological and nonbiological isomers, show active decomposition of organic species in these soils by nonbiological processes. C1 Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Lab Quim Plasmas & Estudios Planetarios, Mexico City 04510, DF, Mexico. Univ Paris 12, Lab Interuniv Syst Atmospher, CNRS, UMR 7583, F-94010 Creteil, France. Univ Paris 07, Lab Interuniv Syst Atmospher, CNRS, UMR 7583, F-94010 Creteil, France. Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. NASA, Div Space Sci, Ames Res Ctr, Moffett Field, CA 94035 USA. NASA, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Antofagasta, Fac Ingn, Inst Desierto, Antofagasta, Chile. Univ Antofagasta, Fac Ingn, Dept Ingn Quim, Antofagasta, Chile. Univ Antofagasta, Fac Ciencias Salud, Inst Desierto, Antofagasta, Chile. Univ Antofagasta, Fac Ciencias Salud, Dept Biomed, Unidad Bioquim, Antofagasta, Chile. RP Navarro-Gonzalez, R (reprint author), Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Lab Quim Plasmas & Estudios Planetarios, Circuito Exterior,Ciudad Univ,Apartado Postal 70-, Mexico City 04510, DF, Mexico. RI Gonzalez, Rafael/D-1748-2009; De la Rosa, Jose/A-3573-2010; Rainey, Fred/C-8767-2013 OI Rainey, Fred/0000-0001-9129-6844 NR 9 TC 240 Z9 248 U1 15 U2 95 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 NOV 7 PY 2003 VL 302 IS 5647 BP 1018 EP 1021 DI 10.1126/science.1089143 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 740HE UT WOS:000186396300039 PM 14605363 ER PT J AU Genkova, I Davies, R AF Genkova, I Davies, R TI Spatial heterogeneity of reflected radiance from globally distributed clouds SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID IMAGING SPECTRORADIOMETER MISR; SOLAR ZENITH ANGLE; RADIATION BUDGET; DEPENDENCE; RESOLUTION; BIASES AB Reflected spectral radiance measured by the Multi-angle Imaging SpectroRadiometer (MISR) on the Terra satellite has been analyzed to determine the fraction of global cloudiness that appears to be spatially homogeneous over regions of various sizes. We exclude scenes with reflectivities less than 0.2 and high latitudes to avoid snow and ice. About 1.4 +/- 0.3%, or 1 in 70, of 8.8 km cloudy regions measured at 275 m have a range of reflectivities less than +/-5% of the central reflectivity value of the region. This pass rate changes slightly with viewing angle, and is sensitive to the size of the test window, rising to 11% for 1.1 km regions. The pass rate rises to a value of 2.3 +/- 0.5% for 8.8 km regions if the measurement resolution is degraded to 1100 m. For the purposes of this study "global" cloudiness is limited to mid-morning clouds. C1 Pacific NW Natl Lab, Richland, WA 99352 USA. CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Genkova, I (reprint author), Pacific NW Natl Lab, Richland, WA 99352 USA. RI Davies, Roger/D-4296-2009 OI Davies, Roger/0000-0002-2991-0409 NR 10 TC 7 Z9 7 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 NOV 6 PY 2003 VL 30 IS 21 AR 2096 DI 10.1029/2003GL018194 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 742FU UT WOS:000186507300003 ER PT J AU Marshall, CH Pielke, RA Steyaert, LT AF Marshall, CH Pielke, RA Steyaert, LT TI Wetlands: Crop freezes and land-use change in Florida SO NATURE LA English DT Editorial Material C1 Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. US Geol Survey, EROS Data Ctr, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Marshall, CH (reprint author), Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. RI Pielke, Roger/A-5015-2009 NR 9 TC 26 Z9 27 U1 2 U2 37 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD NOV 6 PY 2003 VL 426 IS 6962 BP 29 EP 30 DI 10.1038/426029a PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 739WY UT WOS:000186370800028 PM 14603304 ER PT J AU McDonald, FB Stone, EC Cummings, AC Heikkila, B Lal, N Webber, WR AF McDonald, FB Stone, EC Cummings, AC Heikkila, B Lal, N Webber, WR TI Enhancements of energetic particles near the heliospheric termination shock SO NATURE LA English DT Article ID COSMIC-RAYS; SOLAR-WIND; OUTER HELIOSPHERE; ACCELERATION; IONS AB The spacecraft Voyager 1 is at a distance greater than 85 AU from the Sun, in the vicinity of the termination shock that marks the abrupt slowing of the supersonic solar wind and the beginning of the extended and unexplored distant heliosphere(1,2). This shock is expected to accelerate 'anomalous cosmic rays' (3), as well as to reaccelerate Galactic cosmic rays(5) and low-energy particles from the inner Solar System(4). Here we report a significant increase in the numbers of energetic ions and electrons that persisted for seven months beginning in mid-2002. This increase differs from any previously observed in that there was a simultaneous increase in Galactic cosmic ray ions and electrons, anomalous cosmic rays and low-energy ions. The low-intensity level and spectral energy distribution of the anomalous cosmic rays, however, indicates that Voyager 1 still has not reached the termination shock. Rather, the observed increase is an expected precursor event. We argue that the radial anisotropy of the cosmic rays is expected to be small in the foreshock region, as is observed. C1 Univ Maryland, Inst Phys Sci & Technol, College Pk, MD 20742 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. CALTECH, Pasadena, CA 91125 USA. New Mexico State Univ, Dept Phys & Astron, Las Cruces, NM 88003 USA. RP McDonald, FB (reprint author), Univ Maryland, Inst Phys Sci & Technol, College Pk, MD 20742 USA. NR 20 TC 135 Z9 137 U1 0 U2 3 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD NOV 6 PY 2003 VL 426 IS 6962 BP 48 EP 51 DI 10.1038/nature02066 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 739WY UT WOS:000186370800036 PM 14603312 ER PT J AU Chu, DA Kaufman, YJ Zibordi, G Chern, JD Mao, J Li, CC Holben, BN AF Chu, DA Kaufman, YJ Zibordi, G Chern, JD Mao, J Li, CC Holben, BN TI Global monitoring of air pollution over land from the Earth Observing System-Terra Moderate Resolution Imaging Spectroradiometer (MODIS) SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE satellite remote sensing; air pollution; aerosol properties ID SOUTHERN AFRICA; ANTHROPOGENIC AEROSOLS; AIRBORNE SIMULATOR; OPTICAL-PROPERTIES; SIZE DISTRIBUTION; SAFARI 2000; DRY SEASON; REFLECTANCE; VARIABILITY; SMOKE AB Moderate Resolution Imaging Spectroradiometer (MODIS) measurements (7 channels: 0.47-2.1 mum, 250-500 m resolutions) provide us with new insights into the characteristics of global aerosols. MODIS retrieves not only aerosol loading but also the fraction of fine mode particle. In this paper we demonstrate MODIS capability for use in monitoring global, regional, and local air pollution. Three case studies in northern Italy, Los Angeles, and Beijing showed the conclusive results of applying MODIS-derived aerosol optical depths (tau(a)) to regional and local air pollution in terms of accuracy (Deltatau(a)=+/-0.05+/-0.2tau(a)) and spatial sensitivity of the retrievals. Under stagnant condition, accumulated aerosol abundance can reach tau(a)>1 (at 0.55 m) before being removed by wind or precipitation. The correlation found between Aerosol Robotic Network (AERONET) daily averaged tau(a) and 24-hour PM10 (particulate matter with diameter <10 mu m) concentration (mu g/m(3)) in northern Italy is encouraging with correlation coefficient similar to 0.82. The derivation of PM concentration from satellite measurements may be possible once we know the detailed aerosol vertical distribution. To compare aerosol loading in different regions of the globe, we choose the two most populated regions (eastern China and India) and the two most industrialized regions (the eastern United States/Canada and western Europe). The time series of MODIS monthly mean tau(a) from July 2000 to May 2001 depicts a strong seasonal variation with maxima in the spring/summer and minima in the winter. The clear separation between (1) the eastern United States/Canada and western Europe and (2) eastern China and India shows that the tau(a) values in (2) are 50% to 2-3 times higher compared to those in (1). The enhancements of aerosol loading were due to smoke as originated Montana/Idaho forest fires transported to the eastern United States in late August 2000 and dust outbreaks from Taklimakan and Gobi Deserts to eastern China as well as smoke from Southeast Asia to southern China in February-April 2001. C1 Sci Syst & Applicat Inc, Lanham, MD 20706 USA. NASA, GEST, Atmospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, I-21020 Ispra, Italy. NASA, Goddard Earth Sci & Technol Ctr, Atmospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Peking Univ, Sch Phys, Dept Atmospher Sci, Beijing 100871, Peoples R China. NASA, Terr Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Chu, DA (reprint author), Sci Syst & Applicat Inc, 10210 Greenbelt Rd,Suite 600, Lanham, MD 20706 USA. EM achu@climate.gsfc.nasa.gov; kaufman@climate.gsfc.nasa.gov; giuseppe.zibordi@jrc.it; jchern@dao.gsfc.nasa.gov; mjt@pku.edu.cn; ccli@ust.hk; holben@aeronet.gsfc.nasa.gov RI LI, Chengcai/B-4654-2012 OI LI, Chengcai/0000-0001-8860-1916 NR 38 TC 285 Z9 320 U1 8 U2 84 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 NOV 5 PY 2003 VL 108 IS D21 AR 4661 DI 10.1029/2002JD003179 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 742GB UT WOS:000186508100001 ER PT J AU Robock, A Luo, LF Wood, EF Wen, FH Mitchell, KE Houser, PR Schaake, JC Lohmann, D Cosgrove, B Sheffield, J Duan, QY Higgins, RW Pinker, RT Tarpley, JD Basara, JB Crawford, KC AF Robock, A Luo, LF Wood, EF Wen, FH Mitchell, KE Houser, PR Schaake, JC Lohmann, D Cosgrove, B Sheffield, J Duan, QY Higgins, RW Pinker, RT Tarpley, JD Basara, JB Crawford, KC TI Evaluation of the North American Land Data Assimilation System over the southern Great Plains during the warm season SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE data assimilation; soil moisture; surface fluxes ID SOIL-MOISTURE SIMULATIONS; SURFACE PARAMETERIZATION SCHEMES; ETA-MODEL; RIVER BASIN; SPATIAL VARIABILITY; HYDROLOGICAL CYCLE; CLIMATE MODELS; ENERGY BUDGET; WATER-BALANCE; PILPS 2(D) AB North American Land Data Assimilation System (NLDAS) land surface models have been run for a retrospective period forced by atmospheric observations from the Eta analysis and actual precipitation and downward solar radiation to calculate land hydrology. We evaluated these simulations using in situ observations over the southern Great Plains for the periods of May-September of 1998 and 1999 by comparing the model outputs with surface latent, sensible, and ground heat fluxes at 24 Atmospheric Radiation Measurement/Cloud and Radiation Testbed stations and with soil temperature and soil moisture observations at 72 Oklahoma Mesonet stations. The standard NLDAS models do a fairly good job but with differences in the surface energy partition and in soil moisture between models and observations and among models during the summer, while they agree quite well on the soil temperature simulations. To investigate why, we performed a series of experiments accounting for differences between model-specified soil types and vegetation and those observed at the stations, and differences in model treatment of different soil types, vegetation properties, canopy resistance, soil column depth, rooting depth, root density, snow-free albedo, infiltration, aerodynamic resistance, and soil thermal diffusivity. The diagnosis and model enhancements demonstrate how the models can be improved so that they can be used in actual data assimilation mode. C1 Rutgers State Univ, Dept Environm Sci, Ctr Environm Predict, New Brunswick, NJ 08901 USA. Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. Natl Ctr Environm Predict, Environm Modeling Ctr, Camp Springs, MD 20746 USA. NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20740 USA. Natl Weather Ctr, Off Hydrol Dev, Silver Spring, MD 20910 USA. Natl Ctr Environm Predict, Climate Predict Ctr, Camp Springs, MD 20746 USA. Univ Maryland, Dept Meteorol, College Pk, MD 20742 USA. Natl Environm Satellite Data & Informat Serv, Off Res & Applicat, Camp Springs, MD 20746 USA. Univ Oklahoma, Oklahoma Climatol Survey, Norman, OK 73019 USA. RP Robock, A (reprint author), Rutgers State Univ, Dept Environm Sci, Ctr Environm Predict, 14 Coll Farm Rd, New Brunswick, NJ 08901 USA. EM robock@envsci.rutgers.edu RI Sheffield, Justin/A-6388-2008; Luo, Lifeng/C-8734-2009; Pinker, Rachel/F-6565-2010; Houser, Paul/J-9515-2013; Duan, Qingyun/C-7652-2011; Basara, Jeffrey/A-4907-2008; Robock, Alan/B-6385-2016 OI Robock, Alan/0000-0002-6319-5656; Houser, Paul/0000-0002-2991-0441; Duan, Qingyun/0000-0001-9955-1512; Basara, Jeffrey/0000-0002-2096-6844; NR 65 TC 102 Z9 103 U1 1 U2 16 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 5 PY 2003 VL 108 IS D22 AR 8846 DI 10.1029/2002JD003245 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 742GJ UT WOS:000186508800002 ER PT J AU Meskhidze, N Chameides, WL Nenes, A Chen, G AF Meskhidze, N Chameides, WL Nenes, A Chen, G TI Iron mobilization in mineral dust: Can anthropogenic SO2 emissions affect ocean productivity? SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID HETEROGENEOUS REACTIVITY; REDUCTIVE DISSOLUTION; EAST-ASIA; AEROSOL; MODEL; TROPOSPHERE; ALPHA-FE2O3; PARTICLES; CHEMISTRY; TRANSPORT AB For Fe contained in long-range transported aeolian dust to act as a micronutrient for oceanic phytoplankton it must be first dissolved or mobilized. We propose that Fe-mobilization can occur in mineral dust from East Asia by the incorporation of SO2 into the advecting dust plumes and subsequent acidification of the dust through heterogeneous SO2 oxidation. To test this hypothesis, we consider a dust plume that originated from the gobi-deserts and advected over the Pacific Ocean. Data collected over the Yellow Sea confirm that this plume contained high concentrations of dust and SO2. Significant gaseous HNO3 concentrations indicate that the dust particles were acidified (i.e., pH < 2). At these pH's, 1-2% of the Fe contained in a deliquescent mineral dust particle would be mobilized within 3-5 days. These results suggest a possible link between the rate of C-fixation in so-called High-Nitrate-Low-Chlorophyll regions of the Pacific Ocean and SO2 emissions from East Asia. C1 Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. Georgia Inst Technol, Sch Chem Engn, Atlanta, GA 30332 USA. NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Meskhidze, N (reprint author), Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. NR 33 TC 125 Z9 127 U1 6 U2 34 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 NOV 4 PY 2003 VL 30 IS 21 AR 2085 DI 10.1029/2003GL018035 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 742FL UT WOS:000186506500002 ER PT J AU Crawford, J Olson, J Davis, D Chen, G Barrick, J Shetter, R Lefer, B Jordan, C Anderson, B Clarke, A Sachse, G Blake, D Singh, H Sandolm, S Tan, D Kondo, Y Avery, M Flocke, F Eisele, F Mauldin, L Zondlo, M Brune, W Harder, H Martinez, M Talbot, R Bandy, A Thornton, D AF Crawford, J Olson, J Davis, D Chen, G Barrick, J Shetter, R Lefer, B Jordan, C Anderson, B Clarke, A Sachse, G Blake, D Singh, H Sandolm, S Tan, D Kondo, Y Avery, M Flocke, F Eisele, F Mauldin, L Zondlo, M Brune, W Harder, H Martinez, M Talbot, R Bandy, A Thornton, D TI Clouds and trace gas distributions during TRACE-P SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE troposphere; cloud; chemistry; transport; carbon monoxide; TRACE-P ID CHARACTERIZATION EXPERIMENT ACE-1; PHOTOSTATIONARY STATE ANALYSIS; BIOMASS BURNING EMISSIONS; NORTH-ATLANTIC OCEAN; PEM-WEST B; SOUTH-ATLANTIC; AIRBORNE OBSERVATIONS; MIDLATITUDE CYCLONES; CONTINENTAL OUTFLOW; TRANSPORT PATHWAYS AB This paper addresses the question: To what extent do trace gas distributions correspond to cloudiness? Observations taken during NASA's TRACE-P experiment indicate that there can be statistically significant differences in trace gas concentrations between clear-sky and cloudy areas. During the TRACE-P mission, frontal outflow of Asian emissions from the Pacific Rim to the western, North Pacific was sampled by NASA's DC-8 and P-3B aircraft. On several occasions, enhanced CO mixing ratios were observed in and around frontal clouds. A more detailed analysis of trace gas distributions revealed CO enhancements of 30% in the lower free troposphere (1-5 km) for cloudy regions as compared to clear areas. These enhancements exist within clouds as well as above and below clouds. In the upper free troposphere (5-11 km), overall enhancement in CO of 15% was observed although enhancements are mainly restricted to observations within clouds. These in-cloud observations were enhanced by factors of 1.5 to 2 over clear air data. Similar enhancements were seen for many other anthropogenic tracers. By contrast, distributions for O-3 revealed no clear differences between cloudy and clear regions suggesting that other influences (e.g., stratosphere-troposphere exchange) might complicate any correspondence with local cloudiness. Expected cloud influences on oxidation chemistry were evident in enhanced OH concentrations above clouds and depressed OH below clouds. These findings are particularly relevant to current and future satellite investigations of the troposphere. Understanding the potential biases created by the inability to probe cloudy regions will improve the interpretation of regional and globally averaged satellite observations. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA. Univ Hawaii, Sch Ocean & Earth Sci & Technol, Honolulu, HI 96822 USA. Univ Calif Irvine, Dept Chem, Irvine, CA 92697 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Tokyo, Adv Sci & Technol Res Ctr, Meguro Ku, Tokyo 1538904, Japan. Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. Drexel Univ, Dept Chem, Philadelphia, PA 19104 USA. RP NASA, Langley Res Ctr, MS 483, Hampton, VA 23681 USA. EM j.h.crawford@larc.nasa.gov; j.o.olson@larc.nasa.gov; dd16@prism.gatech.edu; g.chen@larc.nasa.gov; j.d.barrick@larc.nasa.gov; shetter@ucar.edu; lefer@ucar.edu; c.e.jordan@larc.nasa.gov; b.e.anderson@larc.nasa.gov; tclarke@soest.hawaii.edu; drblake@uci.edu; drblake@uci.edu; hsingh@mail.arc.nasa.gov; dtan@eas.gatech.edu; kondo@atmos.rcast.u-tokyo.ac.jp; ffl@acd.ucar.edu; mzondlo@swsciences.com; brune@ems.psu.edu; harder@mpch-mainz.mpg.de; martinez@mpch-mainz.mpg.de; robert.talbot@unh.edu; alan.bandy@drexel.edu RI Kondo, Yutaka/D-1459-2012; Crawford, James/L-6632-2013; Harder, Hartwig/L-2511-2014; Lefer, Barry/B-5417-2012; Zondlo, Mark/R-6173-2016 OI Crawford, James/0000-0002-6982-0934; Harder, Hartwig/0000-0002-6868-714X; Lefer, Barry/0000-0001-9520-5495; Zondlo, Mark/0000-0003-2302-9554 NR 39 TC 24 Z9 24 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 4 PY 2003 VL 108 IS D21 AR 8818 DI 10.1029/2002JD003177 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 742GA UT WOS:000186508000005 ER PT J AU Luo, LF Robock, A Mitchell, KE Houser, PR Wood, EF Schaake, JC Lohmann, D Cosgrove, B Wen, FH Sheffield, J Duan, QY Higgins, RW Pinker, RT Tarpley, JD AF Luo, LF Robock, A Mitchell, KE Houser, PR Wood, EF Schaake, JC Lohmann, D Cosgrove, B Wen, FH Sheffield, J Duan, QY Higgins, RW Pinker, RT Tarpley, JD TI Validation of the North American Land Data Assimilation System (NLDAS) retrospective forcing over the southern Great Plains SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE surface fluxes; land surface modeling; LDAS ID SOIL-MOISTURE SIMULATIONS; ETA-MODEL; RIVER BASIN; FIFE DATA; SURFACE; PARAMETERIZATION; PRECIPITATION; BOUNDARY; PROJECT AB Atmospheric forcing used by land surface models is a critical component of the North American Land Data Assimilation System (NLDAS) and its quality crucially affects the final product of NLDAS and our work on model improvement. A three-year (September 1996-September 1999) retrospective forcing data set was created from the Eta Data Assimilation System and observations and used to run the NLDAS land surface models for this period. We compared gridded NLDAS forcing with station observations obtained from networks including the Oklahoma Mesonet and Atmospheric Radiation Measurement/Cloud and Radiation Testbed at the southern Great Plains. Differences in all forcing variables except precipitation between the NLDAS forcing data set and station observations are small at all timescales. While precipitation data do not agree very well at an hourly timescale, they do agree better at longer timescales because of the way NLDAS precipitation forcing is generated. A small high bias in downward solar radiation and a low bias in downward longwave radiation exist in the retrospective forcing. To investigate the impact of these differences on land surface modeling we compared two sets of model simulations, one forced by the standard NLDAS product and one with station-observed meteorology. The differences in the resulting simulations of soil moisture and soil temperature for each model were small, much smaller than the differences between the models and between the models and observations. This indicates that NLDAS retrospective forcing provides an excellent state-of-the-art data set for land surface modeling, at least over the southern Great Plains region. C1 Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ 08901 USA. NOAA Sci Ctr, Environm Modeling Ctr, Natl Ctr Environm Predict, Camp Springs, MD 20746 USA. NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. NOAA, Natl Weather Ctr, Off Hydrol Dev, Silver Spring, MD 20910 USA. NOAA Sci Ctr, Climate Predict Ctr, Natl Ctr Environm Predict, Camp Springs, MD 20746 USA. Univ Maryland, Dept Meteorol, College Pk, MD 20742 USA. Natl Environm Satellite Data & Informat Serv, Off Res & Applicat, Silver Spring, MD 20746 USA. Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. RP Luo, LF (reprint author), Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. EM robock@envsci.rutgers.edu RI Sheffield, Justin/A-6388-2008; Luo, Lifeng/C-8734-2009; Pinker, Rachel/F-6565-2010; Houser, Paul/J-9515-2013; Duan, Qingyun/C-7652-2011; Robock, Alan/B-6385-2016 OI Houser, Paul/0000-0002-2991-0441; Duan, Qingyun/0000-0001-9955-1512; NR 33 TC 72 Z9 74 U1 1 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 4 PY 2003 VL 108 IS D22 AR 8843 DI 10.1029/2002JD003246 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 742GH UT WOS:000186508700003 ER PT J AU Ma, Y Weber, RJ Lee, YN Orsini, DA Maxwell-Meier, K Thornton, DC Bandy, AR Clarke, AD Blake, DR Sachse, GW Fuelberg, HE Kiley, CM Woo, JH Streets, DG Carmichael, GR AF Ma, Y Weber, RJ Lee, YN Orsini, DA Maxwell-Meier, K Thornton, DC Bandy, AR Clarke, AD Blake, DR Sachse, GW Fuelberg, HE Kiley, CM Woo, JH Streets, DG Carmichael, GR TI Characteristics and influence of biosmoke on the fine-particle ionic composition measured in Asian outflow during the Transport and Chemical Evolution Over the Pacific (TRACE-P) experiment SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE atmospheric aerosol; biomass burning; particle chemical composition; Asian air quality ID BIOMASS BURNING AEROSOLS; TROPICAL INDIAN-OCEAN; ORGANIC-COMPOUNDS; MASS-SPECTROMETRY; EMISSIONS; DISTRIBUTIONS; COMBUSTION; MARINE; GASES; HYDROCARBONS AB We investigate the sources, prevalence, and fine-particle inorganic composition of biosmoke over the western Pacific Ocean between 24 February and 10 April 2001. The analysis is based on highly time-resolved airborne measurements of gaseous and fine-particle inorganic chemical composition made during the NASA Transport and Chemical Evolution over the Pacific (TRACE-P) experiment. At latitudes below approximately 25degreesN, relatively pure biomass burning plumes of enhanced fine-particle potassium, nitrate, ammonium, light-absorbing aerosols, and CO concentrations were observed in plumes that back trajectories and satellite fire map data suggest originated from biomass burning in southeast Asia. Fine-particle water-soluble potassium (K+) is confirmed to be a unique biosmoke tracer, and its prevalence throughout the experiment indicates that approximately 20% of the TRACE-P Asian outflow plumes were influenced, to some extent, by biomass or biofuel burning emissions. At latitudes above 25degreesN, highly mixed urban/industrial and biosmoke plumes, indicated by SO42- and K+, were observed in 5 out of 53 plumes. Most plumes were found in the Yellow Sea and generally were associated with much higher fine-particle loadings than plumes lacking a biosmoke influence. The air mass back trajectories of these mixed plumes generally pass through the latitude range of between 34degrees and 40degreesN on the eastern China coast, a region that includes the large urban centers of Beijing and Tianjin. A lack of biomass burning emissions based on fire maps and high correlations between K+ and pollution tracers (e.g., SO42-) suggest biofuel sources. Ratios of fine-particle potassium to sulfate are used to provide an estimate of relative contributions of biosmoke emissions to the mixed Asian plumes. The ratio is highly correlated with fine-particle volume (r(2) = 0.85) and predicts that for the most polluted plume encounter in TRACE-P, approximately 60% of the plume is associated with biosmoke emissions. On average, biosmoke contributes approximately 35-40% to the measured fine inorganic aerosol mass in the mixed TRACE-P plumes intercepted north of 25degreesN latitude. C1 Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. Brookhaven Natl Lab, Dept Environm Sci, Upton, NY 11973 USA. Drexel Univ, Dept Chem, Philadelphia, PA 19104 USA. Univ Hawaii Manoa, Dept Oceanog, Honolulu, HI 96822 USA. Univ Calif Irvine, Dept Chem, Irvine, CA 92697 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Florida State Univ, Dept Meteorol, Tallahassee, FL 32306 USA. Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA 52242 USA. Argonne Natl Lab, Argonne, IL 60439 USA. RP Georgia Inst Technol, Sch Earth & Atmospher Sci, 221 Boddy Dodd Way, Atlanta, GA 30332 USA. EM yma@eas.gatech.edu; rweber@eas.gatech.edu; ynlee@bnl.gov; douglas.orsini@eas.gatech.edu; kmaxwell@eas.gatech.edu; thorntdc@drexel.edu; bandyar@drexel.edu; tclarke@soest.hawaii.edu; drblake@uci.edu; g.w.sachse@larc.nasa.gov; fuelberg@met.fsu.edu; ckiley@huey.met.fsu.edu; woojh21@cgrer.uiowa.edu; dstreets@anl.gov; gcarmich@icaen.uiowa.edu NR 51 TC 64 Z9 66 U1 1 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 4 PY 2003 VL 108 IS D21 AR 8816 DI 10.1029/2002JD003128 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 742GA UT WOS:000186508000004 ER PT J AU Tang, YH Carmichael, GR Woo, JH Thongboonchoo, N Kurata, G Uno, I Streets, DG Blake, DR Weber, RJ Talbot, RW Kondo, Y Singh, HB Wang, T AF Tang, YH Carmichael, GR Woo, JH Thongboonchoo, N Kurata, G Uno, I Streets, DG Blake, DR Weber, RJ Talbot, RW Kondo, Y Singh, HB Wang, T TI Influences of biomass burning during the Transport and Chemical Evolution Over the Pacific (TRACE-P) experiment identified by the regional chemical transport model SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE biomass burning; chemical transport model; TRACE-P; photochemical process; aerosols; radiative influence ID EMISSIONS; AIR AB Using a regional chemical transport model, STEM 2K1, and the emission inventory for the Transport and Chemical Evolution Over the Pacific (TRACE-P) period [Woo et al., 2003 Streets et al., 2003], we successfully simulated important features of the biomass burning ( BB) CO outflow. Simulated results agree well with the TRACE-P aircraft measurements and Thailand surface observations. On the basis of sensitivity studies with and without biomass emissions, we identified nine flight segments that are affected by biomass plumes during the TRACE-P period and compared the characteristics of the BB air masses with the other air masses. The BB air masses emitted from Southeast Asia contain relatively high HCN (DeltaHCN/DeltaCO similar to 0.0015) and potassium (DeltaK(+)/DeltaCO similar to 0.0038) but very low NOy (DeltaNO(y)/DeltaCO similar to 0.005) mixing ratios, which may be associated with the special burning condition in this region. The biomass burning air masses have high ozone production efficiency. The observed DeltaO(3)/DeltaNO(z) values were similar to17 in biomass events and 1.7 in other events. The BB influence on the trace gas distributions can be divided into two categories: the influence through direct reactions and the influence caused by BB aerosols changing J values. These two influences are discussed for the BB-affected TRACE-P flights and for east Asia. The BB influences on chemical species are not only determined by the BB plume intensity but also by the ambient environment caused by other emissions. In Southeast Asia, where the biogenic emissions are very strong, the OH background concentration is low, and the BB gas-phase compounds mainly contribute to OH production. Arranged in the sensitivity to the J value change caused by BB aerosols, we have OH > HO2 > HCHO > O-3 when evaluated on a regional average. Averaged over March, the biomass burning net influence is as high as 50% for OH, 40% for HO2, 60% for HCHO, and 10 ppbv for O-3 for the layers below 1 km. C1 Univ Iowa, Ctr Global & Reg Environm Res, Iowa Adv Technol Labs 402, Iowa City, IA 52242 USA. Toyohashi Univ Technol, Dept Ecol Engn, Toyohashi, Aichi 4418580, Japan. Kyushu Univ, Res Inst Appl Mech, Fukuoka 8168580, Japan. Argonne Natl Lab, Argonne, IL 60439 USA. Univ Calif Irvine, Dept Chem, Irvine, CA 92697 USA. Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. Univ Tokyo, Res Ctr Adv Sci & Technol, Meguro Ku, Tokyo 1538904, Japan. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Hong Kong Polytech Univ, Dept Civil & Struct Engn, Kowloon, Hong Kong, Peoples R China. RP Univ Iowa, Ctr Global & Reg Environm Res, Iowa Adv Technol Labs 402, Iowa City, IA 52242 USA. EM ytang@cgrer.uiowa.edu; gcarmich@icaen.uiowa.edu; woojh21@cgrer.uiowa.edu; nthongbo@cgrer.uiowa.edu; kurata@eco.tut.ac.jp; iuno@riam.kyushu-u.ac.jp; dstreets@anl.gov; drblake@uci.edu; rweber@eas.gatech.edu; robert.talbot@unh.edu; kondo@atmos.rcast.u-tokyo.ac.jp; hanwant.b.singh@nasa.gov; cetwang@polyu.edu.cn RI Uno, Itsushi/B-5952-2011; Kondo, Yutaka/D-1459-2012; WANG, Tao/B-9919-2014; Kyushu, RIAM/F-4018-2015; U-ID, Kyushu/C-5291-2016; Tang, Youhua/D-5205-2016 OI WANG, Tao/0000-0002-4765-9377; Tang, Youhua/0000-0001-7089-7915 NR 12 TC 43 Z9 46 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 4 PY 2003 VL 108 IS D21 AR 8824 DI 10.1029/2002JD003110 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 742GA UT WOS:000186508000003 ER PT J AU Zhang, MG Uno, I Carmichael, GR Akimoto, H Wang, ZF Tang, YH Woo, JH Streets, DG Sachse, GW Avery, MA Weber, RJ Talbot, RW AF Zhang, MG Uno, I Carmichael, GR Akimoto, H Wang, ZF Tang, YH Woo, JH Streets, DG Sachse, GW Avery, MA Weber, RJ Talbot, RW TI Large-scale structure of trace gas and aerosol distributions over the western Pacific Ocean during the Transport and Chemical Evolution Over the Pacific (TRACE-P) experiment SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE tropospheric ozone; sulfate; biomass burning; regional pollution; CMAQ; TRACE-P ID TROPOSPHERIC OZONE PRODUCTION; EAST-ASIA; ANTHROPOGENIC EMISSIONS; MINERAL AEROSOL; NORTH PACIFIC; CONTINENTAL OUTFLOW; AIR-POLLUTION; YELLOW SAND; MODEL; ATMOSPHERE AB The Models-3 Community Multiscale Air Quality modeling system (CMAQ) coupled with the Regional Atmospheric Modeling System (RAMS) is used to analyze the Asian continental outflow of carbon monoxide (CO), ozone (O-3), and aerosol sulfate (SO42-) to the western Pacific Ocean during the period 17-24 March 2001. In this time period eight airborne observations (DC-8 flights 11-14 and P-3B flights 13-16) of the NASA Transport and Chemical Evolution Over the Pacific (TRACE-P) mission were being conducted over a broad area covering Hong Kong, Okinawa, the East China Sea, and southern Japan. Comparison of model results with observations shows that the model reproduces the main observed features of CO, O-3, and SO42-, including horizontal and vertical gradients, of the Asian pollution outflow over the western Pacific. Model results show that the fast boundary outflow from Asia to the western Pacific is largely restricted to the middle latitudes, and the maximum outflow fluxes are in the lower free atmosphere (3-6 km) north of 25degreesN. Simulations with and without biomass burning emissions are conducted to quantify the impacts of biomass burning on tropospheric concentrations of CO and O-3. Biomass burning is found to contribute more than 50% of the CO concentrations and up to 40% of the O-3 concentrations in the boundary layer over the major source regions. The largest percentage contributions to CO and O-3 levels ( up to 40% and 30%, respectively) over the western Pacific are in the lower free troposphere ( 2 6 km). C1 Frontier Res Syst Global Change, Yokohama, Kanagawa 2360001, Japan. Univ Iowa, Dept Chem & Biochem Engn, Iowa City, IA 52242 USA. Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA 52242 USA. Argonne Natl Lab, Decis & Informat Sci Div, Argonne, IL 60439 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. RP Chinese Acad Sci, Inst Atmospher Phys, State Key Lab Atmospher Boundary Layer Phys & Atm, Beijing, Peoples R China. EM mgzhang@mail.iap.ac.cn; iuno@riam.kyushu-u.ac.jp; gcarmich@icaen.uiowa.edu; akimoto@jamstec.go.jp; zifawang@mail.iap.ac.cn; ytang@cgrer.uiowa.edu; woojh21@cgrer.uiowa.edu; dstreets@anl.gov; g.w.sachse@larc.nasa.gov; m.a.avery@larc.nasa.gov; rweber@eas.gatech.edu; robert.talbot@unh.edu RI Wang, Zifa/B-5192-2008; Wang, ZF/D-7202-2012; Wang, Zifa/B-5799-2011; Tang, Youhua/D-5205-2016 OI Wang, ZF/0000-0002-7062-6012; Tang, Youhua/0000-0001-7089-7915 NR 46 TC 48 Z9 60 U1 1 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 4 PY 2003 VL 108 IS D21 AR 8820 DI 10.1029/2002JD002946 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 742GA UT WOS:000186508000002 ER PT J AU Nielsen, AD Pusey, ML Fuglsang, CC Westh, P AF Nielsen, AD Pusey, ML Fuglsang, CC Westh, P TI A proposed mechanism for the thermal denaturation of a recombinant Bacillus halmapalus alpha-amylase - the effect of calcium ions SO BIOCHIMICA ET BIOPHYSICA ACTA-PROTEINS AND PROTEOMICS LA English DT Article DE protein-ligand interaction; calcium binding; calorimetry; circular dichroism; alpha-amylase; denaturation mechanism ID DIFFERENTIAL SCANNING CALORIMETRY; CRYSTAL-STRUCTURE; THEORETICAL-ANALYSIS; AMYLOLYTIC ENZYMES; LICHENIFORMIS; INACTIVATION; RESOLUTION; BINDING; THERMOSTABILITY; ACTIVATION AB The thermal stability of a recombinant a-amylase from Bacillus halmapalus alpha-amylase (BHA) has been investigated using circular dichroism spectroscopy (CD) and differential scanning calorimetry (DSC). This alpha-amylase is homologous to other Bacillus alpha-amylases where crystallographic studies have identified the existence of three calcium binding sites in the structure. Denaturation of BHA is irreversible with a T-m of approximately 89 degreesC and DSC thermograms can be described using a one-step irreversible model. A 5 degreesC increase in T-m in the presence of 10-fold excess CaCl2 was observed. However, a concomitant increase in the tendency to aggregate was also observed. The presence of 30-40-fold excess calcium chelator (ethylenediaminetetraacetic acid (EDTA) or ethylene glycol-bis[beta-aminoethyl ether] N,N,N',N'-tetraacetic acid (EGTA)) results in a large destabilization of BHA, corresponding to about 40 degreesC lower T-m as determined by both CD and DSC. Ten-fold excess EGTA reveals complex DSC thermograms corresponding to both reversible and irreversible transitions, which probably originate from different populations of BHA/calcium complexes. Combined interpretation of these observations and structural information on homologous a-amylases forms the basis for a suggested mechanism underlying the inactivation mechanism of BHA. The mechanism includes irreversible thermal denaturation of different BHA/calcium complexes and the calcium binding equilibria. Furthermore, the model accounts for a temperature-induced reversible structural change associated with calcium binding. (C) 2003 Elsevier B.V. All rights reserved. C1 Roskilde Univ Ctr, Dept Life Sci & Chem, DK-4000 Roskilde, Denmark. Novozymes AS, DK-2880 Bagsvaerd, Denmark. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Westh, P (reprint author), Roskilde Univ Ctr, Dept Life Sci & Chem, POB 260,1 Univ Vej, DK-4000 Roskilde, Denmark. NR 43 TC 33 Z9 36 U1 2 U2 15 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1570-9639 J9 BBA-PROTEINS PROTEOM JI BBA-Proteins Proteomics PD NOV 3 PY 2003 VL 1652 IS 1 BP 52 EP 63 DI 10.1016/j.bbapap.2003.08.002 PG 12 WC Biochemistry & Molecular Biology; Biophysics SC Biochemistry & Molecular Biology; Biophysics GA 739PV UT WOS:000186356400006 PM 14580996 ER PT J AU Povitsky, A Salas, MD AF Povitsky, A Salas, MD TI Thermal regime of catalyst particles in reactor for production of carbon nanotubes SO AIAA JOURNAL LA English DT Article ID FLUID-FLOW; MONOXIDE AB This study was motivated by an attempt to optimize the high-pressure carbon oxide process for the production of carbon nanotubes from gaseous carbon oxide. The goal is to achieve rapid and uniform heating of catalyst particles by an optimal arrangement of jets. A mixed Eulerian and Lagrangian approach is implemented to track the temperature of catalyst particles along their trajectories as a function of time. The poor performance of the original reactor configuration is explained in terms of features of particle trajectories. The trajectories most exposed to the hot jets appear to be the most problematic for heating because they either bend toward the cold-jet interior or rotate upwind of the mixing zone. To reduce undesirable slow and/or oscillatory heating of catalyst particles, a reactor configuration with three central jets is proposed, and the optimal location of the central and peripheral nozzles is determined. C1 Univ Akron, Dept Mech Engn, Akron, OH 44325 USA. NASA, Langley Res Ctr, Vehicle Syst Technol Off, Hampton, VA 23681 USA. RP Povitsky, A (reprint author), Univ Akron, Dept Mech Engn, Akron, OH 44325 USA. EM povitsky@uakron.edu; manuel.d.salas@nasa.gov NR 24 TC 4 Z9 4 U1 0 U2 1 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD NOV PY 2003 VL 41 IS 11 BP 2130 EP 2142 DI 10.2514/2.6831 PG 13 WC Engineering, Aerospace SC Engineering GA 740NR UT WOS:000186408900005 ER PT J AU McIntyre, TJ Bishop, AI Rubinsztein-Dunlop, H Gnoffo, PA AF McIntyre, TJ Bishop, AI Rubinsztein-Dunlop, H Gnoffo, PA TI Comparison of experimental and numerical studies of ionizing flow over a cylinder SO AIAA JOURNAL LA English DT Article ID SUPERORBITAL EXPANSION TUBE AB Comparisons are made between experimental measurements and numerical simulations of ionizing flows generated in a superorbital facility. Nitrogen, with a freestream velocity of around 10 km/s, was passed over a cylindrical model, and images were recorded using two-wavelength holographic interferometry. The resulting density, electron concentration, and temperature maps were compared with numerical simulations from the Langley Research Center aerothermodynamic upwind relaxation algorithm. The results showed generally good agreement in shock location and density distributions. Some discrepancies were observed for the electron concentration, possibly, because simulations were of a two-dimensional flow, whereas the experiments were likely to have small three-dimensional effects. C1 Univ Queensland, Dept Phys, Ctr Hyperson, Brisbane, Qld 4072, Australia. RP McIntyre, TJ (reprint author), NASA, Langley Res Ctr, Aerodynam Aerothermodynam & Acoust Competency, Hampton, VA 23681 USA. RI Rubinsztein-Dunlop, Halina/C-6762-2009; McIntyre, Timothy/D-8491-2013; Rubinsztein-Dunlop, Halina/D-2387-2014 OI Rubinsztein-Dunlop, Halina/0000-0002-8332-2309; NR 10 TC 4 Z9 4 U1 0 U2 0 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 NOV PY 2003 VL 41 IS 11 BP 2157 EP 2161 DI 10.2514/2.6833 PG 5 WC Engineering, Aerospace SC Engineering GA 740NR UT WOS:000186408900007 ER PT J AU Tumin, A Ashpis, DE AF Tumin, A Ashpis, DE TI Optimal disturbances in boundary layers subject to streamwise pressure gradient SO AIAA JOURNAL LA English DT Article ID BYPASS TRANSITION; SPATIAL THEORY; GROWTH C1 Univ Arizona, Dept Aerosp & Mech, Tucson, AZ 85721 USA. NASA, John H Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA. RP Tumin, A (reprint author), Univ Arizona, Dept Aerosp & Mech, Tucson, AZ 85721 USA. NR 12 TC 5 Z9 5 U1 0 U2 0 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 NOV PY 2003 VL 41 IS 11 BP 2297 EP 2300 DI 10.2514/2.6825 PG 4 WC Engineering, Aerospace SC Engineering GA 740NR UT WOS:000186408900024 ER PT J AU Liu, TS Sullivan, JP AF Liu, TS Sullivan, JP TI In situ calibration uncertainty of pressure-sensitive paint SO AIAA JOURNAL LA English DT Article C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47906 USA. RP Liu, TS (reprint author), NASA, Langley Res Ctr, Mail Stop 238, Hampton, VA 23681 USA. NR 7 TC 4 Z9 4 U1 0 U2 3 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD NOV PY 2003 VL 41 IS 11 BP 2300 EP 2302 DI 10.2514/2.6826 PG 3 WC Engineering, Aerospace SC Engineering GA 740NR UT WOS:000186408900025 ER PT J AU Warren-Rhodes, K Sadovy, Y Cesar, H AF Warren-Rhodes, K Sadovy, Y Cesar, H TI Marine ecosystem appropriation in the Indo-Pacific: A case study of the live reef fish food trade SO AMBIO LA English DT Article ID CORAL-REEFS; SERVICES AB Our ecological footprint analyses of coral reef fish fisheries and, in particular, the live reef fish food trade (FT), indicate many countries' current consumption exceeds estimated sustainable per capita global, regional and local coral reef production levels. Hong Kong appropriates 25% of SE Asia's annual reef fish production of 135 260-286 560 tonnes (t) through its FT demand, exceeding regional biocapacity by 8.3 times; reef fish fisheries demand outpaces sustainable production in the Indo-Pacific and SE Asia by 2.5 and 6 times. In contrast, most Pacific islands live within their own reef fisheries means with local demand at < 20% of total capacity in Oceania. The FT annually requisitions up to 40% of SE Asia's estimated reef fish and virtually all of its estimated grouper yields. Our results underscore the unsustainable nature of the FT and the urgent need for regional management and conservation of coral reef fisheries in the Indo-Pacific. C1 Univ Hong Kong, Dept Ecol & Biodivers, Hong Kong, Hong Kong, Peoples R China. RP Warren-Rhodes, K (reprint author), NASA, Ames Res Ctr, Mail Stop 245-3, Moffett Field, CA 94035 USA. NR 46 TC 24 Z9 27 U1 0 U2 21 PU ROYAL SWEDISH ACAD SCIENCES PI STOCKHOLM PA PUBL DEPT BOX 50005, S-104 05 STOCKHOLM, SWEDEN SN 0044-7447 J9 AMBIO JI Ambio PD NOV PY 2003 VL 32 IS 7 BP 481 EP 488 DI 10.1639/0044-7447(2003)032[0481:MEAITI]2.0.CO;2 PG 8 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 751XU UT WOS:000187116300011 PM 14703908 ER PT J AU Ajtic, JV Connor, BJ Randall, CE Lawrence, BN Bodeker, GE Rosenfield, JE Heuff, DN AF Ajtic, JV Connor, BJ Randall, CE Lawrence, BN Bodeker, GE Rosenfield, JE Heuff, DN TI Antarctic air over New Zealand following vortex breakdown in 1998 SO ANNALES GEOPHYSICAE LA English DT Article DE atmospheric composition and structure; middle atmosphere composition and chemistry; meteorology and atmospheric dynamics; middle atmosphere dynamics ID STRATOSPHERIC POLAR VORTEX; OZONE DEPLETION; POTENTIAL VORTICITY; POAM-II; TRANSPORT; HOLE; ER-2; RECONSTRUCTION; SATELLITE; LATITUDES AB An ozonesonde profile over the Network for Detection of Stratospheric Change (NDSC) site at Lauder (45.0degrees S, 169.7degrees E), New Zealand, for 24 December 1998 showed atypically low ozone centered around 24 km altitude (600 K potential temperature). The origin of the anomaly is explained using reverse domain filling (RDF) calculations combined with a PV/O-3 fitting technique applied to ozone measurements from the Polar Ozone and Aerosol Measurement (POAM) III instrument. The RDF calculations for two isentropic surfaces, 550 and 600 K, show that ozone-poor air from the Antarctic polar vortex reached New Zealand on 2426 December 1998. The vortex air on the 550 K isentrope originated in the ozone hole region, unlike the air on 600 K where low ozone values were caused by dynamical effects. High-resolution ozone maps were generated, and their examination shows that a vortex remnant situated above New Zealand was the cause of the altered ozone profile on 24 December. The maps also illustrate mixing of the vortex filaments into southern midlatitudes, whereby the overall midlatitude ozone levels were decreased. C1 Natl Inst Water & Atmospher Res, Omakau 9182, Central Otago, New Zealand. Univ Canterbury, Dept Phys & Astron, Christchurch 8020, New Zealand. Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. Rutherford Appleton Lab, British Atmospher Data Ctr, Didcot OX11 0QX, Oxon, England. NASA, Goddard Space Flight Ctr, Goddard Earth Sci & Technol Ctr, Greenbelt, MD 20771 USA. RP Univ Canterbury, Dept Phys & Astron, Private Bag 4800, Christchurch 8020, New Zealand. EM j.ajtic@niwa.co.nz RI Bodeker, Greg/A-8870-2008; Randall, Cora/L-8760-2014; OI Bodeker, Greg/0000-0003-1094-5852; Randall, Cora/0000-0002-4313-4397; Lawrence, Bryan/0000-0001-9262-7860 NR 29 TC 6 Z9 6 U1 0 U2 2 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 0992-7689 EI 1432-0576 J9 ANN GEOPHYS-GERMANY JI Ann. Geophys. PD NOV PY 2003 VL 21 IS 11 BP 2175 EP 2183 PG 9 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 775NN UT WOS:000189047700005 ER PT J AU Fomalont, EB Petrov, L MacMillan, DS Gordon, D Ma, C AF Fomalont, EB Petrov, L MacMillan, DS Gordon, D Ma, C TI The second VLBA Calibrator Survey: VCS2 SO ASTRONOMICAL JOURNAL LA English DT Article DE astrometry; catalogs; quasars : general; radio continuum; reference systems; techniques : interferometric ID REFERENCE-FRAME AB This paper presents an extension of the Very Long Baseline Array Calibrator Survey, called VCS2, containing 276 sources. This survey fills in regions of the sky that were not completely covered by the previous VCS1 calibrator survey. The VCS2 survey includes calibrator sources near the Galactic plane, -30degrees < δ < -45degrees, and VLA calibrators. The positions have been derived from astrometric analysis of the group delays measured at 2.3 and 8.4 GHz using the Goddard Space Flight Center CALC/SOLVE package. From the VLBA snapshot observations, images of the calibrators are available, and each source is given a quality code for anticipated use. The VCS2 catalog is available from the NRAO Web site. C1 Natl Radio Astron Observ, Charlottesville, VA 22903 USA. NASA, NVI Inc, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Raytheon Informat Technol & Informat Serv, Greenbelt, MD 20771 USA. RP Fomalont, EB (reprint author), Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. RI Ma, Chopo/D-4751-2012 NR 7 TC 98 Z9 100 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 NOV PY 2003 VL 126 IS 5 BP 2562 EP 2566 DI 10.1086/378712 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 742AZ UT WOS:000186494200037 ER PT J AU Attie, D Cordier, B Gros, M Laurent, P Schanne, S Tauzin, G von Ballmoos, P Bouchet, L Jean, P Knodlseder, J Mandrou, P Paul, P Roques, JP Skinner, G Vedrenne, G Georgii, R von Kienlin, A Lichti, G Schonfelder, V Strong, A Wunderer, C Shrader, C Sturner, S Teegarden, B Weidenspointner, G Kiener, J Porquet, MG Tatischeff, V Crespin, S Joly, S Andre, Y Sanchez, F Leleux, P AF Attie, D Cordier, B Gros, M Laurent, P Schanne, S Tauzin, G von Ballmoos, P Bouchet, L Jean, P Knodlseder, J Mandrou, P Paul, P Roques, JP Skinner, G Vedrenne, G Georgii, R von Kienlin, A Lichti, G Schonfelder, V Strong, A Wunderer, C Shrader, C Sturner, S Teegarden, B Weidenspointner, G Kiener, J Porquet, MG Tatischeff, V Crespin, S Joly, S Andre, Y Sanchez, F Leleux, P TI INTEGRAL/SPI ground calibration SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE instrumentation : detectors; instrumentation : spectrographs; space vehicles : instruments; gamma rays : observations AB Three calibration campaigns of the spectrometer SPI have been performed before launch in order to determine the instrument characteristics, such as the effective detection area, the spectral resolution and the angular resolution. Absolute determination of the effective area has been obtained from simulations and measurements. At 1 MeV, the effective area is 65 cm(2) for a point source on the optical axis, the spectral resolution similar to2.3 keV. The angular resolution is better than 2.5degrees and the source separation capability about 1degrees. Some temperature dependant parameters will require permanent in-flight calibration. C1 CEA Saclay, Serv Astrophys, DSM, DAPNIA, F-91191 Gif Sur Yvette, France. Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. CNRS, IN2P3, Ctr Spectrometrie Nucl & Spectrometrie Masse, F-91405 Orsay, France. CEA Bruyeres le Chatel, F-91680 Bruyeres Le Chatel, France. Ctr Spatial Toulouse, CNES, F-31401 Toulouse, France. Univ Valencia, IFIC, E-46100 Valencia, Spain. Univ Louvain, B-1348 Louvain, Belgium. RP Attie, D (reprint author), CEA Saclay, Serv Astrophys, DSM, DAPNIA, F-91191 Gif Sur Yvette, France. RI laurent, philippe/E-6211-2013; Sanchez, Filomeno/D-7859-2014 OI Sanchez, Filomeno/0000-0003-0831-4744 NR 8 TC 49 Z9 49 U1 0 U2 5 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2003 VL 411 IS 1 BP L71 EP L79 DI 10.1051/0004-6361:20031302 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737JZ UT WOS:000186227800013 ER PT J AU Bouchet, L Jourdain, E Roques, JP Mandrou, P von Ballmoos, P Boggs, S Caraveo, P Casse, M Cordier, B Diehl, R Durouchoux, P von Kienlin, A Knodlseder, J Jean, P Leleux, P Lichti, GG Matteson, J Sanchez, F Schanne, S Schoenfelder, V Skinner, G Strong, A Teegarden, B Vedrenne, G Wunderer, C AF Bouchet, L Jourdain, E Roques, JP Mandrou, P von Ballmoos, P Boggs, S Caraveo, P Casse, M Cordier, B Diehl, R Durouchoux, P von Kienlin, A Knodlseder, J Jean, P Leleux, P Lichti, GG Matteson, J Sanchez, F Schanne, S Schoenfelder, V Skinner, G Strong, A Teegarden, B Vedrenne, G Wunderer, C TI SPI/INTEGRAL observation of the Cygnus region SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma rays : observations; X-ray stars : individual : Cyg X-1, Cyg X-3, EXO 2030+375; black hole : physics; space telescope : INTEGRAL : SPI ID X-RAY PULSAR; EXO-2030+375; DISCOVERY AB We present the analysis of the first observations of the Cygnus region by the SPI spectrometer onboard the Integral Gamma Ray Observatory, encompassing similar to600 ks of data. Three sources namely Cyg X-1, Cyg X-3 and EXO 2030+375 were clearly detected. Our data illustrate the temporal variability of Cyg X-1 in the energy range from 20 keV to 300 keV. The spectral analysis shows a remarkable stability of the Cyg X-1 spectra when averaged over one day timescale. The other goal of these observations is SPI inflight calibration and performance verification. The latest objective has been achieved as demonstrated by the results presented in this paper. C1 UPS, CNRS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France. Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. CEA Saclay, DSM, DAPNIA, Sap, F-91191 Gif Sur Yvette, France. IASF, I-20133 Milan, Italy. Univ Valencia, IFIC, E-46100 Burjassot, Spain. Univ Catholique Louvain, Inst Phys Nucl, B-1348 Louvain, Belgium. Univ Calif San Diego, CASS, La Jolla, CA 92093 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Bouchet, L (reprint author), UPS, CNRS, Ctr Etud Spatiale Rayonnements, BP 4346, F-31028 Toulouse, France. RI Sanchez, Filomeno/D-7859-2014; Boggs, Steven/E-4170-2015; OI Sanchez, Filomeno/0000-0003-0831-4744; Boggs, Steven/0000-0001-9567-4224; Caraveo, Patrizia/0000-0003-2478-8018 NR 20 TC 17 Z9 17 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2003 VL 411 IS 1 BP L377 EP L382 DI 10.1051/0004-6361:20031324 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737JZ UT WOS:000186227800061 ER PT J AU Castro-Tirado, AJ Gorosabel, J Guziy, S Reverte, D Ceron, JMC Postigo, AD Tanvir, N Mereghetti, S Tiengo, A Buckle, J Sagar, R Pandey, SB Mohan, V Masetti, N Mannucci, F Feltzing, S Lundstrom, I Pedersen, H Riess, C Trushkin, S Vilchez, J Lund, N Brandt, S Nunez, SM Reglero, V Perez-Ramirez, MD Klose, S Greiner, J Hjorth, J Kaper, L Pian, E Palazzi, E Andersen, MI Fruchter, A Fynbo, JPU Jensen, BL Kouveliotou, C Rhoads, J Rol, E Vreeswijk, PM Wijers, RAMJ van den Heuvel, E AF Castro-Tirado, AJ Gorosabel, J Guziy, S Reverte, D Ceron, JMC Postigo, AD Tanvir, N Mereghetti, S Tiengo, A Buckle, J Sagar, R Pandey, SB Mohan, V Masetti, N Mannucci, F Feltzing, S Lundstrom, I Pedersen, H Riess, C Trushkin, S Vilchez, J Lund, N Brandt, S Nunez, SM Reglero, V Perez-Ramirez, MD Klose, S Greiner, J Hjorth, J Kaper, L Pian, E Palazzi, E Andersen, MI Fruchter, A Fynbo, JPU Jensen, BL Kouveliotou, C Rhoads, J Rol, E Vreeswijk, PM Wijers, RAMJ van den Heuvel, E TI GRB 030227: The first multiwavelength afterglow of an INTEGRAL GRB SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma rays : bursts; techniques : photometric; cosmology : observations ID GAMMA-RAY BURST; OPTICAL AFTERGLOW; LIGHT CURVES; WIND; EMISSION AB We present multiwavelength observations of a gamma-ray burst detected by INTEGRAL (GRB 030227) between 5.3 hours and similar to1.7 days after the event. Here we report the discovery of a dim optical afterglow (OA) that would not have been detected by many previous searches due to its faintess (R similar to 23). This OA was seen to decline following a power law decay with index alpha(R) = - 0.95 +/- 0.16. The spectral index beta(opt/NIR) yielded - 1.25 +/- 0.14. These values may be explained by a relativistic expansion of a fireball ( with p = 2.0) in the cooling regime. We also find evidence for inverse Compton scattering in X-rays. C1 CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Hertfordshire, Dept Phys Sci, Hatfield AL10 9AB, Herts, England. CNR, Ist Astrofis Spaziale & Fis Cosm, Sez Milano, I-20133 Milan, Italy. Joint Astron Ctr, Hilo, HI 96720 USA. Uttar Pradesh State Observ, Naini Tal 263129, India. Ist Astrofis Spaziale & Fis Cosm, Sez Bologna, I-40129 Bologna, Italy. CNR, Ist Radioastron, Sez Firenze, I-50125 Florence, Italy. Lund Observ, S-22100 Lund, Sweden. Univ Copenhagen, Astron Observ, DK-2100 Copenhagen O, Denmark. Univ Observ Munich, D-81679 Munich, Germany. RAS, Special Astrophys Observ, Nizhnii Arkhyz 369167, Russia. Danish Space Res Inst, DK-2100 Copenhagen O, Denmark. Univ Valencia, Grp Astrofis & Ciencias Espacio, Valencia 46071, Spain. European Space Agcy, Res Sci Div, Noordwijk, Netherlands. Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. Univ Amsterdam, NL-1098 SJ Amsterdam, Netherlands. Osserv Astron Trieste, I-34131 Trieste, Italy. Inst Astrophys, D-14482 Potsdam, Germany. Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. NASA, MSFC, NSSTC, Huntsville, AL 35805 USA. European So Observ, Santiago 19, Chile. RP Castro-Tirado, AJ (reprint author), CSIC, Inst Astrofis Andalucia, Apartado Correos 3004, E-18080 Granada, Spain. EM ajct@iaa.es RI Hjorth, Jens/M-5787-2014; Jensen, Brian Lindgren/E-1275-2015; Palazzi, Eliana/N-4746-2015; OI Hjorth, Jens/0000-0002-4571-2306; Palazzi, Eliana/0000-0002-8691-7666; Castro-Tirado, A. J./0000-0003-2999-3563; de Ugarte Postigo, Antonio/0000-0001-7717-5085; Pian, Elena/0000-0001-8646-4858; Jensen, Brian Lindgren/0000-0002-0906-9771; mannucci, filippo/0000-0002-4803-2381 NR 35 TC 22 Z9 22 U1 0 U2 2 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2003 VL 411 IS 1 BP L315 EP L319 DI 10.1051/0004-6361:20031393 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737JZ UT WOS:000186227800051 ER PT J AU Courvoisier, TJL Walter, R Beckmann, V Dean, AJ Dubath, P Hudec, R Kretschmar, P Mereghetti, S Montmerle, T Mowlavi, N Paltani, S Martinez, AP Produit, N Staubert, R Strong, AW Swings, JP Westergaard, NJ White, N Winkler, C Zdziarski, AA AF Courvoisier, TJL Walter, R Beckmann, V Dean, AJ Dubath, P Hudec, R Kretschmar, P Mereghetti, S Montmerle, T Mowlavi, N Paltani, S Martinez, AP Produit, N Staubert, R Strong, AW Swings, JP Westergaard, NJ White, N Winkler, C Zdziarski, AA TI The INTEGRAL science data centre (ISDC) SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods : data analysis; gamma rays : observations AB The INTEGRAL Science Data Centre (ISDC) provides the INTEGRAL data and means to analyse them to the scientific community. The ISDC runs a gamma ray burst alert system that provides the position of gamma ray bursts on the sky within seconds to the community. It operates a quick-look analysis of the data within few hours that detects new and unexpected sources as well as it monitors the instruments. The ISDC processes the data through a standard analysis the results of which are provided to the observers together with their data. C1 INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. Observ Geneva, CH-1290 Sauverny, Switzerland. Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. Univ Southampton, Dept Phys, Astron Grp, Southampton SO17 1BJ, Hants, England. Acad Sci Czech Republ, Inst Astron, CS-25165 Ondrejov, Czech Republic. CNR, Ist Astrofis Spaziale & Fis Cosm, Sez Milano G Ochialini, I-20133 Milan, Italy. Ctr Etud Saclay, Serv Astrophys, F-91190 Gif Sur Yvette, France. Lab Astrophys Marseille, F-13376 Marseille 12, France. Ist Astrofis Spaziale, Area Ric Tor Vergata, I-00133 Rome, Italy. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. Danish Space Res Inst, DK-2100 Copenhagen, Denmark. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. European Space Agcy, Estec, RSSD, NL-2200 AG Noordwijk, Netherlands. Nicholas Copernicus Astron Ctr, PL-00716 Warsaw, Poland. RP Courvoisier, TJL (reprint author), INTEGRAL Sci Data Ctr, Chemin Ecogia 16, CH-1290 Versoix, Switzerland. RI White, Nicholas/B-6428-2012; Hudec, Rene/G-9018-2014; OI White, Nicholas/0000-0003-3853-3462; Kretschmar, Peter/0000-0001-9840-2048; MEREGHETTI, SANDRO/0000-0003-3259-7801 NR 15 TC 243 Z9 243 U1 0 U2 4 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2003 VL 411 IS 1 BP L53 EP L57 DI 10.1051/0004-6361:20031172 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737JZ UT WOS:000186227800010 ER PT J AU Diehl, R Knodlseder, J Lichti, GG Kretschmer, K Schanne, S Schonfelder, V Strong, AW von Kienlin, A Weidenspointner, G Winkler, C Wunderer, C AF Diehl, R Knodlseder, J Lichti, GG Kretschmer, K Schanne, S Schonfelder, V Strong, AW von Kienlin, A Weidenspointner, G Winkler, C Wunderer, C TI SPI measurements of Galactic Al-26 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE nucleosynthesis; galaxy : abundances; ISM : abundances; gamma-rays : observations; methods : observational ID HIGH-VELOCITY AL-26; LINE DATA; EMISSION; HEAO-3 AB The precision measurement of the 1809 keV gamma-ray line from Galactic Al-26 is one of the goals of the SPI spectrometer on INTEGRAL with its Ge detector camera. We aim for determination of the detailed shape of this gamma-ray line, and its variation for different source regions along the plane of the Galaxy. Data from the first part of the core program observations of the first mission year have been inspected. A clear detection of the Al-26 line at similar or equal to5-7 sigma significance demonstrates that SPI will deepen Al-26 studies. The line intensity is consistent with expectations from previous experiments, and the line appears narrower than the 5.4 keV FWHM reported by GRIS, more consistent with RHESSI's recent value. Only preliminary statements can be made at this time, however, due to the multi-component background underlying the signal at similar or equal to40 times higher intensity than the signal from Galactic Al-26. C1 Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France. CEA Saclay, DSM, DAPNIA, Serv Astrophys, F-91191 Gif Sur Yvette, France. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Space Res Assoc, Seabrook, MD 20706 USA. ESA, ESTEC, Sci Operat & Data Syst Div, NL-2201 AZ Noordwijk, Netherlands. RP Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. EM rod@mpe.mpg.de NR 28 TC 30 Z9 30 U1 1 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 NOV PY 2003 VL 411 IS 1 SI SI BP L451 EP L455 DI 10.1051/0004-6361:20031347 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737JZ UT WOS:000186227800075 ER PT J AU Diehl, R Baby, N Beckmann, V Connell, P Dubath, P Jean, P Knodlseder, J Roques, JP Schanne, S Shrader, C Skinner, G Strong, A Sturner, S Teegarden, B von Kienlin, A Weidenspointner, G AF Diehl, R Baby, N Beckmann, V Connell, P Dubath, P Jean, P Knodlseder, J Roques, JP Schanne, S Shrader, C Skinner, G Strong, A Sturner, S Teegarden, B von Kienlin, A Weidenspointner, G TI SPI-specific analysis method and software overview SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma-rays : observations; methods : data analysis AB The SPI spectrometer on INTEGRAL features a camera system with 19 Ge detector modules, imaging photons through a tungsten coded mask. Background is reduced by an anticoincidence detector system surrounding these. The specifics of this instrument lead to data correction and analysis methods which are described here. Raw data for science analysis are detector event messages and spectra for different categories of detector hits and pulse shapes. Preprocessing combines calibrated spectra from these, which are then interpreted using the imaging and spectral response function for measured spectra where parts of the detector plane are occulted by the mask. Background dominates the overall signal, tailored background estimates and models are based on instrument-specific signatures, their correlations, and trends. C1 Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France. Integral Sci Data Ctr, CH-1290 Versoix, Switzerland. Univ Birmingham, Birmingham, W Midlands, England. CEA Saclay, Serv Astrophys, DSM DAPNIA, F-91191 Gif Sur Yvette, France. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. Univ Space Res Assoc, Seabrook, MD 20706 USA. RP Diehl, R (reprint author), Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. NR 17 TC 28 Z9 28 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2003 VL 411 IS 1 BP L117 EP L121 DI 10.1051/0004-6361:20031365 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737JZ UT WOS:000186227800020 ER PT J AU Ebisawa, K Bourban, G Bodaghee, A Mowlavi, N Courvoisier, TJL AF Ebisawa, K Bourban, G Bodaghee, A Mowlavi, N Courvoisier, TJL TI High-energy sources before INTEGRAL - INTEGRAL reference catalog SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE INTEGRAL; X-ray sources; gamma-ray sources; catalog ID X-RAY BINARIES AB We describe the INTEGRAL reference catalog which classifies previously known bright X-ray and gamma-ray sources before the launch of INTEGRAL. These sources are, or have been at least once, brighter than similar to1 mCrab above 3 keV, and are expected to be detected by INTEGRAL. This catalog is being used in the INTEGRAL Quick Look Analysis to discover new sources or significantly variable sources. We compiled several published X-ray and gamma-ray catalogs, and surveyed recent publications for new sources. Consequently, there are 1122 sources in our INTEGRAL reference catalog. In addition to the source positions, we show an approximate spectral model and expected flux for each source, based on which we derive expected INTEGRAL counting rates. Assuming the default instrument performances and at least similar to10(5) s exposure time for any part of the sky, we expect that INTEGRAL will detect at least similar to700 sources below 10 keV and similar to400 sources above 20 keV over the mission life. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Observ Geneva, CH-1290 Sauverny, Switzerland. INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. RP Ebisawa, K (reprint author), Univ Space Res Assoc, Columbia, MD 21044 USA. NR 12 TC 40 Z9 40 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2003 VL 411 IS 1 BP L59 EP L62 DI 10.1051/0004-6361:20031336 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737JZ UT WOS:000186227800011 ER PT J AU Ferguson, C Barlow, EJ Bird, AJ Dean, AJ Hill, AB Shaw, SE Stephen, JB Sturner, S Tikkanen, TV Weidenspointner, G Willis, DR AF Ferguson, C Barlow, EJ Bird, AJ Dean, AJ Hill, AB Shaw, SE Stephen, JB Sturner, S Tikkanen, TV Weidenspointner, G Willis, DR TI The INTEGRAL mass model - TIMM SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma-ray astronomy; instrument simulation AB The INTEGRAL Mass Model (TIMM) was started in 1995 and aimed to create a detailed geometrical model of the whole INTEGRAL satellite on computer. In parallel, a comprehensive Monte Carlo simulation code (called GGOD) has been developed. The mass model and the Monte Carlo code together enable the in-flight operation of INTEGRAL to be simulated at the individual event level. Thus TIMM can be used to provide an independent evaluation of the performance of the individual instruments, to study the interference and complementarity between instruments, to generate test data for software development, and as a powerful tool for post-launch diagnosis. In this paper TIMM is briefly reviewed, some examples from ground calibration are presented, and preliminary comparison to flight data is shown. The future use of TIMM to flat field flight data is also briefly discussed. C1 Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. CNR, IASF, I-40129 Bologna, Italy. NASA, Goddard Space Flight Ctr, LHEA, Greenbelt, MD 20771 USA. Univ Space Res Assoc, Lanham, MD 20706 USA. Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. RP Ferguson, C (reprint author), Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. EM cf@astro.soton.ac.uk OI Hill, Adam/0000-0003-3470-4834 NR 4 TC 14 Z9 14 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2003 VL 411 IS 1 SI SI BP L19 EP L23 DI 10.1051/0004-6361:20031403 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737JZ UT WOS:000186227800004 ER PT J AU Jean, P Vedrenne, G Roques, JP Schonfelder, V Teegarden, BJ von Kienlin, A Knodlseder, J Wunderer, C Skinner, GK Weidenspointner, G Attie, D Boggs, S Caraveo, P Cordier, B Diehl, R Gros, M Leleux, P Lichti, GG Kalemci, E Kiener, J Lonjou, V Mandrou, P Paul, P Schanne, S von Ballmoos, P AF Jean, P Vedrenne, G Roques, JP Schonfelder, V Teegarden, BJ von Kienlin, A Knodlseder, J Wunderer, C Skinner, GK Weidenspointner, G Attie, D Boggs, S Caraveo, P Cordier, B Diehl, R Gros, M Leleux, P Lichti, GG Kalemci, E Kiener, J Lonjou, V Mandrou, P Paul, P Schanne, S von Ballmoos, P TI SPI instrumental background characteristics SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma-ray : instruments ID GAMMA-RAY SPECTROMETERS; PERFORMANCE AB In its space environment the INTEGRAL observatory is subject to an intense irradiation by energetic cosmic-ray particles that leads, via nuclear interactions with the telescope and spacecraft materials, to an important background of false events. In this paper we present the characteristics of the instrumental background that is observed in the spectrometer SPI (SPectrometer of INTEGRAL). We explain the tuning that has been performed on the parameters of the anticoincidence system in order to optimise the telescope sensitivity over the full energy range. Temporal variations of the instrumental background are discussed and methods are proposed that allow for their modelling in first order. C1 UPS, CNRS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. CEA Saclay, Serv Astrophys, DSM DAPNIA, F-91191 Gif Sur Yvette, France. Univ Space Res Assoc, Seabrook, MD 20706 USA. Univ Catholique Louvain, Inst Phys Nucl, B-1348 Louvain, Belgium. CNR G Occhialini, Ist Fis Cosm, I-20133 Milan, Italy. CNRS, IN2P3, Ctr Spectrometrie Nucl & Spectrometrie Masse, F-91405 Orsay, France. RP Jean, P (reprint author), UPS, CNRS, Ctr Etud Spatiale Rayonnements, BP 4346, F-31028 Toulouse 4, France. RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Caraveo, Patrizia/0000-0003-2478-8018 NR 13 TC 42 Z9 42 U1 0 U2 1 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2003 VL 411 IS 1 BP L107 EP L112 DI 10.1051/0004-6361:20031156 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737JZ UT WOS:000186227800018 ER PT J AU Knodlseder, K Lonjou, V Jean, P Allain, M Mandrou, P Roques, JP Skinner, GK Vedrenne, G von Ballmoos, P Weidenspointner, G Caraveo, P Cordier, B Schonfelder, V Teegarden, BJ AF Knodlseder, K Lonjou, V Jean, P Allain, M Mandrou, P Roques, JP Skinner, GK Vedrenne, G von Ballmoos, P Weidenspointner, G Caraveo, P Cordier, B Schonfelder, V Teegarden, BJ TI Early SPI/INTEGRAL constraints on the morphology of the 511 keV line emission in the 4th galactic quadrant SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma rays : observations ID POSITRON-ANNIHILATION RADIATION; PARTICLE INTERACTIONS AB We provide first constraints on the morphology of the 511 keV line emission from the galactic centre region on basis of data taken with the spectrometer SPI on the INTEGRAL gamma-ray observatory. The data suggest an azimuthally symmetric galactic bulge component with FWHM of similar to9degrees with a 2sigma uncertainty range covering 6degrees-18degrees. The 511 keV line flux in the bulge component amounts to 9.9(-2.1)(+4.7)x10(-4) ph cm(-2) s(-1). No evidence for a galactic disk component has been found so far; upper 2sigma flux limits in the range (1.4-3.4)x10(-3) ph cm(-2) s(-1) have been obtained that depend on the assumed disk morphology. These limits correspond to lower limits on the bulge-to-disk ratio of 0.3-0.6. C1 UPS, CNRS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. CEA Saclay, DSM, DAPNIA, SAp, F-91191 Gif Sur Yvette, France. IASF, I-20133 Milan, Italy. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Knodlseder, K (reprint author), UPS, CNRS, Ctr Etud Spatiale Rayonnements, BP 4346, F-31028 Toulouse 4, France. OI Caraveo, Patrizia/0000-0003-2478-8018 NR 20 TC 133 Z9 133 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2003 VL 411 IS 1 BP L457 EP L460 DI 10.1051/0004-6361:20031437 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737JZ UT WOS:000186227800076 ER PT J AU Roques, JP Schanne, S von Kienlin, A Knodlseder, J Briet, R Bouchet, L Paul, P Boggs, S Caraveo, P Casse, M Cordier, B Diehl, R Durouchoux, P Jean, P Leleux, P Lichti, G Mandrou, P Matteson, J Sanchez, F Schonfelder, V Skinner, G Strong, A Teegarden, B Vedrenne, G von Ballmoos, P Wunderer, C AF Roques, JP Schanne, S von Kienlin, A Knodlseder, J Briet, R Bouchet, L Paul, P Boggs, S Caraveo, P Casse, M Cordier, B Diehl, R Durouchoux, P Jean, P Leleux, P Lichti, G Mandrou, P Matteson, J Sanchez, F Schonfelder, V Skinner, G Strong, A Teegarden, B Vedrenne, G von Ballmoos, P Wunderer, C TI SPI/INTEGRAL in-flight performance SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma-ray : instrument, observations; space telescope : INTEGRAL/SPI ID FRONT-END ELECTRONICS; HPGE DETECTORS; DAMAGE AB The SPI instrument has been launched on-board the INTEGRAL observatory on October 17, 2002. SPI is a spectrometer devoted to the sky observation in the 20 keV-8 MeV energy range using 19 germanium detectors. The performance of the cryogenic system is nominal and allows to cool the 19 kg of germanium down to 85 K with a comfortable margin. The energy resolution of the whole camera is 2.5 keV at 1.1 MeV. This resolution degrades with time due to particle irradiation in space. We show that the annealing process allows the recovery of the initial performance. The anticoincidence shield works as expected, with a low threshold at 75 keV, reducing the GeD background by a factor of 20. The digital front-end electronics system allows the perfect alignement in time of all the signals as well as the optimisation of the dead time (12%). We demonstrate that SPI is able to map regions as complex as the galactic plane. The obtained spectrum of the Crab nebula validates the present version of our response matrix. The 3sigma sensitivity of the instrument at 1 MeV is 8x10(-7) ph cm(-2) s(-1) keV(-1) for the continuum and 3x10(-5) ph cm(-2) s(-1) for narrow lines. C1 UPS, CNRS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France. Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. CEA Saclay, DSM DAPNIA SAp, F-91191 Gif Sur Yvette, France. IASF, I-20133 Milan, Italy. Univ Valencia, IFIC, E-46100 Burjassot, Spain. Univ Catholique Louvain, Inst Phys Nucl, B-1348 Louvain, Belgium. Univ Calif San Diego, CASS, La Jolla, CA 92093 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. CNES CST, F-31401 Toulouse 4, France. RP Roques, JP (reprint author), UPS, CNRS, Ctr Etud Spatiale Rayonnements, BP 4346, F-31028 Toulouse, France. RI Sanchez, Filomeno/D-7859-2014; Boggs, Steven/E-4170-2015; OI Sanchez, Filomeno/0000-0003-0831-4744; Boggs, Steven/0000-0001-9567-4224; Caraveo, Patrizia/0000-0003-2478-8018 NR 16 TC 97 Z9 98 U1 0 U2 3 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2003 VL 411 IS 1 BP L91 EP L100 DI 10.1051/0004-6361:20031501 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737JZ UT WOS:000186227800016 ER PT J AU Strong, AW Bouchet, L Diehl, R Mandrou, P Schonfelder, V Teegarden, BJ AF Strong, AW Bouchet, L Diehl, R Mandrou, P Schonfelder, V Teegarden, BJ TI Diffuse continuum emission from the inner Galaxy: First results from INTEGRAL/SPI SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays; gamma rays; galactic structure; interstellar medium; cosmic rays ID X-RAY-EMISSION; POSITRON-ANNIHILATION RADIATION; GALACTIC RIDGE; ORIGIN; LINE AB We present a preliminary analysis of the diffuse hard X- and soft gamma-ray continuum emission from the inner Galactic ridge using INTEGRAL/SPI data from the first Galactic Plane Deep Exposure and Galactic Plane Scans. The spectrum is consistent with results from previous experiments. These early results demonstrate the potential of the INTEGRAL mission for improving our understanding of this emission. C1 Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. UPS, CNRS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Max Planck Inst Extraterr Phys, Postfach 1312, D-85741 Garching, Germany. EM aws@mpe.mpg.de NR 19 TC 11 Z9 11 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2003 VL 411 IS 1 SI SI BP L447 EP L450 DI 10.1051/0004-6361:20031256 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737JZ UT WOS:000186227800074 ER PT J AU Sturner, SJ Shrader, CR Weidenspointner, G Teegarden, BJ Attie, D Cordier, B Diehl, R Ferguson, C Jean, P von Kienlin, A Paul, P Sanchez, F Schanne, S Sizun, P Skinner, G Wunderer, CB AF Sturner, SJ Shrader, CR Weidenspointner, G Teegarden, BJ Attie, D Cordier, B Diehl, R Ferguson, C Jean, P von Kienlin, A Paul, P Sanchez, F Schanne, S Sizun, P Skinner, G Wunderer, CB TI Monte Carlo simulations and generation of the SPI response SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE INTEGRAL; SPI; gamma rays; methods : data analysis; methods : numerical AB In this paper we discuss the methods developed for the production of the INTEGRAL/SPI instrument response. The response files were produced using a suite of Monte Carlo simulation software developed at NASA/GSFC based on the GEANT-3 package available from CERN. The production of the INTEGRAL/SPI instrument response also required the development of a detailed computer mass model for SPI. We discuss our extensive investigations into methods to reduce both the computation time and storage requirements for the SPI response. We also discuss corrections to the simulated response based on our comparison of ground and inflight calibration data with MGEANT simulations. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Space Res Assoc, Seabrook, MD 20706 USA. Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France. CEA Saclay, Serv Astrophys, DSM, DAPNIA, F-91191 Gif Sur Yvette, France. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Univ Southampton, Dept Phys & Astron, Southampton S017 1BJ, Hants, England. CSIC UV, Edificio Inst Paterna, Inst Fis Corpuscular, Valencia 46071, Spain. RP Sturner, SJ (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. RI Sanchez, Filomeno/D-7859-2014 OI Sanchez, Filomeno/0000-0003-0831-4744 NR 5 TC 45 Z9 45 U1 0 U2 2 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2003 VL 411 IS 1 BP L81 EP L84 DI 10.1051/0004-6361:20031171 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737JZ UT WOS:000186227800014 ER PT J AU Ubertini, P Lebrun, F Di Cocco, G Bazzano, A Bird, AJ Broenstad, K Goldwurm, A La Rosa, G Labanti, C Laurent, P Mirabel, IF Quadrini, EM Ramsey, B Reglero, V Sabau, L Sacco, B Staubert, R Vigroux, L Weisskopf, MC Zdziarski, AA AF Ubertini, P Lebrun, F Di Cocco, G Bazzano, A Bird, AJ Broenstad, K Goldwurm, A La Rosa, G Labanti, C Laurent, P Mirabel, IF Quadrini, EM Ramsey, B Reglero, V Sabau, L Sacco, B Staubert, R Vigroux, L Weisskopf, MC Zdziarski, AA TI IBIS: The Imager on-board INTEGRAL SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE INTEGRAL; IBIS; gamma-ray imaging ID PICSIT DETECTOR; IBIS/PICSIT; CALIBRATION; PERFORMANCE; ISGRI AB The IBIS telescope is the high angular resolution gamma-ray imager on-board the INTEGRAL Observatory, successfully launched from Baikonur (Kazakhstan) the 17th of October 2002. This medium size ESA project, planned for a 2 year mission with possible extension to 5, is devoted to the observation of the gamma-ray sky in the energy range from 3 keV to 10 MeV (Winkler 2001). The IBIS imaging system is based on two independent solid state detector arrays optimised for low (15-1000 keV) and high (0.175-10.0 MeV) energies surrounded by an active VETO System. This high efficiency shield is essential to minimise the background induced by high energy particles in the highly excentric out of van Allen belt orbit. A Tungsten Coded Aperture Mask, 16 mm thick and similar to1 squared meter in dimension is the imaging device. The IBIS telescope will serve the scientific community at large providing a unique combination of unprecedented high energy wide field imaging capability coupled with broad band spectroscopy and high resolution timing over the energy range from X to gamma rays. To date the IBIS telescope is working nominally in orbit since more than 9 month. C1 CNR, Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy. CEN, F-91191 Gif Sur Yvette, France. IASF Bologna, I-40129 Bologna, Italy. Univ Southampton, Sch Phys & Astron, Southampton S017 1BJ, Hants, England. Univ Bergen, N-5007 Bergen, Norway. IASF Palermo, I-90146 Palermo, Italy. IASF Milano, I-20133 Milan, Italy. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Univ Valencia, E-46100 Burjassot, Spain. INTA, Madrid 28691, Spain. Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. Copernicus Astron Ctr, PL-00716 Warsaw, Poland. RP Ubertini, P (reprint author), CNR, Ist Astrofis Spaziale & Fis Cosm, via Fosso del Cavaliere 100, I-00133 Rome, Italy. EM ubertini@rm.iasf.cnr.it RI laurent, philippe/E-6211-2013; OI La Rosa, Giovanni/0000-0002-3931-2269; Labanti, Claudio/0000-0002-5086-3619; Bazzano, Angela/0000-0002-2017-4396 NR 17 TC 570 Z9 572 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2003 VL 411 IS 1 SI SI BP L131 EP L139 DI 10.1051/0004-6361:20031224 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737JZ UT WOS:000186227800023 ER PT J AU Vedrenne, G Roques, JP Schonfelder, V Mandrou, P Lichti, GG von Kienlin, A Cordier, B Schanne, S Knodlseder, J Skinner, G Jean, P Sanchez, F Caraveo, P Teegarden, B von Ballmoos, P Bouchet, L Paul, P Matteson, J Boggs, S Wunderer, C Leleux, P Weidenspointner, G Durouchoux, P Diehl, R Strong, A Casse, M Clair, MA Andre, Y AF Vedrenne, G Roques, JP Schonfelder, V Mandrou, P Lichti, GG von Kienlin, A Cordier, B Schanne, S Knodlseder, J Skinner, G Jean, P Sanchez, F Caraveo, P Teegarden, B von Ballmoos, P Bouchet, L Paul, P Matteson, J Boggs, S Wunderer, C Leleux, P Weidenspointner, G Durouchoux, P Diehl, R Strong, A Casse, M Clair, MA Andre, Y TI SPI: The spectrometer aboard INTEGRAL SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE instrumentation : detectors, spectrographs; techniques : spectroscopic ID GAMMA-RAY SPECTROMETERS; FRONT-END ELECTRONICS; PERFORMANCE; ASTROPHYSICS; CALIBRATION; ORBIT AB SPI is a high spectral resolution gamma-ray telescope on board the ESA mission INTEGRAL (International Gamma Ray Astrophysics Laboratory). It consists of an array of 19 closely packed germanium detectors surrounded by an active anticoincidence shield of BGO. The imaging capabilities of the instrument are obtained with a tungsten coded aperture mask located 1.7 m from the Ge array. The fully coded field-of-view is 16degrees, the partially coded field of view amounts to 31degrees, and the angular resolution is 2.5degrees. The energy range extends from 20 keV to 8 MeV with a typical energy resolution of 2.5 keV at 1.3 MeV. Here we present the general concept of the instrument followed by a brief description of each of the main subsystems. INTEGRAL was successfully launched in October 2002 and SPI is functioning extremely well. C1 UPS, CNRS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. CEA Saclay, DSM DAPNIA SAp, F-91191 Gif Sur Yvette, France. IASF, I-20133 Milan, Italy. Univ Valencia, IFIC, E-46100 Burjassot, Spain. Univ Catholique Louvain, Inst Phys Nucl, B-1348 Louvain, Belgium. Univ Calif San Diego, CASS, La Jolla, CA 92093 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. CNES CST, F-31401 Toulouse 4, France. RP Knodlseder, J (reprint author), UPS, CNRS, Ctr Etud Spatiale Rayonnements, BP 4346, F-31028 Toulouse 4, France. EM knodlseder@cesr.fr RI Sanchez, Filomeno/D-7859-2014; Boggs, Steven/E-4170-2015; OI Sanchez, Filomeno/0000-0003-0831-4744; Boggs, Steven/0000-0001-9567-4224; Caraveo, Patrizia/0000-0003-2478-8018 NR 21 TC 364 Z9 364 U1 1 U2 8 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 NOV PY 2003 VL 411 IS 1 SI SI BP L63 EP L70 DI 10.1051/0004-6361:20031482 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737JZ UT WOS:000186227800012 ER PT J AU Vilhu, O Hjalmarsdotter, L Zdziarski, AA Paizis, A McCollough, ML Beckmann, V Courvoisier, TJL Ebisawa, K Goldoni, P Hakala, P Hannikainen, D Kretschmar, P Westergaard, NJ AF Vilhu, O Hjalmarsdotter, L Zdziarski, AA Paizis, A McCollough, ML Beckmann, V Courvoisier, TJL Ebisawa, K Goldoni, P Hakala, P Hannikainen, D Kretschmar, P Westergaard, NJ TI First INTEGRAL observations of Cygnus X-3 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma rays : observations; radiation mechanisms : non-thermal; stars : individual : Cyg X-3; X-rays : binaries; X-rays : general; X-rays : stars ID X-RAY; X-1; DISCOVERY; PLASMAS AB We present the first INTEGRAL results on Cyg X-3 from the PV phase observations of the Cygnus region. The source was clearly detected by the JEM-X, ISGRI and SPI. The INTEGRAL observations were supported by simultaneous pointed RXTE observations. Their lightcurves folded over the 4.8 hour binary period are compatible with the mean RXTE/ASM and CGRO/BATSE light curves. We fit our broad-band X-ray/gamma-ray spectra with a physical model, which represents the first such published model for Cyg X-3. The main physical processes in the source are thermal Comptonization and Compton reflection with parameters similar to those found for black-hole binaries at high Eddington rates. C1 INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. Univ Helsinki Observ, Helsinki 00014, Finland. Centrum Astron M Kopernika, PL-00716 Warsaw, Poland. CNR, IASF, Sez Milano, I-20133 Milan, Italy. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. Observ Geneva, CH-1290 Sauverny, Switzerland. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Ctr Etud Saclay, DAPNIA, Serv Astrophys, F-91191 Gif Sur Yvette, France. Danish Space Res Inst, DK-2100 Copenhagen O, Denmark. RP Vilhu, O (reprint author), INTEGRAL Sci Data Ctr, Chemin Ecogia 16, CH-1290 Versoix, Switzerland. OI Kretschmar, Peter/0000-0001-9840-2048; Paizis, Adamantia/0000-0001-5067-0377 NR 27 TC 23 Z9 23 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2003 VL 411 IS 1 BP L405 EP L410 DI 10.1051/0004-6361:20031257 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737JZ UT WOS:000186227800066 ER PT J AU von Kienlin, A Beckmann, V Covino, S Gotz, D Lichti, GG Malesani, D Mereghetti, S Molinari, E Rau, A Shrader, CR Sturner, SJ Zerbi, F AF von Kienlin, A Beckmann, V Covino, S Gotz, D Lichti, GG Malesani, D Mereghetti, S Molinari, E Rau, A Shrader, CR Sturner, SJ Zerbi, F TI INTEGRAL results on GRB 030320: A long gamma-ray burst detected at the edge of the field of view SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma-ray bursts; GRB; gamma-ray astronomy; INTEGRAL; SPI; IBIS AB GRB 030320 is the 5th gamma-ray burst (GRB) detected by INTEGRAL in the field of view (FoV). It is so far the GRB with the largest off-axis angle with respect to the INTEGRAL pointing direction, near to the edge of the FoV of both main instruments, IBIS and SPI. Nevertheless, it was possible to determine its position and to extract spectra and fluxes. The GRB nature of the event was confirmed by an IPN triangulation. It is a similar to60 s long GRB with two prominent peaks separated by similar to 35 s. The spectral shape of the GRB is best represented by a single power law with a photon index Gamma similar or equal to 1.7. The peak flux in the 20 - 200 keV band is determined to similar to 5.7 photons cm(-2) s(-1) and the GRB fluence to 1.1 x 10(-5) erg cm(-2). Analysing the spectral evolution of the GRB, a "hard-to-soft" behaviour emerges. A search for an optical counterpart has been carried out, but none was found. C1 Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. CNR, Ist Astrofis Spaziale & Fis Cosm, Sez Milano G Occhialini, I-20133 Milan, Italy. Univ Studi Milano Bicocca, Dipartimento Fis, I-20126 Milan, Italy. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Space Res Assoc, Lanham, MD 20706 USA. INAF, Brera Astron Observ, Merate, LC, Italy. SISSA, ISAS, I-34014 Trieste, Italy. RP von Kienlin, A (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. OI Molinari, Emilio/0000-0002-1742-7735; Zerbi, Filippo Maria/0000-0002-9996-973X; MEREGHETTI, SANDRO/0000-0003-3259-7801; Covino, Stefano/0000-0001-9078-5507 NR 26 TC 9 Z9 9 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2003 VL 411 IS 1 BP L321 EP L325 DI 10.1051/0004-6361:20031232 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737JZ UT WOS:000186227800052 ER PT J AU Weidenspointner, G Kiener, J Gros, M Jean, P Teegarden, BJ Wunderer, C Reedy, RC Attie, D Diehl, R Ferguson, C Harris, MJ Knodlseder, J Leleux, P Lonjou, V Roques, JP Schonfelder, V Shrader, C Sturner, S Tatischeff, V Vedrenne, G AF Weidenspointner, G Kiener, J Gros, M Jean, P Teegarden, BJ Wunderer, C Reedy, RC Attie, D Diehl, R Ferguson, C Harris, MJ Knodlseder, J Leleux, P Lonjou, V Roques, JP Schonfelder, V Shrader, C Sturner, S Tatischeff, V Vedrenne, G TI First identification and modelling of SPI background lines SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE line : identification; instrumentation : miscellaneous; methods : data analysis; methods : numerical ID RAYS AB On Oct. 17, 2002, the ESA INTEGRAL observatory was launched into a highly elliptical orbit. SPI, a high resolution Ge spectrometer covering an energy range of 20-8000 keV, is one of its two main instruments. We use data recorded early in the mission (i.e. in March 2003) to characterize the instrumental background, in particular the many gamma-ray lines produced by cosmic-ray interactions in the instrument and spacecraft materials. More than 300 lines and spectral features are observed, for about 220 of which we provide identifications. An electronic version of this list, which will be updated continuously, is available for download at CESR. We also report first results from our efforts to model these lines by ab initio Monte Carlo simulation. C1 Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. NASA, Goddard Space Flight Ctr, LHEA, Greenbelt, MD 20771 USA. Univ Space Res Assoc, Seabrook, MD 20706 USA. CNRS, IN2P3, CSNSM, F-91405 Orsay, France. Univ Paris 11, F-91405 Orsay, France. Ctr Etud Nucl Saclay, DSM DAPNIA SAp, F-91191 Gif Sur Yvette, France. Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. Univ New Mexico, Albuquerque, NM 87131 USA. Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. Univ Catholique Louvain, Inst Phys Nucl, B-1348 Louvain, Belgium. RP Weidenspointner, G (reprint author), Ctr Etud Spatiale Rayonnements, 9 Ave Colonel Roche,BP 4346, F-31028 Toulouse 4, France. OI Reedy, Robert/0000-0002-2189-1303 NR 9 TC 40 Z9 40 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2003 VL 411 IS 1 BP L113 EP U10 DI 10.1051/0004-6361:20031209 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737JZ UT WOS:000186227800019 ER PT J AU Winkler, C Gehrels, N Schonfelder, V Roques, JP Strong, AW Wunderer, C Ubertini, P Lebrun, F Bazzano, A Del Santo, M Lund, N Westergaard, NJ Beckmann, V Kretschmar, P Mereghetti, S AF Winkler, C Gehrels, N Schonfelder, V Roques, JP Strong, AW Wunderer, C Ubertini, P Lebrun, F Bazzano, A Del Santo, M Lund, N Westergaard, NJ Beckmann, V Kretschmar, P Mereghetti, S TI First results from the INTEGRAL galactic plane scans SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE compact objects; high energy transients; nucleosynthesis ID JEM-X; RAY; SPECTROMETER; PERFORMANCE; DISCOVERY; SPI AB Scans of the Galactic plane performed at regular intervals constitute a key element of the guaranteed time observations of the INTEGRAL observing programme. These scans are done for two reasons: frequent monitoring of the Galactic plane in order to detect transient sources, and time resolved mapping of the Galactic plane in continuum and diffuse line emission. This paper describes first results obtained from the Galactic plane scans executed so far during the early phase (Dec. 2002-May 2003) of the nominal mission. C1 ESA, Estec, Res & Sci Support Dept, NL-2201 AZ Noordwijk, Netherlands. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. DSRI, DK-2100 Copenhagen OE, Denmark. MPE, D-85740 Garching, Germany. CNR, IASF, I-00133 Rome, Italy. Ctr Etud Spatiale Rayonnements, F-31029 Toulouse, France. ISDC, CH-1290 Versoix, Switzerland. CNR, IASF, I-20133 Milan, Italy. CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. RP Winkler, C (reprint author), ESA, Estec, Res & Sci Support Dept, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. EM Christoph.Winkler@rssd.esa.int; gehrels@gsfc.nasa.gov; vos@mpe.mpg.de; roques@sigma.o.cesr.cnes.fr; aws@mpe.mpg.de; cow@mpe.mpg.de; ubertini@rm.iasf.cnr.it; flebrun@cea.fr; nl@dsri.dk; njw@dsri.dk; Volker.Beckmann@obs.unige.ch; Peter.Kretschmar@obs.unige.ch; sandro@mi.iasf.cnr.it RI Gehrels, Neil/D-2971-2012; OI Del Santo, Melania/0000-0002-1793-1050; Kretschmar, Peter/0000-0001-9840-2048; MEREGHETTI, SANDRO/0000-0003-3259-7801; Bazzano, Angela/0000-0002-2017-4396 NR 17 TC 32 Z9 32 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 NOV PY 2003 VL 411 IS 1 SI SI BP L349 EP L355 DI 10.1051/0004-6361:20031325 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737JZ UT WOS:000186227800056 ER PT J AU Winkler, C Courvoisier, TJL Di Cocco, G Gehrels, N Gimenez, A Grebenev, S Hermsen, W Mas-Hese, JM Lebrun, F Lund, N Palumbo, GGC Paul, J Roques, JP Schnopper, H Schonfelder, V Sunyaev, R Teegarden, B Ubertini, P Vedrenne, G Dean, AJ AF Winkler, C Courvoisier, TJL Di Cocco, G Gehrels, N Gimenez, A Grebenev, S Hermsen, W Mas-Hese, JM Lebrun, F Lund, N Palumbo, GGC Paul, J Roques, JP Schnopper, H Schonfelder, V Sunyaev, R Teegarden, B Ubertini, P Vedrenne, G Dean, AJ TI The INTEGRAL mission SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma-ray astronomy; space observatory AB The ESA observatory INTEGRAL (International Gamma-Ray Astrophysics Laboratory) is dedicated to the fine spectroscopy (2.5 keV FWHM @ 1 MeV) and fine imaging (angular resolution: 12 arcmin FWHM) of celestial gamma-ray sources in the energy range 15 keV to 10 MeV with concurrent source monitoring in the X-ray (3-35 keV) and optical (V-band, 550 nm) energy ranges. INTEGRAL carries two main gamma-ray instruments, the spectrometer SPI (Vedrenne et al. 2003)-optimized for the high-resolution gamma-ray line spectroscopy (20 keV-8 MeV), and the imager IBIS (Ubertini et al. 2003)-optimized for high-angular resolution imaging (15 keV-10 MeV). Two monitors, JEM-X (Lund et al. 2003) in the (3-35) keV X-ray band, and OMC (Mas-Hesse et al. 2003) in optical Johnson V-band complement the payload. The ground segment includes the Mission Operations Centre at ESOC, ESA and NASA ground stations, the Science Operations Centre at ESTEC and the Science Data Centre near Geneva. INTEGRAL was launched on 17 October 2002. The observing programme is well underway and sky exposure (until June 2003) reaches similar to1800 ks in the Galactic plane. The prospects are excellent for the scientific community to observe the high energy sky using state-of-the-art gamma-ray imaging and spectroscopy. This paper presents a high-level overview of INTEGRAL. C1 ESA, Estec, Res & Sci Support Dept, NL-2201 AZ Noordwijk, Netherlands. INTEGRAL, Sci Data Ctr, CH-1290 Versoix, Switzerland. CNR, IASF, Sez Bologna, I-40129 Bologna, Italy. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Space Res Inst, Moscow 117810, Russia. SRON Utrecht, NL-3584 CA Utrecht, Netherlands. LAEFF INTA, Madrid 28080, Spain. CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. DSRI, DK-2100 Copenhagen OE, Denmark. Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. Ctr Etud Spatiale Rayonnements, F-31029 Toulouse, France. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. CNR, IASF, I-00133 Rome, Italy. Max Planck Inst Astrophys, D-85741 Garching, Germany. Univ Southampton, Dept Phys, Astron Grp, Southampton SO17 1BJ, Hants, England. CSIC, INTA, Ctr Astrobiol, Torrejon De Ardoz 28850, Spain. Observ Geneva, CH-1290 Sauverny, Switzerland. RP Winkler, C (reprint author), ESA, Estec, Res & Sci Support Dept, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. EM Christoph.Winkler@rssd.esa.int RI Gehrels, Neil/D-2971-2012; Mas-Hesse, J. Miguel /K-6805-2014 OI Mas-Hesse, J. Miguel /0000-0002-8823-9723 NR 13 TC 668 Z9 675 U1 2 U2 11 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 NOV PY 2003 VL 411 IS 1 SI SI BP L1 EP L6 DI 10.1051/0004-6361:20031288 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737JZ UT WOS:000186227800002 ER PT J AU Mennella, A Bersanelli, M Seiffert, M Kettle, D Roddis, N Wilkinson, A Meinhold, P AF Mennella, A Bersanelli, M Seiffert, M Kettle, D Roddis, N Wilkinson, A Meinhold, P TI Offset balancing in pseudo-correlation radiometers for CMB measurements SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology : cosmic microwave background, observations; instrumentation : detectors; methods : analytical ID DESIGN; IMPLEMENTATION; FLUCTUATIONS; FREQUENCY; PLANCK; NOISE AB Radiometeric CMB measurements need to be highly stable and this stability is best obtained with differential receivers. The residual 1/f noise in the differential output is strongly dependent on the radiometer input offset which can be cancelled using various balancing strategies. In this paper we discuss a software method implemented in the PLANCK-LFI pseudocorrelation receivers which uses a tunable gain modulation factor, r, in the sky-load difference. Numerical simulations and experimental data show how proper tuning of the parameter r ensures a very stable differential output with knee frequencies of the order of few mHz. Various approaches to calculate r using the radiometer total power data are discussed with some examples relevant to PLANCK-LFI. Although the paper focuses on pseudo-correlation receivers and the examples are relative to PLANCK-LFI, the proposed method and its analysis is general and can be applied to a large class of differential radiometric receivers. C1 CNR, IASF, Sez Milano, I-20133 Milan, Italy. Univ Milan, I-20133 Milan, Italy. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. RP Mennella, A (reprint author), CNR, IASF, Sez Milano, Via Bassini 15, I-20133 Milan, Italy. NR 15 TC 31 Z9 32 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2003 VL 410 IS 3 BP 1089 EP 1100 DI 10.1051/0004-6361:20031266 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 733GH UT WOS:000185991200040 ER PT J AU Stecker, FW AF Stecker, FW TI Constraints on Lorentz invariance violating quantum gravity and large extra dimensions models using high energy gamma-ray observations SO ASTROPARTICLE PHYSICS LA English DT Article DE gamma-rays; BL Lac objects; background radiation; infrared; Lorentz invariance; quantum gravity ID CRAB-NEBULA; TEV; SPECTRUM; LIMITS; MARKARIAN-501; ABSORPTION; SYSTEM; TESTS; FLARE; LIGHT AB Observations of the multi-TeV spectra of the nearby BL objects Mkn 421 and Mkn 501 exhibit the high energy cutoffs predicted to be the result of intergalactic annihilation interactions, primarily with infrared photons having a flux level as determined by various astronomical observations. After correction for this absorption effect, the derived intrinsic spectra of these multi-TeV sources can be explained within the framework of simple synchrotron self-Compton emission models. Stecker and Glashow have shown that the existence of such annihilations via electron-positron pair production interactions up to an energy of 20 TeV puts strong constraints on Lorentz invariance violation. Such constraints have important implications for Lorentz invariance violating (LIV) quantum gravity models as well as LIV models involving large extra dimensions. We also discuss the implications of observations of high energy gamma-rays from the Crab Nebula on constraining quantum gravity models. (C) 2003 Elsevier B.V. All rights reserved. C1 NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Stecker, FW (reprint author), NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Code 661, Greenbelt, MD 20771 USA. EM floyd.w.steeker@nasa.gov RI Stecker, Floyd/D-3169-2012 NR 25 TC 29 Z9 29 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-6505 EI 1873-2852 J9 ASTROPART PHYS JI Astropart Phys. PD NOV PY 2003 VL 20 IS 2 BP 85 EP 90 DI 10.1016/j.astropartphys.2003.08.006 PG 6 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 740EG UT WOS:000186389100001 ER PT J AU Davis, DS Miller, NA Mushotzky, RF AF Davis, DS Miller, NA Mushotzky, RF TI Chandra observations of point sources in A2255 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : clusters : general; galaxies : clusters : individual (A2255); intergalactic medium; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; EARLY-TYPE GALAXIES; X-RAY SOURCES; COOLING FLOWS; RICH CLUSTERS; STAR-FORMATION; RADIO-SOURCES; SAMPLE; LUMINOSITY; ABELL-2255 AB In our search for "hidden'' active galactic nuclei (AGNs), we present results from a Chandra observation of the nearby cluster A2255. Eight cluster galaxies are associated with pointlike X-ray emission, and we classify these galaxies based on their X-ray, radio, and optical properties. At least three are associated with AGNs with no optical signatures of nuclear activity, with a further two being potential AGNs. Of the potential AGNs, one corresponds to a galaxy with a post-starburst optical spectrum. The remaining three X-ray detected cluster galaxies consist of two starbursts and an elliptical with luminous hot gas. Of the eight cluster galaxies, five are associated with luminous (massive) galaxies, and the remaining three lie in much lower luminosity systems. We note that the use of X-ray-to-optical flux ratios for classification of X-ray sources is often misleading and strengthens the claim that the fraction of cluster galaxies hosting an AGN based on optical data is significantly lower than the fraction based on X-ray and radio data. C1 High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Dept Phys, Joint Ctr Astrophys, Baltimore, MD 21250 USA. NASA, Goddard Space Flight Ctr, UV Opt Branch, Greenbelt, MD 20771 USA. RP Davis, DS (reprint author), High Energy Astrophys Lab, Code 661, Greenbelt, MD 20771 USA. NR 54 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 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2003 VL 597 IS 1 BP 202 EP 209 DI 10.1086/378384 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 736KW UT WOS:000186170800018 ER PT J AU Blum, RD Ramirez, SV Sellgren, K Olsen, K AF Blum, RD Ramirez, SV Sellgren, K Olsen, K TI Really cool stars and the star formation history at the Galactic center SO ASTROPHYSICAL JOURNAL LA English DT Review DE Galaxy : center; stars : AGB and post-AGB; stars : late-type; supergiants ID NEAR-INFRARED SPECTRA; BAND LUMINOSITY FUNCTION; SUPERMASSIVE BLACK-HOLE; INITIAL MASS FUNCTION; MILKY-WAY; CHEMICAL-COMPOSITION; RED GIANTS; SUPER-GIANTS; EFFECTIVE TEMPERATURES; METALLICITY GRADIENT AB We present lambda/Deltalambda = 550-1200 near-infrared H and K spectra for a magnitude-limited sample of 79 asymptotic giant branch and cool supergiant stars in the central approximate to5 pc (diameter) of the Galaxy. We use a set of similar spectra obtained for solar neighborhood stars with known T-eff and M-bol that is in the same range as the Galactic center (GC) sample to derive T-eff and M-bol for the GC sample. We then construct the H-R diagram for the GC sample. Using an automated maximum likelihood routine, we derive a coarse star formation history of the GC. We find that (1) roughly 75% of the stars formed in the central few parsecs are older than 5 Gyr; (2) the star formation rate (SFR) is variable over time, with a roughly 4 times higher SFR in the last 100 Myr compared to the average SFR; (3) our model can match dynamical limits on the total mass of stars formed only by limiting the initial mass function to masses above 0.7 M. (this could be a signature of mass segregation or of the bias toward massive star formation from the unique star formation conditions in the GC); (4) blue supergiants account for 12% of the total sample observed, and the ratio of red to blue super-giants is roughly 1.5; and (5) models with isochrones with [Fe/H] = 0.0 over all ages fit the stars in our H-R diagram better than models with lower [Fe/H] in the oldest age bins, consistent with the finding of Ramirez et al. that stars with ages between 10 Myr and 1 Gyr have solar [Fe/H]. C1 Cerro Tololo Interamer Observ, La Serena, Chile. CALTECH, Jet Prop Lab, SIRTF Sci Ctr, Pasadena, CA 91125 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. RP Blum, RD (reprint author), Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile. NR 115 TC 73 Z9 73 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2003 VL 597 IS 1 BP 323 EP 346 DI 10.1086/378380 PN 1 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 736KW UT WOS:000186170800030 ER PT J AU Laming, JM Hwang, U AF Laming, JM Hwang, U TI On the determination of ejecta structure and explosion asymmetry from the X-ray knots of Cassiopeia A SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; ISM : individual (Cassiopeia A); supernova remnants; X-rays : ISM ID SUPERNOVA REMNANT CASSIOPEIA; CORE-COLLAPSE SUPERNOVAE; INTERSTELLAR CLOUDS; HYDRODYNAMIC INTERACTION; PARTICLE-ACCELERATION; IONIZATION BALANCE; MASSIVE STARS; NOVA REMNANT; EMISSION; EVOLUTION AB We present a detailed analysis of Chandra X-ray spectra from individual ejecta knots in the supernova remnant Cassiopeia A. The spectra are fitted to give the electron temperature T-e and (single) ionization age n(e)t. These quantities are compared with the predictions of self-similar hydrodynamic models incorporating time-dependent ionization and radiation losses and Coulomb electron-ion equilibration behind the reverse shock for a variety of different ejecta density profiles described by a uniform-density core and a power-law envelope. We find that the ejecta close to the "jet'' region in the northeast, but not actually in the jet itself, have a systematically shallower outer envelope than ejecta elsewhere in the remnant, and we interpret this as being due to more energy of the initial explosion being directed in this polar direction as opposed to equatorially. The degree of asymmetry we infer is at the low end of that generally modeled in asymmetric core-collapse simulations and may possibly be used to rule out highly asymmetric explosion models. C1 USN, Res Lab, Washington, DC 20375 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland, College Pk, MD 20742 USA. RP Laming, JM (reprint author), USN, Res Lab, Code 7674L, Washington, DC 20375 USA. NR 72 TC 99 Z9 99 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2003 VL 597 IS 1 BP 347 EP 361 DI 10.1086/378268 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 736KW UT WOS:000186170800031 ER PT J AU Hwang, U Laming, JM AF Hwang, U Laming, JM TI Where was the iron synthesized in Cassiopeia A? SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : abundances; ISM : individual (Cassiopeia A); nuclear reactions, nucleosynthesis, abundances; supernova remnants; supernovae : general ID CORE-COLLAPSE SUPERNOVAE; INTERSTELLAR CLOUDS; HYDRODYNAMIC INTERACTION; ACCELERATED ELECTRONS; SHOCKS; TI-44; NUCLEOSYNTHESIS; EXPLOSIONS; REMNANTS; EJECTA AB We investigate the properties of Fe-rich knots on the east limb of the Cassiopeia A supernova remnant using observations with Chandra/ACIS and analysis methods developed in a companion paper. We use the fitted ionization age and electron temperature of the knots to constrain the ejecta density profile and the Lagrangian mass coordinates of the knots. Fe-rich knots that also have strong emission from Si, S, Ar, and Ca are clustered around mass coordinates q similar or equal to 0.35-0.4 in the shocked ejecta; for ejecta mass 2 M., this places the knots 0.7-0.8 M. out from the center (or 2-2.1 M., allowing for a 1.3 M. compact object). We also find an Fe clump that is evidently devoid of line emission from lower mass elements, as would be expected if it were the product of alpha-rich freezeout; the mass coordinate of this clump is similar to those of the other Fe knots. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland, College Pk, MD 20742 USA. USN, Res Lab, Washington, DC 20375 USA. RP Hwang, U (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 48 TC 71 Z9 72 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2003 VL 597 IS 1 BP 362 EP 373 DI 10.1086/378269 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 736KW UT WOS:000186170800032 ER PT J AU Mukai, K Hellier, C Madejski, G Patterson, J Skillman, DR AF Mukai, K Hellier, C Madejski, G Patterson, J Skillman, DR TI X-ray variability of the magnetic cataclysmic variable V1432 Aquilae and the Seyfert galaxy NGC 6814 SO ASTROPHYSICAL JOURNAL LA English DT Article ID HUBBLE-SPACE-TELESCOPE; RX J1940.1-1025; INTERMEDIATE POLARS; ACCRETION GEOMETRY; WHITE-DWARF; AM; ASTRONOMY; ECLIPSES; BINARIES; BEPPOSAX AB V1432 Aquilae (= RX J1940.2 - 1025) is the X-ray - bright, eclipsing magnetic cataclysmic variable similar to37' away from the Seyfert galaxy NGC 6814. Because of a 0.3% difference between the orbital (12,116.3 s) and the spin ( 12,150 s) periods, the accretion geometry changes over the similar to 50 day beat period. Here we report the results of a Rossi X-Ray Timing Explorer campaign to observe the eclipse 25 times, as well as of archival observations with ASCA and BeppoSAX. Having confirmed that the eclipse is indeed caused by the secondary, we use the eclipse timings and profiles to map the accretion geometry as a function of the beat phase. We find that the accretion region is compact and that it moves relative to the center of white dwarf on the beat period. The amplitude of this movement suggests a low-mass white dwarf, in contrast to the high mass previously estimated from its X-ray spectrum. The size of the X-ray emission region appears to be larger than in other eclipsing magnetic cataclysmic variables. We also report on the RXTE data as well as the long-term behavior of NGC 6814, indicating flux variability by a factor of at least 10 on timescales of years. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Keele, Dept Phys, Keele ST5 5BG, Staffs, England. Stanford Linear Accelerator Ctr, Glast Grp, Menlo Pk, CA 94025 USA. Columbia Univ, Dept Astron, New York, NY 10027 USA. Ctr Backyard Astrophys E, Laurel, MD 20723 USA. Univ Space Res Assoc, Columbia, MD USA. Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. RP Mukai, K (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. EM mukai@milkyway.gsfc.nasa.gov RI Skillman, David/C-8995-2013 NR 44 TC 16 Z9 16 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2003 VL 597 IS 1 BP 479 EP 493 DI 10.1086/378318 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 736KW UT WOS:000186170800043 ER PT J AU Butt, YM Benaglia, P Combi, JA Corcoran, M Dame, TM Drake, J Bernado, MK Milne, P Miniati, F Pohl, M Reimer, O Romero, GE Rupen, M AF Butt, YM Benaglia, P Combi, JA Corcoran, M Dame, TM Drake, J Bernado, MK Milne, P Miniati, F Pohl, M Reimer, O Romero, GE Rupen, M TI Chandra/Very Large Array follow-up of TeV J2032+4131, the only unidentified TeV gamma-ray source SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : observations ID STARBURST GALAXY NGC-253; COSMIC-RAYS; CYGNUS OB2; SUPERNOVA-REMNANTS; PARTICLE-ACCELERATION; STELLAR WINDS; SHOCK ACCELERATION; GALACTIC PLANE; MASSIVE STARS; MILKY-WAY AB The High Energy Gamma Ray Astronomy (HEGRA) Cerenkov telescope array group recently reported a steady and extended unidentified TeV gamma-ray source lying at the outskirts of Cygnus OB2. This is the most massive stellar association known in the Galaxy, estimated to contain similar to 2600 OB-type members alone. It has been previously argued that the large-scale shocks and turbulence induced by the multiple interacting supersonic winds from the many young stars in such associations may play a role in accelerating Galactic cosmic rays. Indeed, Cyg OB2 also coincides with the nonvariable MeV - GeV range unidentified EGRET source, 3EG 2033+ 4118. We report on the near-simultaneous follow-up observations of the extended TeV source region with the Chandra X-Ray Observatory and the Very Large Array radio telescope, obtained in order to explore this possibility. Analysis of the CO, H I, and IRAS 100 mum emissions shows that the TeV source region coincides with an outlying subgroup of powerful OB stars that have evacuated or destroyed much of the ambient atomic, molecular, and dust material and that may be related to the very high energy emissions. An interesting supernova-remnant - like structure is also revealed near the TeV source region in the CO, H I, and radio emission maps. Applying a numerical simulation that accurately tracks the radio to gamma-ray emission from primary hadrons as well as primary and secondary e(+/-), we find that the broadband spectrum of the TeV source region favors a predominantly nucleonic - rather than electronic - origin for the high-energy flux, although deeper X-ray and radio observations will help confirm this. A very reasonable, similar to 0.1%, conversion efficiency of Cyg OB2' s extreme stellar wind mechanical luminosity to nucleonic acceleration to similar to PeV (10(15) eV) energies is sufficient to explain the multifrequency emissions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Argentino Radioastron, RA-1894 Buenos Aires, DF, Argentina. Univ Space Res Assoc, Seabrook, MD 20706 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Max Planck Inst Astrophys, D-85741 Garching, Germany. Ruhr Univ Bochum, Inst Theoret Phys, D-44780 Bochum, Germany. Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Butt, YM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Reimer, Olaf/A-3117-2013 OI Reimer, Olaf/0000-0001-6953-1385 NR 75 TC 55 Z9 55 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2003 VL 597 IS 1 BP 494 EP 512 DI 10.1086/378121 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 736KW UT WOS:000186170800044 ER PT J AU Thommes, EW Lissauer, JJ AF Thommes, EW Lissauer, JJ TI Resonant inclination excitation of migrating giant planets SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planetary systems : protoplanetary disks; solar system : formation ID BETA-PICTORIS; ORBITAL RESONANCES; SOLAR NEBULA; DISKS; GROWTH; PROTOPLANETS; EXPLANATION; EVOLUTION; ACCRETION; MIRANDA AB The observed orbits of extrasolar planets suggest that many giant planets migrate a considerable distance toward their parent star as a result of interactions with the protoplanetary disk and that some of these planets become trapped in eccentricity-exciting mean motion resonances with one another during this migration. Using three-dimensional numerical simulations, we find that as long as the timescale for damping of the planets' eccentricities by the disk is close to or longer than the disk-induced migration timescale and the outer planet is more than half the mass of the inner, resonant inclination excitation will also occur. Neither the addition of a ( simple, fixed) disk potential nor the introduction of a massive inner planetary system inhibit entry into the inclination resonance. Therefore, such a mechanism may not be uncommon in the early evolution of a planetary system, and a significant fraction of exoplanetary systemsmay turn out to be non-coplanar. C1 Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Thommes, EW (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. NR 46 TC 70 Z9 70 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2003 VL 597 IS 1 BP 566 EP 580 DI 10.1086/378317 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 736KW UT WOS:000186170800049 ER PT J AU Richardson, LJ Deming, D Seager, S AF Richardson, LJ Deming, D Seager, S TI Infrared observations during the secondary eclipse of HD 209458B. II. Strong limits on the infrared spectrum near 2.2 mu m SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; infrared : stars; planetary systems; stars : individual (HD 209458); techniques : photometric ID EXTRASOLAR GIANT PLANETS; TRANSITING PLANET; ATMOSPHERES; TELESCOPE; ABSORPTION; HD-209458 AB We report observations of the transiting extrasolar planet, HD 209458b, designed to detect the secondary eclipse. We employ the method of "occultation spectroscopy,'' which searches in combined light ( star and planet) for the disappearance and reappearance of weak infrared spectral features due to the planet as it passes behind the star and reappears. Our observations cover two predicted secondary eclipse events, and we obtained 1036 individual spectra of the HD 209458 system using the SpeX instrument at the NASA Infrared Telescope Facility in 2001 September. Our spectra extend from 1.9 to 4.2 mum with a resolution (lambda/Deltalambda) of 1500. We have searched for a continuum peak near 2.2 mum (caused by CO and H2O absorption bands), as predicted by some models of the planetary atmosphere to be similar to 6 x 10(-4) of the stellar flux, but no such peak is detected at a level of similar to 3 x 10(-4) of the stellar flux. Our results represent the strongest limits on the infrared spectrum of the planet to date and carry significant implications for understanding the planetary atmosphere. In particular, some models that assume that the stellar irradiation is reradiated entirely on the substellar hemisphere predict a flux peak that is inconsistent with our observations. Several physical mechanisms can improve agreement with our observations, including the redistribution of heat by global circulation, a nearly isothermal atmosphere, and the presence of a high cloud. C1 NASA, Goddard Space Flight Ctr, Planetary Syst Branch, Greenbelt, MD 20771 USA. Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA. Univ Colorado, Dept Phys, Boulder, CO 80309 USA. Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. RP Richardson, LJ (reprint author), NASA, Goddard Space Flight Ctr, Planetary Syst Branch, Code 693, Greenbelt, MD 20771 USA. NR 33 TC 61 Z9 62 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2003 VL 597 IS 1 BP 581 EP 589 DI 10.1086/378390 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 736KW UT WOS:000186170800050 ER PT J AU Danchi, WC Deming, D Kuchner, MJ Seager, S AF Danchi, WC Deming, D Kuchner, MJ Seager, S TI Detection of close-in extrasolar giant planets using the Fourier-Kelvin Stellar Interferometer SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems; stars : individual (55 Cancri); techniques : high angular resolution; techniques : interferometric ID STARS; SPECTRA AB We evaluate the direct detection of extrasolar giant planets with a two-aperture nulling infrared interferometer, working at angles and using a new theta < λ/2B "ratio-of-two-wavelengths" technique. Simple arguments suggest that interferometric detection and characterization should be quite possible for planets much closer than the conventional inner working angle, or angular resolution limit. We show that the peak signal from a nulling infrared interferometer of baseline &LSIM;40 m will often occur "inside the null" and that the signal variations from path difference fluctuations will cancel to first order in the ratio of two wavelengths. Using a new interferometer simulation code, we evaluate the detectability of all the known extrasolar planets as observed using this two-color method with the proposed Fourier-Kelvin Stellar Interferometer (FKSI). In its minimum configuration FKSI uses two 0.5 m apertures on a 12.5 m baseline and a &PLUSMN;20&DEG; field of regard. We predict that &SIM;7 known extrasolar planets are directly detectable using FKSI, with low-resolution spectroscopy (R &SIM; 20) being possible in the most favorable cases. Spaceborne direct detection of extrasolar giant planets is possible with &SIM;12 m baselines and does not require the much longer baselines provided by formation flying. C1 NASA, Goddard Space Flight Ctr, Infrared Astrophys Branch, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Planetary Syst Branch, Greenbelt, MD 20771 USA. Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. RP Danchi, WC (reprint author), NASA, Goddard Space Flight Ctr, Infrared Astrophys Branch, Code 685, Greenbelt, MD 20771 USA. RI Kuchner, Marc/E-2288-2012 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 NOV 1 PY 2003 VL 597 IS 1 BP L57 EP L60 DI 10.1086/379640 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 736LF UT WOS:000186171700015 ER PT J AU Jones, GH Balogh, A Russell, CT Dougherty, MK AF Jones, GH Balogh, A Russell, CT Dougherty, MK TI Possible distortion of the interplanetary magnetic field by the dust trail of comet 122P/de Vico SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets : general; comets : individual (122P/de Vico); interplanetary medium; meteors, meteoroids ID SOLAR-WIND; STATISTICAL PROPERTIES; ENHANCEMENTS; ENCOUNTER; AU AB Interplanetary field enhancements are unexplained localized increases in the heliospheric magnetic field magnitude. Four such enhancements, detected by the Pioneer Venus Orbiter and Ulysses spacecraft, have been found to be very close to the orbital plane of comet 122P/de Vico. Analysis of the magnetic field during these events reveals that the field perturbations were close to those expected if the interplanetary magnetic field draped at the comet's orbit and that the field enhancements represent crossings of a "sheet" of disturbed solar wind in the comet's orbital plane. The results suggest that a dense dust stream may occupy at least part of the orbit of de Vico and that its effects on the solar wind are apparent almost 1.4 AU downstream. One field enhancement suggests the existence of an annulus of dust extending sunward of the dust trail itself. C1 Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Space & Atmospher Phys Grp, London SW7 2BW, England. Univ Calif Los Angeles, Dept Earth & Space Sci, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. RP Jones, GH (reprint author), CALTECH, Jet Prop Lab, MS 169-506,4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Jones, Geraint/C-1682-2008; OI Jones, Geraint/0000-0002-5859-1136 NR 16 TC 4 Z9 4 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 NOV 1 PY 2003 VL 597 IS 1 BP L61 EP L64 DI 10.1086/379750 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 736LF UT WOS:000186171700016 ER PT J AU Landi, E Bhatia, AK AF Landi, E Bhatia, AK TI Atomic data and spectral line intensities for S XI SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE atomic data; plasmas ID EXTREME-ULTRAVIOLET SPECTRUM; ELECTRON-IMPACT EXCITATION; WAVE COLLISION STRENGTHS; SOLAR ACTIVE-REGION; CARBON-LIKE IONS; C-LIKE IONS; EMISSION-LINES; OSCILLATOR-STRENGTHS; CROSS-SECTIONS; FORBIDDEN TRANSITIONS AB Electron impact collision strengths, energy levels, oscillator strengths, and spontaneous radiative decay rates are calculated for S XI. The configurations included are 2s(2)2p(2), 2s2p(3), 2p(4), 2s(2)2p3iota, and 2s(2)2p4iota (iota = s, p, d), giving rise to 72 fine-structure levels in intermediate coupling. Collision strengths are calculated at five incident energies, 32, 60, 90, 120, and 150 ryd. Excitation rate coefficients are calculated as a function of electron temperature by assuming a Maxwellian electron velocity distribution. Using the excitation rate coefficients and the radiative transition rates, statistical equilibrium equations for level populations are solved. The effects of resonances, proton rates, photoexcitation, and cascades on level populations have been investigated. The predicted S XI line intensities are compared with EUV and UV observations of the quiet and active Sun. C1 Artep Inc, Ellicott City, MD USA. USN, Res Lab, Washington, DC 20375 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Landi, E (reprint author), Artep Inc, Ellicott City, MD USA. RI Landi, Enrico/H-4493-2011 NR 55 TC 3 Z9 3 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD NOV PY 2003 VL 149 IS 1 BP 251 EP 263 DI 10.1086/378717 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 736LL UT WOS:000186172200011 ER PT J AU Bhatia, AK Landi, E AF Bhatia, AK Landi, E TI Atomic data and spectral line intensities for SiVIII SO ATOMIC DATA AND NUCLEAR DATA TABLES LA English DT Article ID EXTREME-ULTRAVIOLET SPECTRUM; ELECTRON-IMPACT EXCITATION; EMISSION-LINES; COLLISION STRENGTHS; SOLAR SPECTRUM; S-X; OSCILLATOR-STRENGTHS; RATE COEFFICIENTS; CROSS-SECTIONS; IONS AB Electron impact collision strengths, energy levels, oscillator strengths, and spontaneous radiative decay rates are calculated for Si VIII. The configurations used are 2s(2)2p(3), 2s2p(4), 2p(5), 2s(2)2p(2)s, 2s(2)2p(2)3p, and 2s(2)2p(2)3d giving rise to 72 fine-structure levels in intermediate coupling. Collision strengths are calculated at four incident energies, 20, 40, 60, and 80 Ry. Excitation rate coefficients are calculated by assuming a Maxwellian electron velocity distribution at an electron temperature of logT(e)(K) = 5.9, corresponding to maximum abundance of Si VIII. Using the excitation rate coefficients and the radiative transition rates, statistical equilibrium equations for level populations are solved at electron densities covering the range of 10(8)-10(14) cm(-3). Relative spectral line intensities are calculated. Proton excitation rates between the lowest five levels have been included in the statistical equilibrium equations. The predicted Si VIII line intensities are compared with SERTS rocket observations of a solar active region and SUMER (SOHO) observations of the quiet sun. (C) 2003 Elsevier Inc. All rights reserved. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. USN, Res Lab, Washington, DC 20375 USA. RP Bhatia, AK (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Landi, Enrico/H-4493-2011 NR 40 TC 7 Z9 7 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 0092-640X J9 ATOM DATA NUCL DATA JI Atom. Data Nucl. Data Tables PD NOV PY 2003 VL 85 IS 2 BP 317 EP 376 DI 10.1016/j.adt.2003.08.002 PG 60 WC Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Physics GA 752JB UT WOS:000187156400004 ER PT J AU Tang, XD Tao, G Joshi, SM AF Tang, XD Tao, G Joshi, SM TI Adaptive actuator failure compensation for parametric strict feedback systems and an aircraft application SO AUTOMATICA LA English DT Article DE actuator failure; adaptive control; aircraft dynamics; failure compensation; nonlinear systems; output tracking; stability ID FAULT-DIAGNOSIS AB Adaptive actuator failure compensation for parametric-strict-feedback systems is studied under different system structure conditions. Adaptive state feedback control schemes are developed, which ensure asymptotic output tracking and closed-loop signal boundedness. An adaptive control scheme is applied to a twin otter aircraft longitudinal nonlinear dynamics model in the presence of unknown failures in a two-segment elevator servomechanism. Simulation results verify the effectiveness of adaptive actuator failure compensation for desired system performance. (C) 2003 Elsevier Ltd. All rights reserved. C1 Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22903 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Tao, G (reprint author), Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22903 USA. EM gt9s@virginia.edu NR 12 TC 97 Z9 105 U1 1 U2 11 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0005-1098 J9 AUTOMATICA JI Automatica PD NOV PY 2003 VL 39 IS 11 BP 1975 EP 1982 DI 10.1016/S0005-1098(03)00219-X PG 8 WC Automation & Control Systems; Engineering, Electrical & Electronic SC Automation & Control Systems; Engineering GA 730EG UT WOS:000185815800014 ER PT J AU Conkin, J Powell, MR Gernhardt, ML AF Conkin, J Powell, MR Gernhardt, ML TI Age affects severity of venous gas emboli on decompression from 14.7 to 4.3 psia SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE probability models; micronuclei; aviator decompression sickness ID MAXIMAL OXYGEN-UPTAKE; MENSTRUAL HISTORY; SICKNESS; ALTITUDE; BUBBLES; RISK; EXERCISE AB Introduction: Variables that define who we are, such as age, weight, and fitness level influence the risk of decompression sickness (DCS) and venous gas emboli (VGE) from diving and aviation decompressions. We focus on age since astronauts that perform space walks are approximately 10 yr older than our test subjects. Our null hypothesis is that age is not statistically associated with the VGE outcomes from decompression to 4.3 psia. Methods: Our data are from 7 different NASA tests where 188 men and 50 women performed light exercise at 4.3 psia for planned exposures no less than 4 h. Prebreathe (PB) time on 100% oxygen ranged from 150-270 min, including ascent time, with exercise of different intensity and length being performed during the PB in four of the seven tests with 150 min of PB. Subjects were monitored for VGE in the pulmonary artery using a Doppler ultrasound bubble detector for a 4-min period every 12 min. There were six design variables; the presence or absence of lower body adynamia and five PB variables; plus five concomitant variables on physical characteristics: age, weight, height, body mass index, and gender that were available for logistic regression (LR). We used LR models for the probability of DCS and VGE, and multinomial logit (ML) models for the probability of Spencer VGE Grades 0-IV at exposure times of 61, 95, 131, 183 min, and for the entire exposure. Results: Age was significantly associated with VGE in both the LR and ML models, so we reject the null hypothesis. Lower body adynamia was significant for all responses. Conclusions: Our selection of tests produced a wide range of the explanatory variables, but only age, lower body adynamia, height, and total PB time was helpful in various combinations to model the probability of DCS and VGE. C1 NASA, Lyndon B Johnson Space Ctr, Environm Physiol Lab, Human Adaptat & Countermeasures Off, Houston, TX 77058 USA. RP Conkin, J (reprint author), NASA, Lyndon B Johnson Space Ctr, Environm Physiol Lab, Human Adaptat & Countermeasures Off, SK2,2101 NASA Rd 1, Houston, TX 77058 USA. NR 29 TC 7 Z9 7 U1 1 U2 2 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 NOV PY 2003 VL 74 IS 11 BP 1142 EP 1150 PG 9 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 738TA UT WOS:000186302900003 PM 14620470 ER PT J AU Waliser, DE Jin, K Kang, IS Stern, WF Schubert, SD Wu, MLC Lau, KM Lee, MI Krishnamurthy, V Kitoh, A Meehl, GA Galin, VY Satyan, V Mandke, SK Wu, G Liu, Y Park, CK AF Waliser, DE Jin, K Kang, IS Stern, WF Schubert, SD Wu, MLC Lau, KM Lee, MI Krishnamurthy, V Kitoh, A Meehl, GA Galin, VY Satyan, V Mandke, SK Wu, G Liu, Y Park, CK TI AGCM simulations of intraseasonal variability associated with the Asian summer monsoon SO CLIMATE DYNAMICS LA English DT Review ID MADDEN-JULIAN OSCILLATION; GENERAL-CIRCULATION MODEL; OUTGOING LONGWAVE RADIATION; COMMUNITY CLIMATE MODEL; INDIAN MONSOON; INTERANNUAL VARIABILITY; SURFACE-TEMPERATURE; EL-NINO; HORIZONTAL RESOLUTION; TROPICAL CONVECTION AB The intraseasonal variability associated with the Asian summer monsoon as simulated by a number of atmospheric general circulation models (AGCMs) are analyzed and assessed against observations. The model data comes from the Monsoon GCM Intercomparison project initiated by the CLIVAR/Asian-Australian Monsoon Panel. Ten GCM groups, i.e., the Center for Ocean-Land-Atmosphere Studies (COLA), Institute of Numerical Mathematics (DNM), Goddard Space Flight Center (GSFC), Geophysical Fluid Dynamics Laboratory (GFDL), Institute of Atmospheric Physics (IAP), Indian Institute of Tropical Meteorology (IITM), Meteorological Research Institute (MRI), National Center for Atmospheric Research (NCAR), Seoul National University (SNU), and the State University of New York (SUNY), participated in the intraseasonal component of the project. Each performed a set of 10 ensemble simulations for 1 September 1996-31 August 1998 using the same observed weekly SST values but with different initial conditions. The focus is on the spatial and seasonal variations associated with intraseasonal variability (ISV) of rainfall, the structure of each model's principal mode of spatial-temporal variation of rainfall [i.e. their depiction of the Intraseasonal Oscillation (ISO)], the teleconnection patterns associated with each model's ISO, and the implications of the models' ISV on seasonal monsoon predictability. The results show that several of the models exhibit ISV levels at or above that found in observations with spatial patterns of ISV that resemble the observed pattern. This includes a number of rather detailed features, including the relative distribution of variability between ocean and land regions. In terms of the area-averaged variance, it is found that the fidelity of a model to represent NH summer versus winter ISV appears to be strongly linked. In addition, most models' ISO patterns do exhibit some form of northeastward propagation. However, the model ISO patterns are typically less coherent, lack sufficient eastward propagation, and have smaller zonal and meridional spatial scales than the observed patterns, and are often limited to one side or the other of the maritime continent. The most pervasive and problematic feature of the models' depiction of ISV and/or their ISO patterns is the overall lack of variability in the equatorial Indian Ocean. In some cases, this characteristic appears to result from some models forming double convergence zones about the equator rather than one region of strong convergence on the equator. This shortcoming results in a poor representation of the local rainfall pattern and also significantly influences the models' representations of the global-scale teleconnection patterns associated with the ISO. Finally, analysis of the model ensemble shows a positive relationship between the strength of a model's ISV of rainfall and its intra-ensemble variability of seasonal monsoon rainfall. The implications of this latter relation are discussed in the context of seasonal monsoon predictability. C1 SUNY Stony Brook, Marine Sci Res Ctr, Stony Brook, NY 11794 USA. Seoul Natl Univ, Sch Earth & Environm Sci, Seoul, South Korea. Princeton Univ, Geophys Fluid Dynam Lab, Princeton, NJ 08544 USA. NASA, Goddard Space Flight Ctr, Data Assimilat Off, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Climate & Radiat Branch, Greenbelt, MD 20771 USA. Ctr Ocean Land Atmosphere Studies, Calverton, MD USA. Meteorol Res Inst, Tsukuba, Ibaraki 305, Japan. Natl Ctr Atmospher Res, Boulder, CO 80307 USA. Russian Acad Sci, Inst Numer Math, Moscow, Russia. Indian Inst Trop Meteorol, Pune, Maharashtra, India. LASG, Inst Atmospher Phys, Beijing, Peoples R China. Korea Meteorol Adm, Climate Predict Div, Seoul, South Korea. RP Waliser, DE (reprint author), SUNY Stony Brook, Marine Sci Res Ctr, Stony Brook, NY 11794 USA. EM duane.waliser@sunysb.edu RI Lau, William /E-1510-2012; 안, 민섭/D-9972-2015; OI Lau, William /0000-0002-3587-3691; Lee, Myong-In/0000-0001-8983-8624 NR 113 TC 142 Z9 148 U1 5 U2 27 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0930-7575 J9 CLIM DYNAM JI Clim. Dyn. PD NOV PY 2003 VL 21 IS 5-6 BP 423 EP 446 DI 10.1007/s00382-003-0337-1 PG 24 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 742CA UT WOS:000186496700005 ER PT J AU Memarsadeghi, N O'Leary, DP AF Memarsadeghi, N O'Leary, DP TI Partial solution to the last issue's assignment, "classified information: The data clustering problem" SO COMPUTING IN SCIENCE & ENGINEERING LA English DT Article C1 Univ Maryland, Dept Comp Sci, College Pk, MD 20742 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Memarsadeghi, N (reprint author), Univ Maryland, Dept Comp Sci, College Pk, MD 20742 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA SN 1521-9615 J9 COMPUT SCI ENG JI Comput. Sci. Eng. PD NOV-DEC PY 2003 VL 5 IS 6 BP 64 EP 70 DI 10.1109/MCISE.2003.1238706 PG 7 WC Computer Science, Interdisciplinary Applications SC Computer Science GA 737QQ UT WOS:000186243600013 ER PT J AU Onstott, TC Moser, DP Pfiffner, SM Fredrickson, JK Brockman, FJ Phelps, TJ White, DC Peacock, A Balkwill, D Hoover, R Krumholz, LR Borscik, M Kieft, TL Wilson, R AF Onstott, TC Moser, DP Pfiffner, SM Fredrickson, JK Brockman, FJ Phelps, TJ White, DC Peacock, A Balkwill, D Hoover, R Krumholz, LR Borscik, M Kieft, TL Wilson, R TI Indigenous and contaminant microbes in ultradeep mines SO ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID WITWATERSRAND BASIN; DEEP SUBSURFACE; SOUTH-AFRICA; SEDIMENTS; GOLD; COLLECTION; REDUCTION; GROWTH; ORIGIN; MICROORGANISMS AB Rock, air and service water samples were collected for microbial analyses from 3.2 kilometres depth in a working Au mine in the Witwatersrand basin, South Africa. The similar to metre-wide mined zone was comprised of a carbonaceous, quartz, sulphide, uraninite and Au bearing layer, called the Carbon Leader, sandwiched by quartzite and conglomerate. The microbial community in the service water was dominated by mesophilic aerobic and anaerobic, alpha-, beta- and gamma-Proteobacteria with a total biomass concentration similar to10(4) cells ml(-1), whereas, that of the mine air was dominated by members of the Chlorobi and Bacteroidetes groups and a fungal component. The microorganisms in the Carbon Leader were predominantly mesophilic, aerobic heterotrophic, nitrate reducing and methylotrophic, beta- and gamma-Proteobacteria that were more closely related to service water microorganisms than to air microbes. Rhodamine WT dye and fluorescent microspheres employed as contaminant tracers, however, indicated that service water contamination of most of the rock samples was < 0.01% during acquisition. The microbial contaminants most likely originated from the service water, infiltrated the low permeability rock through and accumulated within mining-induced fractures where they survived for several days before being mined. Combined PLFA and terminal restriction fragment length profile (T-RFLP) analyses suggest that the maximum concentration of indigenous microorganisms in the Carbon Leader was < 10(2) cells g(-1). PLFA, S-35 autoradiography and enrichments suggest that the adjacent quartzite was less contaminated and contained similar to10(3) cells gram(-1) of thermophilic, sulphate reducing bacteria, SRB, some of which are delta-Proteobacteria. Pore water and rock geochemical analyses suggest that these SRB's may have been sustained by sulphate diffusing from the adjacent U-rich, Carbon Leader where it was formed by radiolysis of sulphide. C1 Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA. Pacific NW Natl Lab, Richland, WA 99352 USA. Univ Tennessee, Ctr Biomarker Anal, Dept Microbiol, Knoxville, TN 37932 USA. Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA. Florida State Univ, Dept Biol Sci, NRB 312, Tallahassee, FL 32306 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Univ Oklahoma, Dept Bot & Microbiol, Norman, OK 73019 USA. New Mexico Inst Min & Technol, Dept Biol, Socorro, NM 87801 USA. SRK Turgis Technol, ZA-2115 Blackheath, South Africa. RP Onstott, TC (reprint author), Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA. RI phelps, tommy/A-5244-2011 NR 55 TC 61 Z9 62 U1 0 U2 31 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1462-2912 J9 ENVIRON MICROBIOL JI Environ. Microbiol. PD NOV PY 2003 VL 5 IS 11 BP 1168 EP 1191 DI 10.1046/j.1462-2920.2003.00512.x PG 24 WC Microbiology SC Microbiology GA 736ME UT WOS:000186173900015 PM 14641596 ER PT J AU Rice, SD Carls, MG Heintz, RA Short, JW AF Rice, SD Carls, MG Heintz, RA Short, JW TI Comment on "hydrocarbon composition and toxicity of sediments following the Exxon valdez oil spill in Prince William Sound, Alaska, USA' SO ENVIRONMENTAL TOXICOLOGY AND CHEMISTRY LA English DT Letter ID RECOVERY; DUCKS C1 Natl Marine Fisheries Serv, Auke Bay Lab, Juneau, AK USA. RP Rice, SD (reprint author), Natl Marine Fisheries Serv, Auke Bay Lab, Juneau, AK USA. NR 21 TC 3 Z9 3 U1 0 U2 7 PU SETAC PI PENSACOLA PA 1010 NORTH 12TH AVE, PENSACOLA, FL 32501-3367 USA SN 0730-7268 J9 ENVIRON TOXICOL CHEM JI Environ. Toxicol. Chem. PD NOV PY 2003 VL 22 IS 11 BP 2539 EP 2540 DI 10.1897/02-631 PG 2 WC Environmental Sciences; Toxicology SC Environmental Sciences & Ecology; Toxicology GA 729RV UT WOS:000185788500001 PM 14587889 ER PT J AU Hshieh, FY Hirsch, DB Beeson, HD AF Hshieh, FY Hirsch, DB Beeson, HD TI Using heat of combustion data to estimate or assess some threshold flammability properties of materials SO FIRE AND MATERIALS LA English DT Article DE threshold flammability properties; heat of combustion; flammability limit AB This paper gives a brief summary of recent studies using heat of combustion data to estimate or assess some threshold flammability properties of materials. Heat of combustion data can be used to estimate the lower flammability limit. upper flammability limit and minimum oxygen concentration for flame propagation of organic and organosilicon compounds. The data can also be used to assess the threshold oxygen pressure for the combustion of metal alloys in high-pressure oxygen environments. Copyright (C) 2003 John Wiley Sons, Ltd. C1 Honeywell Technol Solut Inc, Las Cruces, NM 88004 USA. NASA, Johnson Space Ctr, Honneywell Technol Solut Inc, White Sands Test Facil, White Sands Missile Range, NM USA. RP Hshieh, FY (reprint author), Honeywell Technol Solut Inc, POB 20, Las Cruces, NM 88004 USA. NR 13 TC 3 Z9 3 U1 0 U2 1 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND SN 0308-0501 J9 FIRE MATER JI Fire Mater. PD NOV-DEC PY 2003 VL 27 IS 6 BP 267 EP 273 DI 10.1002/fam.834 PG 7 WC Materials Science, Multidisciplinary SC Materials Science GA 749ZA UT WOS:000186958900002 ER PT J AU Schabetsberger, R Morgan, CA Brodeur, RD Potts, CL Peterson, WT Emmett, RL AF Schabetsberger, R Morgan, CA Brodeur, RD Potts, CL Peterson, WT Emmett, RL TI Prey selectivity and diel feeding chronology of juvenile chinook (Oncorhynchus tshawytscha) and coho (O-kisutch) salmon in the Columbia River plume SO FISHERIES OCEANOGRAPHY LA English DT Article DE diet feeding; predation; prey availability; salmon; selectivity ID ATLANTIC-SALMON; GASTRIC EVACUATION; DAILY RATION; GELATINOUS-ZOOPLANKTON; AMPHIPODA-HYPERIIDEA; BRITISH-COLUMBIA; PACIFIC SALMON; PINK SALMON; OREGON; WASHINGTON AB We studied salmon feeding selectivity and diet feeding chronology in the Columbia River plume. Juvenile chinook and coho salmon were caught by trawling at 2-3 h intervals throughout a diet period on three consecutive days (21-23 June 2000) at stations located 14.8 and 37 km offshore from the mouth of the Columbia River. A total of 170 chinook salmon were caught at the inshore and 79 chinook and 98 coho salmon were caught at the offshore station. After each trawl, potential prey were sampled at different depths with 2-3 different types of nets (1-m diameter ring net, bongo net, neuston net). Despite the variability in zooplankton abundance, feeding selectivity was surprisingly constant. Both salmon species fed selectively on larger and pigmented prey such as hyperiid amphipods, larval and juvenile fish, various crab megalopae, and euphausiids. Hyperiid amphipods were abundant in the salmon diets and we hypothesize that aggregations of gelatinous zooplankton may facilitate the capture of commensal hyperiid amphipods. Small copepods and calyptopis and furcilia stages of euphausiids dominated the prey field by numbers, but were virtually absent from salmon diet. Juvenile chinook salmon, with increasing body size, consumed a larger proportion of fish. Stomach fullness peaked during morning hours and reached a minimum at night, suggesting a predominantly diurnal feeding pattern. In general, both chinook and coho salmon appear to be selective, diurnal predators, preying mostly on large and heavily pigmented prey items, in a manner consistent with visually oriented, size-selective predation. C1 Oregon State Univ, Hatfield Marine Sci Ctr, Cooperat Inst Marine Resources Studies, Newport, OR 97365 USA. Oregon State Univ, Hatfield Marine Sci Ctr, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA. RP Schabetsberger, R (reprint author), Salzburg Univ, Inst Zool, Hellbrunnerstr 34, A-5020 Salzburg, Austria. NR 53 TC 54 Z9 56 U1 2 U2 15 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1054-6006 J9 FISH OCEANOGR JI Fish Oceanogr. PD NOV PY 2003 VL 12 IS 6 BP 523 EP 540 DI 10.1046/j.1365-2419.2003.00231.x PG 18 WC Fisheries; Oceanography SC Fisheries; Oceanography GA 749AD UT WOS:000186895700001 ER PT J AU Logerwell, EA Mantua, N Lawson, PW Francis, RC Agostini, VN AF Logerwell, EA Mantua, N Lawson, PW Francis, RC Agostini, VN TI Tracking environmental processes in the coastal zone for understanding and predicting Oregon coho (Oncorhynchus kisutch) marine survival SO FISHERIES OCEANOGRAPHY LA English DT Article DE climate; coho salmon; General Additive Model; Oncorhynchus kisutch; Oregon; survival ID CALIFORNIA CURRENT SYSTEM; PACIFIC SALMON; WEST-COAST; SEA-LEVEL; CONTINENTAL-SHELF; PRODUCTION AREA; REGIME CONCEPT; NORTH PACIFIC; EL-NINO; OCEAN AB To better understand and predict Oregon coho (Oncorhynchus kisutch) marine survival, we developed a conceptual model of processes occurring during four sequential periods: (1) winter climate prior to smolt migration from freshwater to ocean, (2) spring transition from winter downwelling to spring/summer upwelling, (3) the spring upwelling season and (4) winter ocean conditions near the end of the maturing coho's first year at sea. We then parameterized a General Additive Model (GAM) with Oregon Production Index (OPI) coho smolt-to-adult survival estimates from 1970 to 2001 and environmental data representing processes occurring during each period (presmolt winter SST, spring transition date, spring sea level, and post-smolt winter SST). The model explained a high and significant proportion of the variation in coho survival (R-2 = 0.75). The model forecast of 2002 adult survival rate ranged from 4 to 8%. Our forecast was higher than predictions based on the return of precocious males (`jacks'), and it won't be known until fall 2002 which forecast is most accurate. An advantage to our environmentally based predictive model is the potential for linkages with predictive climate models, which might allow for forecasts more than 1 year in advance. Relationships between the environmental variables in the GAM and others (such as the North Pacific Index and water column stratification) provided insight into the processes driving production in the Pacific Northwest coastal ocean. Thus, coho may be a bellwether for the coastal environment and models such as ours may apply to populations of other species in this habitat. C1 Univ Washington, Sch Aquat & Fisheries Sci, Seattle, WA 98195 USA. Univ Washington, Sch Marine Affairs, Joint Inst Study Atmosphere & Oceans, Climate Impacts Grp, Seattle, WA 98195 USA. NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA. RP Logerwell, EA (reprint author), Alaska Fisheries Sci Ctr, F-AKC2,POB 15700, Seattle, WA 98115 USA. NR 47 TC 130 Z9 131 U1 1 U2 8 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1054-6006 J9 FISH OCEANOGR JI Fish Oceanogr. PD NOV PY 2003 VL 12 IS 6 BP 554 EP 568 DI 10.1046/j.1365-2419.2003.00238.x PG 15 WC Fisheries; Oceanography SC Fisheries; Oceanography GA 749AD UT WOS:000186895700003 ER PT J AU Jakob, C Tselioudis, G AF Jakob, C Tselioudis, G TI Objective identification of cloud regimes in the Tropical Western Pacific SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MIDLATITUDE; RADIATION AB Identifying cloud regimes and their role in the climate system can serve a multitude of purposes, ranging from a better understanding of clouds to guiding field experiments to improving the representation of clouds in models. This study describes early results in identifying cloud regimes from ISCCP data using cluster analysis. A simple algorithm for cloud regime identification is introduced and applied to data in the Tropical Western Pacific region. Four major cloud regimes, namely a shallow cumulus regime, a transparent isolated cirrus regime, thick cirrus with convection and a deep and probably organized convective regime are identified and their frequency of occurrence is quantified. The use of the regime information for various applications is discussed and the use of regime classifications for representativeness studies is presented using the ARM TWP sites as an example. C1 BMRC, Melbourne, Vic 3001, Australia. Columbia Univ, Dept Appl Phys, NASA, GISS, New York, NY 10027 USA. RP Jakob, C (reprint author), BMRC, GPO Box 1289K, Melbourne, Vic 3001, Australia. RI Jakob, Christian/A-1082-2010 OI Jakob, Christian/0000-0002-5012-3207 NR 10 TC 100 Z9 100 U1 1 U2 10 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 NOV 1 PY 2003 VL 30 IS 21 AR 2082 DI 10.1029/2003GL018367 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 740GP UT WOS:000186394900004 ER PT J AU Rickman, D Luvall, JC Shaw, J Mask, P Kissel, D Sullivan, D AF Rickman, D Luvall, JC Shaw, J Mask, P Kissel, D Sullivan, D TI Precision agriculture SO GEOTIMES LA English DT Article C1 NASA, George C Marshall Space Flight Ctr, Dept Earth Sci, Huntsville, AL 35812 USA. Auburn Univ, Auburn, AL 36849 USA. Univ Georgia, Athens, GA 30602 USA. USDA ARS, SE Watershed Res Lab, Washington, DC 20250 USA. RP Rickman, D (reprint author), NASA, George C Marshall Space Flight Ctr, Dept Earth Sci, Huntsville, AL 35812 USA. NR 0 TC 1 Z9 1 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 NOV PY 2003 VL 48 IS 11 BP 28 EP 31 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 779XE UT WOS:000189326700019 ER PT J AU Potter, C Klooster, S Myneni, R Genovese, V Tan, PN Kumar, V AF Potter, C Klooster, S Myneni, R Genovese, V Tan, PN Kumar, V TI Continental-scale comparisons of terrestrial carbon sinks estimated from satellite data and ecosystem modeling 1982-1998 SO GLOBAL AND PLANETARY CHANGE LA English DT Article DE carbon dioxide; ecosystems; remote sensing; ocean climate ID NET PRIMARY PRODUCTION; INTERANNUAL VARIABILITY; SOLAR-RADIATION; GLOBAL SCALES; LAND; EXCHANGE; CLIMATE; CYCLE; CO2; FLUXES AB A simulation model based on satellite observations of monthly vegetation cover was used to estimate monthly carbon fluxes in terrestrial ecosystems from 1982 to 1998. The NASA-CASA model was driven by vegetation properties derived from the Advanced Very High Resolution Radiometer (AVHRR) and radiative transfer algorithms that were developed for Moderate Resolution Imaging Spectroradiometer (MODIS). For the terrestrial biosphere, predicted net ecosystem production (NEP) flux for atmospheric CO2 has varied widely between an annual source of -0.9 Pg C per year and a sink of +2.1 Pg C per year. The southern hemisphere tropical zones (SHT, between 0degrees and 30degreesS) have a major influence over the predicted global trends in interannual variability of NEP. In contrast, the terrestrial NEP sink for atmospheric CO2 on the North American (NA) continent has been fairly consistent between +0.2 and +0.3 Pg C per year, except during relatively cool annual periods when continental NEP fluxes are predicted to total to nearly zero. The predicted NEP sink for atmospheric CO2 over Eurasia (EA) increased notably in the late 1980s and has been fairly consistent between +0.3 and +0.55 Pg C per year since 1988. High correlations can be detected between the El Ni (n) over tildeo Southern Oscillation (ENSO) and predicted NEP fluxes on the EA continent and for the SHT latitude zones, whereas NEP fluxes for the North American continent as a whole do not correlate strongly with ENSO events over the same time series since 1982. These observations support the hypothesis that regional climate warming has had notable but relatively small-scale impacts on high latitude ecosystem (tundra and boreal) sinks for atmospheric CO2. Published by Elsevier B.V. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Calif State Univ Monterey Bay, Seaside, CA USA. Boston Univ, Boston, MA 02215 USA. Univ Minnesota, Minneapolis, MN USA. RP Potter, C (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RI Myneni, Ranga/F-5129-2012 NR 45 TC 105 Z9 112 U1 3 U2 24 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0921-8181 J9 GLOBAL PLANET CHANGE JI Glob. Planet. Change PD NOV PY 2003 VL 39 IS 3-4 BP 201 EP 213 DI 10.1016/j.gloplacha.2003.07.001 PG 13 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 732RD UT WOS:000185958600001 ER PT J AU Formisano, V D'Aversa, E Bellucci, G Baines, KH Bibring, JP Brown, RH Buratti, BJ Capaccioni, E Cerroni, P Clark, RN Coradini, A Cruikshank, DP Drossart, P Jaumann, R Langevin, Y Matson, DL McCord, TB Mennella, V Nelson, RM Nicholson, PD Sicardy, B Sotin, C Chamberlain, MC Hansen, G Hibbits, K Showalter, M Filacchione, G AF Formisano, V D'Aversa, E Bellucci, G Baines, KH Bibring, JP Brown, RH Buratti, BJ Capaccioni, E Cerroni, P Clark, RN Coradini, A Cruikshank, DP Drossart, P Jaumann, R Langevin, Y Matson, DL McCord, TB Mennella, V Nelson, RM Nicholson, PD Sicardy, B Sotin, C Chamberlain, MC Hansen, G Hibbits, K Showalter, M Filacchione, G TI Cassini-VIMS at Jupiter: solar occultation measurements using Io SO ICARUS LA English DT Article DE occultations; Jupiter; infrared observations ID LIGHT CURVES; ATMOSPHERE; COEFFICIENTS; SPECTRA; METHANE; MODEL; PLUTO AB We report unusual and somewhat unexpected observations of the jovian satellite Io, showing strong methane absorption bands. These observations were made by the Cassini VIMS experiment during the Jupiter flyby of December/January 2000/2001. The explanation is straightforward: Entering or exiting from Jupiter's shadow during an eclipse, Io is illuminated by solar light which has transited the atmosphere of Jupiter. This light, therefore becomes imprinted with the spectral signature of Jupiter's upper atmosphere, which includes strong atmospheric methane absorption bands. Intercepting solar light refracted by the jovian atmosphere, Io essentially becomes a "mirror" for solar occultation events of Jupiter. The thickness of the layer where refracted solar light is observed is so large (more than 3000 km at Io's orbit), that we can foresee a nearly continuous multi-year period of similar events at Saturn, utilizing the large and bright ring system. During Cassini's 4-year nominal mission, this probing technique should reveal information of Saturn's atmosphere over a large range of southern latitudes and times. (C) 2003 Elsevier Inc. All rights reserved. C1 CNR, Ist Fis Spazio Interplanetario, Rome, Italy. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Paris, Inst Astrophys Spatiale, F-75252 Paris, France. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Univ Arizona, Steward Observ, Tucson, AZ 85724 USA. CNR, Ist Astrofis Spaziale & Fis Cosm, Rome, Italy. US Geol Survey, Denver, CO 80225 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Observ Paris, Meudon, France. Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. Osserv Astron Capodimonte, INAF, Capodimonte, Italy. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Univ Nantes, Lab Planetol & Geodinam, Nantes, France. RP Formisano, V (reprint author), CNR, Ist Fis Spazio Interplanetario, Rome, Italy. OI Bellucci, Giancarlo/0000-0003-0867-8679; Capaccioni, Fabrizio/0000-0003-1631-4314; Filacchione, Gianrico/0000-0001-9567-0055; D'Aversa, Emiliano/0000-0002-5842-5867 NR 24 TC 4 Z9 4 U1 0 U2 1 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD NOV PY 2003 VL 166 IS 1 BP 75 EP 84 DI 10.1016/S0019-1035(03)00178-7 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 743TL UT WOS:000186589600006 ER PT J AU Brooke, TY Weaver, HA Chin, G Bockele-Morvan, D AF Brooke, TY Weaver, HA Chin, G Bockele-Morvan, D TI Spectroscopy of Comet Hale-Bopp in the infrared SO ICARUS LA English DT Article DE comets; Hale-Bopp; comets; composition; infrared observations; spectroscopy ID C/1996 B2 HYAKUTAKE; CARBON-MONOXIDE; EMISSION FEATURE; 1995 O1; WATER; EXCITATION; MOLECULES; SPECTRUM; METHANOL; CO AB High resolution infrared spectra of Comet C/1995 O1 (Hale-Bopp) were obtained during 2-5 March 1997 UT from the NASA Infrared Telescope Facility on Mauna Kea, Hawaii, when the comet was at r approximate to 1.0 AU from the Sun pre-perihelion. Emission lines of CH(4), C(2)H(6), CN, C(2)H(2). CH(3)OH, H(2)O, CO, and OH were detected. The rotational temperature of CH4 in the inner coma was T(rot) = 110 +/- 20 K. Spatial profiles of CH4, C2H6, and H(2)O were consistent with release solely from the nucleus. The centroid of the CO emission was offset from that of the dust continuum and H(2)O. Spatial profiles of the CO lines were much broader than those of the other molecules and asymmetric. We estimate the CO production rate using a simplified outflow model: constant, symmetric outflow from the peak position. A model of the excitation of CO that includes optical depth effects using an escape probability method is presented. Optical depth effects are not sufficient to explain the broad spatial extent. Using a parent + extended-source model, the broad extent of the CO lines can be explained by CO being produced mostly (similar to90% on 5 March) from an extended source in the coma. The CO rotational temperature was near 100 K. Abundances relative to H(2)O (in percent) were 1.1 +/- 0.3 (CH(4)), 0.39 +/- 0.10 (C(2)H(6)), 0.18 +/- 0.04 (HCN), 0.17 +/- 0.04 (C(2)H(2)), 1.7 +/- 0.5 (CH(3)OH), and 37-41 (CO, parent + extended source). These are roughly comparable to those obtained for other long-period comets also observed in the infrared, though CO appears to vary. (C) 2003 Elsevier Inc. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Johns Hopkins Univ, Dept Phys & Astron, Ctr Astrophys Sci, Baltimore, MD 21218 USA. NASA, Goddard Space Flight Ctr, Planetary Syst Branch, Extraterr Phys Lab, Greenbelt, MD 20771 USA. Observ Paris, F-92195 Meudon, France. Kyung Hee Univ, Inst Nat Sci, Yongin 449701, Kyunggido, South Korea. Univ New Brunswick, Dept Phys Sci, St John, NB E2L 4L5, Canada. RP Brooke, TY (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 169-237, Pasadena, CA 91109 USA. EM tyb@astro.caltech.edu RI Chin, Gordon/E-1520-2012; Kim, Sang Joon/E-2383-2013; Xu, Li-Hong/J-5095-2015; Weaver, Harold/D-9188-2016 NR 48 TC 26 Z9 27 U1 0 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD NOV PY 2003 VL 166 IS 1 BP 167 EP 187 DI 10.1016/j.icarus.2003.08.008 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 743TL UT WOS:000186589600013 ER PT J AU Estrada, PR Cuzzi, JN Showalter, MR AF Estrada, PR Cuzzi, JN Showalter, MR TI Voyager color photometry of Saturn's main rings: a correction SO ICARUS LA English DT Article ID GALILEAN SATELLITES; PHASE; SPECTROPHOTOMETRY; SPECTRA AB We correct a calibration error in our earlier analysis of Voyager color observations of Saturn's main rings at 14degrees phase angle (Estrada and Cuzzi, 1996, Icarus 122, 25 1) and present thoroughly revised and reanalyzed radial profiles of the brightness of the main rings in the Voyager green, violet, and ultraviolet filters and the ratios of these brightnesses. These results are consistent with more recent HST results at 6degrees phase angle, once allowance is made for plausible phase reddening of the rings (Cuzzi et al., 2002, Icarus 158, 199). Unfortunately, the Voyager camera calibration factors are simply not sufficiently well known for a combination of the Voyager and HST data to be used to constrain the phase reddening quantitatively. However, some interesting radial variations in reddening between 6 and 14degrees phase angles are hinted at. We update a ring-and-satellite color vs albedo plot from Cuzzi and Estrada (1998, Icarus 132, 1) in several ways. The A and B rings are still found to be in a significantly redder part of color-albedo space than Saturn's icy satellites. (C) 2003 Elsevier Inc. All rights reserved. C1 NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. Stanford Univ, Stanford, CA 94305 USA. RP Cuzzi, JN (reprint author), NASA, Ames Res Ctr, Div Space Sci, MS 245-3, Moffett Field, CA 94035 USA. NR 18 TC 11 Z9 11 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 NOV PY 2003 VL 166 IS 1 BP 212 EP 222 DI 10.1016/j.icarus.2003.06.001 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 743TL UT WOS:000186589600016 ER PT J AU Filman, RE AF Filman, RE TI Veni, vidi, sensi SO IEEE INTERNET COMPUTING LA English DT Editorial Material C1 NASA, Adv Comp Sci Res Inst, Ames, IA USA. RP Filman, RE (reprint author), NASA, Adv Comp Sci Res Inst, Ames, IA USA. NR 4 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 1089-7801 J9 IEEE INTERNET COMPUT JI IEEE Internet Comput. PD NOV-DEC PY 2003 VL 7 IS 6 BP 4 EP 6 PG 3 WC Computer Science, Software Engineering SC Computer Science GA 745DD UT WOS:000186672900001 ER PT J AU Jackson, DJ Franson, JD Gilbert, G Milburn, G AF Jackson, DJ Franson, JD Gilbert, G Milburn, G TI Introduction to the issue on quantum Internet technologies SO IEEE JOURNAL OF SELECTED TOPICS IN QUANTUM ELECTRONICS LA English DT Article C1 Jet Prop Lab, Quantum Comp Technol Grp, Pasadena, CA 91109 USA. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. Mitre Corp, Quantum Informat Sci Grp, Eatontown, NJ 07724 USA. Univ Queensland, Dept Phys, St Lucia, Qld 4072, Australia. RP Jackson, DJ (reprint author), Jet Prop Lab, Quantum Comp Technol Grp, MS 300-123,4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 0 TC 0 Z9 0 U1 1 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1077-260X J9 IEEE J SEL TOP QUANT JI IEEE J. Sel. Top. Quantum Electron. PD NOV-DEC PY 2003 VL 9 IS 6 BP 1453 EP 1454 DI 10.1109/JSTQE.2003.820942 PG 2 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 772TZ UT WOS:000188858700001 ER PT J AU Pittman, TB Donegan, MM Fitch, MJ Jacobs, BC Franson, JD Kok, P Lee, H Dowling, JP AF Pittman, TB Donegan, MM Fitch, MJ Jacobs, BC Franson, JD Kok, P Lee, H Dowling, JP TI Heralded two-photon entanglement from Probabilistic quantum logic operations on multiple parametric down-conversion sources SO IEEE JOURNAL OF SELECTED TOPICS IN QUANTUM ELECTRONICS LA English DT Article DE heralded entanglement; linear optics; quantum logic; single-photons ID COMPUTATION; PHOTONS AB An ideal controlled-NOT gate followed by projective measurements can be used to identify specific Bell states of its two input qubits. When the input qubits are each members of independent Bell states, these projective measurements, can be used to swap the post-selected entanglement onto the remaining two qubits. Here we apply this strategy to produce heralded two-photon polarization entanglement using Bell states that originate from independent parametric down-conversion sources, and a particular probabilistic controlled-NOT gate that is constructed from linear optical elements. The resulting implementation is closely related to an earlier proposal by Sliwa and Banaszek, and can be intuitively understood in terms of familiar quantum information protocols. The possibility of producing a "pseudo-demand" source of two-photon entanglement by storing and releasing these heralded pairs from independent cyclical quantum memory devices is also discussed. C1 Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. CALTECH, Jet Prop Lab, Quantum Comp Technol Grp, Pasadena, CA 91109 USA. RP Pittman, TB (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. EM todd.pittman@jhuapl.edu RI Kok, Pieter/B-1658-2010; Fitch, Michael/E-5757-2011; DOWLING, JONATHAN/L-2749-2013; Pittman, Todd/M-4686-2013 OI Fitch, Michael/0000-0002-2494-9486; NR 36 TC 11 Z9 11 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1077-260X J9 IEEE J SEL TOP QUANT JI IEEE J. Sel. Top. Quantum Electron. PD NOV-DEC PY 2003 VL 9 IS 6 BP 1478 EP 1482 DI 10.1109/jstqe.2003.820916 PG 5 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 772TZ UT WOS:000188858700004 ER PT J AU Kok, P AF Kok, P TI Limitations on building single-photon-resolution detection devices SO IEEE JOURNAL OF SELECTED TOPICS IN QUANTUM ELECTRONICS LA English DT Article DE linear optics; photodetection; quantum communication; single-photon resolution AB Single-photon resolution (SPR) detectors can tell the difference between incoming wave packets of n and n + 1 photons. Such devices are especially important for linear optical quantum computing with projective measurements. However, in this paper, I show that it is impossible to construct a photodetector with single-photon resolution when we are restricted to single-photon sources, linear optical elements, and projective measurements with standard (nonphoton-number discriminating) photodetectors. These devices include SPR detectors that sometimes fail to distinguish one- and two-photon inputs, but at the same time indicate this failure. C1 CALTECH, Jet Prop Lab, Comp Technol Grp, Pasadena, CA 91109 USA. RP Kok, P (reprint author), CALTECH, Jet Prop Lab, Comp Technol Grp, Pasadena, CA 91109 USA. EM Pieter.Kok@jpl.nasa.gov RI Kok, Pieter/B-1658-2010 NR 18 TC 8 Z9 8 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1077-260X EI 1558-4542 J9 IEEE J SEL TOP QUANT JI IEEE J. Sel. Top. Quantum Electron. PD NOV-DEC PY 2003 VL 9 IS 6 BP 1498 EP 1501 DI 10.1109/tstqe.2003.820909 PG 4 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 772TZ UT WOS:000188858700007 ER PT J AU Ponchak, GE Alterovitz, SA Downey, AN Freeman, JC Schwartz, ZD AF Ponchak, GE Alterovitz, SA Downey, AN Freeman, JC Schwartz, ZD TI Measured propagation characteristics of Coplanar waveguide on semi-insulating 4H-SiC through 800 K SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS LA English DT Article DE Coplanar waveguide; propagation characteristics; SiC; transmission line ID HIGH-TEMPERATURE AB Wireless sensors for high temperature industrial applications and jet engines require RF transmission lines and RF integrated circuits (RFICs) on wide bandgap semiconductors such as SiC. In this paper, the complex propagation constant of coplanar waveguide fabricated on semi-insulating 4H-SiC has been measured through 813 K. It is shown that the attenuation increases 3.4 dB/cm at 50 GHz as the SiC temperature is increased from 300 K to 813 K. Above 500 K, the major contribution to loss is the decrease in SiC resistivity. The effective permittivity of the same line increases. by approximately 5 % at microwave frequencies and 20% at 1 GHz. C1 NASA, Glenn Res Ctr, Analex Corp, Cleveland, OH 44135 USA. RP Ponchak, GE (reprint author), NASA, Glenn Res Ctr, Analex Corp, Cleveland, OH 44135 USA. EM george.ponchak@ieee.org NR 12 TC 6 Z9 6 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1531-1309 J9 IEEE MICROW WIREL CO JI IEEE Microw. Wirel. Compon. Lett. PD NOV PY 2003 VL 13 IS 11 BP 463 EP 465 DI 10.1109/LMWC.2003.819373 PG 3 WC Engineering, Electrical & Electronic SC Engineering GA 740KQ UT WOS:000186401900003 ER PT J AU Thienel, J Sanner, RM AF Thienel, J Sanner, RM TI A coupled nonlinear spacecraft attitude controller and observer with an unknown constant gyro bias and gyro noise SO IEEE TRANSACTIONS ON AUTOMATIC CONTROL LA English DT Article DE gyro bias; nonlinear control; nonlinear observer; state estimation AB We propose a new algorithm for estimating constant biases in gyro measurements of angular velocity, and demonstrate that the resulting estimates converge to the true bias values exponentially fast. The new observer is then combined with a nonlinear attitude tracking control strategy in a certainty equivalence fashion, and the combination shown via Lyapunov analysis to produce globally stable closed-loop dynamics, with asymptotically perfect tracking of any commanded attitude sequence. The analysis is then extended to consider the effects of stochastic measurement noise in the gyro in addition to the bias. A simulation is given for a rigid spacecraft tracking a specified, time-varying attitude sequence to illustrate the theoretical claims. C1 NASA, Goddard Space Flight Ctr, Flight Dynam Anal Branch, Greenbelt, MD 20771 USA. Univ Maryland, Dept Aerosp Engn, College Pk, MD 20742 USA. RP Thienel, J (reprint author), NASA, Goddard Space Flight Ctr, Flight Dynam Anal Branch, Code 661, Greenbelt, MD 20771 USA. NR 14 TC 115 Z9 116 U1 0 U2 7 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9286 J9 IEEE T AUTOMAT CONTR JI IEEE Trans. Autom. Control PD NOV PY 2003 VL 48 IS 11 BP 2011 EP 2015 DI 10.1109/TAC.2003.819289 PG 5 WC Automation & Control Systems; Engineering, Electrical & Electronic SC Automation & Control Systems; Engineering GA 742FE UT WOS:000186505800014 ER PT J AU Bruzzone, L Smits, PC Tilton, JC AF Bruzzone, L Smits, PC Tilton, JC TI Foreword - Special issue on analysis of multitemporal remote sensing images SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Editorial Material C1 Univ Trent, Dept Informat & Commun Technol, I-38050 Trent, Italy. Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, I-21020 Ispra, Italy. NASA, Goddard Space Flight Ctr, Appl Informat Sci Branch, Greenbelt, MD 20771 USA. RP Bruzzone, L (reprint author), Univ Trent, Dept Informat & Commun Technol, I-38050 Trent, Italy. RI Bruzzone, Lorenzo/A-2076-2012 OI Bruzzone, Lorenzo/0000-0002-6036-459X NR 0 TC 16 Z9 18 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD NOV PY 2003 VL 41 IS 11 BP 2419 EP 2422 DI 10.1109/TGRS.2003.820004 PN 1 PG 4 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 743KZ UT WOS:000186572100001 ER PT J AU Cimini, D Westwater, ER Han, Y Keihm, SJ AF Cimini, D Westwater, ER Han, Y Keihm, SJ TI Accuracy of ground-based microwave radiometer and balloon-borne measurements during the WVIOP2000 field experiment SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE microwave radiometry; radiometric accuracy; radiometric calibration; water vapor ID WATER-VAPOR; ATMOSPHERIC RADIATION; CALIBRATION; ABSORPTION; PROGRAM; LIQUID; CLOUD AB We discuss the performances of a set of four microwave water vapor radiometers operating in the 20-30-GHz band during a field experiment, with an emphasis on calibration and achievable accuracy. The field experiment was conducted at the Department of Energy's Atmospheric Radiation Measurement Program's field site in north central Oklahoma, and was focused on clear-sky water vapor measurements by both radiometers and radiosondes. A comparison between two published radiometric tip curve calibration procedures is presented, and these procedures are applied to measurements from two nearly identical instruments placed a few meters apart. Using the instantaneous tip cal method of the Environmental Technology Laboratory, the brightness temperature measurements for the two identical instruments differed by less than 0.2 K over a 24-h period. Results from reference load cryogenic tests and brightness temperature cross comparisons have shown differences within 0.7 K. In addition, we compare radiometric measurements with calculations of brightness temperature based on the Rosenkranz absorption model and radiosonde observations. During the experiment, both Vaisala-type RS80 and RS90 humidity sensors were used. Our comparisons demonstrate the improvements achieved by the new Vaisala RS90 sensors in atmospheric humidity profiling, which reduce or eliminate the "dry bias" problem. C1 Univ Aquila, CETEMPS, I-67010 Coppito, Italy. Univ Colorado, NOAA, Cooperat Inst Res Environm Sci, Environm Technol Lab, Boulder, CO 80305 USA. NOAA, Natl Environm Satellite Data & Informat Serv, Off Res & Appl, Camp Springs, MD 20746 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Cimini, D (reprint author), Univ Aquila, CETEMPS, I-67010 Coppito, Italy. RI Han, Yong/F-5590-2010; Cimini, Domenico/M-8707-2013 OI Han, Yong/0000-0002-0183-7270; Cimini, Domenico/0000-0002-5962-223X NR 32 TC 23 Z9 24 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 NOV PY 2003 VL 41 IS 11 BP 2605 EP 2615 DI 10.1009/TGRS.2003.815673 PN 1 PG 11 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 743KZ UT WOS:000186572100019 ER PT J AU Yueh, SH Stiles, BW Liu, WT AF Yueh, SH Stiles, BW Liu, WT TI QuikSCAT wind retrievals for tropical cyclones SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE hurricane; ocean wind; rain attenuation; rain scattering; scatterometer; tropical cyclone ID KU-BAND; OCEAN BACKSCATTER; RAIN; IMPACT; MODEL AB The use of QuikSCAT data for wind retrievals of tropical cyclones is described. The evidence of QuikSCAT sigma(0) dependence on wind direction for >30-m/s wind speeds is presented. The QuikSCAT sigma(0) s show a peak-to-peak wind direction modulation of similar to1 dB at 35-m/s wind speed, and the amplitude of modulation decreases with increasing wind speed. The decreasing directional sensitivity to wind speed agrees well with the trend of QSCAT1 model function at near 20 m/s. A correction of the QSCAT1 model function for above 23-m/s wind speed is proposed. We explored two microwave radiative transfer models to correct the attenuation and scattering effects of rain for wind retrievals. One is derived from the collocated QuikSCAT and Special Sensor Microwave/Imager (SSM/I) dataset, and the other one is a published parametric model developed for rain radars. These two radiative transfer models account for the effects of volume scattering, scattering from rain-roughened surfaces and rain attenuation. The models suggest that the sigma(0) s of wind-roughened sea surfaces for 40-50-m/s winds are comparable to the sigma(0) s of rain contributions for up to about 10-15 mm/h. Both radiative transfer models have been used to retrieve the ocean wind vectors from the collocated QuikSCAT and SSM/I rain rate data for several tropical cyclones. The resulting wind speed estimates of these tropical cyclones show improved agreement with the wind fields derived from the best track analysis and Holland's model for up to about 15-mm/h SSM/I rain rate. A comparative analysis of maximum wind speed estimates suggests that other rain parameters likely have to be considered for further improvements. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Yueh, SH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 21 TC 36 Z9 37 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 NOV PY 2003 VL 41 IS 11 BP 2616 EP 2628 DI 10.1109/TGRS.2003.814913 PN 1 PG 13 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 743KZ UT WOS:000186572100020 ER PT J AU Chander, G Markham, B AF Chander, G Markham, B TI Revised Landsat-5 TM radiometric calibration procedures and postcalibration dynamic ranges SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE bias; gain; irradiance; Landsat; Lmax; Lmin; lookup table (LUT); National Landsat Archive Production System (NLAPS); radiance; radiometric calibration; reflectance; temperature; Thematic Mapper (TM) AB Effective May 5, 2003, Landsat-5 (L5) Thematic Mapper (TM) data processed and distributed by the U.S. Geological Survey (USGS) Earth Resources Observation System (EROS) Data Center (EDC) will be radiometrically calibrated using a new procedure and revised calibration parameters. This change will improve absolute calibration accuracy, consistency over time, and consistency with Landsat-7 (L7) Enhanced Thematic Mapper Plus (ETM+) data. Users will need to use new parameters to convert the calibrated data products to radiance. The new procedure for the reflective bands (1-5,7) is based on a lifetime radiometric calibration curve for the instrument derived from the instrument's internal calibrator, cross-calibration with the ETM+, and vicarious measurements. The thermal band will continue to be calibrated using the internal calibrator. Further updates to improve the relative detector-to-detector calibration and thermal band calibration are being investigated, as is the calibration of the Landsat-4 (L4) TM. C1 Sci Applicat Int Corp, USGS, EDC, Sioux Falls, SD 57198 USA. NASA, Goddard Space Flight Ctr, LPSO, Greenbelt, MD 20771 USA. RP Chander, G (reprint author), Sci Applicat Int Corp, USGS, EDC, Sioux Falls, SD 57198 USA. RI Markham, Brian/M-4842-2013 OI Markham, Brian/0000-0002-9612-8169 NR 9 TC 408 Z9 488 U1 6 U2 37 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 NOV PY 2003 VL 41 IS 11 BP 2674 EP 2677 DI 10.1109/TGRS.2003.818464 PN 2 PG 4 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 743LA UT WOS:000186572200002 ER PT J AU Gyorgy, A Linder, T Chou, PA Betts, BJ AF Gyorgy, A Linder, T Chou, PA Betts, BJ TI Do optimal entropy-constrained quantizers have a finite or infinite number of codewords? SO IEEE TRANSACTIONS ON INFORMATION THEORY LA English DT Article DE difference distortion measures; entropy coding; infinite-level quantizers; Lagrangian performance; optimal quantization ID VECTOR QUANTIZATION AB An entropy-constrained quantizer Q is optimal if it minimizes the expected distortion D(Q) subject to a constraint on the output entropy H(Q). In this correspondence, we use the Lagrangian formulation to show the existence and study the structure of optimal entropy-constrained quantizers that achieve a point on the lower convex hull of the operational distortion-rate function D-h(R) = inf(Q){D(Q) : H(Q) less than or equal to R}. In general, an optimal entropy-constrained quantizer may have a countably infinite number of codewords. Our main results show that if the tail of the source distribution is sufficiently light (resp., heavy) with respect to the distortion measure, the Lagrangian-optimal entropy-constrained quantizer has a finite (resp., infinite) number of codewords. In particular, for the squared error distortion measure, if the tail of the source distribution is lighter than the tail of a Gaussian distribution, then the Lagrangian-optimal quantizer has only a finite number of codewords, while if the tail is heavier than that of the Gaussian, the Lagrangian-optimal quantizer has an infinite number of codewords. C1 Queens Univ, Dept Math & Stat, Kingston, ON K7L 3N6, Canada. Microsoft Corp, Redmond, WA 98052 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Gyorgy, A (reprint author), Queens Univ, Dept Math & Stat, Kingston, ON K7L 3N6, Canada. NR 11 TC 13 Z9 13 U1 0 U2 0 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9448 J9 IEEE T INFORM THEORY JI IEEE Trans. Inf. Theory PD NOV PY 2003 VL 49 IS 11 BP 3031 EP 3037 DI 10.1109/TIT.2003.819340 PG 7 WC Computer Science, Information Systems; Engineering, Electrical & Electronic SC Computer Science; Engineering GA 744GA UT WOS:000186618500023 ER PT J AU Giglio, L Kendall, JD Mack, R AF Giglio, L Kendall, JD Mack, R TI A multi-year active fire dataset for the tropics derived from the TRMM VIRS SO INTERNATIONAL JOURNAL OF REMOTE SENSING LA English DT Article ID RESOLUTION; IDENTIFICATION; MODIS AB A pan-tropical active fire dataset derived from observations made with the Visible and Infrared Scanner (VIRS), onboard the Tropical Rainfall Measuring Mission (TRMM) satellite, is described. The dataset consists of monthly 0.5degrees resolution fire summary products from January 1998 to the present, with geographical coverage spanning latitudes 38degreesS to 38degreesN. Several key issues previously not considered in summarizing satellite-derived fire 'counts' were addressed during development of the product. The dataset is intended to provide a current, continuous, multi-year record of fire activity in the tropics and subtropics for input to global studies on the Earth's land and atmosphere processes, their interaction, and relation to climate change. Following the availability of improved global fire coverage from the Moderate Resolution Imaging Spectroradiometer (MODIS), the VIRS fire dataset will continue to be useful because it can provide new multi-year information on the diurnal cycle of fire that is difficult to achieve at the global scale. Development of an efficient, operational production stream for this dataset was achieved through an innovative and cost-effective data-mining activity at the Goddard Earth Sciences Distributed Active Archive Center (GES DAAC). For the remainder of the expected six-year lifespan of the TRMM spacecraft (through 2003), the VIRS fire products will continue to be generated through cooperation with the GES DAAC. Facilities for Web-based distribution of the products are currently being developed at http://daac.gsfc.nasa.gov. C1 NASA, Sci Syst & Applicat Inc, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Giglio, L (reprint author), NASA, Sci Syst & Applicat Inc, Goddard Space Flight Ctr, Code 923, Greenbelt, MD 20771 USA. NR 18 TC 82 Z9 88 U1 2 U2 9 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 NOV PY 2003 VL 24 IS 22 BP 4505 EP 4525 DI 10.1080/0143116031000070283 PG 21 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA 742DF UT WOS:000186500100018 ER PT J AU De Jeu, RAM Owe, M AF De Jeu, RAM Owe, M TI Further validation of a new methodology for surface moisture and vegetation optical depth retrieval SO INTERNATIONAL JOURNAL OF REMOTE SENSING LA English DT Article ID SATELLITE MICROWAVE OBSERVATIONS; SOIL-MOISTURE; WATER-CONTENT; POLARIZATION; EMISSION; GHZ; ATTENUATION; SENSITIVITY; CANOPY; MODEL AB A series of validation studies for a recently developed soil moisture and optical depth retrieval algorithm is presented. The approach is largely theoretical, and uses a non-linear iterative optimization procedure to solve a simple radiative transfer equation for the two parameters from dual polarization satellite microwave brightness temperatures. The satellite retrievals were derived from night-time 6.6 GHz Nimbus Scanning Multichannel Microwave Radiometer (SMMR) observations, and were compared to soil moisture data sets from the USA, Mongolia, Turkmenistan and Russia. The surface temperature, which is also an unknown parameter in the model, is derived off-line from 37 GHz vertical polarized brightness temperatures. The new theoretical approach is independent of field observations of soil moisture or canopy biophysical measurements and can be used at any wavelength in the microwave region. The soil moisture retrievals compared well with the surface moisture observations from the various locations. The vegetation optical depth also compared well to time series of Normalized Difference Vegetation Index (NDVI) and showed similar seasonal patterns. From a global perspective, the satellite-derived surface soil moisture was consistent with expected spatial patterns, identifying both known dry areas such as deserts and semi-arid areas and moist agricultural areas very well. Spatial patterns of vegetation optical depth were found to be in agreement with NDVI. The methodology described in this study should be directly transferable to the Advanced Microwave Scanning Radiometer (AMSR) on the recently launched AQUA satellite. C1 NASA, Hydrol Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP De Jeu, RAM (reprint author), NASA, Hydrol Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 36 TC 66 Z9 67 U1 3 U2 14 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 NOV PY 2003 VL 24 IS 22 BP 4559 EP 4578 DI 10.1080/0143116031000095934 PG 20 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA 742DF UT WOS:000186500100021 ER PT J AU Lim, JW Yu, YH Johnson, W AF Lim, JW Yu, YH Johnson, W TI Calculation of rotor blade-vortex interaction airloads using a multiple-trailer free-wake model SO JOURNAL OF AIRCRAFT LA English DT Article AB Analytical results of rotor blade-vortex interaction airloads are presented with two different wake models in the comprehensive analysis CAMRAD II, and these calculated results are compared with the experimental data obtained from the higher-harmonic-control aeroacoustic rotor test (HART-I) program. The HART rotor was a 40%, Mach-scaled model of the hingeless BO-105 main rotor. Two wake models used in the comprehensive analysis are the single-trailer and the multiple-trailer free-wake models. The multiple-trailer wake model shows good prediction of lift distribution, M(2)c(n), as a function of azimuth for baseline, minimum noise, and minimum vibration cases, and shows significant improvement relative to the single-trailer model in prediction of the tip vortex wake geometry. C1 USA, Aviat & Missile Command, NASA, Rotocraft Div,Aeroflightdynam Directorate, Moffett Field, CA 94035 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Lim, JW (reprint author), USA, Aviat & Missile Command, NASA, Rotocraft Div,Aeroflightdynam Directorate, Moffett Field, CA 94035 USA. NR 20 TC 16 Z9 17 U1 0 U2 2 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD NOV-DEC PY 2003 VL 40 IS 6 BP 1123 EP 1130 DI 10.2514/2.7200 PG 8 WC Engineering, Aerospace SC Engineering GA 756EF UT WOS:000187452300010 ER PT J AU Dukhan, N De Witt, KJ Masiulaniec, KC Van Fossen, GJ AF Dukhan, N De Witt, KJ Masiulaniec, KC Van Fossen, GJ TI Experimental Frossling numbers for ice-roughened NACA 0012 airfoils SO JOURNAL OF AIRCRAFT LA English DT Article ID HEAT-TRANSFER; RIME ICE; ROUGHNESS; SURFACES; SHAPES; GLAZE AB Experimental Frossling numbers are presented for two aluminum castings of ice-roughened NACA 0012 airfoil surfaces at 0-deg angle of attack for chord Reynolds number ranging from 4.00 x 10(5) to 1.54 x 10(6). The castings were meticulously obtained from actual ice accretions representing mildly rough glaze and rough glaze ice with horns. A modified investment casting technique was used to capture all of the surface roughness details. The rough glaze ice with horns produced higher heat-transfer rates than those for the mildly rough glaze ice, especially at the horns. Immediately downstream of the horns, stagnation air gaps resulted and caused lower heat-transfer coefficients. For both types of ice, higher Reynolds numbers in general produced higher heat-transfer coefficients. For the same chord Reynolds number and at the same position on the airfoil, the Frossling numbers were generally higher than those for the smooth cage and those for the hemispherical roughness elements of previous studies. A maximum increase of approximately 306% over the smooth case and 192% over the dense hemispherical roughness case was recorded at one rough glaze ice horn. This work provides some directly measured values of the Frossling number needed to improve the prediction of some icing codes. Such icing codes help in the effective design of some deicing systems of aircraft. C1 Univ Puerto Rico, Dept Mech Engn, Mayaguez, PR 00681 USA. Univ Toledo, Dept Chem Engn, Toledo, OH 43606 USA. Univ Toledo, Mech Ind & Mfg Engn Dept, Toledo, OH 43606 USA. NASA, John H Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA. RP Dukhan, N (reprint author), Univ Puerto Rico, Dept Mech Engn, POB 9045, Mayaguez, PR 00681 USA. NR 25 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 NOV-DEC PY 2003 VL 40 IS 6 BP 1161 EP 1167 DI 10.2514/2.7205 PG 7 WC Engineering, Aerospace SC Engineering GA 756EF UT WOS:000187452300015 ER PT J AU Kim, CS Kim, C Rho, OH AF Kim, CS Kim, C Rho, OH TI Feasibility study of constant eddy-viscosity assumption in gradient-based design optimization SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT AIAA 40th Aerospace Sciences Meeting CY JAN 14-18, 2002 CL RENO, NEVADA SP Amer Inst Aeronaut & Astronaut ID NAVIER-STOKES EQUATIONS; 2-EQUATION TURBULENCE MODELS; SENSITIVITY ANALYSIS AB A feasibility study is carried out by investigating the effects of a usual assumption of constant turbulent eddy viscosity on the aerodynamic design using an adjoint variable method, one of the most efficient gradient-based optimization techniques. Accurate unsteady and steady flow analyses are followed by the aerodynamic sensitivity analysis for the Navier-Stokes equations coupled with two-equation turbulence models. A challengeable approach for high-lift design optimization at higher angles of attack is also proposed, which is based on unsteady sensitivity analysis using a dual time-stepping method and the chimera overset grid scheme. Through the comparison of the sensitivity gradients with respect to all of the design variables including angle of attack, it is observed that the constant turbulent eddy-viscosity assumption might provide inaccurate gradients in sensitivity analyses such as transonic airfoil with a strong shock and high-lift airfoil at a high angle of attack close to stall angle. Simultaneously, however, the final design results indicate that both approaches are acceptable in engineering applications. Both the single- and multi-element airfoil design optimizations using the constant eddy-viscosity assumption are carefully assessed in terms of design accuracy, computer memory overheads, and total design time in various design examples. C1 Seoul Natl Univ, Dept Aerosp Engn, Seoul 151742, South Korea. RP Kim, CS (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 28 TC 6 Z9 6 U1 0 U2 0 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 NOV-DEC PY 2003 VL 40 IS 6 BP 1168 EP 1176 PG 9 WC Engineering, Aerospace SC Engineering GA 756EF UT WOS:000187452300016 ER PT J AU Jegley, DC Bush, HG Lovejoy, AE AF Jegley, DC Bush, HG Lovejoy, AE TI Structural response and failure of a full-scale stitched graphite-epoxy wing SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT AIAA/ASME/ASCE/AHS/ASC 42nd Structures, Structural Dynamics, and Materials Conference CY APR 16-19, 2001 CL SEATTLE, WASHINGTON SP Amer Inst Aeronaut & Astronaut, ASME, ASCE, AHS, ASC AB Analytical and experimental results of the test for an all-composite full-scale wing box are presented. The wing box is representative of a section of a 220-passenger commercial transport aircraft wing box and was designed and constructed by The Boeing Company as part of the NASA Advanced Subsonics Technology program. The semispan wing was fabricated from a graphite-epoxy material system with cover panels and spars held together using Kevlar(R) stitches through the thickness. No mechanical fasteners were used to hold the stiffeners to the skin of the cover panels. Tests were conducted with and without low-speed impact damage, discrete source damage, and repairs. Upbending, downbending, and brake roll loading conditions were applied. The structure with nonvisible impact damage carried 97% of design ultimate load before failure through a lower cover panel access hole. Finite element and experimental results agree for the global response of the structure. C1 NASA, Langley Res Ctr, Mech & Durabil Branch, Hampton, VA 23681 USA. Analyt Serv & Mat Inc, Hampton, VA 23666 USA. RP Jegley, DC (reprint author), NASA, Langley Res Ctr, Mech & Durabil Branch, Hampton, VA 23681 USA. NR 7 TC 1 Z9 1 U1 1 U2 4 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD NOV-DEC PY 2003 VL 40 IS 6 BP 1192 EP 1199 PG 8 WC Engineering, Aerospace SC Engineering GA 756EF UT WOS:000187452300019 ER PT J AU Hefferan, TE Evans, GL Lotinun, S Zhang, M Morey-Holton, E Turner, RT AF Hefferan, TE Evans, GL Lotinun, S Zhang, M Morey-Holton, E Turner, RT TI Effect of gender on bone turnover in adult rats during simulated weightlessness SO JOURNAL OF APPLIED PHYSIOLOGY LA English DT Article DE rat bone; bone formation; bone resorption; spaceflight; disuse osteoporosis ID MESSENGER-RNA LEVELS; GROWTH-FACTOR-I; SPACE-FLIGHT; CANCELLOUS BONE; GROWING RATS; OVARIECTOMIZED RATS; SPACEFLIGHT; ESTROGEN; METABOLISM; HISTOMORPHOMETRY AB Prolonged spaceflight results in bone loss in astronauts, but there is considerable individual variation. The goal of this rat study was to determine whether gender influences bone loss during simulated weightlessness. Six-month-old Fisher 344 rats were hindlimb unweighted for 2 wk, after which the proximal tibiae were evaluated by histomorphometry. There were gender differences in tibia length, bone area, cancellous bone architecture, and bone formation. Compared with female rats, male rats had an 11.6% longer tibiae, a 27.8% greater cortical bone area, and a 37.6% greater trabecular separation. Conversely, female rats had greater cortical (316%) and cancellous (145%) bone formation rates, 28.6% more cancellous bone, and 30% greater trabecular number. Hindlimb unweighting resulted in large reductions in periosteal bone formation and mineral apposition rate in both genders. Unweighting also caused cancellous bone loss in both genders; trabecular number was decreased, and trabecular separation was increased. There was, however, no change in trabecular thickness in either gender. These architectural changes in cancellous bone were associated with decreases in bone formation and steady-state mRNA levels for bone matrix proteins and cancellous bone resorption. In conclusion, there are major gender-related differences in bone mass and turnover; however, the bone loss in hindlimb unweighted adult male and female rats appears to be due to similar mechanisms. C1 Mayo Clin & Mayo Fdn, Dept Orthoped, Rochester, MN 55905 USA. Mayo Clin & Mayo Fdn, Dept Biochem, Rochester, MN 55905 USA. Mayo Clin & Mayo Fdn, Dept Mol Biol, Rochester, MN 55905 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Turner, RT (reprint author), Mayo Clin & Mayo Fdn, Dept Orthoped, Rm 3-69 Med Sci Bldg,200 1st St SW, Rochester, MN 55905 USA. NR 43 TC 40 Z9 44 U1 0 U2 4 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 NOV 01 PY 2003 VL 95 IS 5 BP 1775 EP 1780 DI 10.1152/japplphysiol.00455.2002 PG 6 WC Physiology; Sport Sciences SC Physiology; Sport Sciences GA 730VF UT WOS:000185850300004 PM 12882994 ER PT J AU Dalton, P Gould, M Girten, B Stodieck, LS Bateman, TA AF Dalton, P Gould, M Girten, B Stodieck, LS Bateman, TA TI Preventing annoyance from odors in spaceflight: a method for evaluating the sensory impact of rodent housing SO JOURNAL OF APPLIED PHYSIOLOGY LA English DT Article DE animal habitat; sensory evaluation ID BONE-FORMATION; LONG BONES; FLIGHT; MOUSE; RATS AB For the scientific community, the ability to fly mice under weightless conditions in space offers several advantages over the use of rats. These advantages include the option of testing a range of transgenic animals, the ability to increase the number of animals that can be flown, and reduced demands on shuttle resources ( food, water, animal mass) and crew time (for water refill). Mice have been flown in animal enclosure module (AEM) hardware only once [Space Shuttle Transport System (STS)-90] and were dissected early in the mission, whereas rats have been flown in the AEM on >20 missions. This has been due, in part, to concerns that strong and annoying odors from mouse urine (vs. rat urine) will interfere with crew performance in the shuttle middeck. To screen and approve mice for flight, a method was developed to evaluate the odor containment performance of AEMs housing female C57BL/6J mice compared with AEMs housing Sprague-Dawley rats across a 21-day test period. Based on the results of this test, consensus was reached that mice could fly in the AEM hardware for up to 17 days ( including prelaunch and contingency) and that the AEM hardware would likely contain odors beyond this duration. Human sensory and electronic nose analysis of the AEMs postflight demonstrated their success in containing odors from mice for the mission duration of STS-108 ( 13 days). Although this paper focuses specifically on odor evaluations for the space shuttle, the concern is applicable to any confined, closed-system environment for human habitation. C1 Monell Chem Senses Ctr, Philadelphia, PA 19104 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Colorado, Dept Aerosp Engn Sci, BioServe Space Technol, Boulder, CO 80309 USA. Clemson Univ, Dept Bioengn, Clemson, SC 29634 USA. RP Dalton, P (reprint author), Monell Chem Senses Ctr, 3500 Market St, Philadelphia, PA 19104 USA. FU NIDCD NIH HHS [DC-03704] NR 24 TC 8 Z9 8 U1 0 U2 4 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 NOV 01 PY 2003 VL 95 IS 5 BP 2113 EP 2121 DI 10.1152/japplphysiol.00399.2003 PG 9 WC Physiology; Sport Sciences SC Physiology; Sport Sciences GA 730VF UT WOS:000185850300045 PM 14555673 ER PT J AU Tokay, A Wolff, DB Wolff, KR Bashor, P AF Tokay, A Wolff, DB Wolff, KR Bashor, P TI Rain gauge and disdrometer measurements during the keys area microphysics project (KAMP) SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID DROP SIZE DISTRIBUTION; SIMULATION AB Four impact disdrometers and 27 tipping bucket rain gauges were operated at 11 different sites during August and September 2001, as part of the Keys Area Microphysics Project. The rain gauge and disdrometer network was designed to study the range dependency of radar calibration and rainfall verification in tropical storms. The gauges were collocated at eight sites, while three to five gauge clusters were deployed at three sites. Four disdrometers were also collocated with rain gauges. Overall the experiment was quite successful, although some problems did occur including flooding of gauge loggers, vandalism, and excessive noise at disdrometer sites. Both a south-to-north and east-to-west rainfall gradient was observed, whereby the gauges on the western and northern sides of the Lower Keys recorded more rainfall. Considering the campaign-long rain accumulations, collocated gauges agreed well, with differences generally less than 2%, except for one gauge cluster where the rain accumulation difference was attributed to individual gauge calibration error. The duration of a rain event was sensitive to the definition of a rain event, while this was not a factor in rain intensity. Only 7% of the rain events had significant storm total differences in excess of 2.5 mm. All of these events occurred at storm conditional mean and maximum rain rates higher than 5 and 50 mm h(-1), respectively. Nevertheless, there were many other rain events for which the storm total differences were not significant in heavy rainfall. Combining most of the rain events from all collocated gauge sites, the correlation coefficient and mean percent absolute difference between the gauge storm totals were 0.99 and about 9%, respectively, on average. A rain gauge was typically able to measure rainfall within +/-1.2 mm. As the storm total increased, the standard deviation of the rain total difference and correlation coefficient increased, while mean percent absolute difference decreased. Considering the gauge that recorded higher overall accumulation as the reference, and ignoring the natural variability of rainfall between collocated gauges, the gauge rainfall error was about 9%. Two disdrometers that were placed away from noise sources performed well and recorded higher rainfall accumulation than their collocated rain gauges. C1 NASA, Goddard Space Flight Ctr, Sci Syst Applicat Inc, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. Comp Sci Corp, NASA Wallops Flight Facil, Wallops, VA USA. RP Tokay, A (reprint author), NASA, Goddard Space Flight Ctr, Sci Syst Applicat Inc, Code 912-1, Greenbelt, MD 20771 USA. NR 14 TC 34 Z9 36 U1 2 U2 5 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD NOV PY 2003 VL 20 IS 11 BP 1460 EP 1477 DI 10.1175/1520-0426(2003)020<1460:RGADMD>2.0.CO;2 PG 18 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 740XL UT WOS:000186427900003 ER PT J AU Vay, SA Anderson, BE Thornhill, KL Hudgins, CH AF Vay, SA Anderson, BE Thornhill, KL Hudgins, CH TI An assessment of aircraft-generated contamination on in situ trace gas measurements: Determinations from empirical data acquired aloft SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID AIRBORNE OBSERVATIONS; DIOXIDE AB Results are reported from an experiment conducted aboard the NASA DC-8 research aircraft to determine whether cabin air vented upstream of investigator's inlets had potentially contaminated ambient air samples obtained aboard the aircraft during previous airborne scientific expeditions. For the study, three multiport inlet rakes were mounted in windows downstream of an exhaust vent in locations forward, above, and aft of the right wing. These were used to make impact pressure measurements for determining boundary layer thickness (delta) as well as to collect ambient air samples at various distances outward from the airframe. The fraction of cabin air in the samples was determined by doping the vent air with a metered amount of CO2, then monitoring air at the inlet ports for differential CO2 enhancements. Data were collected at altitudes ranging from the surface to 12 km, at various indicated airspeeds, pitch and yaw angles, and during vertical ascents and descents. Results indicate that delta varies from about 13 to 37 cm and depends on inlet position, as well as the aircraft velocity, altitude, and pitch angle. The CO2-doped vent air was observed to mix throughout the depth of the boundary layer, but to be confined vertically to a narrow stream so that its interception by any particular inlet probe was highly dependent upon the aircraft-indicated airspeed and pitch angle. The inlet located forward of the wing was the most highly impacted, as samples collected there contained up to 0.8% cabin air at cruise altitudes under typical aircraft operating conditions. The implications of these findings on previous datasets are discussed, and a modified formula for calculating delta values appropriate for the DC-8 is proposed. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. Sci Applicat Int Corp, Hampton, VA USA. RP Vay, SA (reprint author), NASA, Langley Res Ctr, MS 483, Hampton, VA 23681 USA. NR 7 TC 1 Z9 1 U1 1 U2 4 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD NOV PY 2003 VL 20 IS 11 BP 1478 EP 1487 DI 10.1175/1520-0426(2003)020<1478:AAOACO>2.0.CO;2 PG 10 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 740XL UT WOS:000186427900004 ER PT J AU Lambert, WC Merceret, FJ Taylor, GE Ward, JG AF Lambert, WC Merceret, FJ Taylor, GE Ward, JG TI Performance of five 915-MHz wind profilers and an associated automated quality control algorithm in an operational environment SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article AB The accuracy and availability of data from a network of 915-MHz boundary layer wind profilers operated by the U.S. Air Force on the Eastern Range are assessed using an automated quality control (QC) algorithm developed by the authors. The accuracy and reliability of the automated algorithm is assessed using the results of an extensive manual examination of the same data used for the assessment of the instruments. The details of the automated algorithm and the manual screening process are provided. Data were collected over a 647-day period from five profilers configured to produce one profile every 15 min, resulting in about 200 000 measurements. The results indicate that the instruments provide reliable, accurate data except when maintenance problems or heavy precipitation are present. Precipitation affected as much as 25% of the measurements in the dataset. The automated QC algorithm proved extremely effective in identifying unacceptable data. Only 0.03% of the data passing automated QC were identified as bad by manual review. While some valid data were identified as bad, the automated algorithm appears to provide exceptional performance for use in automated operational assimilation of boundary profiler data for model initialization and data visualization. C1 ENSCO Inc, Cocoa Beach, FL 32931 USA. NASA Kennedy Space Ctr, Kennedy Space Ctr, FL USA. RP Lambert, WC (reprint author), ENSCO Inc, 1980 N Atlantic Ave,Suite 230, Cocoa Beach, FL 32931 USA. NR 11 TC 11 Z9 14 U1 1 U2 1 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD NOV PY 2003 VL 20 IS 11 BP 1488 EP 1495 DI 10.1175/1520-0426(2003)020<1488:POFMWP>2.0.CO;2 PG 8 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 740XL UT WOS:000186427900005 ER PT J AU Evans, KF Lawson, RP Zmarzly, P O'Connor, D Wiscombe, WJ AF Evans, KF Lawson, RP Zmarzly, P O'Connor, D Wiscombe, WJ TI In situ cloud sensing with multiple scattering lidar: Simulations and demonstration SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID WATER-CONTENT; THICKNESS; RADAR AB Due to the spatially inhomogeneous nature of clouds there are large uncertainties in validating remote sensing retrievals of cloud properties with traditional in situ cloud probes, which have sampling volumes measured in liters. This paper introduces a new technique called in situ cloud lidar, which can measure extinction in liquid clouds with sampling volumes of millions of cubic meters. In this technique a laser sends out pulses of light horizontally from an aircraft inside an optically thick cloud, and wide-field-of-view detectors viewing upward and downward measure the time series of the number of photons returned. Diffusion theory calculations indicate that the expected in situ lidar time series depends on the extinction and has a functional form of a power law times an exponential, with the exponential scale depending on the distance to the cloud boundary. Simulations of 532-nm wavelength in situ lidar time series are made with a Monte Carlo radiative transfer model in stochastically generated inhomogeneous stratocumulus clouds. Retrieval simulations are performed using a neural network trained on three parameters fit to the time series of each detector to predict 1) the extinction at four volume-averaging scales, 2) the cloud geometric thickness, and 3) the optical depth at four averaging scales. Even with an assumed 20% lidar calibration error the rms extinction and optical depth retrieval accuracy is only 12%. Simulations with a dual wavelength lidar (532 and 1550 nm) give accurate retrievals of liquid water content and effective radius. The results of a mountain-top demonstration of the in situ lidar technique show the expected power-law time series behavior. C1 Univ Colorado, Program Atmospher & Ocean Sci, Boulder, CO 80309 USA. SPEC Inc, Boulder, CO USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Evans, KF (reprint author), Univ Colorado, Program Atmospher & Ocean Sci, 311 UCB, Boulder, CO 80309 USA. RI Wiscombe, Warren/D-4665-2012 OI Wiscombe, Warren/0000-0001-6844-9849 NR 26 TC 13 Z9 13 U1 0 U2 2 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD NOV PY 2003 VL 20 IS 11 BP 1505 EP 1522 DI 10.1175/1520-0426(2003)020<1505:ISCSWM>2.0.CO;2 PG 18 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 740XL UT WOS:000186427900007 ER PT J AU Salby, M Sassi, F Callaghan, P Read, W Pumphrey, H AF Salby, M Sassi, F Callaghan, P Read, W Pumphrey, H TI Fluctuations of cloud, humidity, and thermal structure near the tropical tropopause SO JOURNAL OF CLIMATE LA English DT Article ID UPPER-TROPOSPHERIC HUMIDITY; MICROWAVE LIMB SOUNDER; MADDEN-JULIAN OSCILLATION; WATER-VAPOR; LOWER STRATOSPHERE; WESTERN PACIFIC; UARS MLS; DEHYDRATION MECHANISM; MULTIPLE SATELLITES; DEEP CONVECTION AB Thermal and humidity structures near the tropical tropopause are studied using microwave satellite retrievals of water vapor, along with contemporaneous dynamical structure in ECMWF analyses and cold clouds in high-resolution global cloud imagery. Examined during November 1991 - February 1992, these fields all vary coherently with the outflow from convective centers - in the upper troposphere as well as in the lowermost stratosphere. The outbreak of deep convection is accompanied by diabatic heating below a level between 250 and 150 mb but by diabatic cooling at higher levels. The reversal from heating to cooling is broadly consistent with cumulus detrainment. Through irreversible mixing, that process serves as a heat source for the environment below the level of neutral buoyancy (LNB) but as a heat sink at higher levels. Calculations, inclusive of entrainment, place the LNB very near the observed reversal from heating to cooling. The outbreak of convection is also accompanied by humidification below 125 mb but by dehydration at higher levels. The reversal from humidification to dehydration coincides with levels where environmental conditions approach saturation. Those conditions suggest the efficient removal of total water from cumulus updrafts, leaving dessicated air to ventilate to higher levels. Cumulus detrainment then acts to humidify the environment beneath the zone of nearly saturated environmental conditions, while dehydrating it at higher levels. Dry air emerges from the region of the coldest cloud. It then extends into the winter hemisphere, along streamlines that characterize the Hadley circulation. Coinciding with diabatic cooling are stratospheric convergence and downwelling. These features of stratospheric motion amplify simultaneously with divergence at tropospheric levels, which represents the major outflow from deep convection. The deepest convection, found over the equatorial Pacific, coincides with the highest moist static energy. The latter yields an LNB that is some 3 km higher over the equatorial Pacific than elsewhere, in agreement with the observed reversal from heating to cooling. Observed brightness temperatures place the level at which cumulus anvils are most extensive very near the cold point over the equatorial Pacific. This, in turn, lies near the tropical tropopause throughout the Tropics. Collectively, these features suggest that the coldest cloud, found over the equatorial Pacific, plays a key role in maintaining temperature and humidity near the tropical tropopause. C1 Atmospher Syst & Anal, Broomfield, CO 80020 USA. Univ Colorado, Boulder, CO 80309 USA. NASA, Jet Prop Lab, Pasadena, CA USA. Univ Edinburgh, Edinburgh, Midlothian, Scotland. RP Sassi, F (reprint author), Atmospher Syst & Anal, 12995 Sheridan Blvd, Broomfield, CO 80020 USA. OI Sassi, Fabrizio/0000-0002-9492-7434 NR 49 TC 22 Z9 24 U1 1 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 NOV 1 PY 2003 VL 16 IS 21 BP 3428 EP 3446 DI 10.1175/1520-0442(2003)016<3428:FOCHAT>2.0.CO;2 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 734WW UT WOS:000186081800003 ER PT J AU Minnis, P Ayers, JK Nordeen, ML Weaver, SP AF Minnis, P Ayers, JK Nordeen, ML Weaver, SP TI Contrail frequency over the United States from surface observations SO JOURNAL OF CLIMATE LA English DT Article ID GLOBAL DISTRIBUTION; CLIMATE; SATELLITE; CIRRUS AB Contrails have the potential for affecting climate because they impact the radiation budget and the vertical distribution of moisture. Estimating the effect requires additional knowledge about the temporal and spatial variations of contrails. The mean hourly, monthly, and annual frequencies of daytime contrail occurrence are estimated using 2 yr of observations from surface observers at military installations scattered over the continental United States. During both years, persistent contrails are most prevalent in the winter and early spring and are seen least often during the summer. They co-occur with cirrus clouds 85% of the time. The annual mean persistent contrail frequencies in unobscured skies dropped from 0.152 during 1993 - 94 to 0.124 in 1998 - 99 despite a rise in air traffic. Mean hourly contrail frequencies reflect the pattern of commercial air traffic, with a rapid increase from sunrise to midmorning followed by a very gradual decrease during the remaining daylight hours. Although highly correlated with air traffic fuel use, contrail occurrence is governed by meteorological conditions. It is negatively and positively correlated with the monthly mean 300-hPa temperature and 300-hPa relative humidity, respectively, from the National Centers for Environmental Prediction (NCEP) reanalyses. A simple empirical model employing the fuel use and the monthly mean 300-hPa temperatures and relative humidities yields a reasonable representation of the seasonal variation in contrail frequency. The interannual drop in contrail frequency coincides with a decrease in mean 300-hPa relative humidities from 45.8% during the first period to 38.2% in 1998 - 99, one of the driest periods in the NCEP record. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. AS&M Inc, Hampton, VA USA. 88th Weather Squadron, Wright Patterson AFB, OH USA. RP Minnis, P (reprint author), NASA, Langley Res Ctr, MS 420, Hampton, VA 23681 USA. RI Minnis, Patrick/G-1902-2010 OI Minnis, Patrick/0000-0002-4733-6148 NR 29 TC 22 Z9 23 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 NOV 1 PY 2003 VL 16 IS 21 BP 3447 EP 3462 DI 10.1175/1520-0442(2003)016<3447:CFOTUS>2.0.CO;2 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 734WW UT WOS:000186081800004 ER PT J AU Comiso, JC AF Comiso, JC TI Warming trends in the Arctic from clear sky satellite observations SO JOURNAL OF CLIMATE LA English DT Article ID GREENLAND ICE-SHEET; SURFACE AIR-TEMPERATURE; SEA-ICE; OCEAN; CLIMATE; VARIABILITY; COVER; OSCILLATION; BALANCE; DECREASE AB Satellite thermal infrared data on surface temperatures provide pan-Arctic coverage from 1981 to 2001 during cloud-free conditions and reveal large warming anomalies in the 1990s compared to the 1980s and regional variability in the trend. The rms error of the derived surface temperatures when compared with in situ data ranges from 1.5 to 3 K over the 20-yr period. Average temperature trends are generally positive at 0.33 +/- 0.16degreesC decade(-1) over sea ice, 0.50 +/- 0.22degreesC decade(-1) over Eurasia, and 1.06 +/- 0.22degreesC decade(-1) over North America. The trend is slightly negative and insignificant at -0.09 +/- 0.25degreesC decade(-1) in Greenland with the negatives mainly at high elevations. The trends are also predominantly positive in spring, summer, and autumn causing the lengthening of the melt season by 10 - 17 days per decade while they are generally negative in winter. The longer-term in situ surface temperature data shows that the 20-yr trend is 8 times larger than the 100-yr trend suggesting a rapid acceleration in the warming that may be associated with the recent change in phase of the Arctic Oscillation that has been linked to increasing greenhouse gases in the atmosphere. C1 NASA, Goddard Space Flight Ctr, Oceans & Ice Branch, Greenbelt, MD 20771 USA. RP Comiso, JC (reprint author), NASA, Goddard Space Flight Ctr, Oceans & Ice Branch, Code 971, Greenbelt, MD 20771 USA. NR 39 TC 206 Z9 209 U1 3 U2 31 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 NOV 1 PY 2003 VL 16 IS 21 BP 3498 EP 3510 DI 10.1175/1520-0442(2003)016<3498:WTITAF>2.0.CO;2 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 734WW UT WOS:000186081800008 ER PT J AU Wang, XC Jin, FF Wang, YQ AF Wang, XC Jin, FF Wang, YQ TI A tropical ocean recharge mechanism for climate variability. Part I: Equatorial heat content changes induced by the off-equatorial wind SO JOURNAL OF CLIMATE LA English DT Article ID INTERDECADAL VARIABILITY; VENTILATED THERMOCLINE; NORTH PACIFIC; MODEL; ENSO; DYNAMICS; IMPACTS; STRESS AB A reduced-gravity shallow-water model, an oceanic general circulation model for the Pacific region, and the analytical model of the equatorial beta plane bounded in the zonal direction are used to investigate the equatorial thermocline response to tropical and subtropical wind stress forcing. The results show that the wind stress forcing in the tropical and subtropical region can generate a nearly zonal uniform thermocline depth change in the equatorial region. The response timescale is longer when the wind stress is placed farther away from the equator. There exist latitude bands around 10degrees-15degreesN and 10degrees-15degreesS where the forcing can cause a relatively large equatorial response. When the forcing is located in the eastern basin, the response timescale is longer and its magnitude is larger than the case when the forcing is located in the western basin. Thus the eastern tropical to subtropical region is a relatively effective area for off-equatorial wind stress to generate an equatorial thermocline response. When the wind stress forcing has a longer period, the response of the equatorial thermocline has a larger magnitude. The results from this study's numerical experiments and the analytical solution are consistent. The present study has implications for the broad-scale ocean-atmosphere interaction in the tropical region. C1 Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Dept Meteorol, Honolulu, HI 96822 USA. Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Int Pacific Res Ctr, Honolulu, HI 96822 USA. RP Wang, XC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 300-323, Pasadena, CA 91109 USA. NR 32 TC 20 Z9 21 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 NOV PY 2003 VL 16 IS 22 BP 3585 EP 3598 DI 10.1175/1520-0442(2003)016<3585:ATORMF>2.0.CO;2 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 742MT UT WOS:000186522100004 ER PT J AU Wang, XC Jin, FF Wang, YQ AF Wang, XC Jin, FF Wang, YQ TI A tropical ocean recharge mechanism for climate variability. Part II: A unified theory for decadal and ENSO modes SO JOURNAL OF CLIMATE LA English DT Article ID SEA-SURFACE TEMPERATURE; NORTH PACIFIC-OCEAN; SELF-EXCITED OSCILLATIONS; ATMOSPHERE INTERACTION; INTERDECADAL VARIABILITY; ANALYTICAL PROTOTYPES; GENERAL-CIRCULATION; SST ANOMALIES; DYNAMICS; SYSTEM AB Decadal to interdecadal timescale variability in the Pacific region, commonly referred to as the Pacific decadal oscillation (PDO), is studied in this research using analytical and numerical models. A coupled analytical model is formulated to analyze the physical mechanism of both the PDO and ENSO. It has the equatorial beta-plane dynamics of a reduced-gravity model coupled with the wind stress of fixed spatial patterns. The amplitude of the latter is proportional to the sea surface temperature (SST) anomaly in the eastern equatorial Pacific. The SST anomaly is governed by a simple thermal dynamic equation used for ENSO modeling. It is found that when a warm SST is coupled with cyclonic wind stress patterns in the eastern subtropical Pacific, an oscillation with a timescale of around 10-15 yr could be generated. In contrast, when a warm SST is coupled with only a westerly wind stress in the central equatorial Pacific, an ENSO-like oscillation could be generated with a timescale of around 3-5 yr. Thus the present research is potentially relevant to aspects of the PDO and the mechanism of the PDO may be understood as a weakly coupled decadal recharge oscillator similar to the recharge oscillator dynamics of ENSO. The sensitivity of these two kinds of coupled modes to different parameters is tested. Numerical integrations with the reduced-gravity shallow-water model in a rectangular basin and a similar coupled framework confirm the results of the analytical model. C1 Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Dept Meteorol, Honolulu, HI 96822 USA. Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Int Pacific Res Ctr, Honolulu, HI 96822 USA. RP Wang, XC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 300-323, Pasadena, CA 91109 USA. NR 50 TC 17 Z9 18 U1 0 U2 4 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 NOV PY 2003 VL 16 IS 22 BP 3599 EP 3616 DI 10.1175/1520-0442(2003)016<3599:ATORMF>2.0.CO;2 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 742MT UT WOS:000186522100005 ER PT J AU Straus, D Shukla, J Paolino, D Schubert, S Suarez, M Pegion, P Kumar, A AF Straus, D Shukla, J Paolino, D Schubert, S Suarez, M Pegion, P Kumar, A TI Predictability of the seasonal mean atmospheric circulation during autumn, winter, and spring SO JOURNAL OF CLIMATE LA English DT Article ID SEA-SURFACE TEMPERATURE; EQUATORIAL PACIFIC; SST ANOMALIES; EL-NINO; ENSO; VARIABILITY; CLIMATE; MODEL; PREDICTIONS; SIMULATIONS AB The predictability of the autumn, boreal winter, and spring seasons with foreknowledge of sea surface temperatures (SSTs) is studied using ensembles of seasonal simulations of three general circulation models (GCMs): the Center for Ocean-Land-Atmosphere Studies (COLA) GCM, the National Aeronautics and Space Administration Seasonal to Interannual Prediction Project (NSIPP) GCM, and the National Centers for Environmental Prediction (NCEP) GCM. Warm-minus-cold composites of the ensemble mean and observed tropical Pacific precipitation, averaged for the three warmest El Nino and three coldest La Nina winters, show large positive anomalies near the date line that extend eastward to the South American coast. The same is true for composites of the spring following the event. In the composites of the autumn preceding the event, the precipitation is weaker and shifted off the equator in the far eastern Pacific, where equatorial SSTs are too low to support convection. The corresponding boreal winter 200-hPa height composites show strong signals in the Tropics and midlatitudes of both hemispheres. The subsequent spring composites are similar, but weaker in the northern extratropics. In the preceding autumn composites, the overall height signal is quite weak, except in the southern Pacific. The model dependence of the signal (variance of ensemble means) and noise (variance about the ensemble means) of the seasonal mean 200-hPa height is small, a result that holds for all three seasons and is in contrast to earlier studies. The signal-to-noise ratio is significantly greater than unity in the Tropics (all seasons), the northern Pacific and continental North America subtropics (boreal winter and spring), and the southern Pacific subtropics (boreal autumn). Rotated empirical orthogonal function analysis of the tropical Pacific SST recovers El Nino-like dominant patterns in boreal winter and spring, but emphasizes two SST patterns in autumn, one with largest SST in the far eastern tropical Pacific and one with a maximum nearer the date line. Two methods are used to assess the precipitation and height field responses to these patterns: linear regression of the ensemble means on the principal component (PC) time series of SST and identification of patterns that optimize the signal-to-noise ratio. The two methods yield remarkably similar results. The optimal height patterns for boreal winter and spring are similar, although the spring response over the northern extratropics is somewhat weaker, and some subtle changes in phase are found in all three GCMs. The associated optimal time series have serial correlations with the leading PC of SST that exceed 0.9 for all GCMs for winter and spring. For autumn the time series of the leading two optimal patterns each has a serial correlation with the corresponding PC of SST that exceeds 0.7 for the COLA and NSIPP GCMs. The autumn 200-hPa-height leading optimal pattern (response to eastern Pacific SST) is quite weak, representing nearly uniform tropical warming. The second optimal pattern (response to central Pacific SST) shows a robust wave train in the southern Pacific, with a consistent belt of low height over northern midlatitudes. C1 Ctr Ocean Land Atmosphere Studies, Calverton, MD USA. George Mason Univ, Fairfax, VA 22030 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Natl Ctr Environm Predict, Washington, DC USA. RP Straus, D (reprint author), 4041 Powder Mill Rd,Ste 302, Calverton, MD 20705 USA. RI Pegion, Philip/E-5247-2012 NR 33 TC 17 Z9 19 U1 0 U2 4 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 NOV PY 2003 VL 16 IS 22 BP 3629 EP 3649 DI 10.1175/1520-0442(2003)016<3629:POTSMA>2.0.CO;2 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 742MT UT WOS:000186522100007 ER PT J AU Steiner, M Bell, TL Zhang, Y Wood, EF AF Steiner, M Bell, TL Zhang, Y Wood, EF TI Comparison of two methods for estimating the sampling-related uncertainty of satellite rainfall averages based on a large radar dataset SO JOURNAL OF CLIMATE LA English DT Article ID MEASURING MISSION TRMM; TIME STOCHASTIC-MODEL; TROPICAL RAINFALL; DIURNAL CYCLE; GAUGE DATA; ERRORS; SPACE; PRECIPITATION; SCALE; SSM/I AB The uncertainty of rainfall estimated from averages of discrete samples collected by a satellite is assessed using a multiyear radar dataset covering a large portion of the United States. The sampling-related uncertainty of rainfall estimates is evaluated for all combinations of 100-, 200-, and 500-km space domains; 1-, 5-, and 30-day rainfall accumulations; and regular sampling time intervals of 1, 3, 6, 8, and 12 h. These extensive analyses are combined to characterize the sampling uncertainty as a function of space and time domain, sampling frequency, and rainfall characteristics by means of a simple scaling law. Moreover, it is shown that both parametric and nonparametric statistical techniques of estimating the sampling uncertainty produce comparable results. Sampling uncertainty estimates, however, do depend on the choice of technique for obtaining them. They can also vary considerably from case to case, reflecting the great variability of natural rainfall, and should therefore be expressed in probabilistic terms. Rainfall calibration errors are shown to affect comparison of results obtained by studies based on data from different climate regions and/or observation platforms. C1 Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Steiner, M (reprint author), Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. RI Bell, Thomas/G-5425-2012; Steiner, Matthias/K-5013-2013; OI Steiner, Matthias/0000-0002-3973-375X; Wood, Eric/0000-0001-7037-9675 NR 47 TC 73 Z9 74 U1 0 U2 5 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 NOV PY 2003 VL 16 IS 22 BP 3759 EP 3778 DI 10.1175/1520-0442(2003)016<3759:COTMFE>2.0.CO;2 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 742MT UT WOS:000186522100015 ER PT J AU Hshieh, FY Hirsch, D Beeson, H AF Hshieh, FY Hirsch, D Beeson, H TI Evaluation of polyimide foam as a fire barrier for spacecraft cushion materials SO JOURNAL OF FIRE SCIENCES LA English DT Article DE polyimide foam; fire barrier; spacecraft cushion materials; NASA upward flame propagation test; cone calorimeter test AB Polyimide foam is an intrinsically flame resistant foam material. This study uses the NASA upward flame propagation test and the cone calorimeter test to evaluate the application of polyimide foam as a fire barrier for spacecraft cushion materials. The flame propagation test results demonstrate that a thin-layer of polyimide foam (3-mm thick) could totally stop the flame spread on the underneath polyurethane foam in an environment containing 30% oxygen. The cone calorimeter test results show that polyimide foam increased the minimum heat flux for ignition of a cushion sample from 27 to 48 kW/m(2). This suggests that application of polyimide foam can significantly reduce the ignition risk. It was also found that polyimide foam significantly reduced the peak heat release rate, mass burning rate, and the generation of carbon monoxide and smoke in the flaming combustion. For polyimide foam-covered polyurethane, smoldering combustion was insignificant at 25 and 35 kW/m(2) incident heat fluxes; it became more important when the incident heat flux reached 45 kW/m(2). The smoldering combustion of polyurethane foam and polyimide foam-covered polyurethane could not be self-sustaining if the external heat source was removed. C1 Honeywell Technol Solut Inc, NASA, Lyndon B Johnson Space Ctr, White Sands Test Facil, Las Cruces, NM 88004 USA. RP Hshieh, FY (reprint author), Honeywell Technol Solut Inc, NASA, Lyndon B Johnson Space Ctr, White Sands Test Facil, POB 20, Las Cruces, NM 88004 USA. NR 8 TC 1 Z9 1 U1 1 U2 9 PU SAGE PUBLICATIONS LTD PI LONDON PA 6 BONHILL STREET, LONDON EC2A 4PU, ENGLAND SN 0734-9041 J9 J FIRE SCI JI J. Fire Sci. PD NOV PY 2003 VL 21 IS 6 BP 485 EP 501 DI 10.1177/073490403038033 PG 17 WC Engineering, Multidisciplinary; Materials Science, Multidisciplinary SC Engineering; Materials Science GA 744ND UT WOS:000186637800005 ER PT J AU Smith, MD Bandfield, JL Christensen, PR Richardson, MI AF Smith, MD Bandfield, JL Christensen, PR Richardson, MI TI Thermal Emission Imaging System (THEMIS) infrared observations of atmospheric dust and water ice cloud optical depth SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; THEMIS; dust; water ice; optical depth; cloud ID SPECTROMETER TES OBSERVATIONS; MARTIAN ATMOSPHERE; MGS-TES; MARS; SURFACE; VIKING; TEMPERATURES; APHELION; MISSION; SPECTROSCOPY AB [1] The Mars Odyssey spacecraft entered into Martian orbit in October 2001 and after successful aerobraking, began mapping in February 2002. Thermal infrared images taken by the Thermal Emission Imaging System (THEMIS) on board the Odyssey spacecraft allow for the quantitative retrieval of atmospheric dust and water ice aerosol optical depth. Data collected so far cover late northern winter, spring, and summer (L-s = 330degrees - 160degrees). During this period, THEMIS observed the decay of a regional dust storm, a number of local dust storms along the edge of the retreating north polar cap, and the growth of the low-latitude aphelion water ice cloud belt. Data from THEMIS complements the concurrent Mars Global Surveyor Thermal Emission Spectrometer (TES) data by sampling a later local time ( similar to 1400 LT for TES versus similar to 1600 - 1730 LT for THEMIS) and by observing at much higher spatial resolution. Comparison of water ice optical depth in the aphelion cloud belt from THEMIS and TES shows a significantly higher optical depth in the late afternoon ( THEMIS) than in the early afternoon ( TES). C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Arizona State Univ, Dept Geol, Tempe, AZ 85287 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Smith, MD (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 693, Greenbelt, MD 20771 USA. RI Smith, Michael/C-8875-2012 NR 34 TC 31 Z9 33 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 NOV 1 PY 2003 VL 108 IS E11 AR 5115 DI 10.1029/2003JE002115 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 740HQ UT WOS:000186397300001 ER PT J AU Kil, H Paxton, LJ Pi, XQ Hairston, MR Zhang, YL AF Kil, H Paxton, LJ Pi, XQ Hairston, MR Zhang, YL TI Case study of the 15 July 2000 magnetic storm effects on the ionosphere-driver of the positive ionospheric storm in the winter hemisphere SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE ionospheric storm; ionosphere-thermosphere coupling; thermospheric disturbance ID GENERAL-CIRCULATION MODEL; EQUATORIAL TOPSIDE IONOSPHERE; TOTAL ELECTRON-CONTENT; GEOMAGNETIC STORMS; FAR-ULTRAVIOLET; F-REGION; THERMOSPHERIC COMPOSITION; MIDDLE LATITUDES; UPPER-ATMOSPHERE; FUV DAYGLOW AB The ionospheric response to the magnetic storm of 15 July 2000 is investigated using the global total electron content (TEC) maps provided by global positioning system and the measurements of ion density, composition, and drift velocity from the Defense Meteorological Satellite Program (DMSP) F13 and F15 spacecraft. The global TEC maps showed clear seasonal effects that can be characterized by a dominance of a negative ionospheric storm (decrease in plasma density) in the summer (northern) hemisphere and the pronounced positive ionospheric storm ( increase in plasma density) in the winter (southern) hemisphere. The northern negative storm phase rapidly expanded to the equator at midnight and even penetrated to the opposite hemisphere during the storm main phase. In the southern hemisphere, the negative storm phase began in the morning sector but was confined to narrow latitude and local time sectors owing to strong poleward winds and ion drag on the dayside. The negative storm phases in the opposite hemispheres kept out of phase, lasted for a day, and corotated with Earth. These characteristics show good qualitative similarity with the predictions of global model simulations. The positive storm phase prevailed in the southern low-middle latitudes and was most pronounced during nighttime. In that region, the quiet time DMSP measurements at 1800 LT, 2100 LT, 0600 LT, and 0900 LT showed low ion density, low O+ proportion, and large downward ion drift velocity compared with those in the northern hemisphere. During storm time the O+ proportion and ion concentration increased to the levels seen in the northern hemisphere while the downward ion drift velocity was much decreased. The excellent temporal and spatial correspondence of the increase in ion concentration with the decrease in downward ion drift velocity indicates that the maintenance of the F layer at high altitudes by the storm-induced equatorward neutral winds was the main driver of the positive ionospheric storm. The quiet time hemispheric asymmetry was most significant at nighttime, and therefore the positive storm effect appeared most pronounced at nighttime in the winter hemisphere. C1 Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. Univ Texas, WB Hanson Ctr Space Sci, Richardson, TX 75083 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kil, H (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. RI Paxton, Larry/D-1934-2015; Kil, Hyosub/C-2577-2016; Zhang, Yongliang/C-2180-2016 OI Paxton, Larry/0000-0002-2597-347X; Kil, Hyosub/0000-0001-8288-6236; Zhang, Yongliang/0000-0003-4851-1662 NR 97 TC 35 Z9 36 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD NOV 1 PY 2003 VL 108 IS A11 AR 1391 DI 10.1029/2002JA009782 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 740JA UT WOS:000186398200002 ER PT J AU Johnson, WR Longuski, JM Lyons, DT AF Johnson, WR Longuski, JM Lyons, DT TI Nondimensional analysis of reaction-wheel control for aerobraking SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article ID MARS GLOBAL SURVEYOR; EXPLORATION; MAGELLAN; DESIGN AB The equations of motion for an aerobraking spacecraft are nondimensionalized. This process yields three dimensionless parameters that intrinsically describe the capability of a reaction-wheel controller to manage angular momentum during an atmospheric drag pass. These parameters, namely aeromoment, desaturation speed, and equilibrium momentum, completely characterize the behavior of all reaction-wheel controllers for aerobraking at any planet. As the names imply, the behavior is determined by the density of the atmosphere, the torque of the reaction wheel, and the moment of inertia of the spacecraft (and associated parameters). Theoretical bounds on the three parameters are found, and comparisons to past aerobraking spacecraft are made. Numerical simulations demonstrate that the established bounds correctly predict the performance exhibited during aerobraking. C1 Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Johnson, WR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 18 TC 1 Z9 2 U1 0 U2 0 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD NOV-DEC PY 2003 VL 26 IS 6 BP 861 EP 868 DI 10.2514/2.6930 PG 8 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 741CY UT WOS:000186442200005 ER PT J AU Ward, BJ Liu, CC Hunter, GW AF Ward, BJ Liu, CC Hunter, GW TI Novel processing of NASICON and sodium carbonate/barium carbonate thin and thick films for a CO2 microsensor SO JOURNAL OF MATERIALS SCIENCE LA English DT Article ID SENSOR AB The use of chemical microsensors can be advantageous for the monitoring of gas species in efforts to accurately monitor environmental conditions, detect fires, and determine emissions. The microsensor described herein shows promise for use as a carbon dioxide sensor. Carbon dioxide levels are of particular concern for passenger environments, as a chemical signature of a fire, and as a combustion product. This amperometric carbon dioxide microsensor was produced using microfabrication and micromachining techniques. Electron beam evaporation, sputtering, and thick film printing were used for deposition of the chemically active layers of the device-Na3Zr2Si2PO12 (NASICON) and Na2CO3/Ba2CO3. The deposition techniques used to deposit these materials were an important processing advance in this development endeavor. The films were incorporated into an amperometric, limiting current type sensor design with overall dimensions of 1.4 mm x 1.5 mm. The inclusion of this type of sensor in an array of differing sensors offers an advantage of high selectivity to analytes of interest. (C) 2003 Kluwer Academic Publishers. C1 Case Western Reserve Univ, Ctr Elect Design, Cleveland, OH 44106 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Ward, BJ (reprint author), Makel Engn Inc, Chico, CA 95973 USA. NR 13 TC 9 Z9 9 U1 1 U2 6 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0022-2461 J9 J MATER SCI JI J. Mater. Sci. PD NOV 1 PY 2003 VL 38 IS 21 BP 4289 EP 4292 DI 10.1023/A:1026374830114 PG 4 WC Materials Science, Multidisciplinary SC Materials Science GA 738CZ UT WOS:000186270300007 ER PT J AU Frisbee, RH AF Frisbee, RH TI Advanced space propulsion for the 21st century SO JOURNAL OF PROPULSION AND POWER LA English DT Article ID TRAVEL C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Frisbee, RH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 98 TC 50 Z9 54 U1 1 U2 5 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 NOV-DEC PY 2003 VL 19 IS 6 BP 1129 EP 1154 DI 10.2514/2.6948 PG 26 WC Engineering, Aerospace SC Engineering GA 746TB UT WOS:000186762800008 ER PT J AU Wang, J Polk, J Brophy, J Katz, I AF Wang, J Polk, J Brophy, J Katz, I TI Three-dimensional particle simulations of ion-optics plasma flow and grid erosion SO JOURNAL OF PROPULSION AND POWER LA English DT Article ID DYNAMIC ADI; ENVIRONMENT; EQUATIONS AB A fully three-dimensional computer particle simulation model for ion optics is developed. This model allows multiple apertures to be included explicitly in the simulation domain and determines the upstream sheath and downstream beam neutralization through simulations. Simulations are performed for the NSTAR ion-thruster optics, and results are compared with grid-erosion measurements obtained during NSTAR long-duration test. It is shown that the simulation not only predicts accurately all of the features in the measured erosion pattern but also gives excellent quantitative agreement with the measured erosion depth. C1 Virginia Polytech Inst & State Univ, Blacksburg, VA 24061 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Wang, J (reprint author), Virginia Polytech Inst & State Univ, Blacksburg, VA 24061 USA. NR 19 TC 21 Z9 30 U1 1 U2 2 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 NOV-DEC PY 2003 VL 19 IS 6 BP 1192 EP 1199 DI 10.2514/2.6939 PG 8 WC Engineering, Aerospace SC Engineering GA 746TB UT WOS:000186762800011 ER PT J AU Cardiff, EH AF Cardiff, EH TI Inconsistent definitions of pressure-coupled responses and admittances of solid propellants SO JOURNAL OF PROPULSION AND POWER LA English DT Article ID SURFACE C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Cardiff, EH (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 4 TC 1 Z9 1 U1 0 U2 1 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 NOV-DEC PY 2003 VL 19 IS 6 BP 1217 EP 1218 DI 10.2514/2.6941 PG 2 WC Engineering, Aerospace SC Engineering GA 746TB UT WOS:000186762800013 ER PT J AU Rothman, LS Barbe, A Benner, DC Brown, LR Camy-Peyret, C Carleer, MR Chance, K Clerbaux, C Dana, V Devi, VM Fayt, A Flaud, JM Gamache, RR Goldman, A Jacquemart, D Jucks, KW Lafferty, WJ Mandin, JY Massie, ST Nemtchinov, V Newnham, DA Perrin, A Rinsland, CP Schroeder, J Smith, KM Smith, MAH Tang, K Toth, RA Vander Auwera, J Varanasi, P Yoshino, K AF Rothman, LS Barbe, A Benner, DC Brown, LR Camy-Peyret, C Carleer, MR Chance, K Clerbaux, C Dana, V Devi, VM Fayt, A Flaud, JM Gamache, RR Goldman, A Jacquemart, D Jucks, KW Lafferty, WJ Mandin, JY Massie, ST Nemtchinov, V Newnham, DA Perrin, A Rinsland, CP Schroeder, J Smith, KM Smith, MAH Tang, K Toth, RA Vander Auwera, J Varanasi, P Yoshino, K TI The HITRAN molecular spectroscopic database: edition of 2000 including updates through 2001 SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Review DE HITRAN; spectroscopic database; molecular spectroscopy; molecular absorption; absorption cross-sections; aerosol refractive indices ID ABSORPTION CROSS-SECTIONS; TUNABLE DIODE-LASER; HETERODYNE FREQUENCY MEASUREMENTS; FOURIER-TRANSFORM SPECTROSCOPY; ABSOLUTE LINE-INTENSITIES; MULTISPECTRUM FITTING PROCEDURE; CARBONYL SULFIDE TRANSITIONS; AIR-BROADENING COEFFICIENTS; COMPLEX REFRACTIVE-INDEXES; INFRARED OPTICAL-CONSTANTS AB This paper describes the status circa 2001, of the HITRAN compilation that comprises the public edition available through 2001. The HITRAN compilation consists of several components useful for radiative transfer calculation codes: high-resolution spectroscopic parameters of molecules in the gas phase, absorption cross-sections for molecules with very dense spectral features, aerosol refractive indices, ultraviolet line-by-line parameters and absorption cross-sections, and associated database management software. The line-by-line portion of the database contains spectroscopic parameters for 38 molecules and their isotopologues and isotopomers suitable for calculating atmospheric transmission and radiance properties. Many more molecular species are presented in the infrared cross-section data than in the previous edition, especially the chlorofluorocarbons and their replacement gases. There is now sufficient representation so that quasi-quantitative simulations can be obtained with the standard radiance codes. In addition to the description and justification of new or modified data that have been incorporated since the last edition of HITRAN (1996), future modifications are indicated for cases considered to have a significant impact on remote-sensing experiments. (C) 2003 Elsevier Ltd. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. Univ Reims, Grp Spectrometrie Mol & Atmospher, F-51062 Reims, France. Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Paris 06, Lab Phys Mol & Applicat, F-75252 Paris, France. Univ Libre Brussels, Lab Chim Phys Mol, B-1050 Brussels, Belgium. Univ Paris 06, Serv Aeron, F-75252 Paris, France. Catholic Univ Louvain, Lab Spect Mol, B-1348 Louvain, Belgium. Univ Paris 11, CNRS, Photophys Mol Lab, F-91405 Orsay, France. Univ Mass Lowell, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA. Univ Denver, Dept Phys, Denver, CO 80208 USA. Natl Ctr Atmospher Res, Boulder, CO 80307 USA. SUNY Stony Brook, Stony Brook, NY 11794 USA. Rutherford Appleton Lab, Didcot OX11 OQX, Oxon, England. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Ontar Corp, N Andover, MA 01845 USA. NIST, Opt Technol Div, Gaithersburg, MD 20899 USA. RP Rothman, LS (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. EM lrothman@cfa.harvard.edu RI clerbaux, cathy/I-5478-2013; OI Rothman, Laurence/0000-0002-3837-4847; Chance, Kelly/0000-0002-7339-7577 NR 178 TC 792 Z9 822 U1 7 U2 52 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 NOV-DEC PY 2003 VL 82 IS 1-4 BP 5 EP 44 DI 10.1016/S0022-4073(03)00146-8 PG 40 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 711KG UT WOS:000184738800002 ER PT J AU Goldman, A Stephen, TM Rothman, LS Giver, LP Mandin, JY Gamache, RR Rinsland, CP Murcray, FJ AF Goldman, A Stephen, TM Rothman, LS Giver, LP Mandin, JY Gamache, RR Rinsland, CP Murcray, FJ TI The 1-mu m CO2 bands and the O-2 (0-1) X-3 Sigma(-)(g) a(1)Delta(g) and (1-0) X-3 Sigma(-)(g)- b(1)Sigma g(+) bands in the Earth atmosphere SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article ID INTEGRATED ABSORPTION INTENSITIES; INTERACTING VIBRATIONAL-STATES; IMPROVED SPECTRAL PARAMETERS; COLLISION-INDUCED ABSORPTION; LINE POSITIONS; PRESSURE-SHIFT; BROADENING COEFFICIENTS; MOLECULAR-OXYGEN; WAVE-NUMBERS; MU-M AB The CO2 triad of bands in the 9300-9700 cm(-1) region have been observed in near infrared 0.05 cm(-1) resolution ground-based solar absorption spectra. This interval is a portion of spectra taken in the 900012,000 cm(-1) region, at large solar zenith angles. Considering the available line positions and pressure line shifts for CO2, H2O and O-2 in this region as of 2000, it was concluded that these observations show significant inconsistencies among the line positions of the species as listed in the atmospheric spectroscopy databases. The spectra allow a better definition of the O-2 (0-1) X(3)Sigma(g)(-) - a(1)Delta(g) band, with the discrete (0-1) transitions observable in the 9300-9450 cm(-1), superimposed on a collision-induced continuum covering the 9200-9700 cm(-1) region. This continuum, as well as the (0-0) continuum in the 7900 cm(-1) region, have been previously studied only from atmospheric spectra with much lower spectral resolution. The discrete O-2 (1-0) transitions of the X(3)Sigma(g)(-) - b(1)Sigma(g)(+) atmospheric B-band are observed in the 11,500-11,600 cm(-1) region, but no evidence is found for an underlying continuum. A recent laboratory study of the 2v(1) + 3v(3) (CO2)-C-12 triad significantly improves the consistency between the O-2, H2O and CO2 lines in the atmospheric spectra. (C) 2003 Elsevier Ltd. All rights reserved. C1 Univ Denver, Dept Phys, Denver, CO 80208 USA. Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. NASA, Ames Res Ctr, Atmospher Phys Branch, Moffett Field, CA 94035 USA. Univ Paris 06, CNRS, Lab Phys Mol & Applicat, F-75252 Paris 05, France. Univ Massachusetts, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA. NASA, Langley Res Ctr, Div Atmospher Sci, Hampton, VA 23681 USA. RP Goldman, A (reprint author), Univ Denver, Dept Phys, 2112 E Wesley Ave, Denver, CO 80208 USA. EM goldman@acd.ucar.edu NR 41 TC 12 Z9 12 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD NOV-DEC PY 2003 VL 82 IS 1-4 BP 197 EP 205 DI 10.1016/S0022-4073(03)00153-5 PG 9 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 711KG UT WOS:000184738800009 ER PT J AU Rinsland, CP Flaud, JM Perrin, A Birk, A Wagner, G Goldman, A Barbe, A De Backer-Barilly, MR Mikhailenko, SN Tyuterev, VG Smith, MAH Devi, VM Benner, DC Schreier, F Chance, KV Orphal, J Stephen, TM AF Rinsland, CP Flaud, JM Perrin, A Birk, A Wagner, G Goldman, A Barbe, A De Backer-Barilly, MR Mikhailenko, SN Tyuterev, VG Smith, MAH Devi, VM Benner, DC Schreier, F Chance, KV Orphal, J Stephen, TM TI Spectroscopic parameters for ozone and its isotopes: recent measurements, outstanding issues, and prospects for improvements to HITRAN SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE laboratory spectroscopy; ozone; remote sensing ID ABSORPTION CROSS-SECTIONS; HIGH-RESOLUTION MEASUREMENTS; ATMOSPHERIC TRACE GASES; FTIR SOLAR SPECTRA; LINE POSITIONS; TEMPERATURE-DEPENDENCE; ABSOLUTE INTENSITIES; SHIFT COEFFICIENTS; NU(1)+NU(3) BANDS; CM(-1) REGION AB In this article we review ozone spectroscopy from the microwave to the ultraviolet since the release of the 1996 HITRAN database. Uncertainties, deficiencies, areas of potential improvement, and anticipated new spectral line parameters datasets are highlighted. Published by Elsevier Ltd. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. Univ Paris 11, CNRS, Photophys Mol Lab, F-91405 Orsay, France. German Aerosp Ctr, Remote Sensing Technol Inst, Oberpfaffenhofen, Germany. Univ Denver, Dept Phys, Denver, CO 80208 USA. UFR Sci, CNRS, UMR 6089, Grp Spectrometrie Mol & Atmospher, F-51687 Reims 2, France. Inst Atmospher Opt, Lab Theoret Spect, Tomsk 634055, Russia. Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rinsland, CP (reprint author), NASA, Langley Res Ctr, Mail Stop 402, Hampton, VA 23681 USA. RI Orphal, Johannes/A-8667-2012; OI Orphal, Johannes/0000-0002-1943-4496; Chance, Kelly/0000-0002-7339-7577 NR 73 TC 19 Z9 20 U1 1 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD NOV-DEC PY 2003 VL 82 IS 1-4 BP 207 EP 218 DI 10.1016/S0022-4073(03)00154-7 PG 12 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 711KG UT WOS:000184738800010 ER PT J AU Brown, LR Benner, DC Champion, JP Devi, VM Fejard, L Gamache, RR Gabard, T Hilico, JC Lavorel, B Loete, M Mellau, GC Nikitin, A Pine, AS Predoi-Cross, A Rinsland, CP Robert, O Sams, RL Smith, MAH Tashkun, SA Tyuterev, VG AF Brown, LR Benner, DC Champion, JP Devi, VM Fejard, L Gamache, RR Gabard, T Hilico, JC Lavorel, B Loete, M Mellau, GC Nikitin, A Pine, AS Predoi-Cross, A Rinsland, CP Robert, O Sams, RL Smith, MAH Tashkun, SA Tyuterev, VG TI Methane line parameters in HITRAN SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE methane; database; line parameters; CH3D ID PRESSURE-SHIFT COEFFICIENTS; AIR-BROADENED WIDTH; BAND Q-BRANCH; NU(3) BAND; GROUND-STATE; TETRAHEDRAL MOLECULES; VIBRATIONAL POLYADS; ROTATIONAL ANALYSIS; INFRARED-SPECTRUM; MU-M AB Two editions of the methane line parameters (line positions, intensities and broadening coefficients) available from HITRAN in 2000 and 2001 are described., In both versions, the spectral interval covered was the same (from 0.01 to 6184.5 cm(-1)), but the database increased from 48,033 transitions in 2000 to 211,465 lines in 2001 because weaker transitions of (CH4)-C-12 and new bands of (CH4)-C-13 and CH3D were included. The newer list became available in 2001 in the "Update" section of HITRAN. The sources of information are described, and the prospects for future improvements are discussed. (C) 2003 Elsevier Ltd. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA. Univ Bourgogne, Phys Lab, CNRS, UMR 5027, F-21078 Dijon, France. Univ Massachusetts Lowell, Dept Earth & Atmospher Sci, Lowell, MA 01854 USA. Univ Giessen, Inst Phys Chem, D-35392 Giessen, Germany. Russian Acad Sci, Inst Atmospher Opt, Lab Theoret Spectroscopy, Tomsk 634055, Russia. Alpine Technol, Germantown, MD 20874 USA. Univ Ottawa, Dept Phys, Ottawa, ON K1N 6N5, Canada. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Pacific NW Natl Lab, Richland, WA 99352 USA. Univ Reims, UFR Sci, Grp Spectrometrie Mol & Atmospher, UMR N6089,CNRS, F-51687 Reims, France. RP Brown, LR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mailstop 183-601, Pasadena, CA 91109 USA. EM linda.brown@jpl.nasa.gov RI Champion, Jean-Paul/C-3963-2009; Nikitin, Andrei/K-2624-2013; Tashkun, Sergey/E-8682-2014; Mellau, Georg Christopher/A-8886-2017 OI Nikitin, Andrei/0000-0002-4280-4096; Mellau, Georg Christopher/0000-0001-8209-5733 NR 98 TC 90 Z9 92 U1 3 U2 18 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD NOV-DEC PY 2003 VL 82 IS 1-4 BP 219 EP 238 DI 10.1016/S0022-4073(03)00155-9 PG 20 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 711KG UT WOS:000184738800011 ER PT J AU Kleiner, I Tarrago, G Cottaz, C Sagui, L Brown, LR Poynter, RL Pickett, HM Chen, P Pearson, JC Sams, RL Blake, GA Matsuura, S Nemtchinov, V Varanasi, P Fusina, L Di Lonardo, G AF Kleiner, I Tarrago, G Cottaz, C Sagui, L Brown, LR Poynter, RL Pickett, HM Chen, P Pearson, JC Sams, RL Blake, GA Matsuura, S Nemtchinov, V Varanasi, P Fusina, L Di Lonardo, G TI NH3 and PH3 line parameters: the 2000 HITRAN update and new results SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE ammonia; phosphine; molecular parameters; database ID MICROWAVE 2-PHOTON SPECTROSCOPY; LASER STARK SPECTROSCOPY; INVERSION-ROTATION SPECTRA; SUB-DOPPLER SPECTROSCOPY; FAR-INFRARED-SPECTRUM; ISO-SWS OBSERVATIONS; 10 MU-M; GROUND-STATE; VIBRATIONAL SYSTEM; HETERODYNE MEASUREMENTS AB This paper describes the improvements incorporated into the 2000 version of the HITRAN database for ammonia (NH3), as well as newer results for phosphine (PH3) not included in HITRAN 2000. For ammonia the HITRAN 2000 database contains some 29084 ammonia lines, more than double the number of lines in HITRAN 1996. Specifically, the 2000 update involved replacing pure-rotational and infrared transitions from 0 to 3700 cm(-1) with new calculations for the (NH3)-N-14 isotopomer, whereas in the 4000 to 5300 cm(-1) region, parameters from the 1996 database were retained. The rotational quantum number range for line positions, intensities and line broadening parameters updated in this new HITRAN version goes up to J = 22, 15, 13 and 10 in the 8-1000 mum, 5 mum, 4 mum and 2.8-3.3 mum spectral regions respectively. For phosphine, a new database from 770 to 2156 cm(-1) available for future updates is described and contrasted with parameters in HITRAN 2000. (C) 2003 Elsevier Ltd. All rights reserved. C1 Univ Paris 11, Photophys Mol Lab, F-91405 Orsay, France. CNRS, F-75700 Paris, France. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Pacific NW Natl Lab, Richland, WA 99352 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. ISAS, Sagamihara, Kanagawa 2298510, Japan. SUNY Stony Brook, Inst Terr & Planetary Atmospheres, Stony Brook, NY 11794 USA. Dipartimento Chim Fis & Inorgan, I-40136 Bologna, Italy. RP Kleiner, I (reprint author), Univ Paris 11, Photophys Mol Lab, Batiment 350, F-91405 Orsay, France. RI Chen, Pin/B-1112-2008 OI Chen, Pin/0000-0003-1195-9666 NR 97 TC 47 Z9 47 U1 0 U2 13 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD NOV-DEC PY 2003 VL 82 IS 1-4 BP 293 EP 312 DI 10.1016/S0022-4073(03)00159-6 PG 20 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 711KG UT WOS:000184738800015 ER PT J AU Goldman, A Coffey, MT Hannigan, JW Mankin, WG Chance, KV Rinsland, CP AF Goldman, A Coffey, MT Hannigan, JW Mankin, WG Chance, KV Rinsland, CP TI HBr and HI line parameters update for atmospheric spectroscopy databases SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE HBr; HI; infrared; line parameters; spectroscopic databases ID INFRARED-EMISSION-SPECTROSCOPY; SUBMILLIMETER; SPECTRUM AB Recent work on new line parameters for the X(1)Sigma(+)(0-0),(0-1) (HBr)-Br-79, (HBr)-Br-81 bands and the X(1)Sigma(+)(0-0), (0-1) HI bands, which include hyperfine structure components, has been extended for an update of spectroscopic databases in use for atmospheric spectroscopy. The updated line parameters, now incorporated in HITRAN 2001, are discussed in comparison to HITRAN 1996. (C) 2003 Elsevier Ltd. All rights reserved. C1 Univ Denver, Dept Phys, Denver, CO 80208 USA. Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80303 USA. Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. NASA, Langley Res Ctr, Div Atmospher Sci, Hampton, VA 23681 USA. RP Goldman, A (reprint author), Univ Denver, Dept Phys, Denver, CO 80208 USA. OI Chance, Kelly/0000-0002-7339-7577 NR 20 TC 8 Z9 8 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 NOV-DEC PY 2003 VL 82 IS 1-4 BP 313 EP 317 DI 10.1016/S0022-4073(03)00160-2 PG 5 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 711KG UT WOS:000184738800016 ER PT J AU Devi, VM Benner, DC Smith, MAH Rinsland, CP Sharpe, SW Sams, RL AF Devi, VM Benner, DC Smith, MAH Rinsland, CP Sharpe, SW Sams, RL TI A multispectrum analysis of the v(1) band of (HCN)-C-12-N-14: Part I. Intensities, self-broadening and self-shift coefficients SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE HCN; HCN v(1) band; infrared spectra; Fourier transform infrared (FTIR) spectroscopy; absolute intensity; broadening and shifts ID FOURIER-TRANSFORM SPECTRA; INTEGRATED-INTENSITIES; INFRARED MEASUREMENTS; OVERTONE TRANSITIONS; ABSOLUTE INTENSITY; LASER BANDS; HCN; REGION; CM-1; TEMPERATURE AB The infrared spectrum of HCN in the region between 3150 and 3450 cm(-1) has been recorded at 0.005 and 0.008 cm(-1) resolution using two different Fourier transform spectrometers, the McMath-Pierce Fourier transform spectrometer located at the National Solar Observatory (on Kitt Peak) and the Bruker-120HR Fourier transform spectrometer situated at the Pacific Northwest National Laboratory at Richland, Washington. Room temperature measurements were made of positions, absolute intensities, self-broadening and self-shift coefficients for individual lines belonging to the HCN vi band centered near 3311 cm(-1). These are to our knowledge the first extensive set of self-broadening and self shift, measurements in the band. In addition, intensities, self-broadening and self-shift coefficients for several lines of the v(1) + v(2)(1) - v(2)(1) hot band and several intensities for lines in the (HCN)-C-13-N-14 and (HCN)-C-12-N-15 isotopomers were also determined. A multispectrum nonlinear least-squares fitting algorithm was used to fit the entire spectral region covering the 3200-3400 cm(-1) region of up to 27 spectra simultaneously. The measured line intensities in the v(1) band were further analyzed to derive the vibrational band intensity and the Herman-Wallis coefficients. Differences in line intensities between 5 and 10% are found with respect to present measurements and the values given in the HITRAN database for m values beyond 25 in the P branch and 5 in the R branch. Published by Elsevier Ltd. C1 Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. PNNL, Richland, WA 99352 USA. RP Benner, DC (reprint author), Coll William & Mary, Dept Phys, Box 8795, Williamsburg, VA 23187 USA. NR 39 TC 18 Z9 18 U1 1 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD NOV-DEC PY 2003 VL 82 IS 1-4 BP 319 EP 341 DI 10.1016/S0022-4073(03)00161-4 PG 23 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 711KG UT WOS:000184738800017 ER PT J AU Rinsland, CP Devi, VM Smith, MAH Benner, DC Sharpe, SW Sams, RL AF Rinsland, CP Devi, VM Smith, MAH Benner, DC Sharpe, SW Sams, RL TI A multispectrum analysis of the v(1) band of (HCN)-C-12-N-14: Part II. Air- and N-2-broadening, shifts and their temperature dependences SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE hydrogen cyanide; infrared spectra; Fourier transform infrared (FTIR) spectroscopy ID FOURIER-TRANSFORM SPECTRA; ATMOSPHERIC HYDROGEN-CYANIDE; DIODE-LASER MEASUREMENTS; FREE TROPOSPHERIC CO; SPECTROSCOPIC MEASUREMENTS; OVERTONE TRANSITIONS; HCN; C2H6; CM-1; COEFFICIENTS AB Air- and N-2-broadening, air- and N-2-pressure-induced shift coefficients and the temperature dependence exponent of the broadening coefficients and the temperature dependent coefficient of pressure-induced shifts have been determined for transitions of the v(1) band of (HCN)-C-12-N-14 from 39 laboratory absorption spectra recorded at 0.005 and 0.008 cm(-1) resolutions with two different Fourier transform spectrometers. The parameters were retrieved from the multispectrum nonlinear least-squares fits to the 3200-3400 cm(-1) region of spectra recorded at temperatures between +26degreesC and -60degreesC. Pure samples of HCN in a 19.95 cell and a 0.958 cm cell at room temperature as well as lean mixtures of HCN in N-2 or dry air in a coolable cell with a 50 cm absorption path were used in the experiments. Line parameters for N-2 broadening were determined by fitting 27 spectra simultaneously while air-broadening parameters were quantified from simultaneous fits to 22 spectra. The average ratio and the standard deviation of the room-temperature air- to N-2-broadening coefficient of lines with assignments between P(29) and R(28) are 0.904 +/- 0.001. Pressure-induced shift coefficients at 296 K are all negative with values between 0 and similar to -0.006 cm(-1) atm(-1) and different rotational dependences in the P-and R-branches. Differences between our results, previous measurements and the parameters that are reported in the 2000 edition of HITRAN (HIgh-resolution TRANsmission) database are quantified and discussed. Published by Elsevier Ltd. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA. Pacific NW Natl Lab, Richland, WA 99352 USA. RP Rinsland, CP (reprint author), NASA, Langley Res Ctr, Mail Stop 401A,21 Langley Blvd, Hampton, VA 23681 USA. NR 29 TC 20 Z9 20 U1 1 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD NOV-DEC PY 2003 VL 82 IS 1-4 BP 343 EP 362 DI 10.1016/S0022-4073(03)00162-6 PG 20 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 711KG UT WOS:000184738800018 ER PT J AU Yamada, MM Kobayashi, M Habara, H Amano, T Drouin, BJ AF Yamada, MM Kobayashi, M Habara, H Amano, T Drouin, BJ TI Submillimeter-wave measurements of the pressure broadening of BrO SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE bromine monoxide; linewidths; halfwidths; pressure broadening; atmospheric spectra; lineshape ID STATE; O-2 AB The N-2 and O-2 pressure broadening coefficients of the J = 23.5 <-- 22.5 and J = 25.5 <-- 24.5 rotational transitions in the ground vibronic state X(2)Pi(3/2) of (BrO)-Br-81 at 624.768 and 650.178 GHz have been independently measured at Ibaraki University and Jet Propulsion Laboratory. These lines are expected to be monitored by the superconducting submillimeter-wave limb emission sounder in the Japanese Experiment Module on the International Space Station (JEM/SMILES) as well as the earth observing system microwave limb sounder (EOS-MLS). This work provides temperature-dependent pressure broadening parameters of BrO needed by the space station and satellite based observations. The BrO pressure broadening coefficients and their la uncertainties are: gamma(0)(N-2) = 3.24 +/- 0.05 MHz/Torr and gamma(0)(O-2) = 2.33 +/- 0.06 MHz/Torr for the 624.768 GHz transition at room temperature'(296 K). For the 650.178 GHz line, the results are: gamma(0)(N-2) = 3.20 +/- 0.07 MHz/Torr and gamma(0)(O-2) = 2.41 +/- 0.06 MHz/Torr. The temperature dependence exponents and their 1sigma error are determined to be: n(N-2) = -0.76 +/- 0.05 and n(O-2) = -0.93 +/- 0.07 for the 624.768 GHz transition, and n(N2) = -0.84 +/- 0.07 and n(O-2) = -0.70 +/- 0.07 for the 650.178 GHz transition. (C) 2003 Elsevier Ltd. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Ibaraki Univ, Inst Astrophys & Planetary Sci, Natl Space Dev Agcy, Mito, Ibaraki 3108512, Japan. RP Drouin, BJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 10 TC 16 Z9 16 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD NOV-DEC PY 2003 VL 82 IS 1-4 BP 391 EP 399 DI 10.1016/S0022-4073(03)00165-1 PG 9 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 711KG UT WOS:000184738800021 ER PT J AU Chackerian, C Sharpe, SW Blake, TA AF Chackerian, C Sharpe, SW Blake, TA TI Anhydrous nitric acid integrated absorption cross sections: 820-5300 cm(-1) SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE nitric acid; band intensities; absorption cross sections ID TUNABLE DIODE-LASER; RESOLUTION SPECTRAL MEASUREMENT; INFRARED-SPECTRUM; LINE POSITIONS; HNO3; BAND; CM-1; INTENSITIES; LINESTRENGTHS; PARAMETERS AB Fourier transform infrared absorbance measurements of small aliquots of anhydrous nitric acid were used to determine regional, integrated cross sections at 278.2, 298.22 and 323.15 K. Spectra were recorded with pressure broadened samples (I atmosphere nitrogen), in a 20 cm path length cell at a spectral resolution of 0.112 cm(-1). Spectral regions measured include the vibrational bands: v(1) (similar to 3552 cm(-1)), v(2) (similar to 1710 cm(-1)), v(3), v(4) (similar to 1320 cm(-1)), and v(5), 2v(9) (similar to 890 cm(-1)) and regions of weaker absorption between 820 and 5300 cm(-1). We observe expected changes in the distribution of rovibrational intensities with temperature, but to the accuracy of our measurements, cross-sections integrated over entire vibrational bands are independent of temperature. (C) 2003 Elsevier Ltd. All rights reserved. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Battelle Mem Inst, Pacific NW Natl Lab, Richland, WA 99352 USA. RP Chackerian, C (reprint author), NASA, Ames Res Ctr, Mail Stop 245-4, Moffett Field, CA 94035 USA. NR 25 TC 31 Z9 31 U1 0 U2 5 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 NOV-DEC PY 2003 VL 82 IS 1-4 BP 429 EP 441 DI 10.1016/S0022-4073(03)00168-7 PG 13 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 711KG UT WOS:000184738800024 ER PT J AU Rinsland, CP Sharpe, SW Sams, RL AF Rinsland, CP Sharpe, SW Sams, RL TI Temperature-dependent absorption cross-sections in the thermal infrared bands Of SF5CF3 SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE global warming; absorption cross-section; infrared spectroscopy ID GREENHOUSE-GAS; SPECTRUM; CF3SF5; SF6 AB Absorption cross-sections have been measured at five temperatures between 213 and 323 K in the infrared bands of SF5CF3. The spectra were recorded at a resolution of 0.112 cm(-1) using a commercial Fourier transform infrared spectrometer and a 20 cm temperature-controlled sample cell. Samples of SF5CF3 were pressurized with high-purity nitrogen to a total pressure of 1013.3 hPa (760 Torr). Six or more spectra with varying SF5CF3 column amounts were analyzed at each temperature. The full spectral range of the measurements was 520-6500 cm(-1), with only weak bands observed beyond 1400 cm(-1). Absorption of thermal radiation in the 8-12 mum atmospheric window region being important for climate change, we report here the integrated cross-sections of the significant absorption bands in that spectral region. Our results closely match room temperature values reported previously. Only small variation of the integrated absorption cross-sections with temperature was found. Our results confirm the accuracy of the previous measurements, which find SF5CF3 important for global climate change on a per molecule basis. Absorption cross-sections derived from a single, near Doppler-limited spectrum recorded at room temperature do not show any rotational fine structure in the 700-950 cm(-1) region. Published by Elsevier Ltd. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. PNNL, Richland, WA 99352 USA. RP Rinsland, CP (reprint author), NASA, Langley Res Ctr, 21 Langley Blvd,Mail Stop 401 A, Hampton, VA 23681 USA. NR 14 TC 10 Z9 10 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD NOV-DEC PY 2003 VL 82 IS 1-4 BP 483 EP 490 DI 10.1016/S0022-4073(03)00172-9 PG 8 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 711KG UT WOS:000184738800028 ER PT J AU Boissoles, J Boulet, C Tipping, RH Brown, A Ma, Q AF Boissoles, J Boulet, C Tipping, RH Brown, A Ma, Q TI Theoretical calculation of the translation-rotation collision-induced absorption in N-2-N-2, O-2-O-2, and N-2-O-2 pairs SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE collision-induced absorption; translation-rotation band; atmospheric molecular pairs ID FAR-INFRARED-SPECTRUM; WING LINE-SHAPE; WATER-VAPOR; COORDINATE REPRESENTATION; N2-N2 PAIRS; N-2; TEMPERATURES; MOMENTS; GASES; O-2 AB The translation-rotation collision-induced spectra of N-2-N-2, O-2-O-2 and N-2-O-2 mixtures are calculated theoretically. For N-2-N-2, using the matrix elements for the quadrupole and hexadecapole moments and the isotropic and anisotropic polarizabilities obtained previously from a global analysis of the fundamental band spectra, we obtain numerical values for the zeroth moment that are smaller than the measured values by 9-14%, depending on the temperature. By increasing the value for the matrix element of the isotropic polarizability slightly, good agreement with experiment is obtained. For O-2-O-2, the theoretical spectrum is significantly smaller than the experimental result. By increasing the matrix element of the hexadecapole moment by a factor of 1.7, we can obtain good agreement. This larger value for the hexadecapole moment will not appreciably affect the agreement found previously in the fundamental region because the hexadecapole contribution to the intensity is very small, unlike the translation-rotation band where it is larger than the contribution due to the quadrupole moment. Using these parameters, we then calculate the collision-induced absorption for N-2-O-2 mixtures for which no experimental data exist. Finally, we calculate the collision-induced absorption for air, and compare our results with previous work; we express the results for the ratio of the absorption coefficient of air to that of N-2-N-2 as a function of wavenumber and temperature, R(omega, T), which can easily be implemented in atmospheric models. (C) 2003 Elsevier Ltd. All rights reserved. C1 Univ Alabama, Coll Arts & Sci, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. Univ Rennes 1, PALMS, UMR, F-35042 Rennes, France. Univ Paris 11, CNRS, Photophys Mol Lab, F-91405 Orsay, France. Columbia Univ, Dept Appl Phys, New York, NY 10027 USA. Goddard Space Flight Ctr, Inst Space Studies, New York, NY 10025 USA. RP Tipping, RH (reprint author), Univ Alabama, Coll Arts & Sci, Dept Phys & Astron, 206 Gallalee Box 870324, Tuscaloosa, AL 35487 USA. NR 28 TC 25 Z9 25 U1 1 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD NOV-DEC PY 2003 VL 82 IS 1-4 BP 505 EP 516 DI 10.1016/S0022-4073(03)00174-2 PG 12 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 711KG UT WOS:000184738800030 ER PT J AU Ma, Q Tipping, RH AF Ma, Q Tipping, RH TI A simple analytical parameterization for the water vapor millimeter wave foreign continuum SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE millimeter wave absorption; water vapor; Lanczos algorithm ID COORDINATE REPRESENTATION; ATMOSPHERIC WINDOW; DENSITY-MATRIX; LINE-SHAPES; ABSORPTION; GHZ; H2O-N-2; MODEL; H2O AB We present a theoretical calculation of the millimeter wave foreign continuum due to colliding pairs of H2O-N-2 molecules. The theory is formulated using the symmetrized spectral density which ensures that the principle of detailed balance is. satisfied. It is based on the Lanczos algorithm, and the resulting tri-diagonal matrix is written in terms of continued fractions. The calculations are carried out in the coordinate representation in which the basis functions are delta functions whose arguments are the angular variables necessary to specify the molecular orientations. In this representation, the anisotropic interaction potential responsible for the continuum absorption is diagonal, and the ensemble averages over the states become. multidimensional integrations. These are computed using the Monte Carlo method. The results, computed for a range of temperatures relevant to the atmosphere, are compared to laboratory measurements and to widely used empirical models. For easy use, we fit our results for the absorption coefficient to a simple analytic function of frequency and temperature. (C) 2003 Elsevier Ltd. All rights reserved. C1 Columbia Univ, Dept Appl Phys, NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. RP Ma, Q (reprint author), Columbia Univ, Dept Appl Phys, NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. NR 21 TC 13 Z9 14 U1 0 U2 0 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 NOV-DEC PY 2003 VL 82 IS 1-4 BP 517 EP 531 DI 10.1016/S0022-4073(03)00175-4 PG 15 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 711KG UT WOS:000184738800031 ER PT J AU Tonui, E de Caritat, P AF Tonui, E de Caritat, P TI Composition, diagenesis, and weathering of the sediments and basement of the Callabonna Sub-basin, central Australia: Implications for landscape evolution SO JOURNAL OF SEDIMENTARY RESEARCH LA English DT Article ID NEW-SOUTH-WALES; TRANSMISSION ELECTRON-MICROSCOPE; BROKEN-HILL BLOCK; WILLYAMA SUPERGROUP; PROFILES; KAOLINITE; ROCKS; CHEMISTRY; CARBONATE; MECHANISM AB The evolution of the Callabonna Sub-basin (central Australia) is described in terms of sediment provenance, stratigraphy, sedimentology, and postdepositional mineral and chemical alteration. Six mineral exploration drillholes in the Mundi Mundi Plain were studied using a combination of qualitative and quantitative XRD, PIMAI, (portable infrared mineral analyzer), XRF, normative analysis, and SEM. The sedimentary cover consists of 160-210 m of diagenetically modified fluvio-lacustrine Tertiary clay, silt, and sand comprising sandy, mottled, and gray clay units overlain by Quaternary soil. The basement consists of weathered Proterozoic schist, gneiss, siltstone, and shale. Quartz, kaolinite, smectite, and muscovite are the dominant minerals within the sediments, whereas the weathered bedrock contains quartz, feldspar, kaolinite, illite, and muscovite. Characteristic wavelength absorption features from PIMA(TM) show that the youngest sandy clay unit exhibits the lowest reflectance intensities because of its lower diagenetic maturity. Weathering of primary minerals within the basement produced an illite-kaolinite-rich saprolite whose clays exhibit strong reflectance intensities and well-developed crystallinity. The micromorphology of all secondary products reflects their environment of crystallization. Low porosity and anoxic conditions within the sediments resulted in poorly developed clays of variable textures, colors, and compositions. Conversely, the weathered bedrock developed over protracted periods of in-situ weathering resulting in better-developed secondary products. This study distinguishes between preburial weathering of the basement, detrital mineralogy, postdepositional alteration of the sedimentary cover, and subsequent weathering of previously formed mineral assemblages. This has widespread implications for paleotopographic (-weathering) reconstitution and landscape evolution thus: (1) the extent of weathering of basement relative to diagenesis and maturity of sediments and gradational nature of their unconformity suggests that most of the alteration of basement occurred prior to, and was sustained after, deposition of sediments, and (2) morphotectonic evolution of the region controlled the composition of transported materials by changing the style and patterns of fluvial systems, further influencing the distribution and preservation of sediments and weathered bedrock, and hence regional landscape morphology. C1 Univ Canberra, CRC, LEME, Canberra, ACT 2601, Australia. Australia Geol Survey Org, CRC, LEME, Canberra, ACT 2601, Australia. RP Tonui, E (reprint author), CALTECH, Jet Prop Lab, Div Geol & Planetary Sci, Mail Code 170-25, Pasadena, CA 91125 USA. OI de Caritat, Patrice/0000-0002-4185-9124 NR 78 TC 4 Z9 4 U1 2 U2 7 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA SN 1527-1404 J9 J SEDIMENT RES JI J. Sediment. Res. PD NOV PY 2003 VL 73 IS 6 BP 1036 EP 1050 DI 10.1306/041303731036 PG 15 WC Geology SC Geology GA 739ZA UT WOS:000186375400014 ER PT J AU Duque, EPN Burklund, MD Johnson, W AF Duque, EPN Burklund, MD Johnson, W TI Navier-Stokes and comprehensive analysis performance predictions of the NREL phase VI experiment SO JOURNAL OF SOLAR ENERGY ENGINEERING-TRANSACTIONS OF THE ASME LA English DT Article AB A lifting-line code, CAMRAD II, and a Reynolds-Averaged Navier-Stokes code, OVERFLOW-D, were used to predict the aerodynamic performance of a two-bladed horizontal axis wind turbine. All computations were compared with experimental data that was collected at the NASA Ames Research Center 80-by-120-foot Wind Tunnel. Lifting-line computations were performed for both axial and yawed operating conditions while the Navier-Stokes computations were performed for only the axial conditions. Various stall delay models and dynamic stall models were used by the CAMRAD H code. For axial operating conditions, the predicted rotor performance varied significantly, particularly for stalled wind speeds. The lifting-line required the use of stall delay models to obtain the proper stall behavior yet it still has difficulty in predicting the proper power magnitude in stall. The Navier-Stokes method captures the stall behavior and gives a detailed insight into the fluid mechanics of the stall behavior. C1 No Arizona Univ, Dept Mech Engn, Flagstaff, AZ 86011 USA. NASA, Ames Res Ctr, Army NASA Rotorcraft Div, Moffett Field, CA 94035 USA. RP Duque, EPN (reprint author), No Arizona Univ, Dept Mech Engn, Flagstaff, AZ 86011 USA. NR 32 TC 54 Z9 62 U1 1 U2 8 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA SN 0199-6231 J9 J SOL ENERG-T ASME JI J. Sol. Energy Eng. Trans.-ASME PD NOV PY 2003 VL 125 IS 4 BP 457 EP 467 DI 10.1115/1.1624088 PG 11 WC Energy & Fuels; Engineering, Mechanical SC Energy & Fuels; Engineering GA 754HW UT WOS:000187310900012 ER PT J AU Pappa, RS Black, JT Blandino, JR Jones, TW Danehy, PM Dorrington, AA AF Pappa, RS Black, JT Blandino, JR Jones, TW Danehy, PM Dorrington, AA TI Dot-projection photogrammetry and videogrammetry of gossamer space structures SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article AB The technique of using hundreds or thousands of projected dots of light as targets for photogrammetry and videogrammetry of gossamer space structures is documented. Photogrammetry calculates the three-dimensional coordinates of each target on the structure, and videogrammetry tracks the coordinates vs time. Gossamer structures characteristically contain large areas of delicate, thin-film membranes. Examples include solar sails, large antennas, inflatable solar arrays, solar-power concentrators and transmitters, sun shields, and planetary balloons and habitats. Using projected-dot targets avoids the unwanted mass, stiffness, and installation costs of traditional retroreflective adhesive targets. Four laboratory applications are covered that demonstrate the practical effectiveness of white-light dot projection for both static-shape and dynamic measurement of reflective and diffuse surfaces, respectively. Comparisons are made between dot-projection videogrammetry and traditional laser vibrometry for membrane vibration measurements. A promising extension of existing techniques using a novel laser-induced fluorescence approach is introduced. C1 NASA, Langley Res Ctr, Struct Dynam Branch, Struct & Mat Competency, Hampton, VA 23681 USA. George Washington Univ, Joint Inst Advancement Flight Sci, Hampton, VA 23681 USA. James Madison Univ, Dept Integrated Sci & Technol, Harrisonburg, VA 22807 USA. NASA, Langley Res Ctr, Instrumentat Syst Dev Branch, Aerodynam Aerothermodynam & Acoust Competency, Hampton, VA 23681 USA. RP Pappa, RS (reprint author), NASA, Langley Res Ctr, Struct Dynam Branch, Struct & Mat Competency, Hampton, VA 23681 USA. RI Black, Jonathan/R-4875-2016 OI Black, Jonathan/0000-0001-9315-3994 NR 17 TC 26 Z9 27 U1 0 U2 4 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 NOV-DEC PY 2003 VL 40 IS 6 BP 858 EP 867 DI 10.2514/2.7047 PG 10 WC Engineering, Aerospace SC Engineering GA 754BF UT WOS:000187282300002 ER PT J AU Wuerl, A Crain, T Braden, E AF Wuerl, A Crain, T Braden, E TI Genetic algorithm and calculus of variations-based trajectory optimization technique SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article AB A genetic algorithm is used cooperatively with the Davidon-Fletcher-Powell penalty function method and the calculus of variations to optimize low-thrust, Mars-to-Earth trajectories for the Mars Sample Return Mission. The return trajectory is chosen thrust-coast-thrust a priori, has a fixed time of flight, and is subject to initial and final position and velocity equality constraints. The global search properties of the genetic algorithm combine with the local search capabilities of the calculus of variations to produce solutions that are superior to those generated with the calculus of variations alone, and these solutions are obtained more quickly and require less user interaction than previously possible. The genetic algorithm is not hampered by ill-behaved gradients and is relatively insensitive to problems with a small radius of convergence, allowing it to optimize trajectories for which solutions had not yet been obtained. The use of the calculus of variations within the genetic algorithm optimization routine increased the precision of the final solutions to levels uncommon for a genetic algorithm. C1 Univ Washington, Dept Aeronaut & Astronaut, Seattle, WA 98195 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Wuerl, A (reprint author), Univ Washington, Dept Aeronaut & Astronaut, Seattle, WA 98195 USA. NR 16 TC 11 Z9 12 U1 1 U2 2 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 NOV-DEC PY 2003 VL 40 IS 6 BP 882 EP 888 PG 7 WC Engineering, Aerospace SC Engineering GA 754BF UT WOS:000187282300005 ER PT J AU Stein, M AF Stein, M TI Some recent advances in the investigation of shell buckling SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Reprint ID CIRCULAR CYLINDRICAL SHELLS; SPHERICAL SHELLS; STABILITY; SHALLOW AB A survey is presented which includes the buckling of shells under loads for which the shell is sensitive to initial imperfections. Results for such cases show that improvements in experiment and theory have produced previously unobtainable agreement. The necessity of the correct (and consistent) theoretical specification of boundary conditions is then demonstrated. Recent stiffened cylinder results are surveyed to expose the large effects on the buckling strength of internal or external stiffening, axial load applied eccentric to the wall neutral surface, and the addition of small meridional curvature. C1 NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Stein, M (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. NR 36 TC 0 Z9 0 U1 1 U2 3 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD NOV-DEC PY 2003 VL 40 IS 6 BP 908 EP 914 PG 7 WC Engineering, Aerospace SC Engineering GA 754BF UT WOS:000187282300009 ER PT J AU Stein, M AF Stein, M TI Comments on "some recent advances in the investigation of shell buckling" - Reply by author to L.J Hart-Smith SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Editorial Material C1 NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Stein, M (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD NOV-DEC PY 2003 VL 40 IS 6 BP 916 EP 917 PG 2 WC Engineering, Aerospace SC Engineering GA 754BF UT WOS:000187282300011 ER PT J AU Newton, B Jacksier, T Beeson, H Stradling, J Odom, G AF Newton, B Jacksier, T Beeson, H Stradling, J Odom, G TI Evaluation of the ignition susceptibility of plastics in nitrogen trifluoride (NF3) by autogenous ignition testing SO JOURNAL OF TESTING AND EVALUATION LA English DT Article DE NF3; nitrogen trifluoride; oxygen; fluorine; flammability; autogenous ignition; Kel-F 81; Neoflon; PCTFE; PTFE; Nylon 101; PVDF; PVC AB This paper presents the development of a test system to evaluate the ignition susceptibility of several common plastics in nitrogen trifluoride (NF3) as compared to gaseous oxygen. A test system was developed to allow for measurement of the autogenous ignition temperature (AIT) in both gaseous oxygen and NF3. The autogenous ignition temperatures of Kel-F(R) 81 PCTFE, Neoflon(R) PCTFE5, Teflon(R) PTFE, Nylon 101, PVDF, and PVC were determined in gaseous NF3 and in gaseous oxygen. C1 Wendell Hull & Associates Inc, Las Cruces, NM 88005 USA. Air Liquide, Res & Dev, Countryside, IL 60525 USA. NASA, White Sands Test Facil, Las Cruces, NM 88004 USA. RP Newton, B (reprint author), Wendell Hull & Associates Inc, 1020 S Main St, Las Cruces, NM 88005 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC TESTING MATERIALS PI W CONSHOHOCKEN PA 100 BARR HARBOR DR, W CONSHOHOCKEN, PA 19428-2959 USA SN 0090-3973 J9 J TEST EVAL JI J. Test. Eval. PD NOV PY 2003 VL 31 IS 6 BP 486 EP 496 PG 11 WC Materials Science, Characterization & Testing SC Materials Science GA 742KP UT WOS:000186516200006 ER PT J AU Horinouchi, T Pawson, S Shibata, K Langematz, U Manzini, E Giorgetta, MA Sassi, F Wilson, RJ Hamilton, K de Grandpre, J Scaife, AA AF Horinouchi, T Pawson, S Shibata, K Langematz, U Manzini, E Giorgetta, MA Sassi, F Wilson, RJ Hamilton, K de Grandpre, J Scaife, AA TI Tropical cumulus convection and upward-propagating waves in middle-atmospheric GCMs SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID GENERAL-CIRCULATION MODEL; QUASI-BIENNIAL OSCILLATION; COMMUNITY CLIMATE MODEL; STRATOSPHERE-MESOSPHERE GCM; SEMIANNUAL OSCILLATION; EQUATORIAL WAVES; GRAVITY-WAVES; VERTICAL RESOLUTION; NATIONAL CENTER; CLOUD ENSEMBLE AB It is recognized that the resolved tropical wave spectrum can vary considerably among general circulation models (GCMs) and that these differences can have an important impact on the simulated climate. A comprehensive comparison of low-latitude waves is presented for the December-January-February period using high-frequency data from nine GCMs participating in the GCM Reality Intercomparison Project for Stratospheric Processes and Their Role in Climate (GRIPS; SPARC). Quantitative measures of the wavenumber-frequency structure of resolved waves and their impacts on the zonal mean circulation are given. Space-time spectral analysis reveals that the wave spectrum throughout the middle atmosphere is linked to the variability of convective precipitation, which is determined by the parameterized convection. The variability of the precipitation spectrum differs by more than an order of magnitude among the models, with additional changes in the spectral distribution (especially the frequency). These differences can be explained primarily by the choice of different cumulus parameterizations: quasi-equilibrium mass-flux schemes tend to produce small variability, while the moist-convective adjustment scheme is the most active. Comparison with observational estimates of precipitation variability suggests that the model values are scattered around the observational estimates. Among the models, only those that produce the largest precipitation variability can reproduce the equatorial quasi-biennial oscillation (QBO). This implies that in the real atmosphere, the forcing from the waves, which are resolvable with the typical resolutions of present-day GCMs, is insufficient to drive the QBO. Parameterized cumulus convection also impacts the nonmigrating tides in the equatorial region. In most of the models, momentum transport by diurnal nonmigrating tides in the mesosphere is comparable to or larger than that by planetary-scale Kelvin waves, being more significant than has been thought. It is shown that the westerly accelerations in the equatorial semi-annual oscillation in the models examined are driven mainly by gravity waves with periods shorter than 3 days, with some contribution from parameterized gravity waves, and that the contribution from the wavenumber-1 Kelvin waves is negligible. These results provide a state-of-the-art assessment of the links between convective parameterizations and middle-atmospheric waves in present-day middle-atmosphere climate models. C1 Kyoto Univ, Radio Sci Ctr Space & Atmosphere, Uji 6110011, Japan. NASA, Goddard Space Flight Ctr, Data Assimilat Off, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. Meteorol Res Inst, Tsukuba, Ibaraki 305, Japan. Free Univ Berlin, D-1000 Berlin, Germany. Max Planck Inst Meteorol, Hamburg, Germany. Inst Nazl Geofis & Vulcanol, Bologna, Italy. NCAR, Boulder, CO USA. GFDL, Princeton, NJ USA. Univ Hawaii Manoa, Honolulu, HI 96822 USA. York Univ, Toronto, ON M3J 2R7, Canada. Met Off, Bracknell, Berks, England. RP Horinouchi, T (reprint author), Kyoto Univ, Radio Sci Ctr Space & Atmosphere, Uji 6110011, Japan. EM horinout@kurasc.kyoto-u.ac.jp RI Manzini, Elisa/H-5760-2011; Horinouchi, Takeshi/K-8535-2012; Pawson, Steven/I-1865-2014 OI Horinouchi, Takeshi/0000-0002-2296-1975; Pawson, Steven/0000-0003-0200-717X NR 60 TC 77 Z9 77 U1 2 U2 17 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 EI 1520-0469 J9 J ATMOS SCI JI J. Atmos. Sci. PD NOV PY 2003 VL 60 IS 22 BP 2765 EP 2782 DI 10.1175/1520-0469(2003)060<2765:TCCAUW>2.0.CO;2 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 740XD UT WOS:000186426900003 ER PT J AU Kim, JY Yang, ZG Chang, CC Valdez, TI Narayanan, SR Kumta, PN AF Kim, JY Yang, ZG Chang, CC Valdez, TI Narayanan, SR Kumta, PN TI A sol-gel-based approach to synthesize high-surface-area Pt-Ru catalysts as anodes for DMFCs SO JOURNAL OF THE ELECTROCHEMICAL SOCIETY LA English DT Article ID METHANOL FUEL-CELLS; PLATINUM-TIN CATALYSTS; ELECTROCATALYTIC ACTIVITY; ALLOY COLLOIDS; OXIDATION; ELECTROOXIDATION; ELECTRODES; SYSTEMS; BINARY AB A novel sol-gel based chemical process was developed to synthesize Pt-Ru catalysts possessing high specific surface area and good catalytic activity, for direct methanal fuel cells (DMFCs). In this process, tetramethylammonium hydroxide was used to hydrolyze platinum (II) acetylacetonate and ruthenium (III) acetylacetonate to form a homogeneous gel. Phase-pure powders possessing a high specific surface area as high as 136.9 m(2)/g were produced using controlled oxidizing atmospheres such as 1% O-2 balanced with N-2. The resultant powder consisted of nanocrystalline Pt-Ru particles (less than 10 nm) and also revealed an excellent catalytic activity in standard three-electrode half-cell tests (cell potential of 0.295 V at currents of ln(mA/g) of 8), demonstrating the potential of the sol-gel-based processes for synthesizing high-performance catalysts for DMFCs. The key factor in obtaining phase-pure powders with high specific surface area is the controlled removal of carbon species in the as-prepared precursors. The rapid kinetics of carbon removal in air caused the growth of particles as well as the formation of Ru oxide, thus leading to a low specific surface area powder, combined with the segregation of Ru oxide from the homogeneous Pt-Ru precursors. A limited oxidizing ability of the heat-treatment atmospheres used such as 0.1% O-2 also yielded a low specific surface area powder due to the insufficient removal of carbon. (C) 2003 The Electrochemical Society. C1 Carnegie Mellon Univ, Dept Mat Sci & Engn, Pittsburgh, PA 15213 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kim, JY (reprint author), AMTEK Res Int LLC, Lebanon, OR 97355 USA. NR 21 TC 22 Z9 23 U1 2 U2 3 PU ELECTROCHEMICAL SOC INC PI PENNINGTON PA 65 SOUTH MAIN STREET, PENNINGTON, NJ 08534 USA SN 0013-4651 J9 J ELECTROCHEM SOC JI J. Electrochem. Soc. PD NOV PY 2003 VL 150 IS 11 BP A1421 EP A1431 DI 10.1149/1.1612503 PG 11 WC Electrochemistry; Materials Science, Coatings & Films SC Electrochemistry; Materials Science GA 734HM UT WOS:000186049600005 ER PT J AU Matsko, AB Ilchenko, VS Savchenkov, AA Maleki, L AF Matsko, AB Ilchenko, VS Savchenkov, AA Maleki, L TI Active mode locking with whispering-gallery modes SO JOURNAL OF THE OPTICAL SOCIETY OF AMERICA B-OPTICAL PHYSICS LA English DT Article ID WAVE-GUIDE LASERS; MICROWAVE RECEIVER; FM; MODULATOR AB We theoretically propose an architecture of a whispering-gallery mode-locked laser with an integrated intracavity microphotonic electro-optic modulator based on an Er:LiNbO3 disk resonator. The laser promises to be small in size, to have a high pulse repetition rate, and to use a small amount of microwave power. (C) 2003 Optical Society of America. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Matsko, AB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Matsko, Andrey/A-1272-2007 NR 23 TC 9 Z9 9 U1 0 U2 5 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0740-3224 J9 J OPT SOC AM B JI J. Opt. Soc. Am. B-Opt. Phys. PD NOV PY 2003 VL 20 IS 11 BP 2292 EP 2296 DI 10.1364/JOSAB.20.002292 PG 5 WC Optics SC Optics GA 741CP UT WOS:000186441400007 ER PT J AU Librescu, L Hasanyan, D Qin, ZM Ambur, DR AF Librescu, L Hasanyan, D Qin, ZM Ambur, DR TI Nonlinear magnetothermoelasticity of anisotropic plates immersed in a magnetic field SO JOURNAL OF THERMAL STRESSES LA English DT Article; Proceedings Paper CT 5th International Congress on Thermal Stresses CY JUN 08-11, 2003 CL VIRGINIA TECH, BLACKSBURG, VIRGINIA HO VIRGINIA TECH DE geometrical nonlinearities; magnetoelastic vibration; magnetothermoelasticity; composite materials ID CARRYING ELECTRIC-CURRENT; VIBRATION AB A geometrically nonlinear theory of magnetothermoelasticity of electroconductive anisotropic plates in a magnetic field is developed. In this context, the Kirchhoff hypothesis is adopted for the plate modeling and the geometrical nonlinearities are considered in the von Karman sense. In addition, the assumptions related to the distribution of electric and magnetic field disturbances through the plate thickness as proposed by Ambartsumyan and his collaborators are adopted. Based on the electromagnetic equations (i.e., the ones by Faraday, Ampere, Ohm, Maxwell, and Lorentz), on the modified Fourier law of heat conduction, and elastokinetic field equations, the three-dimensional coupled problem is reduced to an equivalent two-dimensional one appropriate to the theory of plates. The theory developed herein enables one to investigate the interacting effects among the magnetic, thermal, and elastic fields in orthotropic thin plates. As a special case, the problem of the free vibration of simply supported plate strips immersed in a transversal magnetic field is considered. Effects of the directionality property of the constituent material, magnetic and temperature fields, and electric conductivity, as well as thermal expansion coefficients, on the characteristics of vibrational behavior of the plate strips are investigated. C1 Virginia Polytech Inst & State Univ, Dept Engn Sci & Mech, Blacksburg, VA 24061 USA. NASA, Mech & Durabil Branch, Langley Res Ctr, Hampton, VA 23665 USA. RP Librescu, L (reprint author), Virginia Polytech Inst & State Univ, Dept Engn Sci & Mech, Blacksburg, VA 24061 USA. NR 31 TC 24 Z9 24 U1 0 U2 1 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 0149-5739 J9 J THERM STRESSES JI J. Therm. Stresses PD NOV-DEC PY 2003 VL 26 IS 11-12 BP 1277 EP 1304 DI 10.1080/01495730390240238 PG 28 WC Thermodynamics; Mechanics SC Thermodynamics; Mechanics GA 749QF UT WOS:000186930900016 ER PT J AU Rahmani, RK Keith, TG Cottam, R AF Rahmani, RK Keith, TG Cottam, R TI An approximate spectral method for accurate solution of Fourier and non-Fourier heat conduction problems SO JSME INTERNATIONAL JOURNAL SERIES B-FLUIDS AND THERMAL ENGINEERING LA English DT Article; Proceedings Paper CT 6th ASME/JSME Thermal Engineering Joint Conference CY MAR 16-20, 2003 CL HAWAII ISL, HAWAII SP Amer Soc Mech Engineers, Japan Soc Mech Engineers DE pseudo-spectral; Chebyshev polynomials; parabolic and hyperbolic; heat conduction ID STABILITY; FLUX; FLOW AB In this paper a new form of the pseudo-spectral method is presented. The method is theoretically simple yet robust enough to produce very accurate solutions to hyperbolic and parabolic PDE's while avoiding the effects of Gibb's phenomenon. Moreover the method uses a relatively small amount of computational memory. The method is based on the observation that an analytical function may be well represented in a set of small neighborhoods that share common boundaries, called sub-domains, by low order Chebyshev polynomials. A collocation solution scheme is used in each subdomain to march facilitate a time. Throughout this process the Chebyshev expansion coefficients of the highest order terms are monitored. If these coefficients grow beyond a specified small size, the new sub-domains are then redefined so that the function is again well represented by Chebyshev polynomial expansions. An approach for the determination of computational sub-domains of the physical domain for the special case of a discontinuous function is discussed. The strategy for solving the PDE's is presented. The method is then applied to Fourier and non-Fourier heat conduction problems. C1 Univ Toledo, Dept Mech Ind & Mfg Engn, Toledo, OH 43606 USA. NASA, Glenn Res Ctr, Ohio Aerosp Inst, Cleveland, OH 44135 USA. RP Rahmani, RK (reprint author), Univ Toledo, Dept Mech Ind & Mfg Engn, 2801 W Bancroft St, Toledo, OH 43606 USA. NR 27 TC 1 Z9 1 U1 0 U2 0 PU JAPAN SOC MECHANICAL ENGINEERS PI TOKYO PA SHINANOMACHI-RENGAKAN BLDG, SHINANOMACHI 35, SHINJUKU-KU, TOKYO, 160-0016, JAPAN SN 1340-8054 J9 JSME INT J B-FLUID T JI JSME Int. J. Ser. B-Fluids Therm. Eng. PD NOV PY 2003 VL 46 IS 4 BP 519 EP 527 DI 10.1299/jsmeb.46.519 PG 9 WC Thermodynamics; Engineering, Mechanical SC Thermodynamics; Engineering GA 757HY UT WOS:000187558000007 ER PT J AU Boland, RC Donohue, MJ AF Boland, RC Donohue, MJ TI Marine debris accumulation in the nearshore marine habitat of the endangered Hawaiian monk seal, Monachus schauinslandi 1999-2001 SO MARINE POLLUTION BULLETIN LA English DT Article ID ACANTHASTER-PLANCI; FUR SEALS; ISLANDS AB Large amounts of marine debris are present in shallow reefs adjacent to beach haulouts of the critically endangered Hawaiian monk seal, Monachus schauinslandi. These areas serve as seal pup nurseries, and injury and death caused by entanglement in marine debris are undermining population recovery efforts. We investigated the extent of this threat by measuring the accumulation of potentially entangling derelict fishing gear in nursery zones, 1999-2001. Plots of reef 1.0-1.3 km(2) at three Northwestern Hawaiian Islands were initially cleaned of derelict fishing gear in 1999 then resurveyed in 2000 and 2001. Submerged debris densities across sites ranged from 16 to 165 debris items/km(2). Resurveyed sites yielded annual marine debris accumulation rates from 0 to 141 debris items/km(2). This large range was attributed to the physiography of reef areas surveyed. Trawl net webbing was significantly more common than other types of debris recovered and represented 84% of all debris encountered, suggesting that much of the debris originated from distant North Pacific Ocean fisheries. The likely source of most debris is the multinational trawl fisheries of the North Pacific Ocean. An international solution to this problem is needed. Targeted marine debris removal is a short-term, successful, entanglement mitigation strategy. Published by Elsevier Ltd. C1 Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA. Univ Hawaii, Sch Ocean & Earth Sci & Technol, Sea Grant Coll Program, Honolulu, HI 96822 USA. RP Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, 2570 Dole St, Honolulu, HI 96822 USA. NR 27 TC 30 Z9 35 U1 5 U2 28 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 NOV PY 2003 VL 46 IS 11 BP 1385 EP 1394 DI 10.1016/S0025-326X(03)00291-1 PG 10 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 748GK UT WOS:000186854000016 PM 14607537 ER PT J AU Abdul-Aziz, A Ghosn, LJ Baaklini, G Bhatt, R AF Abdul-Aziz, A Ghosn, LJ Baaklini, G Bhatt, R TI A combined NDT/Finite element technique to study the effects of matrix porosity on the behavior of ceramic matrix composites SO MATERIALS EVALUATION LA English DT Article DE finite element analysis; computed tomography; ceramic matrix composites; stress analysis; nondestructive testing AB Ceramic matrix composites are being considered as candidate materials for high temperature aircraft engine components to replace the current high density metal alloys. Ceramic matrix composites are engineered material composed of coated, two dimensional, woven, high strength fiber tows and melt infiltrated ceramic matrix. Matrix voids are commonly generated during the melt infiltration process. The effects of these matrix voids are usually associated with a reduction in the initial overall composite stiffness and a decrease in the thermal conductivity of the component. Furthermore, the role of the matrix, as well as the coating, is to protect the fibers from the harsh engine environment. Hence, the current design approach is to limit the design stress level of ceramic matrix composite components to always be below the first matrix cracking stress. In this study, the stress concentrations around observed macroscopic matrix voids are calculated using a combined nondestructive testing (NDT)/finite element scheme. Computed tomography is utilized as the NDT technique to characterize the initial macroscopic matrix void's locations and sizes in a ceramic matrix composite tensile test specimen. The finite element is utilized to calculate the localized stress field around these voids, based on the two dimensional computed tomography images. The same specimen was also scanned after tensile testing to a maximum nominal stress of 150 MPa (21756 lb/in.(2)) to depict any growth of the previous observed voids. The computed tomography scans taken after testing depicted an enlargement and some coalescence of the existing voids. C1 Cleveland State Univ, NASA, Dept Civil Engn, Glenn Res Ctr, Cleveland, OH 44135 USA. NASA, Glenn Res Ctr, Ohio Aerosp Inst, Cleveland, OH 44135 USA. NASA, Glenn Res Ctr, Life Predict Branch, Cleveland, OH 44135 USA. USA, Aviat Syst Command, NASA, Ceram Branch,Glenn Res Ctr, Cleveland, OH 44135 USA. RP Abdul-Aziz, A (reprint author), Cleveland State Univ, NASA, Dept Civil Engn, Glenn Res Ctr, 21000 Brookpk Rd,MS 6-1, Cleveland, OH 44135 USA. NR 9 TC 4 Z9 4 U1 0 U2 2 PU AMER SOC NON-DESTRUCTIVE TEST PI COLUMBUS PA 1711 ARLINGATE LANE PO BOX 28518, COLUMBUS, OH 43228-0518 USA SN 0025-5327 J9 MATER EVAL JI Mater. Eval. PD NOV PY 2003 VL 61 IS 11 BP 1217 EP 1221 PG 5 WC Materials Science, Characterization & Testing SC Materials Science GA 741JX UT WOS:000186455900005 ER PT J AU Nielsen, PD Noor, AK Venneri, SL AF Nielsen, PD Noor, AK Venneri, SL TI The next century of air power SO MECHANICAL ENGINEERING LA English DT Article C1 USAF, Res Lab, Wright Patterson AFB, OH 45433 USA. Old Dominion Univ, Ctr Adv Engn Environm, Norfolk, VA USA. Univ Florida, Gainesville, FL USA. NASA, Washington, DC 20546 USA. RP Nielsen, PD (reprint author), USAF, Res Lab, Wright Patterson AFB, OH 45433 USA. NR 0 TC 1 Z9 1 U1 0 U2 1 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA SN 0025-6501 J9 MECH ENG JI Mech. Eng. PD NOV PY 2003 VL 125 IS 11 BP 34 EP 40 PG 7 WC Engineering, Mechanical SC Engineering GA 738UV UT WOS:000186307000031 ER PT J AU Lin, CS Lee, T AF Lin, CS Lee, T TI A classification method for input joints of planar five-bar mechanisms SO MECHANISM AND MACHINE THEORY LA English DT Article ID PARALLEL MANIPULATORS; MULTILOOP MECHANISMS; 4-BAR MECHANISMS; LINKAGES; POSITION; CHAINS; BRANCH; ORDER AB This paper presents a classification method for input joints of planar five-bar two-degree-of-freedom mechanisms or in-parallel manipulators. This classification method emphasizes on the applicability of the classification method in input actuator selection and dimension design. Input joints considered in this study are the two ground joints of five-bar mechanisms. The criteria applied to classify the input joints are based on practical types of motions of drivers. The classification method classifies input joints of all five-bar mechanisms into four classes and they are incomplete-rotation joints, unconditioned complete-rotation joints, position-conditioned complete-rotation joints, and coordination-conditioned complete-rotation joints. Three groups of sets of symbolic inequalities in link lengths, which can be used to identify the classes of the input joints of all five-bar mechanisms, are derived, applying geometric algebra formula and simple logic operations. Also included in this study are the verification of the completeness of the classification method and explicit equations, in link lengths, of rotation ranges for input joints of all classes. Examples are given to demonstrate how to use the classification method to determine the class of input joints and eligible motion ranges of the input joints. Finally, a discussion is given for possible applications of this classification method in design. (C) 2003 Elsevier Ltd. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lin, CS (reprint author), Univ Alaska Fairbanks, Fairbanks, AK 99775 USA. NR 30 TC 9 Z9 9 U1 1 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-114X J9 MECH MACH THEORY JI Mech. Mach. Theory PD NOV PY 2003 VL 38 IS 11 BP 1307 EP 1322 DI 10.1016/S0094-114X(03)00088-0 PG 16 WC Engineering, Mechanical SC Engineering GA 724RF UT WOS:000185500000012 ER PT J AU Schneider, SM Amonette, WE Blazine, K Bentley, J Lee, SMC Loehr, JA Moore, AD Rapley, M Mulder, ER Smith, SM AF Schneider, SM Amonette, WE Blazine, K Bentley, J Lee, SMC Loehr, JA Moore, AD Rapley, M Mulder, ER Smith, SM TI Training with the international space station interim resistive exercise device SO MEDICINE AND SCIENCE IN SPORTS AND EXERCISE LA English DT Article DE weight training; BMD; lean ody mass; spaceflight; microgravity; resistive exercise ID BONE-MINERAL DENSITY; BED REST; WEIGHT LIFTERS; ADAPTATIONS; MEN; SPACEFLIGHT; STRENGTH; PROGRAM; ADULTS AB Purpose: This study characterized iRED training responses in a 1-g environment by: 1) determining whether 16 wk of high-intensity training with iRED produces increases in muscle strength and volume and bone mineral density (BMD), 2) comparing training responses with iRED to free weights, and 3) comparing iRED training responses at two training volumes. Methods: Twenty-eight untrained men were assigned to four groups of seven subjects each: a no exercise control group (CON), an iRED group who trained with three sets/exercise (iRED3), a free-weight group (FW) who trained with three sets/exercise, and an iRED group who trained with six sets/exercise (iRED6). Training exercises included squat (SQ), heel raise (HR), and dead lift (DL) exercises, 3 d(.)wk(-1) for 16 wk. Results: For CON, no changes occurred pre- to posttraining. For iRED3, increases (P less than or equal to 0.05) in one-repetition maximum (1-RM) strength (SQ 21 +/- 4%, HR 17 +/- 4%, DL 29 +/- 5%), leg lean mass (3.1 +/- 0.5%) by dual energy x-ray absorptiometry (DXA), and thigh (4.5 +/- 0.9%) and calf (5.9 +/- 0.7%) muscle volume (by magnetic resonance imaging) occurred after training with no changes in BMD (DXA). For FW, increases in 1-RM strength (SQ 22 +/- 5%, HR 24 +/- 3%, DL 41 +/- 7%), whole body (3.0 +/- 1.1%) and leg lean mass (5.4 +/- 1.2%), thigh (9.2 +/- 1.3%) and calf (4.2 +/- 1.0%) muscle volumes, and lumbar BMD (4.2 +/- 0.7%) occurred after training. For iRED6, all responses were similar to iRED3. Conclusion: High-intensity training with the iRED produced muscle responses similar to FW but was not effective in stimulating bone. Bed rest and spaceflight studies are needed to evaluate the effectiveness of the iRED to prevent microgravity deconditioning. C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Bergalia Enterprises, Houston, TX USA. Wyle Life Sci Inc, Houston, TX USA. Vrije Univ Amsterdam, Fac Movement Sci, Amsterdam, Netherlands. RP Schneider, SM (reprint author), Univ New Mexico, Dept Phys Performance & Dev, MSC 042610,1, Albuquerque, NM 87131 USA. NR 30 TC 41 Z9 42 U1 1 U2 5 PU LIPPINCOTT WILLIAMS & WILKINS PI PHILADELPHIA PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA SN 0195-9131 J9 MED SCI SPORT EXER JI Med. Sci. Sports Exerc. PD NOV PY 2003 VL 35 IS 11 BP 1935 EP 1945 DI 10.1249/01.MSS.0000093611.88198.08 PG 11 WC Sport Sciences SC Sport Sciences GA 741WH UT WOS:000186483000024 PM 14600562 ER PT J AU Mittlefehldt, DW Bogard, DD Berkley, JL Garrison, DH AF Mittlefehldt, DW Bogard, DD Berkley, JL Garrison, DH TI Brachinites: Igneous rocks from a differentiated asteroid SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID CHONDRITE PARENT BODY; NOBLE-GASES; PRIMITIVE ACHONDRITE; COOLING HISTORY; CORE FORMATION; UPPER-MANTLE; METEORITE; OLIVINE; UREILITE; ORIGIN AB We have done petrologic studies of brachinites Allan Hills (ALH) 84025, Elephant Moraine (EET) 99402, and EET 99407; bulk geochemical studies of EET 99402 and EET 99407; Ar-Ar studies of Brachina and EET 99402; and a Xe isotopic study of Brachina. Textural, mineral compositional, and bulk compositional evidence show that EET 99402 and EET 99407 are paired. ALH 84025, EET 99402, and EET 99407 have igneous textures. Petrofabric analyses of ALH 84025 and EET 99407 demonstrate the presence of lineations and probable foliations of olivine grains that support formation as igneous cumulates. Mineral minor element chemistry and bulk rock incompatible lithophile element contents of the brachinites are distinct from those of acapulcoite-lodranite clan meteorites, a suite of high-grade metamorphic rocks and anatectic residues. The differences demonstrate a higher blocking temperature of equilibration for the brachinites and that cumulus plagioclase is present in EET 99402, EET 99407, and probably ALH 84025, thus indicating an igneous origin. Brachinites are differentiated, ultramafic achondrites, and are not part of a suite of primitive achondrites. We infer that their parent asteroid is a differentiated body. Brachina has an excess of Xe-129 correlated with reactor-produced Xe-128, demonstrating that short-lived 1291 was present at the time of formation. This, plus literature data, attests to early formation of the brachinites, within a few Ma of the formation of chondrites. Ar-Ar age data show that Brachina and EET 99407 were degassed about 4.13 Ga ago, possibly by a common impact event. EET 99402 and EET 99407 show petrographic evidence for shock, including possible conversion of plagioclase to maskelynite followed by devitrification. Brachina is unshocked, making a direct association between the Ar-Ar age and textures ambiguous. C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. SUNY Coll Fredonia, Dept Geosci, Fredonia, NY 14063 USA. Lockheed Martin, Houston, TX 77058 USA. RP Mittlefehldt, DW (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM david.w.mittlefehldt@nasa.gov NR 63 TC 28 Z9 28 U1 1 U2 7 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD NOV PY 2003 VL 38 IS 11 BP 1601 EP 1625 PG 25 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 766QG UT WOS:000188386600004 ER PT J AU Pounds, KA Reeves, JN King, AR Page, KL O'Brien, PT Turner, MJL AF Pounds, KA Reeves, JN King, AR Page, KL O'Brien, PT Turner, MJL TI A high-velocity ionized outflow and XUV photosphere in the narrow emission line quasar PG1211+143 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : active; galaxies : general; galaxies : individual : PG1211+143; galaxies : Seyfert; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; BROAD ABSORPTION-LINE; PHOTON IMAGING CAMERA; X-RAY-SPECTRUM; XMM-NEWTON; STELLAR OBJECTS; BLACK-HOLE; COLUMN DENSITIES; PG 1211+143; IRON LINES AB We report on the analysis of a similar to60-ks XMM-Newton observation of the bright, narrow emission line quasar PG1211+143. Absorption lines are seen in both European Photon Imaging Camera and Reflection Grating Spectrometer spectra corresponding to H- and He-like ions of Fe, S, Mg, Ne, O, N and C. The observed line energies indicate an ionized outflow velocity of similar to24 000 km s(-1). The highest energy lines require a column density of N(H)similar to 5 x 10(23) cm(-2), at an ionization parameter of log xisimilar to 3.4. If the origin of this high-velocity outflow lies in matter being driven from the inner disc, then the flow is likely to be optically thick within a radius of similar to130 Schwarzschild radii, providing a natural explanation for the big blue bump (and strong soft X-ray) emission in PG1211+143. C1 Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Pounds, KA (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. NR 43 TC 258 Z9 260 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 1 PY 2003 VL 345 IS 3 BP 705 EP 713 DI 10.1046/j.1365-8711.2003.07006.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 736JX UT WOS:000186168600004 ER PT J AU McGowan, KE Charles, PA O'Donoghue, D Smale, AP AF McGowan, KE Charles, PA O'Donoghue, D Smale, AP TI Correlated optical and X-ray variability in LMC X-2 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries : close; stars : individual : LMC X-2; stars : individual : Sco X-1; X-rays : stars ID LARGE MAGELLANIC CLOUD; SCORPIUS X-1; LIGHT-CURVE; EMISSION; BINARIES; BURSTS; MODULATION; PHOTOMETRY; ECHOES; PERIOD AB We have obtained high time resolution (seconds) photometry of LMC X-2 in 1997 December, simultaneously with the Rossi X-ray Timing Explorer (RXTE), in order to search for correlated X-ray and optical variability on time-scales from seconds to hours. We find that the optical and X-ray data are correlated only when the source is in a high, active X-ray state. Our analysis shows evidence for the X-ray emission leading the optical with a mean delay of <20 s. The time-scale for the lag can be reconciled with disc reprocessing, driven by the higher-energy X-rays, only by considering the lower limit for the delay. The results are compared with a similar analysis of archival data of Sco X-1. C1 Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Univ Oxford, Dept Phys, Oxford OX1 3RH, England. Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. S African Astron Observ, ZA-7935 Cape Town, South Africa. NASA, High Energy Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP McGowan, KE (reprint author), Los Alamos Natl Lab, MS D436, Los Alamos, NM 87545 USA. NR 33 TC 17 Z9 17 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 1 PY 2003 VL 345 IS 3 BP 1039 EP 1048 DI 10.1046/j.1365-8711.2003.07029.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 736JX UT WOS:000186168600034 ER PT J AU Jorgensen, DP Pu, ZX Persson, POG Tao, WK AF Jorgensen, DP Pu, ZX Persson, POG Tao, WK TI Variations associated with cores and gaps of a Pacific narrow cold frontal rainband SO MONTHLY WEATHER REVIEW LA English DT Article ID NUMERICAL SIMULATIONS; EXTRATROPICAL CYCLONES; DOPPLER OBSERVATIONS; MICROSCALE STRUCTURE; MESOSCALE RAINBANDS; PRECIPITATION CORES; SQUALL LINES; BOW ECHO; MODEL; ORGANIZATION AB A NOAA P-3 instrumented aircraft observed an intense, fast-moving narrow cold frontal rainband (NCFR) as it approached the California coast on 19 February 2001 during the Pacific Coastal Jets Experiment. Airborne Doppler radar data obtained while the frontal system was well offshore indicated that a narrow ribbon of very high radar reflectivity convective cores characterized the rainband at low levels with echo tops to similar to4-5 km, and pseudo-dual-Doppler analyses showed the low-level convergence of the prefrontal air. The NCFR consisted of gaps of weaker reflectivity and cores of stronger reflectivity along its length, perhaps as a result of hydrodynamic instability along its advancing leading edge. In contrast to some earlier studies of cold frontal rainbands, density-current theory described well the motion of the overall front. The character of the updraft structure along the NCFR varied systematically along the length of the precipitation cores and in the gap regions. The vertical shear of the cross-frontal low-level ambient flow exerted a strong influence on the updraft character, consistent with theoretical arguments developed for squall lines describing the balance of vorticity at the leading edge. In short segments at the northern ends of the cores, the vertical wind shear was strongest with the updrafts and rain shafts more intense, narrower, and more erect or even downshear tilted. At the southern ends of the cores and just north of the gaps, the wind shear weakened with less intense updrafts that tilted upshear and contained a broader band of rainfall. Simulations using the nonhydrostatic nested grid version of the fifth-generation Pennsylvania State University National Center for Atmospheric Research (PSU-NCAR) Mesoscale Model (MM5) are used to investigate the core and gap regions, focusing on the relationship between the character of the modeled updrafts and the balance between the cold-air-induced vorticity and the prefrontal ambient shear vorticity. The cold air behind the NCFR, which forces new convection along its leading edge, is probably maintained by large-scale advection of cold air plus evaporative cooling processes within the heavy rain region of the NCFR. Observations confirm the model results; that is, that the updraft character depends on the balance of vorticity at the leading edge. Downshear-tilted updrafts imply that convection at the northern ends of cores may weaken with time relative to the frontal segments at the southern ends, because inflow air would be affected by passage through the heavy rain region before ascent. A mechanism for line modification is thus implied. C1 NOAA, NSSL, MRAD Boulder, Boulder, CO 80305 USA. Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NOAA, Environm Technol Lab, Boulder, CO USA. Univ Colorado, CIRES, Boulder, CO 80309 USA. RP Jorgensen, DP (reprint author), NOAA, NSSL, MRAD Boulder, Mail Code N-C-MRD,325 Broadway, Boulder, CO 80305 USA. NR 41 TC 21 Z9 21 U1 0 U2 4 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0027-0644 J9 MON WEATHER REV JI Mon. Weather Rev. PD NOV PY 2003 VL 131 IS 11 BP 2705 EP 2729 DI 10.1175/1520-0493(2003)131<2705:VAWCAG>2.0.CO;2 PG 25 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 740XJ UT WOS:000186427700013 ER PT J AU Mauskopf, PD Ade, PAR Balbi, A Cabella, P De Gasperis, G Natoli, P Vittorio, N Bock, JJ Hristov, VV Jones, WC Lange, AE Bond, JR Contaldi, CR Borrill, JJ Boscaleri, A Crill, BP de Bernardis, P De Troia, G Iacoangeli, A Masi, S Melchiorri, A Nati, F Piacentini, F Polenta, G Ricciardi, S de Oliveira-Costa, A Tegmark, M di Stefano, G Romeo, G Ganga, K Hivon, E Jaffe, AH Ruhl, JE Kisner, TS Montroy, T Torbet, E Mactavish, C Netterfield, CB Pascale, E Pogosyan, D Prunet, S AF Mauskopf, PD Ade, PAR Balbi, A Cabella, P De Gasperis, G Natoli, P Vittorio, N Bock, JJ Hristov, VV Jones, WC Lange, AE Bond, JR Contaldi, CR Borrill, JJ Boscaleri, A Crill, BP de Bernardis, P De Troia, G Iacoangeli, A Masi, S Melchiorri, A Nati, F Piacentini, F Polenta, G Ricciardi, S de Oliveira-Costa, A Tegmark, M di Stefano, G Romeo, G Ganga, K Hivon, E Jaffe, AH Ruhl, JE Kisner, TS Montroy, T Torbet, E Mactavish, C Netterfield, CB Pascale, E Pogosyan, D Prunet, S TI BOOMERANG returns SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT 2nd CMBNet Workshop on Science and Parameter Extraction CY FEB 20-21, 2003 CL OXFORD, ENGLAND SP CMBNet, European Comm, 5th Framework Improving Human Potential Program DE CMB; Sunyaev-Zel'dovich effect; component separation; CMB polarisation ID MULTIFREQUENCY MAPS; POWER SPECTRUM; POLARIZATION AB BOOMERANG was one of the first experiments to map large areas of the cosmic microwave background (CMB) with high signal-to-noise during a long duration balloon (LDB) flight in 1998/99. BOOMERANG uses bolometric detectors measuring frequency bands from 90 to 400 GHz, a frequency range that complements the lower frequency range of experiments using HEMT amplifiers such as DASI and WMAP. Here, we discuss the status of the analysis of the B98 data including initial comparison of the B98 data with WMAP and component separation of the B98 maps in order to measure the Sunyaev-Zel'dovich effect. Finally, we describe the second LDB flight of the BOOMERANG telescope in January, 2003 with a receiver designed to map the polarisation of the CMB. (C) 2003 Elsevier B.V. All rights reserved. C1 Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy. CALTECH, Jet Prop Lab, Pasadena, CA USA. Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 1A1, Canada. LBNL, Natl Energy Res Sci Comp Ctr, Berkeley, CA USA. Univ Calif Berkeley, Ctr Particle Astrophys, Berkeley, CA 94720 USA. CNR, IFAC, Florence, Italy. CSU Dominguez Hills, Carson, CA USA. Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. Univ Penn, Dept Phys, Philadelphia, PA 19104 USA. Ist Nazl Geofis, I-00161 Rome, Italy. CALTECH, IPAC, Pasadena, CA 91125 USA. Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, London, England. 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, Canada. Univ Alberta, Dept Phys, Edmonton, AB, Canada. Inst Astrophys, F-75014 Paris, France. RP Mauskopf, PD (reprint author), Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. RI Jaffe, Andrew/D-3526-2009; de Gasperis, Giancarlo/C-8534-2012; Nati, Federico/I-4469-2016; Piacentini, Francesco/E-7234-2010; OI Hivon, Eric/0000-0003-1880-2733; Polenta, Gianluca/0000-0003-4067-9196; Ricciardi, Sara/0000-0002-3807-4043; de Gasperis, Giancarlo/0000-0003-2899-2171; Nati, Federico/0000-0002-8307-5088; 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 NR 17 TC 1 Z9 1 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD NOV PY 2003 VL 47 IS 8-10 BP 733 EP 740 DI 10.1016/j.newar.2003.07.019 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 758QZ UT WOS:000187662800005 ER PT J AU Black, JK Brunton, AN Bannister, NP Deines-Jones, P Jahoda, K AF Black, JK Brunton, AN Bannister, NP Deines-Jones, P Jahoda, K TI The imaging X-ray detector for Lobster-ISS SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article; Proceedings Paper CT 6th International Conference on Position Sensitive Detectors CY SEP 09-13, 2002 CL UNIV LEICESTER, LEICESTER, ENGLAND HO UNIV LEICESTER DE micro-well proportional counters; micro-pattern gas detectors; microchannel plates; X-ray astronomy; X-ray telescopes AB Lobster-ISS is a revolutionary astrophysical X-ray all-sky monitor scheduled for deployment as an attached payload on the International Space Station (ISS) in 2009. Using a new wide field-of-view focusing optic, Lobster-ISS provides an order-of-magnitude improvement in the sensitivity of all-sky monitors in the soft X-ray band (0.1-3.0keV). This lobster-eye optic presents unique challenges to the imaging X-ray detector at its focus. Micro-patterned imaging proportional counters, with their mechanical simplicity and high performance are the most practical means of meeting the requirements. We describe our design for the Lobster-ISS X-ray imaging detector based on direct-imaging microwell proportional counters and the expected performance. (C) 2003 Elsevier B.V. All rights reserved. C1 NASA, Goddard Space Flight Ctr, Forbin Sci, Greenbelt, MD 20771 USA. Univ Leicester, Dept Phys & Astron, Space Res Ctr, Leicester LE1 7RH, Leics, England. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Greenbelt, MD 20771 USA. RP Black, JK (reprint author), NASA, Goddard Space Flight Ctr, Forbin Sci, Code 662, Greenbelt, MD 20771 USA. RI Jahoda, Keith/D-5616-2012 NR 8 TC 10 Z9 11 U1 1 U2 4 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 NOV 1 PY 2003 VL 513 IS 1-2 BP 123 EP 126 DI 10.1016/j.nima.2003.08.015 PG 4 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 741DB UT WOS:000186442500027 ER PT J AU Tou, J Grindeland, R Barrett, J Dalton, B Mandel, A Wade, C AF Tou, J Grindeland, R Barrett, J Dalton, B Mandel, A Wade, C TI Evaluation of NASA foodbars as a standard diet for use in short-term rodent space flight studies SO NUTRITION LA English DT Article DE foodbars; space flight; standard diet; nutrients; extrusion; irradiation ID ENERGY METABOLISM; RATS; MASS; BODY AB OBJECTIVES: A standard rodent diet for space flight must meet the unique conditions imposed by the space environment and must be nutritionally adequate because diet can influence the outcome of experiments. We evaluated the use of National Aeronautics,and Space Administration (NASA) Foodbars as a standard space flight diet for rats. METHODS: The Foodbar's semi-purified formulation permitted criteria such as nutrient consistency, high nutrient bioavailability, and flexibility of formulation to be met. Extrusion of the semi-purified diet produced Foodbars with the proper texture and a non-crumbing solid form for use in space. Treatment of Foodbar with 0.1% potassium sorbate prevented mold growth. Irradiation (15 to 25 kGy) prevented bacterial growth and, in combination with sorbate treatment, added protection against mold for shelf stability. RESULTS: During the development process, nutrient analyses indicated that extrusion and irradiation produces nutrient losses. Nutrients were adjusted accordingly to compensate for processing losses. Nutrient analysis of Foodbars continues to be performed routinely to monitor nutrient levels. It is important that the standard rodent diet provide nutrients that will prevent deficiency but also avoid excess that may mask physiologic changes produced by space flight. All vitamin levels in the Foodbars, except for vitamin K, conformed to or exceeded the current National Research Council (NRC) 1995 recommendations. All indispensable amino acids in Foodbar conformed to or exceeded the NRC nutrient recommendation for mouse growth and rat maintenance. However, some indispensable amino acids were slightly below recommendations for rat reproduction and growth. Short-term (18 to 20 d) animal feeding studies indicated that Foodbars are palatable, support growth, and maintain health in rats. CONCLUSIONS: Results indicated that NASA Rodent Foodbars meet the physical and nutritional criteria required to support rodents in the space environment and thus may be used successfully as a standard diet for short-term space flight studies. However, the nutritional adequacy of NASA Rodent Foodbars as a standard diet on longer-duration (>20 d) space flight missions remains to be determined. (C) Elsevier Inc. 2003. C1 NASA, Ames Res Ctr, Div Life Sci, Moffett Field, CA 94043 USA. NASA, Ames Res Ctr, Lockheed Martin Space Operat, Moffett Field, CA 94043 USA. RP Tou, J (reprint author), NASA, Ames Res Ctr, Div Life Sci, MS 239-11, Moffett Field, CA 94043 USA. NR 36 TC 9 Z9 9 U1 0 U2 0 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0899-9007 J9 NUTRITION JI Nutrition PD NOV-DEC PY 2003 VL 19 IS 11-12 BP 947 EP 954 DI 10.1016/S0899-9007(03)00190-4 PG 8 WC Nutrition & Dietetics SC Nutrition & Dietetics GA 744GQ UT WOS:000186619900008 PM 14624944 ER PT J AU Dorrington, AA Kunnemeyer, R AF Dorrington, AA Kunnemeyer, R TI Single sideband techniques for laser Doppler velocimeter frequency offset SO OPTICAL ENGINEERING LA English DT Article DE laser Doppler velocimetry; frequency shift; single sideband ID COUPLER AB Frequency shifting is a commonly used technique to determine the direction of motion and enable simpler processing of Doppler signals generated by laser Doppler velocimeter (LDV) and Doppler lidar systems. This shift is most commonly achieved by passing the reference, measurement, or injection-locking laser beam though an acousto-optic modulator (AOM). However, AOMs are expensive and require specialized drive electronics, hence methods of generating a frequency shift without the use of an AOM are desirable to reduce the overall cost and size of LDV systems. Various methods of frequency shifting without AOMs have been reported, along with direction discriminating processing systems that do not require a frequency shift. However, these systems are either not applicable to or are of limited use for pulsed Doppler lidar. We have developed a new frequency shifting technique that is applicable to pulsed Doppler lidar and does not require an AOM. The method is based on the principles of radio frequency single-sideband modulation. Two implementations are presented, along with the results from concept validation experiments that illustrate successful decoding, including direction discrimination, of Doppler signals. The first implementation is a fully electronic method that uses an electronic modulator fed with quadrature signals generated optically, and in the second, semioptical implementation the modulation function is performed optically. (C) 2003 Society of Photo-Optical Instrumentation Engineers. C1 Univ Waikato, Dept Phys & Elect Engn, Hamilton, New Zealand. RP Dorrington, AA (reprint author), NASA, Langley Res Ctr, Mail Stop 236, Hampton, VA 23681 USA. NR 14 TC 3 Z9 3 U1 0 U2 1 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 NOV PY 2003 VL 42 IS 11 BP 3239 EP 3246 DI 10.1117/1.1612928 PG 8 WC Optics SC Optics GA 745ZN UT WOS:000186721600026 ER PT J AU Djomehri, MJ Biswas, R AF Djomehri, MJ Biswas, R TI Performance enhancement strategies for multi-block overset grid CFD applications SO PARALLEL COMPUTING LA English DT Article DE parallel performance; load balancing; multi-block applications; computational fluid dynamics AB The overset grid methodology has significantly reduced time-to-solution of high-fidelity computational fluid dynamics (CFD) simulations about complex aerospace configurations. The solution process resolves the geometrical complexity of the problem domain by using separately generated but overlapping structured discretization grids that periodically exchange information through interpolation. However, high performance computations of such large-scale realistic applications must be handled efficiently on state-of-the-art parallel supercomputers. This paper analyzes the effects of various performance enhancement strategies on the parallel efficiency of an overset grid Navier-Stokes CFD application running on an SGI Origin2000 machine. Specifically, the role of asynchronous communication, grid splitting, and grid grouping strategies are presented and discussed. Details of a sophisticated graph partitioning technique for grid grouping are also provided. Results indicate that performance depends critically on the level of latency hiding and the quality of load balancing across the processors. (C) 2003 Elsevier B.V. All rights reserved. C1 NASA, Ames Res Ctr, NAS Div, Moffett Field, CA 94035 USA. NASA, Ames Res Ctr, CSC, Moffett Field, CA 94035 USA. RP NASA, Ames Res Ctr, NAS Div, Moffett Field, CA 94035 USA. EM djomehri@nas.nasa.gov; rupak.biswas@nasa.gov NR 20 TC 7 Z9 7 U1 0 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0167-8191 EI 1872-7336 J9 PARALLEL COMPUT JI Parallel Comput. PD NOV-DEC PY 2003 VL 29 IS 11-12 BP 1791 EP 1810 DI 10.1016/j.parco.2003.05.019 PG 20 WC Computer Science, Theory & Methods SC Computer Science GA 747QL UT WOS:000186815700014 ER PT J AU Lipa, JA Nissen, JA Stricker, DA Swanson, DR Chui, TCP AF Lipa, JA Nissen, JA Stricker, DA Swanson, DR Chui, TCP TI Specific heat of liquid helium in zero gravity very near the lambda point SO PHYSICAL REVIEW B LA English DT Article ID THERMAL-EXPANSION COEFFICIENT; SUPERFLUID TRANSITION; RENORMALIZATION-GROUP; CRITICAL-BEHAVIOR; RESISTANCE THERMOMETRY; CAPACITY MEASUREMENTS; HE-3-HE-4 MIXTURES; CRITICAL EXPONENT; 2ND SOUND; HE-4 AB We report the details and revised analysis of an experiment to measure the specific heat of helium with subnanokelvin temperature resolution near the lambda point. The measurements were made at the vapor pressure spanning the region from 22 mK below the superfluid transition to 4 muK above. The experiment was performed in Earth orbit to reduce the rounding of the transition caused by gravitationally induced pressure gradients on Earth. Specific-heat measurements were made deep in the asymptotic region to within 2 nK of the transition. No evidence of rounding was found to this resolution. The optimum value of the critical exponent describing the specific-heat singularity was found to be alpha=-0.0127+/-0.0003. This is bracketed by two recent estimates based on renormalization-group techniques, but is slightly outside the range of the error of the most recent result. The ratio of the coefficients of the leading-order singularity on the two sides of the transition is A(+)/A(-)=1.053+/-0.002, which agrees well with a recent estimate. By combining the specific-heat and superfluid density exponents a test of the Josephson scaling relation can be made. Excellent agreement is found based on high-precision measurements of the superfluid density made elsewhere. These results represent the most precise tests of theoretical predictions for critical phenomena to date. C1 Stanford Univ, Dept Phys, Stanford, CA 94305 USA. Callida Genom, Sunnyvale, CA 94085 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lipa, JA (reprint author), Stanford Univ, Dept Phys, Stanford, CA 94305 USA. NR 76 TC 93 Z9 93 U1 5 U2 12 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 NOV PY 2003 VL 68 IS 17 AR 174518 DI 10.1103/PhysRevB.68.174518 PG 25 WC Physics, Condensed Matter SC Physics GA 750BN UT WOS:000186971600086 ER PT J AU Sylvestre, J Tinto, M AF Sylvestre, J Tinto, M TI Noise characterization for LISA SO PHYSICAL REVIEW D LA English DT Article ID TIME-DELAY INTERFEROMETRY; GRAVITATIONAL-RADIATION; BINARIES AB We consider the general problem of estimating the in-flight Laser Interferometer Space Antenna (LISA) noise power spectra and cross-spectra, which are needed for detecting and estimating the gravitational wave signals present in the LISA data. For the LISA baseline design and in the long wavelength limit, we bound the error on all spectrum estimators that rely on the use of the fully symmetric Sagnac combination (zeta). This procedure avoids biases in the estimation that would otherwise be introduced by the presence of a strong galactic background in the LISA data. We specialize our discussion to the detection and study of the galactic white-dwarf-white-dwarf binary stochastic signal. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Sylvestre, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Sylvestre, Julien/A-8610-2009 OI Sylvestre, Julien/0000-0001-8136-4348 NR 22 TC 4 Z9 4 U1 0 U2 0 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0556-2821 J9 PHYS REV D JI Phys. Rev. D PD NOV PY 2003 VL 68 IS 10 AR 102002 DI 10.1103/PhysRevD.68.102002 PG 10 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 750PH UT WOS:000187004600005 ER PT J AU Landis, GA AF Landis, GA TI Moving through curved spacetime SO PHYSICS TODAY LA English DT Letter C1 NASA, Glenn Res Ctr, Cleveland, OH USA. RP Landis, GA (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA. NR 2 TC 2 Z9 2 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0031-9228 J9 PHYS TODAY JI Phys. Today PD NOV PY 2003 VL 56 IS 11 BP 12 EP 12 DI 10.1063/1.1634516 PG 1 WC Physics, Multidisciplinary SC Physics GA 738HQ UT WOS:000186281500006 ER PT J AU Bozzolo, G Garces, JE Noebe, RD Abel, P Mosca, HO AF Bozzolo, G Garces, JE Noebe, RD Abel, P Mosca, HO TI Atomistic modeling of surface and bulk properties of Cu, Pd and the Cu-Pd system SO PROGRESS IN SURFACE SCIENCE LA English DT Review DE copper; palladium; surface energies; segregation; surface relaxation; surface alloys; alloy surfaces; solid solution; order-disorder transitions; computational methods ID LOW-ENERGY ELECTRON; EQUIVALENT-CRYSTAL THEORY; TRANSITION-METAL ALLOYS; LEED INTENSITY ANALYSIS; MULTILAYER RELAXATION; FCC METALS; CU(110) SURFACE; MULTICOMPONENT SYSTEMS; OSCILLATORY RELAXATION; STRUCTURAL-ANALYSIS AB The BFS method for alloys is applied to the study of the Cu-Pd system. A variety of issues are analyzed and discussed, including the properties of pure Cu or Pd crystals (surface energies, surface relaxations), Pd/Cu and Cu/Pd surface alloys, segregation of Pd (or Cu) in Cu (or Pd), concentration dependence of the lattice parameter of the high temperature fcc CuPd solid solution, the formation and properties of low temperature ordered phases, and order-disorder transition temperatures. Emphasis is made on the ability of the method to describe these properties on the basis of a minimum set of BFS universal parameters that uniquely characterize the Cu-Pd system. (C) 2003 Elsevier Ltd. All rights reserved. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. Ohio Aerosp Inst, Cleveland, OH 44142 USA. Ctr Atom Bariloche, RA-8400 San Carlos De Bariloche, Rio Negro, Argentina. Comis Nacl Energia Atom, RA-1429 Buenos Aires, DF, Argentina. RP Bozzolo, G (reprint author), NASA, Glenn Res Ctr, Mail Stop 23-2, Cleveland, OH 44135 USA. NR 110 TC 29 Z9 29 U1 3 U2 21 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0079-6816 J9 PROG SURF SCI JI Prog. Surf. Sci. PD NOV PY 2003 VL 73 IS 4-8 BP 79 EP 116 DI 10.1016/j.progsurf.2003.08.034 PG 38 WC Chemistry, Physical; Physics, Condensed Matter SC Chemistry; Physics GA 749VE UT WOS:000186948900003 ER PT J AU Palmeri, P Quinet, P Zitane, N Vaeck, N AF Palmeri, P Quinet, P Zitane, N Vaeck, N TI Auger processes in hollow atoms SO REVISTA MEXICANA DE FISICA LA English DT Article; Proceedings Paper CT 3rd Congress of the Venezolano-de-Fisica CY DEC 10-14, 2001 CL CARACAS, VENEZUELA SP Venezolano Fisica DE atomic processes; Auger processes; autoionization; hollow atoms AB Hollow atoms are characterized by a large number of vacant inner shells and electrons occupying the outer shells. These 'exotic' atomic species are formed in collision processes between highly-charged ions and several types of targets. The scope of the present contribution is to estimate, using a global approach, the Auger rates of the complex configurations belonging to these atoms. C1 NASA, Goddard Space Flight Ctr, LHEA, Greenbelt, MD 20771 USA. Free Univ Brussels, Lab Chim Phys Mol, B-1050 Brussels, Belgium. Univ Liege, IPNAS, B-4000 Liege, Belgium. Univ Mons, B-7000 Mons, Belgium. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Palmeri, P (reprint author), NASA, Goddard Space Flight Ctr, LHEA, Code 662, Greenbelt, MD 20771 USA. NR 6 TC 0 Z9 0 U1 0 U2 1 PU SOCIEDAD MEXICANA DE FISICA PI COYOACAN PA APARTADO POSTAL 70-348, COYOACAN 04511, MEXICO SN 0035-001X J9 REV MEX FIS JI Rev. Mex. Fis. PD NOV PY 2003 VL 49 SU 3 BP 76 EP 78 PG 3 WC Physics, Multidisciplinary SC Physics GA 751GD UT WOS:000187043700023 ER PT J AU Hartley, TT Lorenzo, CF AF Hartley, TT Lorenzo, CF TI Fractional-order system identification based on continuous order-distributions SO SIGNAL PROCESSING LA English DT Article DE fractional-order systems; order-distributions ID PARAMETRIC IDENTIFICATION; FREQUENCY-DOMAIN; OPERATORS; CALCULUS; POWER AB This paper discusses the identification of fractional- and integer-order systems using the concept of continuous order-distribution. Based on the ability to define systems using continuous order-distributions, it is shown that frequency domain system identification can be performed. Least-squares techniques are applied to discretized order-distributions. Methods are presented for properly discretizing the order-distribution. (C) 2003 Published by Elsevier B.V. C1 Univ Akron, Dept Elect & Comp Engn, Akron, OH 44325 USA. NASA, Glenn Res Ctr, Div Instrumentat & Controls, Cleveland, OH 44135 USA. RP Hartley, TT (reprint author), Univ Akron, Dept Elect & Comp Engn, Akron, OH 44325 USA. NR 35 TC 88 Z9 101 U1 1 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0165-1684 J9 SIGNAL PROCESS JI Signal Process. PD NOV PY 2003 VL 83 IS 11 BP 2287 EP 2300 DI 10.1016/S0165-1684(03)00182-8 PG 14 WC Engineering, Electrical & Electronic SC Engineering GA 733TL UT WOS:000186016700002 ER PT J AU Sutter, B Ming, DW Clearfield, A Hossner, LR AF Sutter, B Ming, DW Clearfield, A Hossner, LR TI Mineralogical and chemical characterization of iron-, manganese-, and copper-containing synthetic hydroxyapatites SO SOIL SCIENCE SOCIETY OF AMERICA JOURNAL LA English DT Article ID X-RAY-DIFFRACTION; STRUCTURE REFINEMENTS; CARBONATED APATITES; HYDROXYLAPATITE; CRYSTALLINITY; FLUORAPATITE; SPECTROSCOPY; TEMPERATURE; SOLUBILITY; RESONANCE AB The National Aeronautics and Space Administration's (NASA) Advanced Life Support (ALS) Program is evaluating the use of Fe-, Mn-, and Cu-containing synthetic hydroxyapatite (SHA) as a slow release fertilizer for crops that might be grown on the International Space Station or at Lunar and Martian outposts. Separate Fe-, Mn-, and Cu-containing SHA materials along with a transition-metal free SHA (pure-SHA) were synthesized using a precipitation method. Chemical and mineralogical analyses determined if and how Fe, Mn, and Cu were incorporated into the SHA structure. X-ray diffraction (XRD), Rietveld refinement, and transmission electron microscopy (TEM) confirmed that SHA materials with the apatite structure were produced. Chemical analyses indicated that the metal containing SHA materials were deficient in Ca relative to pure-SHA. The shift in the infrared PO4-nu(3) vibrations, smaller unit cell parameters, smaller particle size, and greater structural strain for Fe-, Mn-, and Cu-containing SHA compared with pure-SHA suggested that Fe, Mn, and Cu were incorporated into SHA structure. Rietveld analyses revealed that Fe, Mn, and Cu substituted into the Ca(2) site of SHA. An Fe-rich phase was detected by TEM analyses and backscattered electron microscopy in the Fe-containing SHA material with the greatest Fe content. The substitution of metals into SHA suggests that metal-SHA materials are potential slow-release sources of micronutrients for plant uptake in addition to Ca and P. C1 Texas A&M Univ, Dept Soil & Crop Sci, College Stn, TX 77843 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Texas A&M Univ, Dept Chem, College Stn, TX 77843 USA. RP Sutter, B (reprint author), NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. RI Clearfield, Abraham/D-4184-2015 OI Clearfield, Abraham/0000-0001-8318-8122 NR 37 TC 28 Z9 29 U1 5 U2 33 PU SOIL SCI SOC AMER PI MADISON PA 677 SOUTH SEGOE ROAD, MADISON, WI 53711 USA SN 0361-5995 J9 SOIL SCI SOC AM J JI Soil Sci. Soc. Am. J. PD NOV-DEC PY 2003 VL 67 IS 6 BP 1935 EP 1942 PG 8 WC Soil Science SC Agriculture GA 741GN UT WOS:000186450500035 PM 14740607 ER PT J AU Aikens, CM Webb, SP Bell, RL Fletcher, GD Schmidt, MW Gordon, MS AF Aikens, CM Webb, SP Bell, RL Fletcher, GD Schmidt, MW Gordon, MS TI A derivation of the frozen-orbital unrestricted open-shell and restricted closed-shell second-order perturbation theory analytic gradient expressions SO THEORETICAL CHEMISTRY ACCOUNTS LA English DT Article DE analytic derivative; Moller-Plesset perturbation theory; frozen core ID CORRELATED WAVE-FUNCTIONS; MAIN-GROUP ELEMENTS; COUPLED-CLUSTER; ELECTRONIC-STRUCTURE; ENERGY GRADIENTS; EXCITED-STATES; BASIS SETS; IMPLEMENTATION; SILICOCENE; COMPOUND AB A detailed derivation of the frozen-orbital second-order perturbation theory (MP2) analytic gradient in the spin-orbital basis is presented. The summation ranges and modification of the MP2 gradient terms that result from the frozen-orbital approximation are clearly identified. The frozen-orbital analytic gradients for unrestricted MP2 and closed-shell MP2 are determined from the spin-orbital derivation. A discussion of useful implementation procedures is included. Timings from full and frozen-orbital MP2 gradient calculations on the molecule silicocene (the silicon analog of the sandwich compound ferrocene) are also presented. C1 Iowa State Univ, Dept Chem, Ames, IA 50011 USA. Iowa State Univ, Ames Lab, Ames, IA 50011 USA. NCI, Adv Biomed Comp Ctr, SAIC Frederick, Frederick, MD 21702 USA. Univ Pittsburgh, Dept Chem, Pittsburgh, PA 15260 USA. NASA, ELORET Corp, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Gordon, MS (reprint author), Iowa State Univ, Dept Chem, Ames, IA 50011 USA. EM mark@si.fi.ameslab.gov OI Aikens, Christine/0000-0002-0854-7997 NR 35 TC 117 Z9 118 U1 3 U2 16 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1432-881X J9 THEOR CHEM ACC JI Theor. Chem. Acc. PD NOV PY 2003 VL 110 IS 4 BP 233 EP 253 DI 10.1007/s00214-003-0453-3 PG 21 WC Chemistry, Physical SC Chemistry GA 742XH UT WOS:000186543000001 ER PT J AU Lefsrud, MG Giacomelli, GA Janes, HW Kliss, MH AF Lefsrud, MG Giacomelli, GA Janes, HW Kliss, MH TI Development of the microgravity plant growth pocket SO TRANSACTIONS OF THE ASAE LA English DT Article; Proceedings Paper CT 2000 ASAE Annual International Meeting CY JUL 09-12, 2000 CL MILWAUKEE, WISCONSIN SP ASAE DE advanced life support; nutrient delivery system; root crop production; salad machine AB The Microgravity Pocket (MGP) was designed for continuous production of root crops in microgravity within a controlled environment. The MGP is intended to provide NASA with a "Salad Machine" to grow carrot and radish for consumption by astronauts. Attributes of the pocket system, include light weight; ease of planting, monitoring, and harvesting; no free water; and low energy requirements. The MGP system uses porous sheets of plastic to wick water to the plant roots, which are enclosed within a watertight pouch. An experiment was conducted growing carrot and radish root crops in a horizontal orientation adjacent to a water-cooled high-pressure sodium lamp. The hydrophilic property of the porous sheet provided nutrient solution to the root zone of the plants, but the small size of the pores prevented root growth into the sheet. The MGP was successful in growing both carrot and radish to harvestable size. C1 Univ New Hampshire, Dept Plant Biol, Durham, NH 03824 USA. Univ Arizona, Dept Agr & Biosyst Engn, Tucson, AZ USA. Rutgers State Univ, Dept Plant Biol & Pathol, New Brunswick, NJ 08903 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Lefsrud, MG (reprint author), Univ New Hampshire, Dept Plant Biol, G37 Spaulding Hall,38 Coll Rd, Durham, NH 03824 USA. EM mlefsrud@cisunix.unh.edu NR 10 TC 0 Z9 0 U1 0 U2 1 PU AMER SOC AGRICULTURAL ENGINEERS PI ST JOSEPH PA 2950 NILES RD, ST JOSEPH, MI 49085-9659 USA SN 0001-2351 J9 T ASAE JI Trans. ASAE PD NOV-DEC PY 2003 VL 46 IS 6 BP 1647 EP 1651 PG 5 WC Agricultural Engineering SC Agriculture GA 765PH UT WOS:000188292200019 ER PT J AU DellaCorte, C AF DellaCorte, C TI Picking up the gauntlet SO TRIBOLOGY & LUBRICATION TECHNOLOGY LA English DT Editorial Material C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP DellaCorte, C (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOC TRIBOLOGISTS & LUBRICATION ENGINEERS PI PARK RIDGE PA 840 BUSSE HIGHWAY, PARK RIDGE, IL 60068 USA SN 0024-7154 J9 TRIBOL LUBR TECHNOL JI Tribol. Lubr. Technol. PD NOV PY 2003 VL 59 IS 11 BP 9 EP 9 PG 1 WC Engineering, Mechanical SC Engineering GA 755CW UT WOS:000187387000002 ER PT J AU van den Broek, MMP van Aalst, MK Bregman, A Krol, M Lelieveld, J Toon, GC Garcelon, S Hansford, GM Jones, RL Gardiner, TD AF van den Broek, MMP van Aalst, MK Bregman, A Krol, M Lelieveld, J Toon, GC Garcelon, S Hansford, GM Jones, RL Gardiner, TD TI The impact of model grid zooming on tracer transport in the 1999/2000 Arctic polar vortex SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID HALOGEN OCCULTATION EXPERIMENT; LOWERMOST STRATOSPHERE; OZONE LOSS; CHEMISTRY; SCHEME; WINTER AB We have used a 3-D chemistry transport model to evaluate the transport of HF and CH4 in the stratosphere during the Arctic winter of 1999/2000. Several model experiments were carried out with the use of a zoom algorithm to investigate the effect of different horizontal resolutions. Balloon-borne and satellite-borne observations of HF and CH4 were used to test the model. In addition, air mass descent rates within the polar vortex were calculated and compared to observations. Outside the vortex the model results agree well with the observations, but inside the vortex the model underestimates the observed vertical gradient in HF and CH4, even when the highest available resolution (1degrees x 1degrees) is applied. The calculated diabatic descent rates agree with observations above potential temperature levels of 450 K. These model results suggest that too strong mixing through the vortex edge could be a plausible cause for the model discrepancies, associated with the calculated mass fluxes, although other reasons are also discussed. Based on our model experiments we conclude that a global 6degrees x 9degrees resolution is too coarse to represent the polar vortex, whereas the higher resolutions, 3degrees x 2degrees and 1degrees x 1degrees, yield similar results, even with a 6degrees x 9degrees resolution in the tropical region. C1 SRON, Utrecht, Netherlands. IMAU, Utrecht, Netherlands. Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands. Max Planck Inst Chem, D-55128 Mainz, Germany. Jet Prop Lab, Pasadena, CA USA. Univ Cambridge, Cambridge, England. Natl Phys Lab, Teddington TW11 0LW, Middx, England. RP van den Broek, MMP (reprint author), SRON, Utrecht, Netherlands. EM broekvd@knmi.nl RI Krol, Maarten/B-3597-2010; Krol, Maarten/E-3414-2013; Lelieveld, Johannes/A-1986-2013; OI Jones, Roderic /0000-0002-6761-3966 NR 30 TC 11 Z9 11 U1 0 U2 2 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PD OCT 31 PY 2003 VL 3 BP 1833 EP 1847 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 740FJ UT WOS:000186392100001 ER PT J AU Cosgrove, BA Lohmann, D Mitchell, KE Houser, PR Wood, EF Schaake, JC Robock, A Marshall, C Sheffield, J Duan, QY Luo, LF Higgins, RW Pinker, RT Tarpley, JD Meng, J AF Cosgrove, BA Lohmann, D Mitchell, KE Houser, PR Wood, EF Schaake, JC Robock, A Marshall, C Sheffield, J Duan, QY Luo, LF Higgins, RW Pinker, RT Tarpley, JD Meng, J TI Real-time and retrospective forcing in the North American Land Data Assimilation System (NLDAS) project SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE NLDAS; North American Land Data Assimilation System; forcing data; LSM; land surface modeling; LDAS ID MODEL; SURFACE AB [1] The accuracy of forcing data greatly impacts the ability of land surface models (LSMs) to produce realistic simulations of land surface processes. With this in mind, the multi-institutional North American Land Data Assimilation System (NLDAS) project has produced retrospective ( 1996 - 2002) and real- time ( 1999 - present) data sets to support its LSM modeling activities. Featuring 0.125degrees spatial resolution, hourly temporal resolution, nine primary forcing fields, and six secondary validation/model development fields, each data set is based on a backbone of Eta Data Assimilation System/Eta data and is supplemented with observation-based precipitation and radiation data. Hourly observation-based precipitation data are derived from a combination of daily National Center for Environmental Prediction Climate Prediction Center (CPC) gauge-based precipitation analyses and hourly National Weather Service Doppler radar-based (WSR-88D) precipitation analyses, wherein the hourly radar-based analyses are used to temporally disaggregate the daily CPC analyses. NLDAS observation-based shortwave values are derived from Geostationary Operational Environmental Satellite radiation data processed at the University of Maryland and at the National Environmental Satellite Data and Information Service. Extensive quality control and validation efforts have been conducted on the NLDAS forcing data sets, and favorable comparisons have taken place with Oklahoma Mesonet, Atmospheric Radiation Measurement Program/cloud and radiation test bed, and Surface Radiation observation data. The real- time forcing data set is constantly evolving to make use of the latest advances in forcing- related data sets, and all of the real- time and retrospective data are available online at http:// ldas. gsfc. nasa. gov for visualization and downloading in both full and subset forms. C1 NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. Sci Applicat Int Corp, Gen Sci Operat, Beltsville, MD USA. NOAA, Environm Modeling Ctr, Natl Ctr Environm Predict, Camp Springs, MD 20746 USA. Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. NOAA, Natl Weather Serv, Off Hydrol Dev, Silver Spring, MD 20910 USA. Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ 08901 USA. Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. NOAA, Environm Modeling Ctr, Natl Ctr Environm Predict, Camp Springs, MD 20746 USA. Univ Maryland, Dept Meteorol, College Pk, MD 20742 USA. NOAA, Res Off, Natl Environm Satellite Data & Informat Serv, Camp Springs, MD 20746 USA. RP Cosgrove, BA (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Mail Code 974-1, Greenbelt, MD 20771 USA. EM brian.cosgrove@gsfc.nasa.gov; dlohmann@ncep.noaa.gov; kenneth.mitchell@noaa.gov; paul.r.houser@nasa.gov; efwood@princeton.edu; john.schaake@noaa.gov; robock@envsci.rutgers.edu; curtis@atmos.colostate.edu; justin@princeton.edu; qingyun.duan@noaa.gov; lluo@rutgers.edu; wayne.higgins@noaa.gov; pinker@atmos.umd.edu; dan.tarpley@noaa.gov; jesse.meng@noaa.gov RI Sheffield, Justin/A-6388-2008; Luo, Lifeng/C-8734-2009; Pinker, Rachel/F-6565-2010; Houser, Paul/J-9515-2013; Duan, Qingyun/C-7652-2011; Robock, Alan/B-6385-2016 OI Houser, Paul/0000-0002-2991-0441; Duan, Qingyun/0000-0001-9955-1512; NR 15 TC 281 Z9 284 U1 0 U2 23 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 OCT 31 PY 2003 VL 108 IS D22 AR 8842 DI 10.1029/2002JD003118 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 740HG UT WOS:000186396500001 ER PT J AU Koike, M Kondo, Y Kita, K Takegawa, N Masui, Y Miyazaki, Y Ko, MW Weinheimer, AJ Flocke, F Weber, RJ Thornton, DC Sachse, GW Vay, SA Blake, DR Streets, DG Eisele, FL Sandholm, ST Singh, HB Talbot, RW AF Koike, M Kondo, Y Kita, K Takegawa, N Masui, Y Miyazaki, Y Ko, MW Weinheimer, AJ Flocke, F Weber, RJ Thornton, DC Sachse, GW Vay, SA Blake, DR Streets, DG Eisele, FL Sandholm, ST Singh, HB Talbot, RW TI Export of anthropogenic reactive nitrogen and sulfur compounds from the East Asia region in spring SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE reactive nitrogen; nitrate; sulfur dioxide; sulfate; transport; East Asia ID AIRBORNE OBSERVATIONS; AEROSOL COMPOSITION; WESTERN PACIFIC; CHEJU ISLAND; NITRIC-ACID; TRANSPORT; EMISSIONS; OUTFLOW; KOREA; DISTRIBUTIONS AB Measurements of gaseous and particulate reactive nitrogen and sulfur species, as well as other chemical species, were made using the P-3B and DC-8 aircraft over the western Pacific during the NASA Transport and Chemical Evolution over the Pacific (TRACE-P) experiment, conducted between February and April 2001. These measurements provide a good opportunity to study the extent to which anthropogenic NOx and SO2 emitted over the East Asian countries remain as NOy and SOx (=SO2 + nssSO(4)(2-)) in the form of gas or fine particles when an air mass is transported into the western Pacific region. In this paper a method to estimate transport efficiencies, epsilon(NOy) and epsilon(SOx), in an air mass that has experienced multiple injection, mixing, and loss processes is described. In this analysis, CO and CO2 are used as passive tracers of transport, and the emission inventories of CO, CO2, NOx, and SO2 over the East Asia region are used. Results from the P-3B presented in this study indicate that 20-40% and 15% of NOx emitted over the northeastern part of China remained as NOy over the western Pacific in the boundary layer (BL) and free troposphere (FT), respectively. In the FT, PAN is found to have been the dominant form of NOy, while only 0.5% of emitted NOx remained as NOx. The transport efficiency of SOx is estimated to have been 25-45% and 15-20% in the BL and FT, respectively. Median values of the nssSO(4)(2-)/SOx ratio are 0.4-0.6 both in the BL and FT, however large variability is found in the FT. These results are generally consistent with those derived using DC-8 data. The results obtained in this study indicate that more than half of NOy and SOx were lost over the continent and that the vertical transport from the BL to FT further reduced their amounts by a factor of 2, likely due to wet removal. Budgets of NOy and SOx were also studied for air masses, which we sampled during TRACE-P and the flux out from the continent in these cases is estimated to be 20% of the emissions. Flux in the BL and FT is found to have a similar contribution. C1 Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan. Univ Tokyo, Adv Sci & Technol Res Ctr, Tokyo 1538904, Japan. Ibaraki Univ, Grad Sch Sci, Dept Environm Sci, Fac Sci, Mito, Ibaraki 3108512, Japan. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80303 USA. Georgia Inst Technol, Dept Earth & Atmospher Sci, Atlanta, GA 30332 USA. Drexel Univ, Dept Chem, Philadelphia, PA 19104 USA. Univ Calif Irvine, Dept Chem, Irvine, CA 92697 USA. Argonne Natl Lab, Decis & Informat Sci Div, Argonne, IL 60439 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ New Hampshire, Durham, NH 03820 USA. RP Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Bunkyo Ku, Hongo 7-3-1, Tokyo 1130033, Japan. EM koike@eps.s.u-tokyo.ac.jp; kondo@atmos.rcast.u-tokyo.ac.jp; kita@env.sci.ibaraki.ac.jp; takegawa@atmos.rcast.u-tokyo.ac.jp; masui@aos.eps.s.u-tokyo.ac.jp; yuzom@atmos.rcast.u-tokyo.ac.jp; m.k.ko@larc.nasa.gov; wein@ucar.edu; ffl@acd.ucar.edu; rweber@eas.gatech.edu; dct@drexel.edu; g.w.sachse@larc.nasa.gov; s.a.vay@larc.nasa.gov; dblake@orion.oac.uci.edu; dstreets@anl.gov; eisele@ncar.ucar.edu; scott.sandholm@eas.gatech.edu; hsingh@mail.arc.nasa.gov; robert.talbot@unh.edu RI Koike, Makoto/F-4366-2011; Kondo, Yutaka/D-1459-2012; Miyazaki, Yuzo/C-6920-2010 NR 47 TC 56 Z9 56 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD OCT 31 PY 2003 VL 108 IS D20 AR 8789 DI 10.1029/2002JD003284 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 740GW UT WOS:000186395500005 ER PT J AU Talbot, R Dibb, J Scheuer, E Seid, G Russo, R Sandholm, S Tan, D Singh, H Blake, D Blake, N Atlas, E Sachse, G Jordan, C Avery, M AF Talbot, R Dibb, J Scheuer, E Seid, G Russo, R Sandholm, S Tan, D Singh, H Blake, D Blake, N Atlas, E Sachse, G Jordan, C Avery, M TI Reactive nitrogen in Asian continental outflow over the western Pacific: Results from the NASA Transport and Chemical Evolution over the Pacific (TRACE-P) airborne mission SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SEPTEMBER OCTOBER 1991; FEBRUARY-MARCH 1994; PEM-TROPICS-A; ORGANIC-COMPOUNDS; UNITED-STATES; TROPOSPHERE; EMISSIONS; OCEAN; DISTRIBUTIONS; OZONE AB We present here results for reactive nitrogen species measured aboard the NASA DC-8 aircraft during the Transport and Chemical Evolution over the Pacific (TRACE-P) mission. The large-scale distributions total reactive nitrogen (NOy,sum =NO+NO2+HNO3+PAN+C-1-C-5 alkyl nitrates) and O-3 and CO were better defined in the boundary layer with significant degradation of the relationships as altitude increased. Typically, NOy,sum was enhanced over background levels of similar to260 pptv by 20-to-30-fold. The ratio C2H2/CO had values of 1-4 at altitudes up to 10 km and as far eastward as 150degreesE, implying significant vertical mixing of air parcels followed by rapid advection across the Pacific. Analysis air parcels originating from five principal Asian source regions showed that HNO3 and PAN dominated NOy,sum. Correlations of NOy,sum with C2Cl4 (urban tracer) were not well defined in any of the source regions, and they were only slightly better with CH3Cl (biomass tracer). Air parcels over the western Pacific contained a complex mixture of emission sources that are not easily resolvable as shown by analysis of the Shanghai mega-city plume. It contained an intricate mixture of pollution emissions and exhibited the highest mixing ratios of NOy,sum species observed during TRACE-P. Comparison of tropospheric chemistry between the earlier PEM-West B mission and the recent TRACE-P data showed that in the boundary layer significant increases in the mixing ratios of NOy,sum species have occurred, but the middle and upper troposphere seems to have been affected minimally by increasing emissions on the Asian continent over the last 7 years. C1 Univ New Hampshire, Climate Change Res Ctr, Inst Study Earth Oceans & Space, Durham, NH 03820 USA. Georgia Inst Technol, Atlanta, GA 30332 USA. Univ Calif Irvine, Irvine, CA 92716 USA. Natl Ctr Atmospher Res, Boulder, CO 80305 USA. NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Univ New Hampshire, Climate Change Res Ctr, Inst Study Earth Oceans & Space, Durham, NH 03820 USA. EM robert.talbot@unh.edu; jack.dibb@unh.edu; eric.scheuer@unh.edu; gseid@mail.kgi.edu; rsrusso@cisunix.unh.edu; sts@minitower.eas.gatech.edu; dtan@eas.gatech.edu; hanwat.b.singh@nasa.gov; drblake@uci.edu; nblake@uci.edu; atlas@acd.ucar.edu; g.w.sachse@larc.nasa.gov; c.e.jordan@larc.nasa.gov; m.a.avery@larc.nasa.gov RI Atlas, Elliot/J-8171-2015 NR 36 TC 37 Z9 37 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD OCT 31 PY 2003 VL 108 IS D20 AR 8803 DI 10.1029/2002JD003129 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 740GW UT WOS:000186395500001 ER PT J AU Brownlee, DE Tsou, P Anderson, JD Hanner, MS Newburn, RL Sekanina, Z Clark, BC Horz, F Zolensky, ME Kissel, J McDonnell, JAM Sandford, SA Tuzzolino, AJ AF Brownlee, DE Tsou, P Anderson, JD Hanner, MS Newburn, RL Sekanina, Z Clark, BC Horz, F Zolensky, ME Kissel, J McDonnell, JAM Sandford, SA Tuzzolino, AJ TI Stardust: Comet and interstellar dust sample return mission SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Stardust; Wild 2; interstellar dust; sample return; comet coma sample; silica aerogel ID INTERPLANETARY DUST; ICE ANALOGS; PARTICLES; DISCOVERY; INTACT; GRAINS; HALLEY AB [1] Stardust, the 4th Discovery mission launched in February 1999, will collect coma samples from the recently deflected comet 81P/Wild 2 on 2 January 2004 and return them to Earth on 15 January 2006 for detailed laboratory analyses. Stardust will be the first mission to bring samples back to Earth from a known comet and also the first to bring back contemporary interstellar particles recently discovered. These samples should provide important insights into the nature and amount of dust released by comets, the roles of comets in planetary systems, clues to the importance of comets in producing dust in our zodiacal cloud as well as circumstellar dust around other stars, and the links between collected meteoritic samples with a known cometary body. Samples are collected in newly invented continuous gradient density silica aerogel. Stardust is facilitated by a magnificent trajectory designed to accomplish a complex and ambitious flyby sample return mission within the Discovery program restrictions. The remaining science payload, which provides important context for the captured samples, includes a time-of-flight spectrometer measuring the chemical and isotopic composition of dust grains; a polyvinylidene fluoride dust flux monitor determining dust flux profiles; a CCD camera for imaging Wild 2 coma and its nucleus; a shared X band transponder providing two-way Doppler shifts to estimate limits to Wild 2 mass and integrated dust fluence; and tracking of the spacecraft's attitude sensing for the detection of large particle impacts. The graphite composite spacecraft brings the collected sample back to Earth by a direct reentry in a capsule. C1 Univ Washington, Dept Astron, Seattle, WA 98195 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Lockheed Martin Astronaut, Denver, CO 80201 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Max Planck Inst Extraterr Phys, D-37075 Garching, Germany. Open Univ, Planetary & Space Sci Res Inst, Space Sci Res Grp, Milton Keynes MK7 6AA, Bucks, England. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Chicago, Enrico Fermi Inst, Lab Astrophys & Space Res, Chicago, IL 60637 USA. RP Brownlee, DE (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. EM brownlee@astro.washington.edu; peter.tsou@jpl.nasa.gov; john.d.anderson@jpl.nasa.gov; msh@mhanner.jpl.nasa.gov; ray.l.newburn@jpl.nasa.gov; zs@sek.jpl.nasa.gov; benton.c.clark@lmco.com; friedrich.p.horzl@jsc.nasa.gov; michael.e.zolensky1@jsc.nasa.gov; kissel@mpe.mpg.de NR 42 TC 59 Z9 59 U1 0 U2 9 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 OCT 31 PY 2003 VL 108 IS E10 AR 8111 DI 10.1029/2003JE002087 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 740HP UT WOS:000186397200001 ER PT J AU Burlaga, LF Ness, NF Stone, EC McDonald, FB Acuna, MH Lepping, RP Connerney, JEP AF Burlaga, LF Ness, NF Stone, EC McDonald, FB Acuna, MH Lepping, RP Connerney, JEP TI Search for the heliosheath with Voyager 1 magnetic field measurements SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID COSMIC-RAY MODULATION; TERMINATION SHOCK; SOLAR-WIND; INTERSTELLAR-MEDIUM; AU; HELIOSPHERE; STRENGTH; PICKUP; SPEED AB The magnetic field measured by Voyager 1 (V1) near 85 AU from 2002.0 to 2003.17 has the expected properties for the heliospheric magnetic field at that distance and epoch of the solar cycle. These V1 magnetic field observations do not provide evidence for exit from the solar wind, entry into a subsonic region such as the heliosheath, or transit of the termination shock near 85 AU. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. CALTECH, Pasadena, CA 91109 USA. Univ Maryland, Inst Phys Sci & Technol, College Pk, MD 20742 USA. RP NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM leonard.f.burlaga@nasa.gov RI connerney, john/I-5127-2013 NR 26 TC 40 Z9 41 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 OCT 30 PY 2003 VL 30 IS 20 AR 2072 DI 10.1029/2003GL018291 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 740GM UT WOS:000186394700004 ER PT J AU Kissel, J Glasmachers, A Grun, E Henkel, H Hofner, H Haerendel, G von Hoerner, H Hornung, K Jessberger, EK Krueger, FR Mohlmann, D Greenberg, JM Langevin, Y Silen, J Brownlee, D Clark, BC Hanner, MS Hoerz, F Sandford, S Sekanina, Z Tsou, P Utterback, NG Zolensky, ME Heiss, C AF Kissel, J Glasmachers, A Grun, E Henkel, H Hofner, H Haerendel, G von Hoerner, H Hornung, K Jessberger, EK Krueger, FR Mohlmann, D Greenberg, JM Langevin, Y Silen, J Brownlee, D Clark, BC Hanner, MS Hoerz, F Sandford, S Sekanina, Z Tsou, P Utterback, NG Zolensky, ME Heiss, C TI Cometary and Interstellar Dust Analyzer for comet Wild 2 SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE dust mass spectrometer; interstellar and cometary dust; composition; positive and negative ions; instrument description ID VEGA OBSERVATIONS; ION FORMATION; HALLEY; PARTICLES; P/HALLEY; IMPACT AB [1] The Cometary and Interstellar Dust Analyzer (CIDA) instrument analyzes the composition of individual grains in the cometary coma. As each particle impacts a silver plate, the high-impact energy due to the relative velocity of the spacecraft as it flies through the coma causes the elements and molecular compounds in the particle to become ionized. Using a fast time-of-flight mass spectrometer, a complete set of ions are detected for each impact, from a mass range of 1 ( atomic hydrogen) up to a few thousand atomic mass units, encompassing all elements in the periodic table and many molecules, such as organic compounds. This experimental technique has already been applied with excellent success at Halley's comet, and the CIDA derivative instrument is flying on the Stardust mission, which will encounter comet Wild 2 in January of 2004. The data returned will give clues to the elemental and chemical composition of the dust component of this comet. C1 Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Univ Wuppertal, Fachbereich Elektrotech & Informat Tech, D-42119 Wuppertal, Germany. Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. Von Hoerner & Sulgar GmbH, D-68723 Schwetzingen, Germany. Int Univ Bremen, D-28725 Bremen, Germany. Univ Neubiberg, D-85577 Neubiberg, Germany. Univ Munster, Inst Planetol, D-48149 Munster, Germany. Ingenieurbuero Krueger, D-64291 Darmstadt, Germany. DLR Inst Weltraumsensorik, D-12489 Berlin, Germany. Fac Sci Orsay, Inst Astrophys, F-91405 Orsay, France. Finnish Meteorol Inst, Dept Geophys, SF-00101 Helsinki, Finland. Univ Washington, Dept Astron, Seattle, WA 98105 USA. Lockheed Martin Aerosp, Denver, CO 80201 USA. Jet Prop Lab, Pasadena, CA 91103 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Merck AG, Darmstadt, Germany. RP Kissel, J (reprint author), Max Planck Inst Aeron, Max Planck Str 2, D-37191 Katlenburg Lindau, Germany. EM cometkissel@onlinehome.de; glasmachers@uni-wuppertal.de; eberhard.gruen@mpi-hd.mpg.de; henkel@vh-s.de; hhh@mpe.mpg.de; hae@iu-bremen.de; vonhoerner@vh-s.de; klaus.hornung@unibw-muenchen.de; ekj@nwz.uni-muenster.de; frkrueger@aol.com; dirk.moehlmann@dlr.de; yves.langevin@ias.u-psud.fr; johan.silen@fmi.fi; brownlee@bluemoon.astro.washington.edu; benton.c.clark@lmco.com; glasmachers@uni-wuppertal.de; friedrich.p.horzl@jsc.nasa.gov; ssandford@mail.arc.nasa.gov; zs@sek.jpl.nasa.gov; peter.tsou@jpl.nasa.gov; jb3@silcom.com; e.zolensky1@jsc.nasa.gov; christian.heiss@arcormail.de NR 22 TC 36 Z9 36 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD OCT 30 PY 2003 VL 108 IS E10 AR 8114 DI 10.1029/2003JE002091 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 740HN UT WOS:000186397100001 ER PT J AU Singer, BA Lockard, DP AF Singer, BA Lockard, DP TI Shear effects in aeroacoustic predictions SO JOURNAL OF SOUND AND VIBRATION LA English DT Letter ID TRAILING-EDGE; SURFACES; FLOW; SLAT C1 NASA, Langley Res Ctr, Computat Modeling & Simulat Branch, Hampton, VA 23681 USA. RP Singer, BA (reprint author), NASA, Langley Res Ctr, Computat Modeling & Simulat Branch, MS 128, Hampton, VA 23681 USA. NR 8 TC 0 Z9 0 U1 1 U2 1 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 OCT 30 PY 2003 VL 267 IS 4 BP 961 EP 966 DI 10.1016/S0022-460X(03)00216-5 PG 6 WC Acoustics; Engineering, Mechanical; Mechanics SC Acoustics; Engineering; Mechanics GA 735PY UT WOS:000186124800011 ER PT J AU Bell, NF Rawlinson, AA Sawyer, RF AF Bell, NF Rawlinson, AA Sawyer, RF TI Speed-up through entanglement - many-body effects in neutrino processes SO PHYSICS LETTERS B LA English DT Article ID OSCILLATIONS AB We study a system containing many particles of identical kinematics with a zero range interaction that scatters one from the other, and with the possible exchange of an attribute. Taking an initial condition in which the attribute is asymmetrically distributed in the regions of momentum space occupied by the particles, we study the rate at which it becomes uniformly distributed, through collisions. We find, in some circumstances, a rate that is much faster than that which would be estimated from cross-sections. This behavior is attributable in some general sense to N-particle entanglement. We suggest applications to neutrino physics, where the attribute is neutrino flavor. (C) 2003 Elsevier B.V. All rights reserved. C1 Fermilab Natl Accelerator Lab, NASA, Fermilab Astrophys Ctr, Batavia, IL 60510 USA. Univ Melbourne, Sch Phys, Melbourne, Vic 3010, Australia. Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. RP Bell, NF (reprint author), Fermilab Natl Accelerator Lab, NASA, Fermilab Astrophys Ctr, POB 500, Batavia, IL 60510 USA. EM nfb@fnal.gov; a.rawlinson@physics.unimelb.edu.au; sawyer@vulcan.physics.ucsb.edu NR 12 TC 23 Z9 23 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0370-2693 EI 1873-2445 J9 PHYS LETT B JI Phys. Lett. B PD OCT 30 PY 2003 VL 573 IS 1-4 BP 86 EP 93 DI 10.1016/j.physletb.2003.08.035 PG 8 WC Astronomy & Astrophysics; Physics, Nuclear; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 737TL UT WOS:000186247800011 ER PT J AU Brooks, SD Baumgardner, D Gandrud, B Dye, JE Northway, MJ Fahey, DW Bui, TP Toon, OB Tolbert, MA AF Brooks, SD Baumgardner, D Gandrud, B Dye, JE Northway, MJ Fahey, DW Bui, TP Toon, OB Tolbert, MA TI Measurements of large stratospheric particles in the Arctic polar vortex SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE PSC; MASP; denitrification ID LARGE HNO3-CONTAINING PARTICLES; ANTARCTIC SPRING STRATOSPHERE; NITRIC-ACID TRIHYDRATE; OZONE LOSS; REFRACTIVE-INDEXES; REACTIVE NITROGEN; VAPOR-PRESSURES; DENITRIFICATION; CLOUDS; WINTER AB [1] During the SAGE III Ozone Loss and Validation Experiment/Third European Stratospheric Experiment on Ozone 2000 mission, the Multiangle Aerosol Spectrometer Probe ( MASP) was flown aboard the ER-2 aircraft sampling the Arctic polar vortex. On several of the flights the ER-2 flew directly through polar stratospheric clouds (PSCs), and on six of these flights the MASP sampled large particles ( 2 - 22 mum diameter). MASP large particle observations are correlated in time with the large particle signal from the NOAA NOy measurements. This is direct evidence supporting the inference of particle size made by the NOy instrument. On 20 January 2000, the day of the most intense PSC encounter, the shapes of the large particle size distributions above 9 mum observed by the MASP and simulated based on the NOy instruments are in reasonable agreement. The MASP observations show a dramatic increase in large particle volume as the temperature approaches the nitric acid trihydrate equilibrium temperature. Our study suggests that large particles containing nitric acid are present in the Arctic polar stratosphere and may lead to denitrification. C1 Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA. Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. Univ Mexicana, Mexico City 04510, DF, Mexico. Natl Ctr Atmospher Res, Boulder, CO 80301 USA. NOAA, Aeron Lab, Boulder, CO 80303 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Colorado, Program Atmospher & Ocean Sci, Boulder, CO 80309 USA. Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. RP Univ Colorado, Dept Chem & Biochem, Campus Box 215, Boulder, CO 80309 USA. EM sbrooks@lamar.colostate.edu; darrel@servidor.unam.mx; northway@al.noaa.gov; dfahey@al.noaa.gov; toon@lasp.colorado.edu RI Brooks, Sarah/H-1176-2012; Fahey, David/G-4499-2013 OI Fahey, David/0000-0003-1720-0634 NR 45 TC 9 Z9 9 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD OCT 29 PY 2003 VL 108 IS D20 AR 4652 DI 10.1029/2002JD003278 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 740GU UT WOS:000186395300001 ER PT J AU Perigaud, C McCreary, JP AF Perigaud, C McCreary, JP TI Influence of interannual rainfall anomalies on sea level variations in the tropical Indian Ocean SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article DE rainfall; salinity; sea level; Indian Ocean; TOPEX; ERS ID MIXED-LAYER; TEMPERATURE ANALYSES; SURFACE TEMPERATURE; PACIFIC-OCEAN; DYNAMICS; SALINITY; THERMODYNAMICS; VARIABILITY; BENGAL; BAY AB [1] A halo-thermal, reduced- gravity model with four active layers is used to investigate how interannual rainfall anomalies affect sea surface height (SSH) variability in the Indian Ocean. The model is forced by monthly varying winds observed over the period 1980 2000 in two experiments that differ by their rainfall forcing, Run FSU and Run Arkin, forced by climatological and interannually varying rainfall, respectively. Compared to the large impact of wind on SSH ( about 30 cm), the impact of rain is much smaller. Its maximum ( found in the southeastern Indian Ocean during the rainfall deficits of 1994 and 1997) is only 2 cm. Because rainfall significantly affects model salinity and temperature, the deficits make the layers of Run Arkin colder and saltier than in Run FSU, causing a - 5 cm change in sea level. Baroclinic adjustments also occur such that the top ( bottom) two layers are thicker ( thinner), increasing sea level by 3 cm and hence significantly reducing the SSH change due to steric effects alone. SSH variability in either Run Arkin or Run FSU compares very well with TOPEX data. Although the impact of rainfall on SSH is negligible, salinity variations significantly affect dynamic- height calculations of SSH. In the model, the neglect of salinity variations leads to an error of 5 to 10 cm along the eastern boundary, in the Bay of Bengal, and in the interior ocean south of 8 degreesS. This error is validated by the difference between TOPEX data and SSH derived from observed temperature profiles. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Hawaii Manoa, Int Pacific Res Ctr, Honolulu, HI 96822 USA. RP Perigaud, C (reprint author), CALTECH, Jet Prop Lab, MS 300-323,4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 38 TC 5 Z9 5 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-OCEANS JI J. Geophys. Res.-Oceans PD OCT 29 PY 2003 VL 108 IS C10 AR 3335 DI 10.1029/2003JC001857 PG 16 WC Oceanography SC Oceanography GA 740HK UT WOS:000186396800002 ER PT J AU Falconer, DA Moore, RL Gary, GA AF Falconer, DA Moore, RL Gary, GA TI A measure from line-of-sight magnetograms for prediction of coronal mass ejections SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE coronal mass ejection; prediction; halo; space weather; flare; active region ID SOLAR ACTIVE REGIONS; VECTOR MAGNETOGRAPH; MAGNETIC-FIELD; FLARE; SHEAR AB [1] From a sample of 17 vector magnetograms of 12 bipolar active regions we have recently found ( 1) that a measure of the overall nonpotentiality ( the overall twist and shear in the magnetic field) of an active region is given by the strong shear length L-SS, the length of the portion of the main neutral line on which the observed transverse fields is strong (> 150 Guass ( G)) and strongly sheared ( shear angle > 45degrees), and ( 2) that L-SS is well correlated with the coronal mass ejection (CME) productivity of the active regions during the +/- 2-day time window centered on the day of the magnetogram. In the present paper, from the same sample of 17 vector magnetograms, we show that there is a viable proxy for L-SS that can be measured from a line-of-sight magnetogram. This proxy is the strong gradient length L-SG, the length of the portion of the main neutral line on which the potential transverse field is strong (> 150 G), and the gradient of the line-of-sight field is sufficiently steep ( greater than similar to 50 G/Mm). In our sample of active regions, L-SG is statistically significantly correlated with L-SS ( correlation confidence level > 95%), and L-SG is as strongly correlated with active region CME productivity as is L-SS ( correlation confidence level similar to99.7%). Because L-SG can be measured from line-of-sight magnetograms obtained from conventional magnetographs, such as the magnetograph mode of the Michelson Doppler Imager (MDI) on board the Solar and Heliospheric Observatory, it is a dependable substitute for L-SS for use in operational CME forecasting. In addition, via measurement of L-SG, the years-long, nearly continuous sequence of 1.5-hour cadence full disk line-of-sight magnetograms from MDI can be used to track the growth and decay of the large-scale nonpotentiality in active regions and to examine the role of this evolution in active region CME productivity. C1 NASA, George C Marshall Space Flight Ctr, SD 50, Huntsville, AL 35812 USA. Univ Alabama, Huntsville, AL 35899 USA. RP Falconer, DA (reprint author), NASA, George C Marshall Space Flight Ctr, SD 50, Huntsville, AL 35812 USA. NR 29 TC 37 Z9 38 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 OCT 29 PY 2003 VL 108 IS A10 AR 1380 DI 10.1029/2003JA010030 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 740HY UT WOS:000186398000008 ER PT J AU Santos-Costa, D Blanc, M Maurice, S Bolton, SJ AF Santos-Costa, D Blanc, M Maurice, S Bolton, SJ TI Modeling the electron and proton radiation belts of Saturn SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ENERGETIC NEUTRAL ATOMS; MAGNETOSPHERE; PLASMA; DISTRIBUTIONS; PARTICLES; SALAMMBO; RINGS AB We present results from a three-dimensional model of the Saturnian radiation belts. This model draws on preexisting physical radiation-belt models, developed to study the belts of the Earth and Jupiter. In the present work, transport processes and interactions with dust and gas clouds, moons, and plasma are considered to determine the trapped particle distribution in Saturn's inner magnetosphere. The results of the modeling are: absorption by dust is the dominant loss effect in the innermost region while local losses from satellites act as the prominent physical process in the outer part of the inner magnetosphere. Results suggest strong energetic neutral atom emission and weak synchrotron emission. Comparisons between data and model results are presented. C1 Observ Midi Pyrenees, Astrophys Lab, F-31400 Toulouse, France. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Santos-Costa, D (reprint author), Observ Midi Pyrenees, Astrophys Lab, 14 Ave Ed Belin, F-31400 Toulouse, France. NR 20 TC 19 Z9 19 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 OCT 28 PY 2003 VL 30 IS 20 AR 2059 DI 10.1029/2003GL017972 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 740GK UT WOS:000186394500001 ER PT J AU Greeley, R Kuzmin, RO Rafkin, SCR Michaels, TI Haberle, R AF Greeley, R Kuzmin, RO Rafkin, SCR Michaels, TI Haberle, R TI Wind-related features in Gusev crater, Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars-aeolian; Mars-geology; Gusev ID GENERAL-CIRCULATION MODEL; GLOBAL SURVEYOR; ORBITER CAMERA; SURFACE; SYSTEM; SIMULATIONS; VIEWS; LAKE AB [1] Gusev crater has a complex history beginning with its formation by an impact in the Noachian Period and subsequent evolution, including erosion and deposition associated with Ma'adim Vallis, which cut through Gusev crater from the south. Various wind-related features are found on the crater floor, including albedo patterns, bedforms ( such as barchan dunes), and elongated hills possibly reflecting erosion by the wind. Comparisons of the orientations of these features with predictions from global and atmospheric models show wind patterns as functions of season and time of day. Strongest global winds occur out of the southeast in the late fall and early winter and appear to be responsible for the formation of a large dark streak that drapes 100 km across the crater floor. On an intermediate- scale, bright wind streaks correlate with nighttime winds that flow into the crater from the rim and outlying high areas; these streaks are interpreted to be deposits of dust settled from the atmosphere during times of positive atmospheric static stability. Smaller features include various dark streaks and duneforms, the orientations of which are inferred to represent local zones of high wind-shear surface stress. These features also tend to correlate with strong afternoon upslope winds caused by the uneven heating of the atmosphere across the crater. Thus the large dark streak reflects global-scale wind patterns, the smaller dark features and duneforms represent flow of strong winds out of the crater in the afternoon, and the small bright streaks represent deposition of dust associated with nighttime flow of wind into the crater. The correlation between the wind regime predicted by the models and the orientations of the aeolian features gives confidence that the models are essentially correct. Because Gusev is a prime candidate landing site for landers, including the Mars Exploration Rovers, understanding the interplay of the atmosphere and the surface ( including the erosion and deposition of windblown particles) is important in assessments of the science potential for these missions. Despite the abundance of wind-related features on the floor of Gusev, only about 1.2% of the proposed landing ellipse area is covered with organized bedforms ( e. g., dunes), although mantles of sand and dust are also likely to be present. On the basis of an analysis of random landing points within the ellipse, traverse distances to ridges, ejecta from small craters, and other potential sources of rocks are within 150 m traverse distance for 95% of the touchdown points. C1 Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. Russian Acad Sci, Vernadsky Inst, Moscow 117975, Russia. San Jose State Univ, Dept Meteorol, San Jose, CA 95192 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Arizona State Univ, Dept Geol Sci, Box 871404, Tempe, AZ 85287 USA. EM greeley@asu.edu RI de Souza, Paulo/B-8961-2008; Lemmon, Mark/E-9983-2010; Moersch, Jeffrey/F-7189-2010; Whelley, Patrick/B-9560-2012 OI de Souza, Paulo/0000-0002-0091-8925; Lemmon, Mark/0000-0002-4504-5136; Whelley, Patrick/0000-0003-3266-9772 NR 44 TC 152 Z9 152 U1 6 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD OCT 28 PY 2003 VL 108 IS E12 AR 8077 DI 10.1029/2002JE002006 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 740HR UT WOS:000186397400001 ER PT J AU Samanta, MP Liang, S AF Samanta, MP Liang, S TI Predicting protein functions from redundancies in large-scale protein interaction networks SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article ID SACCHAROMYCES-CEREVISIAE; DATA SETS; YEAST; GENOME; ORGANIZATION; COMPLEXES AB Interpreting data from large-scale protein interaction experiments has been a challenging task because of the widespread presence of random false positives. Here, we present a network-based statistical algorithm that overcomes this difficulty and allows us to derive functions of unannotated proteins from large-scale interaction data. Our algorithm uses the insight that if two proteins share significantly larger number of common interaction partners than random, they have close functional associations. Analysis of publicly available data from Saccharomyces cerevisiae reveals >2,800 reliable functional associations, 29% of which involve at least one unannotated protein. By further analyzing these associations, we derive tentative functions for 81 unannotated proteins with high certainty. Our method is not overly sensitive to the false positives present in the data. Even after adding 50% randomly generated interactions to the measured data set, we are able to recover almost all (approximate to89%) of the original associations. C1 NASA, Ames Res Ctr, Adv Supercomp Div, Moffett Field, CA 94035 USA. RP Liang, S (reprint author), NASA, Ames Res Ctr, Adv Supercomp Div, Moffett Field, CA 94035 USA. NR 19 TC 182 Z9 199 U1 0 U2 7 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 OCT 28 PY 2003 VL 100 IS 22 BP 12579 EP 12583 DI 10.1073/pnas.2132527100 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 738RF UT WOS:000186301100015 PM 14566057 ER PT J AU Brinks, HW Maeland, AJ Hauback, BC Bowman, RC Cantrell, JS AF Brinks, HW Maeland, AJ Hauback, BC Bowman, RC Cantrell, JS TI Determination of deuterium site occupation in Zr4Pd2OD4.5 SO JOURNAL OF ALLOYS AND COMPOUNDS LA English DT Article DE metal hydrides; crystal structure; neutron diffraction; synchrotron radiation ID NEUTRON POWDER DIFFRACTION; ETA-CARBIDES ZR3V3ODX; GEOMETRIC MODEL; TI4FE2O; PHASES AB Powder neutron diffraction analysis has been used to determine hydrogen site occupation at room temperature in the lattice of the oxygen-stabilized Zr4Pd2O phase. For the composition Zr4Pd2OD4.5 it was established that only two types of interstices, designated as D7 and D2, were occupied. Hydrogen in the D7 site is octahedrally surrounded by 6Zr. This site is nearly filled. In the D2 site hydrogen is tetrahedrally co-ordinated to 3Zr and Pd and is 1/3 filled. The distribution of hydrogen on the D2 sites is random. (C) 2003 Elsevier B.V. All rights reserved. C1 Inst Energy Technol, Dept Phys, N-2027 Kjeller, Norway. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Miami Univ, Dept Chem, Oxford, OH 45056 USA. RP Brinks, HW (reprint author), Inst Energy Technol, Dept Phys, POB 40, N-2027 Kjeller, Norway. OI Bowman, Robert/0000-0002-2114-1713 NR 10 TC 2 Z9 2 U1 0 U2 0 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0925-8388 J9 J ALLOY COMPD JI J. Alloy. Compd. PD OCT 27 PY 2003 VL 361 IS 1-2 BP 108 EP 112 DI 10.1016/S0925-8388(03)00446-8 PG 5 WC Chemistry, Physical; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Chemistry; Materials Science; Metallurgy & Metallurgical Engineering GA 735QJ UT WOS:000186125800021 ER PT J AU Cantrell, CA Edwards, GD Stephens, S Mauldin, RL Zondlo, MA Kosciuch, E Eisele, FL Shetter, RE Lefer, BL Hall, S Flocke, F Weinheimer, A Fried, A Apel, E Kondo, Y Blake, DR Blake, NJ Simpson, IJ Bandy, AR Thornton, DC Heikes, BG Singh, HB Brune, WH Harder, H Martinez, M Jacob, DJ Avery, MA Barrick, JD Sachse, GW Olson, JR Crawford, JH Clarke, AD AF Cantrell, CA Edwards, GD Stephens, S Mauldin, RL Zondlo, MA Kosciuch, E Eisele, FL Shetter, RE Lefer, BL Hall, S Flocke, F Weinheimer, A Fried, A Apel, E Kondo, Y Blake, DR Blake, NJ Simpson, IJ Bandy, AR Thornton, DC Heikes, BG Singh, HB Brune, WH Harder, H Martinez, M Jacob, DJ Avery, MA Barrick, JD Sachse, GW Olson, JR Crawford, JH Clarke, AD TI Peroxy radical behavior during the Transport and Chemical Evolution over the Pacific (TRACE-P) campaign as measured aboard the NASA P-3B aircraft SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE photochemistry; peroxy radicals; ozone ID LASER-INDUCED FLUORESCENCE; PEM-TROPICS-B; OZONE PHOTOCHEMISTRY; UPPER TROPOSPHERE; GAS MEASUREMENTS; BOUNDARY-LAYER; NORTH-ATLANTIC; HO2 RADICALS; OH; COEFFICIENT AB [1] Peroxy radical concentrations were measured aboard the NASA P-3B aircraft during the Transport and Chemical Evolution over the Pacific (TRACE-P) campaign in the spring of 2001 and varied in ways that depended on radical production rates and reactive nitrogen concentrations. Measurements of HO2, HO2 + RO2, and OH during this study allowed calculation of radical ratios, examination of functional relationships of these ratios on controlling variables, and comparison with numerical model estimations. Radical production terms show changes in relative contributions at low, middle, and high total production rates that are understandable in terms of systematic variations in the controlling components ( trace gas concentrations and photolysis rate coefficients). Ozone tendency calculations indicate net ozone production in the western Pacific basin because the concentrations of critical precursor trace gases ( e. g., NOx, hydrocarbons) are highest there. The dependence of ozone tendency follows the concentration of NO systematically. Peroxy radical levels on the two aircraft (HO2 + RO2 on the P-3B and HO2 on the DC-8) during two relatively short prescribed intercomparison periods were in good agreement in one instance and poorer in another given reasonable assumptions about the apportioning of radicals between HO2 and RO2. Recommended changes to CH2O photolysis quantum yields, HO2 self reaction, and O(D-1) quenching kinetics lead to small changes (< 5%) in calculated peroxy radical levels for TRACE-P conditions. There is evidence from this campaign that peroxy radicals are lost by interaction with aerosols and cloud droplets. C1 Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80305 USA. Georgia Inst Technol, Atlanta, GA 30332 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Drexel Univ, Philadelphia, PA 19104 USA. Univ Calif Irvine, Irvine, CA 92697 USA. Penn State Univ, University Pk, PA 16802 USA. Univ Hawaii Manoa, Sch Oceanog, Honolulu, HI 96822 USA. Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Honolulu, HI 96822 USA. Univ Rhode Isl, Kingston, RI 02881 USA. Harvard Univ, Cambridge, MA 02138 USA. Univ Tokyo, Adv Sci & Technol Res Ctr, Tokyo 1538904, Japan. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Cantrell, CA (reprint author), Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80305 USA. EM gdedward@perdue.edu; mzondlo@swisciences.com; kondo@atmos.rcast.u-tokyo.ac.jp; zagar@notos.gso.uri.edu; hsingh@mail.arc.nasa.gov; whb2@psu.edu; harder@mpch-mainz.mpg.de; martinez@mpch-mainz.mpg.de; djj@io.harvard.edu; tclarke@soest.hawaii.edu RI Kondo, Yutaka/D-1459-2012; Crawford, James/L-6632-2013; Harder, Hartwig/L-2511-2014; Lefer, Barry/B-5417-2012; Zondlo, Mark/R-6173-2016 OI Crawford, James/0000-0002-6982-0934; Harder, Hartwig/0000-0002-6868-714X; Lefer, Barry/0000-0001-9520-5495; Zondlo, Mark/0000-0003-2302-9554 NR 47 TC 29 Z9 29 U1 1 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 OCT 25 PY 2003 VL 108 IS D20 AR 8797 DI 10.1029/2003JD003674 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 736XR UT WOS:000186199000004 ER PT J AU Tuzzolino, AJ Economou, TE McKibben, RB Simpson, JA McDonnell, JAM Burchell, MJ Vaughan, BAM Tsou, P Hanner, MS Clark, BC Brownlee, DE AF Tuzzolino, AJ Economou, TE McKibben, RB Simpson, JA McDonnell, JAM Burchell, MJ Vaughan, BAM Tsou, P Hanner, MS Clark, BC Brownlee, DE TI Dust Flux Monitor instrument for the Stardust mission to comet Wild 2 SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Stardust; DFMI; PVDF; PVDF dust detectors; Wild 2 comet; dust fluxes ID VEGA SPACECRAFT; MASS; PARTICLES AB [1] The Dust Flux Monitor Instrument ( DFMI) is part of the Stardust instrument payload. The prime goal of the DFMI is to measure the particle flux, intensity profile, and mass distribution during passage through the coma of comet Wild 2 in January 2004. This information is valuable for assessment of spacecraft risk and health and also for interpretation of the laboratory analysis of dust captured by the Aerogel dust collectors and returned to Earth. At the encounter speed of 6.1 km/s, the DFMI measurements will extend over the particle mass range of 8 decades, from 10(-11) to > 10(-3) g. A secondary science goal is to measure the particle flux and mass distribution during the similar to 7 year interplanetary portions of the mission, where, in addition to measurements of the background interplanetary dust over the radial range 0.98 AU to 2.7 AU, multiple opportunities exist for possible detection by the DFMI of interplanetary meteor-stream particles and interstellar dust. The DFMI consists of two different dust detector systems: a polyvinylidene fluoride ( PVDF) Dust Sensor Unit (SU), which measures particles with mass < similar to 10(-4) g, and a Dual Acoustic Sensor System (DASS), which utilizes two quartz piezoelectric accelerometers mounted on the first two layers of the spacecraft Whipple dust shield to measure the flux of particles with mass > 10(-4) g. The large Whipple shield structures provide the large effective sensitive area required for detection of the expected low flux of high-mass particles. C1 Univ Chicago, Enrico Fermi Inst, Lab Astrophys & Space Res, Chicago, IL 60637 USA. Open Univ, Unit Space Sci & Astrophys, Milton Keynes MK7 6A, Bucks, England. NASA, Jet Prop Lab, Pasadena, CA 91109 USA. Lockheed Martin Astronaut, Denver, CO 80201 USA. Univ Washington, Dept Astron, Seattle, WA 98125 USA. RP Tuzzolino, AJ (reprint author), Univ Chicago, Enrico Fermi Inst, Lab Astrophys & Space Res, 5640 S Ellis Ave, Chicago, IL 60637 USA. EM tecon@tecon.uchicago.edu NR 19 TC 24 Z9 24 U1 1 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD OCT 25 PY 2003 VL 108 IS E10 AR 8115 DI 10.1029/2003JE002086 PG 24 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 736YB UT WOS:000186199900001 ER PT J AU Hamaguchi, K Corcoran, MF Imanishi, K AF Hamaguchi, K Corcoran, MF Imanishi, K TI Chandra observations of a young embedded magnetic B star in the rho ophiuchus cloud SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE stars : abundances; stars : chemically peculiar; stars : individual (rho Ophiuchus S1); stars : macynetic fields; X-rays : stars ID X-RAY-EMISSION; HERBIG AE/BE STARS; T-TAURI STARS; DARK CLOUD; ASCA OBSERVATIONS; FORMING REGIONS; SPECTRA; AP; VARIABILITY; PLASMAS AB This paper reports on an analysis of two Chandra X-ray observations of the young magnetic B star rho Ophiuchus S1. X-ray emission from the star, was detected in both observations. The average flux was almost the same in both, but during each observation the flux showed significant time variations by a factor of two on time-scales of 20-40 ks. Each spectrum could be fit by either an absorbed power-law model with a photon index of similar to 3 or a thin-thermal plasma model with a temperature of similar to 2keV and an extremely low metal abundance (less than or similar to 0.1 solar). The spectrum of the first observation has a weak-line feature at about 6.8 keV, which might correspond to highly ionized iron Kalpha. In contrast, the spectrum of the second observation apparently shows a weak edge absorption component at E similar to 4keV. The continuum emission and log(L-X/L-bol) similar to -6 are similar to those of young intermediate-mass stars (Herbig Ae/Be stars), although the presence of a strong magnetic field (inferred from the detection of non-thermal radio emission) has drawn an analogy between rho Ophiuchus S1 and magnetic chemically peculiar (MCP) stars. If the X-ray emission is thermal, the small abundances that we derived might be related to the inverse first-ionization potential (FIP) effect, though there is no significant trend as a function of FIP from our model fits. If the emission is non-thermal, it might be produced by high-energy electrons in the magnetosphere. C1 NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. CNR, Washington, DC 20001 USA. Univ Space Res Assoc, Lanham, MD 20706 USA. Kyoto Univ, Fac Sci, Dept Phys, Sakyo Ku, Kyoto 6068502, Japan. RP NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. EM kenji@milkyway.gsfc.nasa.gov; corcoran@barnegat.gsfc.nasa.gov; kensuke@cr.scphys.kyoto-u.ac.jp NR 42 TC 4 Z9 4 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD OCT 25 PY 2003 VL 55 IS 5 BP 981 EP 987 DI 10.1093/pasj/55.5.981 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 738HK UT WOS:000186281000013 ER PT J AU Farrell, WM Delory, GT Cummer, SA Marshall, JR AF Farrell, WM Delory, GT Cummer, SA Marshall, JR TI A simple electrodynamic model of a dust devil SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ELECTRIC FIELD; MARS; ELECTRIFICATION; GENERATION AB [1] We present an electrodynamic model of a dust devil applying a similar methodology as performed previously for charging in terrestrial thunderstorms. While thunderstorm processes focus on inductive charging between large graupel and smaller ice and water droplets, we tailor the model to focus on the electric charge transfer between dust grains of different sizes and compositions. We specifically compare and contrast the triboelectric dust charging processes presented previously in Melnik and Parrot [ 1998] and Desch and Cuzzi [ 2000] in the development of macroscopic dust devil electric fields. We find that large vertical E-fields ( similar to 20 kV/m) can develop in the devil. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Duke Univ, Dept Elect & Comp Engn, Durham, NC USA. SETI Inst, Mountain View, CA 94043 USA. RP Farrell, WM (reprint author), NASA, Goddard Space Flight Ctr, Code 695, Greenbelt, MD 20771 USA. RI Cummer, Steven/A-6118-2008; Farrell, William/I-4865-2013 OI Cummer, Steven/0000-0002-0002-0613; NR 18 TC 32 Z9 33 U1 2 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 OCT 24 PY 2003 VL 30 IS 20 AR 2050 DI 10.1029/2003GL017606 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 736XH UT WOS:000186198200002 ER PT J AU Arvidson, RE Anderson, RC Haldemann, AFC Landis, GA Li, R Lindemann, RA Matijevic, JR Morris, RV Richter, L Squyres, SW Sullivan, RJ Snider, NO AF Arvidson, RE Anderson, RC Haldemann, AFC Landis, GA Li, R Lindemann, RA Matijevic, JR Morris, RV Richter, L Squyres, SW Sullivan, RJ Snider, NO TI Physical properties and localization investigations associated with the 2003 Mars Exploration rovers SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; physical properties; soils; rocks; Mars Exploration Rover Mission; terramechanics ID PATHFINDER LANDING SITE; THERMAL EMISSION SPECTROMETER; VIKING LANDERS; TERRA-MERIDIANI; MARTIAN SURFACE; DEPOSITS; MISSION; DISTRIBUTIONS; OPERATIONS; SOJOURNER AB [1] A number of physical properties experiments will be conducted during the NASA 2003 Mars Exploration Rover Mission as the two vehicles explore Meridiani Planum and the floor of Gusev Crater. The investigations will include quantifying dust accumulation and dispersal dynamics by periodically monitoring the rover decks with the Athena Pancam and Mini-TES instruments. Properties of soil-like materials will be inferred from analyses of wheel track patterns, depths, and wheel slippage dynamics during traverses. The rovers will be modeled as dynamic mechanical systems to extract along-track terrain topography and physical properties from times series of rover tilt vectors, wheel encoder counts, azimuths, motor currents, and rocker and bogie angles. Trenches will be excavated using rover wheels to characterize mechanical properties of soil-like materials with depth and to expose subsurface materials for remote and in situ observations using the Athena Payload. The Rock Abrasion Tools will be used to expose rock subsurfaces for detailed analyses. Motor currents and penetration magnitudes will be compared to a database of rocks excavated by an engineering model of the Rock Abrasion Tool to understand Martian rock mechanical properties. Image-based localization analyses will be pursued to better understand rover traverse directions and magnitudes and thus rover locations as a function of time. The physical properties and localization investigations, when combined with analyses of the full ensemble of Athena observations, will greatly improve our understanding of Martian surface properties and provide significant technology lessons for future landed missions. C1 Washington Univ, Dept Earth & Planetary Sci, McDonnell Ctr Space Sci, St Louis, MO 63130 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. Ohio State Univ, Dept Civil & Environm Engn & Geodet Sci, Columbus, OH 43210 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. DLR, Inst Raumsimulat, D-5000 Cologne, Germany. Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. RP Washington Univ, Dept Earth & Planetary Sci, McDonnell Ctr Space Sci, St Louis, MO 63130 USA. EM arvidson@wunder.wustl.edu RI Mellon, Michael/C-3456-2016; Seelos, Frank/C-7875-2016 OI Seelos, Frank/0000-0001-9721-941X NR 67 TC 97 Z9 100 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD OCT 24 PY 2003 VL 108 IS E12 AR 8070 DI 10.1029/2002JE002041 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 736YF UT WOS:000186200300003 ER PT J AU Crisp, JA Adler, M Matijevic, JR Squyres, SW Arvidson, RE Kass, DM AF Crisp, JA Adler, M Matijevic, JR Squyres, SW Arvidson, RE Kass, DM TI Mars Exploration Rover mission SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; rover; Mars Exploration Rover ID SPECTROMETER; PATHFINDER AB [1] In January 2004 the Mars Exploration Rover mission will land two rovers at two different landing sites that show possible evidence for past liquid-water activity. The spacecraft design is based on the Mars Pathfinder configuration for cruise and entry, descent, and landing. Each of the identical rovers is equipped with a science payload of two remote-sensing instruments that will view the surrounding terrain from the top of a mast, a robotic arm that can place three instruments and a rock abrasion tool on selected rock and soil samples, and several onboard magnets and calibration targets. Engineering sensors and components useful for science investigations include stereo navigation cameras, stereo hazard cameras in front and rear, wheel motors, wheel motor current and voltage, the wheels themselves for digging, gyros, accelerometers, and reference solar cell readings. Mission operations will allow commanding of the rover each Martian day, or sol, on the basis of the previous sol's data. Over a 90-sol mission lifetime, the rovers are expected to drive hundreds of meters while carrying out field geology investigations, exploration, and atmospheric characterization. The data products will be delivered to the Planetary Data System as integrated batch archives. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Washington Univ, Dept Earth & Planetary Sci, McDonnell Ctr Space Sci, St Louis, MO 63130 USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM joy.a.crisp@jpl.nasa.gov RI Crisp, Joy/H-8287-2016 OI Crisp, Joy/0000-0002-3202-4416 NR 17 TC 39 Z9 39 U1 1 U2 8 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 OCT 24 PY 2003 VL 108 IS E12 AR 8061 DI 10.1029/2002JE002038 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 736YF UT WOS:000186200300002 ER PT J AU Garvin, JB Weitz, C Figueroa, O Crisp, J AF Garvin, JB Weitz, C Figueroa, O Crisp, J TI Introduction to the special section: Mars Exploration Rover mission and landing sites SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; rover; Mars Exploration Rover; Mars Exploration Program; landing sites C1 NASA Headquarters, Washington, DC 20546 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP NASA Headquarters, 300 E St SW, Washington, DC 20546 USA. EM james.b.garvin@nasa.gov; catherine.m.weitz@nasa.gov; orlando.figueroa-1@nasa.gov; joy.a.crisp@jpl.nasa.gov NR 3 TC 1 Z9 1 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD OCT 24 PY 2003 VL 108 IS E12 AR 8060 DI 10.1029/2003JE002072 PG 2 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 736YF UT WOS:000186200300005 ER PT J AU Tsou, P Brownlee, DE Sandford, SA Horz, F Zolensky, ME AF Tsou, P Brownlee, DE Sandford, SA Horz, F Zolensky, ME TI Wild 2 and interstellar sample collection and Earth return SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Wild 2; comet coma dust; interstellar dust; sample return; silica aerogel; intact capture ID COMET 81P/WILD-2; INTACT CAPTURE; DUST; MISSION; AEROGEL AB [1] Stardust, launched in 1999, is the first mission designed to bring samples from a known, recently deflected comet, 81P/Wild 2, on 2 January 2004 and is also the first to capture newly discovered contemporary interstellar dust streaming through our solar system. The Stardust aerogel collector accomplishes Stardust's primary science and will be returned to Earth with its captured samples on 15 January 2006 in a reentry capsule. Wild 2 samples will be captured at 6.12 km/s and represent well-preserved relics of the outer regions of our solar nebula and fundamental building blocks of our planetary system. Interstellar grains captured at velocities of less than 10 km/s are expected to survive intact and represent the main repositories of condensable elements that permeate the galaxy. These solid cometary and interstellar samples will be captured in two back-to-back sample collection trays filled with variable-density aerogel. There are 132 silica aerogel capture cells of 3 cm and 1 cm thickness for the cometary and the interstellar sides, respectively. The aerogel capture cells were wedged into the sample collection trays and wrapped on all four sides with 100-mum-thick pure aluminum foil to facilitate aerogel cell removal. The total exposed Wild 2 surface area is 1039 cm(2) of aerogel and 153 cm(2) of aluminum foil. Results from a preliminary examination for the Wild 2 samples will be reported within 9 months of sample return and for the interstellar samples a year later. After preliminary examination the samples will be transferred to the NASA Office of the Curator and made available to the general science community. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Washington, Dept Astron, Seattle, WA 98195 USA. NASA, Ames Res Ctr, Div Space Sci, Astrophys Branch, Moffett Field, CA 94035 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Tsou, P (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM peter.tsou@jpl.nasa.gov; brownlee@astro.washington.edu; ssandford@mail.arc.nasa.gov; friedrich.p.horzl@jsc.nasa.gov; michael.e.zolensky1@jsc.nasa.gov NR 57 TC 81 Z9 83 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD OCT 24 PY 2003 VL 108 IS E10 AR 8113 DI 10.1029/2003JE002109 PG 21 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 736YA UT WOS:000186199800001 ER PT J AU Shvedova, AA Castranova, V Kisin, ER Schwegler-Berry, D Murray, AR Gandelsman, VZ Maynard, A Baron, P AF Shvedova, AA Castranova, V Kisin, ER Schwegler-Berry, D Murray, AR Gandelsman, VZ Maynard, A Baron, P TI Exposure to carbon nanotube material: Assessment of nanotube cytotoxicity using human keratinocyte cells SO JOURNAL OF TOXICOLOGY AND ENVIRONMENTAL HEALTH-PART A LA English DT Article ID OXIDATIVE STRESS; CONTACT-DERMATITIS; FREE-RADICALS; IRON; PARTICLES; CANCER; TOXICOLOGY; ACTIVATION; MINERS; LAYER AB Carbon nanotubes are new members of carbon allotropes similar to fullerenes and graphite. Because of their unique electrical, mechanical, and thermal properties, carbon nanotubes are important for novel applications in the electronics, aerospace, and computer industries. Exposure to graphite and carbon materials has been associated with increased incidence of skin diseases, such as carbon fiber dermatitis, hyperkeratosis, and naevi. We investigated adverse effects of single-wall carbon nanotubes (SWCNT) using a cell culture of immortalized human epidermal keratinocytes (HaCaT). After 18 h of exposure of HaCaT to SWCNT, oxidative stress and cellular toxicity were indicated by formation of free radicals, accumulation of peroxidative products, antioxidant depletion, and loss of cell viability. Exposure to SWCNT also resulted in ultrastructural and morphological changes in cultured skin cells. These data indicate that dermal exposure to unrefined SWCNT may lead to dermal toxicity due to accelerated oxidative stress in the skin of exposed workers. C1 NIOSH, Pathol & Physiol Res Branch, Morgantown, WV 26505 USA. W Virginia Univ, Dept Physiol & Pharmacol, Morgantown, WV 26506 USA. NASA, Sci Applicat Int Corp, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NIOSH, Monitoring Res & Stat Act, DART, Cincinnati, OH 45226 USA. RP Shvedova, AA (reprint author), NIOSH, Pathol & Physiol Res Branch, 1095 Willowdale Rd, Morgantown, WV 26505 USA. RI Maynard, Andrew/D-1076-2010; OI Maynard, Andrew/0000-0003-2117-5128 NR 53 TC 711 Z9 766 U1 12 U2 103 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1528-7394 J9 J TOXICOL ENV HEAL A JI J. TOXICOL. ENV. HEALTH PT A PD OCT 24 PY 2003 VL 66 IS 20 BP 1909 EP 1926 DI 10.1080/15287390390231566 PG 18 WC Environmental Sciences; Public, Environmental & Occupational Health; Toxicology SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health; Toxicology GA 737LK UT WOS:000186231700002 PM 14514433 ER PT J AU Hoefen, TM Clark, RN Bandfield, JL Smith, MD Pearl, JC Christensen, PR AF Hoefen, TM Clark, RN Bandfield, JL Smith, MD Pearl, JC Christensen, PR TI Discovery of olivine in the Nili Fossae region of Mars SO SCIENCE LA English DT Article ID THERMAL EMISSION SPECTROMETER; SURFACE; SPECTROSCOPY; MISSION; AVIRIS AB We have detected a 30,000-square-kilometer area rich in olivine in the Nili Fossae region of Mars. Nili Fossae has been interpreted as a complex of grabens and fractures related to the formation of the Isidis impact basin. We propose that post-impact faulting of this area has exposed subsurface layers rich in olivine. Linear mixture analysis of Thermal Emission Spectrometer spectra shows surface exposures of 30% olivine, where the composition of the olivine ranges from Fo(30) to Fo(70). C1 US Geol Survey, Denver, CO 80225 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Arizona State Univ, Tempe, AZ 85287 USA. RP Hoefen, TM (reprint author), US Geol Survey, Box 25046, Denver, CO 80225 USA. RI Smith, Michael/C-8875-2012 NR 25 TC 161 Z9 161 U1 4 U2 13 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 OCT 24 PY 2003 VL 302 IS 5645 BP 627 EP 630 DI 10.1126/science.1089647 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 735MV UT WOS:000186119900054 PM 14576430 ER PT J AU Day, PK LeDuc, HG Mazin, BA Vayonakis, A Zmuidzinas, J AF Day, PK LeDuc, HG Mazin, BA Vayonakis, A Zmuidzinas, J TI A broadband superconducting detector suitable for use in large arrays SO NATURE LA English DT Article ID TRANSITION EDGE SENSORS; X-RAY-DETECTION; ENERGY RESOLUTION; ELECTROTHERMAL FEEDBACK; IMAGING SPECTROMETERS; TUNNEL-JUNCTIONS; MICROCALORIMETER; TEMPERATURE; INDUCTANCE; MULTIPLEXER AB Cryogenic detectors are extremely sensitive and have a wide variety of applications(1-3) (particularly in astronomy(4-8)), but are difficult to integrate into large arrays like a modern CCD ( charge-coupled device) camera. As current detectors of the cosmic microwave background (CMB) already have sensitivities comparable to the noise arising from the random arrival of CMB photons, the further gains in sensitivity needed to probe the very early Universe will have to arise from large arrays. A similar situation is encountered at other wavelengths. Single-pixel X-ray detectors now have a resolving power of DeltaE < 5 eV for single 6-keV photons, and future X-ray astronomy missions(7) anticipate the need for 1,000-pixel arrays. Here we report the demonstration of a superconducting detector that is easily fabricated and can readily be incorporated into such an array. Its sensitivity is already within an order of magnitude of that needed for CMB observations, and its energy resolution is similarly close to the targets required for future X-ray astronomy missions. C1 Jet Prop Lab, Pasadena, CA 91107 USA. CALTECH, Pasadena, CA 91125 USA. RP Day, PK (reprint author), Jet Prop Lab, Pasadena, CA 91107 USA. RI Mazin, Ben/B-8704-2011 OI Mazin, Ben/0000-0003-0526-1114 NR 29 TC 595 Z9 600 U1 9 U2 79 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD OCT 23 PY 2003 VL 425 IS 6960 BP 817 EP 821 DI 10.1038/nature02037 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 735ME UT WOS:000186118500040 PM 14574407 ER PT J AU Weitz, CM Parker, TJ Bulmer, MH Anderson, FS Grant, JA AF Weitz, CM Parker, TJ Bulmer, MH Anderson, FS Grant, JA TI Geology of the Melas Chasma landing site for the Mars Exploration Rover mission SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Valles Marineris; Melas Chasma; MER; landslides; valleys; mass wasting ID VALLES MARINERIS MARS; SUBMARINE LANDSLIDES; LAYERED DEPOSITS; DEBRIS FLOWS; SPECTROMETER; TOPOGRAPHY; TECTONICS; EVOLUTION; PATTERNS; ORIGIN AB [1] The Melas Chasma landing site was considered a high-priority site for the Mars Exploration Rover ( MER) mission because of the opportunity to land on and study potential layered sedimentary deposits. Though no longer considered a candidate site because of safety concerns, the site remains a scientifically interesting area that provides insight into the geologic history of Valles Marineris. Within the landing ellipse are dunes, landslide material, and unusual blocky deposits. The blocky deposits are composed of rounded blocks, some of which have meter-scale layering, and they show evidence of ductile deformation, including bending and distortion of coherent blocks around each other. The morphologic characteristics of the blocks are unique, and they appear to have no terrestrial analogue. However, the gross morphology of these blocky deposits and their superposition on adjacent wallrock is consistent with the blocks having been transported downslope. Given the existence of other large mass failures in the area, we propose the blocky deposits may also have originated from mass movement events. The size of the blocks coupled with the distances they traveled indicates high mobility. The distances the blocks were transported and their rounded, irregular shapes suggest either water in the source material or deposition in a subaqueous environment. The source for the main blocky deposit inside the landing ellipse is considered to be the wallrock to the south, while the other two blocky deposits have source regions along the northern canyon walls. The southern wallrock of Melas Chasma contains numerous valleys not seen elsewhere in Valles Marineris. The identification of valley networks along the southern wallrock suggests that a source of water existed below the surface of the plateau and produced the valleys after intersecting the edge of the exposed canyon walls. C1 Planetary Sci Inst, Tucson, AZ 85719 USA. NASA Headquarters, Washington, DC USA. Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Weitz, CM (reprint author), Planetary Sci Inst, 1700 E Ft Lowell,Suite 106, Tucson, AZ 85719 USA. NR 77 TC 23 Z9 23 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD OCT 22 PY 2003 VL 108 IS E12 AR 8082 DI 10.1029/2002JE002022 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 736YE UT WOS:000186200200001 ER PT J AU Tsyganenko, NA Mukai, T AF Tsyganenko, NA Mukai, T TI Tail plasma sheet models derived from Geotail particle data (vol 108, art no 1136, 2003) SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Correction C1 NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Extraterr Phys Lab, Greenbelt, MD 20771 USA. Inst Space & Astronaut Sci, Sagamihara, Kanagawa 229, Japan. RP Tsyganenko, NA (reprint author), NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Greenbelt, MD 20771 USA. RI Tsyganenko, Nikolai/J-7377-2012 OI Tsyganenko, Nikolai/0000-0002-5938-1579 NR 2 TC 2 Z9 2 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 OCT 22 PY 2003 VL 108 IS A10 AR 1374 DI 10.1029/2003JA010127 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 736YL UT WOS:000186200800006 ER PT J AU Beig, G Keckhut, P Lowe, RP Roble, RG Mlynczak, MG Scheer, J Fomichev, VI Offermann, D French, WJR Shepherd, MG Semenov, AI Remsberg, EE She, CY Lubken, FJ Bremer, J Clemesha, BR Stegman, J Sigernes, F Fadnavis, S AF Beig, G Keckhut, P Lowe, RP Roble, RG Mlynczak, MG Scheer, J Fomichev, VI Offermann, D French, WJR Shepherd, MG Semenov, AI Remsberg, EE She, CY Lubken, FJ Bremer, J Clemesha, BR Stegman, J Sigernes, F Fadnavis, S TI Review of mesospheric temperature trends SO REVIEWS OF GEOPHYSICS LA English DT Review DE temperature trends; thermal shrinking; mesosphere; greenhouse gases ID GENERAL-CIRCULATION MODEL; LOCAL-THERMODYNAMIC-EQUILIBRIUM; NOCTILUCENT CLOUD OCCURRENCE; MIDLATITUDE MESOPAUSE REGION; EQUATORIAL MIDDLE ATMOSPHERE; SOLAR ULTRAVIOLET VARIATIONS; ZONAL-MEAN CLIMATOLOGY; GRAVITY-WAVE ACTIVITY; LONG-TERM CHANGES; LOWER THERMOSPHERE AB [1] In recent times it has become increasingly clear that releases of trace gases from human activity have a potential for causing change in the upper atmosphere. However, our knowledge of systematic changes and trends in the temperature of the mesosphere and lower thermosphere is relatively limited compared to the Earth's lower atmosphere, and not much effort has been made to synthesize these results so far. In this article, a comprehensive review of long-term trends in the temperature of the region from 50 to 100 km is made on the basis of the available up-to-date understanding of measurements and model calculations. An objective evaluation of the available data sets is attempted, and important uncertainly factors are discussed. Some natural variability factors, which are likely to play a role in modulating temperature trends, are also briefly touched upon. There are a growing number of experimental results centered on, or consistent with, zero temperature trend in the mesopause region ( 80 - 100 km). The most reliable data sets show no significant trend but an uncertainty of at least 2 K/decade. On the other hand, a majority of studies indicate negative trends in the lower and middle mesosphere with an amplitude of a few degrees ( 2 - 3 K) per decade. In tropical latitudes the cooling trend increases in the upper mesosphere. The most recent general circulation models indicate increased cooling closer to both poles in the middle mesosphere and a decrease in cooling toward the summer pole in the upper mesosphere. Quantitatively, the simulated cooling trend in the middle mesosphere produced only by CO2 increase is usually below the observed level. However, including other greenhouse gases and taking into account a "thermal shrinking" of the upper atmosphere result in a cooling of a few degrees per decade. This is close to the lower limit of the observed nonzero trends. In the mesopause region, recent model simulations produce trends, usually below 1 K/decade, that appear to be consistent with most observations in this region. C1 Indian Inst Trop Meteorol, Pune 411008, Maharashtra, India. Leibniz Inst Atmospher Phys, D-18255 Kuhlungborn, Germany. Inst Nacl Pesquisas Espaciais, BR-12245970 Sao Jose Dos Campos, Brazil. York Univ, Dept Earth & Atmospher Sci, N York, ON M3J 1P3, Canada. Australian Antarctic Div, Atmospher & Space Phys Grp, Kingston, Tas 7050, Australia. IPSL, Serv Aeron, F-91371 Verrieres Le Buisson, France. Univ Western Ontario, Ctr Res Earth & Space Technol, London, ON M7A 3K7, Canada. NASA, Radiat & Aerosol Branch, Langley Res Ctr, Hampton, VA 23681 USA. Berg Univ Wuppertal, Dept Phys, D-42097 Wuppertal, Germany. Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. Russian Acad Sci, Obukhov Inst Atmospher Phys, Moscow 109017, Russia. Colorado State Univ, Dept Phys, Ft Collins, CO 80523 USA. York Univ, Dept Earth & Atmospher Sci, Ctr Res Earth & Space Sci, N York, ON M3J 1P3, Canada. Univ Courses Svalbard, N-9171 Longyearbyen, Norway. Stockholm Univ, Inst Meteorol, S-10691 Stockholm, Sweden. RP Indian Inst Trop Meteorol, Pune 411008, Maharashtra, India. EM beig@tropmet.res.in; keckhut@aerov.jussieu.fr; lowe@physics.uwo.ca; roble@hoa.ucar.edu; m.g.mlynczak@larc.nasa.gov; jurgen@caerce.edu.ar; victor@nimbus.yorku.ca; offerm@uniwuppertal.de; john.french@aad.gov.au; marianna@stpl.cress.yorku.ca; meso@omega.ifaran.ru; e.e.remsberg@larc.nasa.gov; joeshe@lamar.colostate.edu; luebken@iap-kborn.de; bremer@iap-kborn.de; clem@laser.inpe.br; jacek@misu.su.se; Fred.Sigernes@unis.no; suvarna@tropmet.res.in RI Mlynczak, Martin/K-3396-2012 NR 210 TC 147 Z9 149 U1 2 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 8755-1209 EI 1944-9208 J9 REV GEOPHYS JI Rev. Geophys. PD OCT 22 PY 2003 VL 41 IS 4 AR 1015 DI 10.1029/2002RG000121 PG 41 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 736YT UT WOS:000186201400001 ER PT J AU Gutsev, GL Bauschlicher, CW AF Gutsev, GL Bauschlicher, CW TI Oxidation of carbon monoxide on small iron clusters SO CHEMICAL PHYSICS LETTERS LA English DT Article ID GAUSSIAN-BASIS SETS; CATALYTIC-OXIDATION; ELECTRONIC-STRUCTURE; GOLD CLUSTERS; CO OXIDATION; SURFACE; PT(111); ATOMS; O-2; REPRESENTATION AB The oxidation of carbon monoxide adsorbed on Fe-n (n = 1-6) clusters is studied using density functional theory. Both neutral and anionic clusters are studied. The reactions of chemisorbed CO with O-2 are found to be highly exothermic for all of the iron clusters considered. Effects of higher coverages are estimated using the Fe-4 cluster with two adsorbates. namely Fe-4(CO)(2), Fe4C2, and Fe4O2 clusters. Our results suggest that the iron clusters sustain a full catalytic cycle of carbon monoxide oxidation. Published by Elsevier B.V. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Gutsev, GL (reprint author), ELORET Corp, Mail Stop 230-3, Sunnyvale, CA 94087 USA. NR 35 TC 8 Z9 8 U1 0 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2614 J9 CHEM PHYS LETT JI Chem. Phys. Lett. PD OCT 21 PY 2003 VL 380 IS 3-4 BP 435 EP 443 DI 10.1016/j.cplett.2003.08.123 PG 9 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 736CW UT WOS:000186154000032 ER PT J AU Eck, TF Holben, BN Reid, JS O'Neill, NT Schafer, JS Dubovik, O Smirnov, A Yamasoe, MA Artaxo, P AF Eck, TF Holben, BN Reid, JS O'Neill, NT Schafer, JS Dubovik, O Smirnov, A Yamasoe, MA Artaxo, P TI High aerosol optical depth biomass burning events: A comparison of optical properties for different source regions SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SKY RADIANCE MEASUREMENTS; WAVELENGTH DEPENDENCE; BRAZIL; SMOKE; SUN; ABSORPTION; AERONET; NETWORK AB [1] The optical properties of aerosols such as smoke from biomass burning vary due to aging processes and these particles reach larger sizes at high concentrations. We compare the spectra of aerosol optical depth (tau(a)), column-integrated volume size distributions, refractive indices, and single scattering albedo retrieved from AERONET observations for four selected events of very high smoke optical depth (tau(a) similar to 2 at 500 nm). Two case studies are from tropical biomass burning regions ( Brazil and Zambia) and two are cases of boreal forest and peat fire smoke transported long distances to sites in the US and Moldova. Smoke properties for these extreme events can be significantly different from those reported in more typical plumes. In particular, large differences in smoke fine mode particle radius ( similar to 0.17 to 0.25 mum) and single scattering albedo ( similar to 0.88 to 0.99 at 440 nm) were observed as a result of differences in fuels burned, combustion phase, and aging. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. USN, Marine Meteorol Div, Res Lab, Monterey, CA 93943 USA. Univ Sherbrooke, CARTEL, Sherbrooke, PQ J1K 2R1, Canada. Sci Syst & Applicat Inc, Lanham, MD USA. Univ Sao Paulo, Sao Paulo, Brazil. RP Eck, TF (reprint author), NASA, Goddard Space Flight Ctr, Code 923, Greenbelt, MD 20771 USA. RI Dubovik, Oleg/A-8235-2009; Schafer, Joel/A-3978-2010; Smirnov, Alexander/C-2121-2009; ECK, THOMAS/D-7407-2012; Yamasoe, Marcia/L-3667-2013; Reid, Jeffrey/B-7633-2014; Artaxo, Paulo/E-8874-2010 OI Dubovik, Oleg/0000-0003-3482-6460; Smirnov, Alexander/0000-0002-8208-1304; Yamasoe, Marcia/0000-0003-3066-9146; Reid, Jeffrey/0000-0002-5147-7955; Artaxo, Paulo/0000-0001-7754-3036 NR 18 TC 110 Z9 112 U1 1 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD OCT 21 PY 2003 VL 30 IS 20 AR 2035 DI 10.1029/2003GL017861 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 736XE UT WOS:000186197900002 ER PT J AU Kinne, S Lohmann, U Feichter, J Schulz, M Timmreck, C Ghan, S Easter, R Chin, M Ginoux, P Takemura, T Tegen, I Koch, D Herzog, M Penner, J Pitari, G Holben, B Eck, T Smirnov, A Dubovik, O Slutsker, I Tanre, D Torres, O Mishchenko, M Geogdzhayev, I Chu, DA Kaufman, Y AF Kinne, S Lohmann, U Feichter, J Schulz, M Timmreck, C Ghan, S Easter, R Chin, M Ginoux, P Takemura, T Tegen, I Koch, D Herzog, M Penner, J Pitari, G Holben, B Eck, T Smirnov, A Dubovik, O Slutsker, I Tanre, D Torres, O Mishchenko, M Geogdzhayev, I Chu, DA Kaufman, Y TI Monthly averages of aerosol properties: A global comparison among models, satellite data, and AERONET ground data SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE tropospheric aerosol; aerosol component modeling; aerosol module evaluation; direct aerosol radiative forcing; regional comparisons ID SKY RADIANCE MEASUREMENTS; OPTICAL-THICKNESS; SEA-SALT; TROPOSPHERIC AEROSOL; 3-DIMENSIONAL SIMULATION; CARBONACEOUS AEROSOLS; SULFATE AEROSOL; MINERAL AEROSOL; UNITED-STATES; DUST AEROSOLS AB [1] New aerosol modules of global ( circulation and chemical transport) models are evaluated. These new modules distinguish among at least five aerosol components: sulfate, organic carbon, black carbon, sea salt, and dust. Monthly and regionally averaged predictions for aerosol mass and aerosol optical depth are compared. Differences among models are significant for all aerosol types. The largest differences were found near expected source regions of biomass burning ( carbon) and dust. Assumptions for the permitted water uptake also contribute to optical depth differences ( of sulfate, organic carbon, and sea salt) at higher latitudes. The decline of mass or optical depth away from recognized sources reveals strong differences in aerosol transport or removal among models. These differences are also a function of altitude, as transport biases of dust do not always extend to other aerosol types. Ratios of optical depth and mass demonstrate large differences in the mass extinction efficiency, even for hydrophobic aerosol. This suggests that efforts of good mass simulations could be wasted or that conversions are misused to cover for poor mass simulations. In an attempt to provide an absolute measure for model skill, simulated total optical depths ( when adding contributions from all five aerosol types) are compared to measurements from ground and space. Comparisons to the Aerosol Robotic Network (AERONET) suggest a source strength underestimate in many models, most frequently for ( subtropical) tropical biomass or dust. Comparisons to the combined best of Moderate-Resolution Imaging Spectroradiometer ( MODIS) and Total Ozone Mapping Spectrometer ( TOMS) indicate that away from sources, model simulations are usually smaller. Particularly large are discrepancies over tropical oceans and oceans of the Southern Hemisphere, raising issues on the treatment of sea salt in models. Totals for mass or optical depth in many models are defined by the absence or dominance of only one aerosol component. With appropriate corrections to that component ( e. g., to removal, to source strength, or to seasonality) a much better model performance can be expected. Still, many important modeling issues remain inconclusive as the combined result of poor coordination ( different emissions and meteorology), insufficient model output ( vertical distributions, water uptake by aerosol type), and unresolved measurement issues ( retrieval assumptions and temporal or spatial sampling biases). C1 Max Planck Inst Meteorol, D-20146 Hamburg, Germany. Dalhousie Univ, Dept Phys, Atmospher Sci Program, Halifax, NS B3H 3J5, Canada. CEA, CNRS, LSCE, F-91191 Gif Sur Yvette, France. Battelle Mem Inst, Pacific NW Natl Lab, Richland, WA 99352 USA. NASA, GIT, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NOAA, Geophys Fluid Dynam Lab, Princeton, NJ 08542 USA. Kyushu Univ, Appl Mech Res Inst, Fukuoka 8168580, Japan. Max Planck Inst Biogeochem, D-07745 Jena, Germany. Columbia Univ, Dept Appl Phys & Appl Math, NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. Univ Aquila, Dipartimento Fis, I-67010 Coppito, Laquila, Italy. Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Lille 1, Opt Atmospher Lab, F-59655 Villeneuve Dascq, France. Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Max Planck Inst Meteorol, Bundesstr 55, D-20146 Hamburg, Germany. EM kinne@dkrz.de; ulrike.lohmann@dal.ca; feichter@dkrz.de; schulz@lsce.saclay.cea.fr; timmreck@dkrz.de; steve.ghan@pnl.gov; richard.easter@pnl.gov; chin@gator1.gsfc.nasa.gov; ginoux@rondo.gsfc; toshi@riam.kyushu-u.ac.jp; itegen@bgc-jena.mpg.de; dorothy.koch@yale.edu; herzogm@umich.edu; penner@umich.edu; pitari@vxscaq.aquila.infn.it; brent@aeronet.gsfc.nasa.gov; tom@aeronet.gsfc.nasa.gov; asmirnov@spamer.gsfc.nasa.gov; dubovik@aeronet.gsfc.nasa.gov; ilya@aeronet.nasa.gov; didier.tanre@univ-lille1.fr; torres@tparty.gsfc.nasa.gov; mmishchenko@giss.nasa.gov; ig117@columbia.edu; achu@climate.gsfc.nasa.gov; yoram.j.kaufman@nasa.gov RI Dubovik, Oleg/A-8235-2009; Penner, Joyce/J-1719-2012; Torres, Omar/G-4929-2013; Kyushu, RIAM/F-4018-2015; Mishchenko, Michael/D-4426-2012; Schulz, Michael/A-6930-2011; U-ID, Kyushu/C-5291-2016; Herzog, Michael/B-4722-2010; Smirnov, Alexander/C-2121-2009; ECK, THOMAS/D-7407-2012; Takemura, Toshihiko/C-2822-2009; Ginoux, Paul/C-2326-2008; Chin, Mian/J-8354-2012; Ghan, Steven/H-4301-2011; Lohmann, Ulrike/B-6153-2009; Pitari, Giovanni/O-7458-2016 OI Dubovik, Oleg/0000-0003-3482-6460; Schulz, Michael/0000-0003-4493-4158; Smirnov, Alexander/0000-0002-8208-1304; Takemura, Toshihiko/0000-0002-2859-6067; Ginoux, Paul/0000-0003-3642-2988; Ghan, Steven/0000-0001-8355-8699; Lohmann, Ulrike/0000-0001-8885-3785; Pitari, Giovanni/0000-0001-7051-9578 NR 64 TC 179 Z9 181 U1 5 U2 42 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 OCT 21 PY 2003 VL 108 IS D20 AR 4634 DI 10.1029/2001JD001253 PG 42 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 736XL UT WOS:000186198500001 ER PT J AU Mizoguchi, K Morey, SL Zavala-Hidalgo, J Suginohara, N Hakkinen, S O'Brien, JJ AF Mizoguchi, K Morey, SL Zavala-Hidalgo, J Suginohara, N Hakkinen, S O'Brien, JJ TI Convective activity in the Labrador Sea: Preconditioning associated with decadal variability in subsurface ocean stratification SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article DE decadal oscillation; North Atlantic; convection; Labrador Sea ID NORTH-ATLANTIC-OCEAN; SURFACE TEMPERATURE; DEEP CONVECTION; THERMOHALINE CIRCULATION; CLIMATE; ICE; FLUCTUATIONS; HYDROGRAPHY; TRANSPORT; SYSTEM AB [1] The decadal variability of the convective activity in the Labrador Sea is investigated using 43 years of model output from a prognostic coupled ice-ocean model that simulates both the Arctic and the North Atlantic Oceans. The fields of the surface density and the mixed-layer depth indicate that the center of the convective activity is located in western Labrador Sea. The decadal variations of the convective depth are controlled to large extent by the oceanic preconditioning associated with changes in subsurface stratification. The intensity of the convective mixing varies from year to year, depending upon how strong the isopycnal doming is at the preconditioning stage at the center of the convective region. The variations of the subsurface stratification seem to be related to the subsurface temperature changes. C1 Univ Maryland Baltimore Cty, GEST, Baltimore, MD 21250 USA. Florida State Univ, COAPS, Tallahassee, FL 32306 USA. Frontier Observat Res Syst Global Change, Kanazawa Ku, Yokohama, Kanagawa 2370001, Japan. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Mizoguchi, K (reprint author), Univ Maryland Baltimore Cty, GEST, 1000 Hilltop Circle, Baltimore, MD 21250 USA. EM mizoguchi@ltpmailx.gsfc.nasa.gov; morey@coaps.fsu.edu; zavala@coaps.fsu.edu; nobuo@jamstec.go.jp; sirpa@ltpmail.gsfc.nasa.gov; obrien@coaps.fsu.edu RI Zavala-Hidalgo, Jorge/H-3185-2011; Hakkinen, Sirpa/E-1461-2012 NR 37 TC 3 Z9 3 U1 3 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD OCT 21 PY 2003 VL 108 IS C10 AR 3330 DI 10.1029/2002JC001735 PG 10 WC Oceanography SC Oceanography GA 736XV UT WOS:000186199300003 ER PT J AU Stammerjohn, SE Drinkwater, MR Smith, RC Liu, X AF Stammerjohn, SE Drinkwater, MR Smith, RC Liu, X TI Ice-atmosphere interactions during sea-ice advance and retreat in the western Antarctic Peninsula region SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article DE ice-atmosphere interactions; ice motion; Antarctic sea ice; remote sensing ID SOUTHERN-OCEAN CLIMATE; SEMIANNUAL OSCILLATION; BELLINGSHAUSEN SEAS; AMUNDSEN SEAS; WEDDELL SEA; TEMPERATURE-GRADIENTS; CIRCUMPOLAR WAVE; AIR-TEMPERATURE; SNOW COVER; OPEN WATER AB [1] The seasonal evolution of sea-ice extent, concentration, and drift in the western Antarctic Peninsula (WAP) region, along with regional atmospheric synoptic variability, are described for a winter period ( 1992) when sea-ice advance and retreat were both anomalously early. Daily time series of winds, opening and closing of the sea-ice cover, and volume fluxes in and out of the WAP region indicate that synoptic variability in meridional winds determines whether the ice-edge advances or retreats on daily to weekly timescales. The importance of this finding is that the dynamics, as opposed to the thermodynamics, initiate, and thereby dominate, in the production of ice-edge anomalies. Further, the abrupt mid-winter shift from persistently positive to negative ice-edge anomalies indicates that there was a distinct change in the regional atmospheric circulation. The ice-atmosphere interactions in the winter of 1992 are then compared to those in the winter of 1990, when sea-ice advance and retreat were both late instead of early, but again the mid-winter shift was abrupt. The comparison highlights possible circumpolar and tropical-polar atmospheric linkages in the South Pacific that involve changes in the amplitude/phase of the semi-annual oscillation (SAO), which in turn appear to be related to El Nino-Southern Oscillation (ENSO) changes in the tropical Pacific. The implication of a dynamically driven ice-atmosphere system, together with an intraseasonal ENSO linkage, further supports the idea that the WAP region is particularly sensitive to changes in the tropical Pacific. C1 Columbia Univ, Lamont Doherty Earth Observ, Dept Earth & Environm Sci, Palisades, NY 10964 USA. European Space Agcy, ESTEC, FSO, EOP,Oceans Ice Unit, NL-2200 AG Noordwijk ZH, Netherlands. Inst Computat Earth Syst Sci, Santa Barbara, CA 93106 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91009 USA. RP Stammerjohn, SE (reprint author), Columbia Univ, Lamont Doherty Earth Observ, Dept Earth & Environm Sci, Palisades, NY 10964 USA. RI Drinkwater, Mark/C-2478-2011 OI Drinkwater, Mark/0000-0002-9250-3806 NR 74 TC 28 Z9 28 U1 2 U2 8 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 OCT 21 PY 2003 VL 108 IS C10 AR 3329 DI 10.1029/2002JC001543 PG 15 WC Oceanography SC Oceanography GA 736XV UT WOS:000186199300002 ER PT J AU Golombek, MP Haldemann, AFC Forsberg-Taylor, NK DiMaggio, EN Schroeder, RD Jakosky, BM Mellon, MT Matijevic, JR AF Golombek, MP Haldemann, AFC Forsberg-Taylor, NK DiMaggio, EN Schroeder, RD Jakosky, BM Mellon, MT Matijevic, JR TI Rock size-frequency distributions on Mars and implications for Mars Exploration Rover landing safety and operations SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars Exploration Rover landing sites; Mars Pathfinder landing site; thermal inertia; rocks; Gusev; Meridiani ID PHYSICAL-PROPERTIES; GLOBAL SURVEYOR; PATHFINDER MISSION; SITE PREDICTIONS; THERMAL EMISSION; MARTIAN SURFACE; ORBITER CAMERA; BRITTLE SOLIDS; FRAGMENT SIZE; DUST AB [1] The cumulative fractional area covered by rocks versus diameter measured at the Pathfinder site was predicted by a rock distribution model that follows simple exponential functions that approach the total measured rock abundance (19%), with a steep decrease in rocks with increasing diameter. The distribution of rocks > 1.5 m diameter visible in rare boulder fields also follows this steep decrease with increasing diameter. The effective thermal inertia of rock populations calculated from a simple empirical model of the effective inertia of rocks versus diameter shows that most natural rock populations have cumulative effective thermal inertias of 1700 - 2100 J m(-2) s(-0.5) K-1 and are consistent with the model rock distributions applied to total rock abundance estimates. The Mars Exploration Rover ( MER) airbags have been successfully tested against extreme rock distributions with a higher percentage of potentially hazardous triangular buried rocks than observed at the Pathfinder and Viking landing sites. The probability of the lander impacting a > 1 m diameter rock in the first 2 bounces is < 3% and < 5% for the Meridiani and Gusev landing sites, respectively, and is < 0.14% and < 0.03% for rocks > 1.5 m and > 2 m diameter, respectively. Finally, the model rock size-frequency distributions indicate that rocks > 0.1 m and > 0.3 m in diameter, large enough to place contact sensor instruments against and abrade, respectively, should be plentiful within a single sol's drive at the Meridiani and Gusev landing sites. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Virol Unit, Dept Environm Sci, Charlottesville, VA 22904 USA. Univ Michigan, Dept Geol Sci, Ann Arbor, MI 48109 USA. Calif State Univ, Dept Geol, Bakersfield, CA 93311 USA. Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. RP Golombek, MP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Mellon, Michael/C-3456-2016 NR 55 TC 51 Z9 53 U1 2 U2 5 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 OCT 21 PY 2003 VL 108 IS E12 AR 8086 DI 10.1029/2002JE002035 PG 23 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 736YC UT WOS:000186200000002 ER PT J AU Kuan, YJ Yan, CH Charnley, SB Kisiel, Z Ehrenfreund, P Huang, HC AF Kuan, YJ Yan, CH Charnley, SB Kisiel, Z Ehrenfreund, P Huang, HC TI A search for interstellar pyrimidine SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE astrobiology; line : identification; ISM : individual : Orion KL; ISM : individual : Sgr B2(N); ISM : individual : W51 e1/e2; ISM : molecules ID NITROGEN-HETEROCYCLIC COMPOUNDS; LINE SURVEY; ETHYLENE-OXIDE; ORION-KL; MOLECULES; GHZ; CHEMISTRY; CRL-618; HYDROCARBONS; ABUNDANCES AB We have searched three hot molecular cores for submillimetre emission from the nucleic acid building block pyrimidine. We obtain upper limits to the total pyrimidine (beam-averaged) column densities towards Sgr B2(N), Orion KL and W51 e1/e2 of 1.7 x 10(14), 2.4 x 10(14) and 3.4 x 10(14) cm(-2), respectively. The associated upper limits to the pyrimidine fractional abundances lie in the range (0.3-3) x 10(-10). Implications of this result for interstellar organic chemistry, and for the prospects of detecting nitrogen heterocycles in general, are discussed briefly. C1 Natl Taiwan Normal Univ, Dept Earth Sci, Taipei 116, Taiwan. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. NASA, Div Space Sci, Ames Res Ctr, Moffett Field, CA 94035 USA. Polish Acad Sci, Inst Phys, PL-02668 Warsaw, Poland. Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Kuan, YJ (reprint author), Natl Taiwan Normal Univ, Dept Earth Sci, Taipei 116, Taiwan. RI Charnley, Steven/C-9538-2012; Kisiel, Zbigniew/K-8798-2016 OI Kisiel, Zbigniew/0000-0002-2570-3154 NR 36 TC 45 Z9 45 U1 1 U2 8 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 21 PY 2003 VL 345 IS 2 BP 650 EP 656 DI 10.1046/j.1365-8711.2003.06975.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 731FG UT WOS:000185873400024 ER PT J AU Bottcher, M Marscher, AP Ravasio, M Villata, M Raiteri, CM Aller, HD Aller, MF Terasranta, H Mang, O Tagliaferri, G Aharonian, F Krawczynski, H Kurtanidze, OM Nikolashvili, MG Ibrahimov, MA Papadakis, IE Tsinganos, K Sadakane, K Okada, N Takalo, LO Sililanpaa, A Tosti, G Ciprini, S Frasca, A Marilli, E Robb, R Noble, JC Jorstad, SG Hagen-Thorn, VA Larionov, VM Nesci, R Maesano, M Schwartz, RD Basler, J Gorham, PW Iwamatsu, H Kato, T Pullen, C Benitez, E de Diego, JA Moilanen, M Oksanan, A Rodriguez, D Sadun, AC Kelly, M Carini, MT Miller, HR Catalano, S Dultzin-Hacyan, D Fan, JH Ghisellini, G Ishioka, R Karttunen, H Keinanen, P Kudryavtseva, NA Lainela, M Lanteri, L Larionova, EG Matsumoto, K Mattox, JR McHardy, I Montagni, F Nucciarelli, G Ostorero, L Papamastorakis, J Pasanen, M Sobrito, G Uemura, M AF Bottcher, M Marscher, AP Ravasio, M Villata, M Raiteri, CM Aller, HD Aller, MF Terasranta, H Mang, O Tagliaferri, G Aharonian, F Krawczynski, H Kurtanidze, OM Nikolashvili, MG Ibrahimov, MA Papadakis, IE Tsinganos, K Sadakane, K Okada, N Takalo, LO Sililanpaa, A Tosti, G Ciprini, S Frasca, A Marilli, E Robb, R Noble, JC Jorstad, SG Hagen-Thorn, VA Larionov, VM Nesci, R Maesano, M Schwartz, RD Basler, J Gorham, PW Iwamatsu, H Kato, T Pullen, C Benitez, E de Diego, JA Moilanen, M Oksanan, A Rodriguez, D Sadun, AC Kelly, M Carini, MT Miller, HR Catalano, S Dultzin-Hacyan, D Fan, JH Ghisellini, G Ishioka, R Karttunen, H Keinanen, P Kudryavtseva, NA Lainela, M Lanteri, L Larionova, EG Matsumoto, K Mattox, JR McHardy, I Montagni, F Nucciarelli, G Ostorero, L Papamastorakis, J Pasanen, M Sobrito, G Uemura, M TI Coordinated multiwavelength observations of BL Lacertae in 2000 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects : individual (BL Lacertae); galaxies : active; gamma rays : theory; radiation mechanisms : nonthermal ID HIGH-ENERGY EMISSION; TEV GAMMA-RAYS; X-RAY; 1997 OUTBURST; SPECTRAL VARIABILITY; BACKGROUND-RADIATION; OBJECT PKS-2155-304; BLAZAR MODEL; JETS; LAC AB BL Lacertae (BL Lac) was the target of an extensive multiwavelength monitoring campaign in the second half of 2000. Simultaneous or quasi-simultaneous observations were taken at radio (University of Michigan Radio Astronomy Observatory and Metsahovi Radio Telescope) and optical ( Whole Earth Blazar Telescope [WEBT] collaboration) frequencies, in X-rays (BeppoSAX and RXTE), and at very high energy gamma rays (HEGRA). The WEBT optical campaign achieved an unprecedented time coverage, virtually continuous over several 10 - 20 hr segments. It revealed intraday variability on timescales of similar to 1.5 hr and evidence for spectral hardening associated with increasing optical flux. During the campaign, BL Lac underwent a major transition from a rather quiescent state prior to 2000 September, to a flaring state for the rest of the year. This was also evident in the X-ray activity of the source. BeppoSAX observations on July 26-27 revealed a rather low X-ray flux and a hard spectrum, while a BeppoSAX pointing on 2000 October 31 - November 2 indicated significant variability on timescales of less than or similar to a few hours and provided evidence for the synchrotron spectrum extending out to similar to 10 keV during that time. During the July 26-27 observation, there is a tantalizing, although not statistically significant, indication of a time delay of similar to 4-5 hr between the BeppoSAX and the R-band light curves. Also, a low-significance detection of a time delay of 15 days between the 14.5 and 22 GHz radio light curves is reported. Several independent methods to estimate the comoving magnetic field in the source are presented, suggesting a value of similar to 2e(B)(2/7) G, where e(B) is the magnetic field equipartition factor with respect to the electron energy density in the jet. C1 Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. Boston Univ, Dept Astron, Boston, MA 02215 USA. Osserv Astron Brera, I-23807 Merate, Italy. Osserv Astron Torino, Ist Nazl Astrofis, I-0025 Pino Torinese, Italy. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Helsinki Univ Technol, Metsahovi Radio Observ, Kylmala 02540, Finland. Univ Kiel, Inst Expt & Angew Phys, D-24118 Kiel, Germany. Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. Washington Univ, Dept Phys, St Louis, MO 63110 USA. Abastumani Observ, GE-383762 Abastumani, Rep of Georgia. Astrophys Inst Potsdam, D-14482 Potsdam, Germany. Landessternwarte Heidelberg Konigstuhl, D-69117 Heidelberg, Germany. Uzbek Acad Sci, Ulugh Beg Astron Inst, Tashkent 700052, Uzbekistan. Isaac Newton Inst Chile, Uzbekistan Branch, Tashkent, Uzbekistan. Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece. Fdn Res & Technol Hellas, IESL, Iraklion 71110, Crete, Greece. Osaka Kyoiku Univ, Astron Inst, Kashiwara, Osaka 5828582, Japan. Tuorla Observ, Piikkio 21500, Finland. Univ Perugia, Osservatorio Astron, I-06126 Perugia, Italy. Osserv Astrofis Catania, I-95125 Catania, Italy. Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 2Y2, Canada. Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. Guangzhou Univ, Ctr Astrophys, Guangzhou 510400, Peoples R China. St Petersburg State Univ, Astron Inst, St Petersburg 198504, Russia. Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. Univ Missouri, Dept Phys & Astron, St Louis, MO 63121 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Kyoto Univ, Fac Sci, Dept Astron, Kyoto, Japan. Clarke & Coyote Astrophys Observ, Wilton, CA 95693 USA. Natl Autonomous Univ Mexico, Inst Astron, Mexico City 04510, DF, Mexico. Nyrola Observ, Jyvaskyla 40950, Finland. Guadarrama Observ, Madrid 28409, Spain. Univ Colorado, Dept Phys, Denver, CO 80217 USA. Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42104 USA. Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. Francis Marion Univ, Dept Chem Phys & Astron, Florence, SC 29501 USA. Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. Univ Turin, Dipartimento Fis Gen, I-10125 Turin, Italy. RP Bottcher, M (reprint author), Ohio Univ, Dept Phys & Astron, Clippinger 339, Athens, OH 45701 USA. RI Hagen-Thorn, Vladimir/H-3983-2013; de Diego, Jose/B-4093-2009; Papadakis, Iossif/C-3235-2011; Papamastorakis, Ioannis/G-7324-2011; Tosti, Gino/E-9976-2013; Larionov, Valeri/H-1349-2013; Larionova, Elena/H-7287-2013; Kudryavtseva, Nadezhda/F-2472-2013; Kurtanidze, Omar/J-6237-2014; Jorstad, Svetlana/H-6913-2013; OI Hagen-Thorn, Vladimir/0000-0002-6431-8590; Villata, Massimo/0000-0003-1743-6946; Ostorero, Luisa/0000-0003-3983-5980; Ghisellini, Gabriele/0000-0002-0037-1974; Larionov, Valeri/0000-0002-4640-4356; Larionova, Elena/0000-0002-2471-6500; Jorstad, Svetlana/0000-0001-9522-5453; Frasca, Antonio/0000-0002-0474-0896; Raiteri, Claudia Maria/0000-0003-1784-2784; Jose A., de Diego/0000-0001-7040-069X; Kudryavtseva, Nadia/0000-0002-1372-0942; Tagliaferri, Gianpiero/0000-0003-0121-0723 NR 53 TC 42 Z9 42 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 OCT 20 PY 2003 VL 596 IS 2 BP 847 EP 859 DI 10.1086/378156 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 731ZH UT WOS:000185916000011 ER PT J AU Harrison, FA Eckart, ME Mao, PH Helfand, DJ Stern, D AF Harrison, FA Eckart, ME Mao, PH Helfand, DJ Stern, D TI The Serendipitous Extragalactic X-Ray Source Identification program. I. Characteristics of the hard X-ray sample SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; surveys; X-rays : galaxies; X-rays : general ID DEEP FIELD-SOUTH; LARGE-AREA SURVEY; NUMBER COUNTS; IMAGING SPECTROMETER; SPECTRAL PROPERTIES; EXPOSURE; CATALOG; GALAXY; AXAF; SKY AB The Serendipitous Extragalactic X-Ray Source Identification (SEXSI) program is designed to extend greatly the sample of identified extragalactic hard X-ray (2 - 10 keV) sources at intermediate fluxes (similar to10(-13) to 10(-15) ergs cm(-2) s(-1)). SEXSI, which studies sources selected from more than 2 deg(2), provides an essential complement to the Chandra Deep Fields, which reach depths of 5 x 10(-16) ergs cm(-2) s(-1) (2 - 10 keV) but over a total area of less than 0.2 deg(2). In this paper we describe the characteristics of the survey and our X-ray data analysis methodology. We present the cumulative flux distribution for the X-ray sample of 1034 hard sources and discuss the distribution of spectral hardness ratios. Our log N-log S in this intermediate flux range connects to those found in the Deep Fields, and by combining the data sets, we constrain the hard X-ray population over the flux range in which the differential number counts change slope and from which the bulk of the 2 - 10 keV X-ray background arises. We further investigate the log N-log S distribution separately for soft and hard sources in our sample, finding that while a clear change in slope is seen for the softer sample, the hardest sources are well described by a single power law down to the faintest fluxes, consistent with the notion that they lie at lower average redshift. C1 CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. Columbia Univ, Dept Astron, New York, NY 10027 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Harrison, FA (reprint author), CALTECH, Space Radiat Lab, MS 220-47, Pasadena, CA 91125 USA. NR 27 TC 49 Z9 49 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 OCT 20 PY 2003 VL 596 IS 2 BP 944 EP 956 DI 10.1086/378087 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 731ZH UT WOS:000185916000017 ER EF