FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Zak, M Fijany, A AF Zak, M Fijany, A TI Quantum resonance for simulating combinatorial problems SO PHYSICS LETTERS A LA English DT Article AB Quantum computing by simulations is based upon similarity between mathematical formalism of a quantum phenomenon and phenomena to be analyzed. In this Letter, the mathematical formalism of quantum resonance combined with tensor product decomposability of unitary evolutions is mapped onto a class of NP-complete combinatorial problems. It has been demonstrated that nature has polynomial resources for solving NP-complete problems and that will help to develop a new strategy for artificial intelligence, as well as to re-evaluate the role of natural selection in biological evolution. (c) 2005 Elsevier B.V. All rights reserved. C1 CALTECH, Jet Prop Lab, Adv Comp Algorithms & ISHM Grp, Pasadena, CA 91109 USA. RP Zak, M (reprint author), CALTECH, Jet Prop Lab, Adv Comp Algorithms & ISHM Grp, Mail Stop 126-347, Pasadena, CA 91109 USA. EM michail.zak@jpl.nasa.gov NR 10 TC 4 Z9 4 U1 0 U2 1 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 SEP 26 PY 2005 VL 345 IS 1-3 BP 167 EP 172 DI 10.1016/j.physleta.2005.07.012 PG 6 WC Physics, Multidisciplinary SC Physics GA 967CY UT WOS:000232070300020 ER PT J AU Berdichevsky, DB Richardson, IG Lepping, RP Martin, SF AF Berdichevsky, DB Richardson, IG Lepping, RP Martin, SF TI On the origin and configuration of the 20 March 2003 interplanetary shock and magnetic cloud at 1 AU SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID CORONAL MASS EJECTIONS; 23RD SOLAR MINIMUM; WIND; HELIUM; TEMPERATURE; PARTICLES; HELICITY; EVENTS AB On 20 March 2003, a forward shock was observed in the near-Earth solar wind, followed 8 hours later by an interplanetary magnetic cloud (IMC), in a configuration having several uncommon features: Both were parts of a 38-hour interval containing transient solar outflows that occurred in an extended high-speed stream from a Y-shaped extension of the south polar coronal hole. (In contrast, IMCs, and ejecta in general, were rarely observed within high-speed streams at low heliolatitudes during cycle 23.) The most likely solar source for the IMC is AR 10314, located at S15 degrees, just above the "fork" of the Y-shaped coronal hole. Several solar flares occurred in this active region on 17-18 March, as well as a succession of four coronal mass ejections (CMEs). Velocity considerations narrow the most likely source of the 38-hour interval of activity to two CMEs on 17 March 2003 associated with solar flares at W33 degrees and W39 degrees. The IMC axis had a north-south orientation, which is unusual for IMCs during this solar cycle. Its left-handedness implies an association with a left-skewed coronal arcade, which is less common in the Southern Hemisphere. Considering the shock observed ahead of the IMC, we conclude based on orientation and ram pressure arguments that this shock was not driven by the IMC, as might be presumed, but was the flank of an unrelated shock that overtook the IMC approximately halfway between Sun and Earth, heating the plasma and accelerating particles within the IMC. The CME associated with the X-class flare, at 1208 UT on 18 March in AR 10314 appears to be the solar source for this shock. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Helio Res, La Crescenta, CA 91214 USA. RP Berdichevsky, DB (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 690, Greenbelt, MD 20771 USA. EM dberdich@pop600.gsfc.nasa.gov OI Richardson, Ian/0000-0002-3855-3634 NR 41 TC 12 Z9 12 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 SEP 23 PY 2005 VL 110 IS A9 AR A09105 DI 10.1029/2004JA010662 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 968SP UT WOS:000232182900001 ER PT J AU Stone, EC Cummings, AC McDonald, FB Heikkila, BC Lal, N Webber, WR AF Stone, EC Cummings, AC McDonald, FB Heikkila, BC Lal, N Webber, WR TI Voyager 1 explores the termination shock region and the heliosheath beyond SO SCIENCE LA English DT Article ID ANOMALOUS COSMIC-RAYS; INTERSTELLAR MAGNETIC-FIELD; ENERGETIC PARTICLES; SOLAR-WIND; ACCELERATION; HELIOSPHERE; IONS AB Voyager 1 crossed the termination shock of the supersonic flow of the solar wind on 16 December 2004 at a distance of 94.01 astronomical units from the Sun, becoming the first spacecraft to begin exploring the heliosheath, the outermost layer of the heliosphere. The shock is a steady source of low-energy protons with an energy spectrum similar to E-1.41 +/- 0.15 from 0.5 to similar to 3.5 megaelectron volts, consistent with a weak termination shock having a solar wind velocity jump ratio r = 2.6(-0.2)(+0.4). However, in contradiction to many predictions, the intensity of anomalous cosmic ray (ACR) helium did not peak at the shock, indicating that the ACR source is not in the shock region local to Voyager 1. The intensities of similar to 10-megaelectron volt electrons, ACRs, and galactic cosmic rays have steadily increased since late 2004 as the effects of solar modulation have decreased. C1 CALTECH, Pasadena, CA 91125 USA. Univ Maryland, Inst Phys Sci & Technol, College Pk, MD 20742 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. New Mexico State Univ, Dept Phys & Astron, Las Cruces, NM 88003 USA. RP Stone, EC (reprint author), CALTECH, Pasadena, CA 91125 USA. EM ecs@srl.caltech.edu NR 21 TC 391 Z9 392 U1 2 U2 4 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD SEP 23 PY 2005 VL 309 IS 5743 BP 2017 EP 2020 DI 10.1126/science.1117684 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 968SF UT WOS:000232181900038 PM 16179468 ER PT J AU Burlaga, LF Ness, NF Acuna, IH Acuna, MH Lepping, RP Connerney, JEP Stone, EC McDonald, FB AF Burlaga, LF Ness, NF Acuna, IH Acuna, MH Lepping, RP Connerney, JEP Stone, EC McDonald, FB TI Crossing the termination shock into the hetiosheath: Magnetic fields SO SCIENCE LA English DT Article ID SOLAR-WIND; INTERSTELLAR-MEDIUM; VOYAGER-1; PICKUP; AU; HELIOSPHERE; MOTION; SPEED; MODEL AB Magnetic fields measured by Voyager 1 show that the spacecraft crossed or was crossed by the termination shock on about 16 December 2004 at 94.0 astronomical units. An estimate of the compression ratio of the magnetic field strength B (+/- standard error of the mean) across the shock is B-2/B-1 = 3.05 +/- 0.04, but ratios in the range from 2 to 4 are admissible. The average B in the heliosheath from day 1 through day 110 of 2005 was 0.136 +/- 0.035 nanoteslas, similar to 4.2 times that predicted by Parker's model for B. The magnetic field in the heliosheath from day 361 of 2004 through day 110 of 2005 was pointing away from the Sun along the Parker spiral. The probability distribution of hourly averages of B in the heliosheath is a Gaussian distribution. The cosmic ray intensity increased when B was relatively large in the hetiosheath. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Catholic Univ Amer, Washington, DC 20064 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 30 TC 198 Z9 200 U1 0 U2 5 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD SEP 23 PY 2005 VL 309 IS 5743 BP 2027 EP 2029 DI 10.1126/science.1117542 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 968SF UT WOS:000232181900041 PM 16179471 ER PT J AU Andersen, OB Seneviratne, SI Hinderer, J Viterbo, P AF Andersen, OB Seneviratne, SI Hinderer, J Viterbo, P TI GRACE-derived terrestrial water storage depletion associated with the 2003 European heat wave SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SUPERCONDUCTING GRAVIMETERS; CLIMATE EXPERIMENT; GRAVITY RECOVERY; VARIABILITY; SYSTEM AB The GRACE twin satellites reveal large inter-annual terrestrial water-storage variations between 2002 and 2003 for central Europe. GRACE observes a negative trend in regional water storage from 2002 to 2003 peaking at -7.8 cm in central Europe with an accuracy of 1 cm. The 2003 excess terrestrial water storage depletion observed from GRACE can be related to the record-breaking heat wave that occurred in central Europe in 2003. We validate the measurements from GRACE using two independent hydrological estimates and direct gravity observations from superconducting gravimeters in Europe. All datasets agree well with the GRACE measurements despite the disparity of the employed information; the difference between datasets tends to be within GRACE margin of error. The April-to-August terrestrial water storage depletion is found to be significantly larger in 2003 than in 2002 from both models and observations. C1 Danish Natl Space Ctr, DK-2100 Copenhagen, Denmark. NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. Ecole & Observ Sci Terre, Inst Phys Globe Strasbourg, F-67084 Strasbourg, France. European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England. RP Andersen, OB (reprint author), Danish Natl Space Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark. EM oa@spacecenter.dk RI Viterbo, Pedro/B-7184-2008; Seneviratne, Sonia/G-8761-2011; Andersen, Ole /H-7481-2016 OI Viterbo, Pedro/0000-0001-6587-3062; Seneviratne, Sonia/0000-0001-9528-2917; Andersen, Ole /0000-0002-6685-3415 NR 22 TC 66 Z9 70 U1 0 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 22 PY 2005 VL 32 IS 18 AR L18405 DI 10.1029/2005GL023574 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 968QN UT WOS:000232177300003 ER PT J AU Anderson, TL Wu, YH Chu, DA Schmid, B Redemann, J Dubovik, O AF Anderson, TL Wu, YH Chu, DA Schmid, B Redemann, J Dubovik, O TI Testing the MODIS satellite retrieval of aerosol fine-mode fraction SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID AIRBORNE SUN PHOTOMETER; PULSED CAVITY RING; OPTICAL-PROPERTIES; ACE-ASIA; WATER-VAPOR; PASSING EFFICIENCY; SIZE DISTRIBUTION; COLUMN CLOSURE; NCAR C-130; IN-SITU AB Satellite retrievals of the fine-mode fraction (FMF) of midvisible aerosol optical depth, tau, are potentially valuable for constraining chemical transport models and for assessing the global distribution of anthropogenic aerosols. Here we compare satellite retrievals of FMF from the Moderate Resolution Imaging Spectroradiometer (MODIS) to suborbital data on the submicrometer fraction (SMF) of tau. SMF is a closely related parameter that is directly measurable by in situ techniques. The primary suborbital method uses in situ profiling of SMF combined with airborne Sun photometry both to validate the in situ estimate of ambient extinction and to take into account the aerosol above the highest flight level. This method is independent of the satellite retrieval and has well-known accuracy but entails considerable logistical and technical difficulties. An alternate method uses Sun photometer measurements near the surface and an empirical relation between SMF and the angstrom ngstrorm exponent, (a) over circle, a measure of the wavelength dependence of optical depth or extinction. Eleven primary and fifteen alternate comparisons are examined involving varying mixtures of dust, sea salt, and pollution in the vicinity of Korea and Japan. MODIS ocean retrievals of FMF are shown to be systematically higher than suborbital estimates of SMF by about 0.2. The most significant cause of this discrepancy involves the relationship between (a) over circle and fine-mode partitioning; in situ measurements indicate a systematically different relationship from what is assumed in the satellite retrievals. Based on these findings, we recommend: (1) satellite programs should concentrate on retrieving and validating (a) over circle since an excellent validation program is in place for doing this, and (2) suborbital measurements should be used to derive relationships between a and fine-mode partitioning to allow interpretation of the satellite data in terms of fine-mode aerosol optical depth. C1 Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Terr Phys Lab, Greenbelt, MD 20771 USA. Bay Area Environm Res Inst, Sonoma, CA 95476 USA. Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21201 USA. Univ Maryland, Goddard Earth Sci & Technol Ctr, Greenbelt, MD USA. RP Univ Washington, Dept Atmospher Sci, Room 408 ATG,Box 351640, Seattle, WA 98195 USA. EM tadand@u.washington.edu RI Dubovik, Oleg/A-8235-2009 OI Dubovik, Oleg/0000-0003-3482-6460 NR 42 TC 37 Z9 37 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP 22 PY 2005 VL 110 IS D18 AR D18204 DI 10.1029/2005JD005978 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 968RE UT WOS:000232179000003 ER PT J AU Edlund, JA Tinto, M Krolak, A Nelemans, G AF Edlund, JA Tinto, M Krolak, A Nelemans, G TI Simulation of the white dwarf-white dwarf galactic background in the LISA data SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article; Proceedings Paper CT 9th Gravitational Wave Data Analysis Workshop CY DEC 15-18, 2004 CL Annecy, FRANCE SP Lab Annecy Vieux Phys Particules, European Gravitat Observat, Univ Savoie, Grp Rech, Phenomenes Cosmiques Haute Energ, Inst Natl Phys Nucl Phys Particules, Conseil Gen Haute Savoie, Conseil Reg Rhone Alpes, Assemblee Pays Savoie ID TIME-DELAY INTERFEROMETRY; GRAVITATIONAL-RADIATION; BINARIES AB Laser Interferometer Space Antenna (LISA) is a proposed mission to detect and study gravitational radiation in the frequency range from 10(-4) to 10(-1) Hz. In the low part of its frequency band, the LISA data will contain a stochastic signal consisting of an incoherent superposition of hundreds of millions of gravitational wave signals radiated by inspiraling white-dwarf binaries present in our own galaxy. In order to estimate the LISA response to this background, we have simulated a population of white-dwarf binaries recently synthesized by one of us. Our approach relies on an analytic expressions of the LISA Time-Delay Interferometric responses to the gravitational radiation emitted by such systems, and it allows us to implement a computationally efficient and accurate simulation of the background in the LISA data. We find the amplitude of the galactic white-dwarf binary background in the LISA data to be modulated in time with a period of 1 year, reaching a minimum equal to about twice that of the LISA noise for a period of about 2 months around the time when the Sun-LISA direction is roughly oriented towards the Autumn equinox. This modulation means that the galactic white-dwarf background that will be observable by LISA is a cyclostationary random process with a period of I year. We summarize the theory of cyclostationary random processes and present the corresponding generalized spectral method needed to characterize such a process in the LISA data. We find that, by measuring the generalized spectral components of the white-dwarf background, LISA will be able to inferproperties of the distribution of the white-dwarf binary systems present in our galaxy. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany. Radboud Univ Nijmegen, IMAPP, Dept Astrophys, Nijmegen, Netherlands. RP Edlund, JA (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM Massimo.Tinto@jpl.nasa.gov RI Nelemans, Gijs/D-3177-2012 OI Nelemans, Gijs/0000-0002-0752-2974 NR 20 TC 4 Z9 4 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD SEP 21 PY 2005 VL 22 IS 18 SI SI BP S913 EP S926 DI 10.1088/0264-9381/22/18/S05 PG 14 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 970QX UT WOS:000232325800006 ER PT J AU Haghighipour, N AF Haghighipour, N TI Growth and sedimentation of dust particles in the vicinity of local pressure enhancements in a solar nebula SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE planetary systems : formation; planetary systems : protoplanetary discs ID GIANT PLANET FORMATION; TURBULENT PROTOPLANETARY DISKS; GRAVITATIONAL-INSTABILITY; ICY PLANETESIMALS; GLOBAL EVOLUTION; RAPID MIGRATION; SURFACE-ENERGY; SOLID MATTER; COAGULATION; CONTACT AB A planet-forming nebula is a dynamic environment whose properties and structure vary with time. At the early stage of planet fort-nation, when small grains coagulate to form larger objects, the dynamics of such an environment and its time-varying structure have considerable effects on that process. Among such structures, regions where the pressure of the gas is locally enhanced are of particular interest. In the vicinity of these regions, the combined effect of gas drag and pressure gradients, which in a nebula with a monotonic pressure gradient creates gas drag-induced migration of solids towards the central star causes solid particles to migrate inward/outward, and accumulate at the location of the pressure-enhanced region. While migrating, solid particles sweep up smaller objects and grow in size. In this paper, the effects of the appearance of pressure-enhanced structures on the growth and sedimentation of micron-sized particles are studied, and the effects of gas drag and pressure gradients on the rate of accumulation of centimetre-sized objects in the regions of local maximum pressure on the midplane are discussed. To portray a more detailed picture of the dynamical influence of such structures on the motions and interactions of particles, comparisons are made with the results of similar studies in a nebula without pressure-enhanced structures, and the cases, in which the changes in the physical properties of the gas and particles will enhance the growth rates of solids, are discussed. A discussion is also presented on the inelastic collision of dust particles and the corrections to the formulae of sticking velocity that currently exist in the literature. C1 Univ Hawaii Manoa, Inst Astron, Honolulu, HI USA. Univ Hawaii Manoa, NASA, Astrobiol Inst, Honolulu, HI USA. RP Haghighipour, N (reprint author), Univ Hawaii Manoa, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI USA. EM nader@ifa.hawaii.edu NR 48 TC 8 Z9 8 U1 0 U2 3 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 21 PY 2005 VL 362 IS 3 BP 1015 EP 1024 DI 10.1111/j.1365-2966.2005.09362.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 968JH UT WOS:000232158300027 ER PT J AU Stern, D Eisenhardt, P Gorjian, V Kochanek, CS Caldwell, N Eisenstein, D Brodwin, M Brown, MJI Cool, R Dey, A Green, P Jannuzi, BT Murray, SS Pahre, MA Willner, SP AF Stern, D Eisenhardt, P Gorjian, V Kochanek, CS Caldwell, N Eisenstein, D Brodwin, M Brown, MJI Cool, R Dey, A Green, P Jannuzi, BT Murray, SS Pahre, MA Willner, SP TI Mid-infrared selection of active galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : formation ID SPITZER-SPACE-TELESCOPE; DIGITAL SKY SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; ARRAY CAMERA IRAC; X-RAY; GALACTIC NUCLEI; REDSHIFT SURVEY; QUASARS; CHANDRA; POPULATION AB Mid-infrared photometry provides a robust technique for identifying active galaxies. While the ultraviolet to mid-infrared (lambda less than or similar to 5 mu m) continuum of stellar populations is dominated by the composite blackbody curve and peaks at approximately 1.6 mu m, the ultraviolet to mid-infrared continuum of active galactic nuclei (AGNs) is dominated by a power law. Consequently, with a sufficient wavelength baseline, one can easily distinguish AGNs from stellar populations. Mirroring the tendency of AGNs to be bluer than galaxies in the ultraviolet, where galaxies (and stars) sample the blue, rising portion of stellar spectra, AGNs tend to be redder than galaxies in the mid-infrared, where galaxies sample the red, falling portion of the stellar spectra. We report on Spitzer Space Telescope mid-infrared colors, derived from the IRAC Shallow Survey, of nearly 10,000 spectroscopically identified sources from the AGN and Galaxy Evolution Survey. On the basis of this spectroscopic sample, we find that simple mid-infrared color criteria provide remarkably robust separation of active galaxies from normal galaxies and Galactic stars, with over 80% completeness and less than 20% contamination. Considering only broad-lined AGNs, these mid-infrared color criteria identify over 90% of spectroscopically identified quasars and Seyfert 1 galaxies. Applying these color criteria to the full imaging data set, we discuss the implied surface density of AGNs and find evidence for a large population of optically obscured active galaxies. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Princeton Univ Observ, Princeton, NJ 08544 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. RP Stern, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM stern@zwolfkinder.jpl.nasa.gov RI Brown, Michael/B-1181-2015; Barmby, Pauline/I-7194-2016 OI Brown, Michael/0000-0002-1207-9137; Barmby, Pauline/0000-0003-2767-0090 NR 36 TC 539 Z9 539 U1 2 U2 8 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2005 VL 631 IS 1 BP 163 EP 168 DI 10.1086/432523 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 965OD UT WOS:000231959100010 ER PT J AU Bender, R Kormendy, J Bower, G Green, R Thomas, J Danks, AC Gull, T Hutchings, JB Joseph, CL Kaiser, ME Lauer, TR Nelson, CH Richstone, D Weistrop, D Woodgate, B AF Bender, R Kormendy, J Bower, G Green, R Thomas, J Danks, AC Gull, T Hutchings, JB Joseph, CL Kaiser, ME Lauer, TR Nelson, CH Richstone, D Weistrop, D Woodgate, B TI HST STIS spectroscopy of the triple nucleus of M31: Two nested disks in keplerian rotation around a supermassive black hole SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies : individual (M31); galaxies : nuclei ID AXISYMMETRICAL DYNAMICAL MODELS; EARLY-TYPE GALAXIES; DA WHITE-DWARFS; GALACTIC-CENTER; STELLAR DYNAMICS; VELOCITY DISPERSION; MASS-DISTRIBUTION; CENTRAL REGIONS; STAR-FORMATION; CENTERS AB We present Hubble Space Telescope (HST) spectroscopy of the nucleus of M31 obtained with the Space Telescope Imaging Spectrograph (STIS). Spectra that include the Ca II infrared triplet (lambda similar or equal to 8500 angstrom) see only the red giant stars in the double brightness peaks P1 and P2. In contrast, spectra taken at lambda similar or equal to 3600 - 5100 angstrom are sensitive to the tiny blue nucleus embedded in P2, the lower surface brightness nucleus of the galaxy. P2 has a K-type spectrum, but we find that the blue nucleus has an A- type spectrum: it shows strong Balmer absorption lines. Hence, the blue nucleus is blue not because of AGN light but rather because it is dominated by hot stars. We show that the spectrum is well described by A0 giant stars, A0 dwarf stars, or a 200 Myr old, single-burst stellar population. White dwarfs, in contrast, cannot fit the blue nucleus spectrum. Given the small likelihood for stellar collisions, recent star formation appears to be the most plausible origin of the blue nucleus. In stellar population, size, and velocity dispersion, the blue nucleus is so different from P1 and P2 that we call it P3 and refer to the nucleus of M31 as triple. Because P2 and P3 have very different spectra, we can make a clean decomposition of the red and blue stars and hence measure the light distribution and kinematics of each uncontaminated by the other. The line-of-sight velocity distributions of the red stars near P2 strengthen the support for Tremaine's eccentric disk model. Their wings indicate the presence of stars with velocities of up to 1000 km s(-1) on the anti-P1 side of P2. The kinematics of P3 are consistent with a circular stellar disk in Keplerian rotation around a supermassive black hole. If the P3 disk is perfectly thin, then the inclination angle i similar or equal to 55 degrees is identical within the errors to the inclination of the eccentric disk models for P1+ P2 by Peiris & Tremaine and by Salow & Statler. Both disks rotate in the same sense and are almost coplanar. The observed velocity dispersion of P3 is largely caused by blurred rotation and has a maximum value of sigma 1183 +/- 201 km s(-1) . This is much larger than the dispersion sigma similar or equal to 250 km s(-1) of the red stars along the same line of sight and is the largest integrated velocity dispersion observed in any galaxy. The rotation curve of P3 is symmetric around its center. It reaches an observed velocity of V 618 +/- 81 km s(-1) at radius 0''.05 0.19 pc, where the observed velocity dispersion is sigma 674 +/- 95 km s(-1). The corresponding circular rotation velocity at this radius is similar to 1700 km s(-1). We therefore confirm earlier suggestions that the central dark object interpreted as a supermassive black hole is located in P3. Thin-disk and Schwarzschild models with intrinsic axial ratios b/a less than or similar to 0.26 corresponding to inclinations between 55 degrees and 58 degrees match the P3 observations very well. Among these models, the best fit and the lowest black hole mass are obtained for a thin- disk model with M center dot = 1.4 x 10(8) M circle dot. Allowing P3 to have some intrinsic thickness and considering possible systematic errors, the 1 sigma confidence range becomes (1.1- 2.3) x 10(8) M circle dot. The black hole mass determined from P3 is independent of but consistent with Peiris & Tremaine's mass estimate based on the eccentric disk model for P1+ P2. It is similar to 2 times larger than the prediction by the correlation between M. and bulge velocity dispersion sigma bulge. Taken together with other reliable black hole mass determinations in nearby galaxies, notably the Milky Way and M32, this strengthens the evidence that the M center dot-sigma bulge relation has significant intrinsic scatter, at least at low black hole masses. We show that any dark star cluster alternative to a black hole must have a half- mass radius less than or similar to 0''.03 = 0.11 pc in order to match the observations. Based on this, M31 becomes the third galaxy (after NGC 4258 and our Galaxy) in which clusters of brown dwarf stars or dead stars can be excluded on astrophysical grounds. C1 Univ Sternwarte, D-81679 Munich, Germany. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Univ Texas, Dept Astron, Austin, TX 78712 USA. Space Telescope Sci Inst, Comp Sci Corp, Baltimore, MD 21218 USA. Natl Opt Astron Observ, Tucson, AZ 85726 USA. Emergent IT, Bowie, MD 20721 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08855 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Bender, R (reprint author), Univ Sternwarte, Scheinerstr 1, D-81679 Munich, Germany. EM bender@usm.uni-muenchen.de; kormendy@astro.as.utexas.edu; bower@stsci.edu; green@noao.edu; jthomas@usm.uni-muenchen.de; danks@yahoo.com; gull@sea.gsfc.nasa.gov; john.hutchings@hia.nrc.ca; cjoseph@physics.rutgers.edu; kaiser@pha.jhu.edu; lauer@noao.edu; cnelson@physics.unlv.edu; dor@umich.edu; weistrop@physics.unlv.edu; woodgate@stars.gsfc.nasa.gov RI Gull, Theodore/D-2753-2012; OI Gull, Theodore/0000-0002-6851-5380; Weistrop, Donna/0000-0001-8935-0792 NR 86 TC 132 Z9 132 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2005 VL 631 IS 1 BP 280 EP 300 DI 10.1086/432434 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 965OD UT WOS:000231959100019 ER PT J AU Beckmann, V Kennea, JA Markwardt, C Paizis, A Soldi, S Rodriguez, J Barthelmy, SD Burrows, DN Chester, M Gehrels, N Mowlavi, N Nousek, J AF Beckmann, V Kennea, JA Markwardt, C Paizis, A Soldi, S Rodriguez, J Barthelmy, SD Burrows, DN Chester, M Gehrels, N Mowlavi, N Nousek, J TI Swift, INTEGRAL, RXTE, and SPITZER reveal IGR J16283-4838 SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : observations; stars : neutron; X-rays : binaries; X-rays : individual (IGR J16283-4838) ID BACKGROUND-RADIATION; SEYFERT-1 GALAXY; IGR J16318-4848; SPACE-TELESCOPE; GALACTIC-CENTER; RAY-EMISSION; XMM-NEWTON; MISSION; J16358-4726 AB We present the first combined study of the recently discovered source IGR J16283-4838 with Swift, INTEGRAL, and RXTE. The source, discovered by INTEGRAL on 2005 April 7, shows a highly absorbed [variable N-H = 0.4-1.7 x 10(23) cm(-2)] and flat (Gamma similar to 1) spectrum in the Swift XRT and RXTE PCA data. No optical counterpart is detectable (V > 20 mag), but a possible infrared counterpart within the Swift XRT error radius is detected in the 2MASS and Spitzer GLIMPSE. The observations suggest that IGR J16283-4838 is a high-mass X-ray binary (HMXB) containing a neutron star embedded in Compton thick material. This makes IGR J16283-4838 a member of the class of highly absorbed HMXBs, discovered by INTEGRAL. C1 Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. Univ Maryland Baltimore Cty, Dept Phys, Joint Ctr Astrophys, Baltimore, MD 21250 USA. NASA, Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. CNR, Ist Astrofis Spaziale Fis & Cosm, Sez Milano, I-20133 Milan, Italy. DSM, DAPNIA, SAp, CNRS,UMR 7158,AIM,CES, F-91191 Gif Sur Yvette, France. Observ Geneva, CH-1290 Sauverny, Switzerland. RP Beckmann, V (reprint author), Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. EM beckmann@milkyway.gsfc.nasa.gov RI Gehrels, Neil/D-2971-2012; Barthelmy, Scott/D-2943-2012; OI Rodriguez, Jerome/0000-0002-4151-4468; Paizis, Adamantia/0000-0001-5067-0377 NR 40 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 SEP 20 PY 2005 VL 631 IS 1 BP 506 EP 510 DI 10.1086/432600 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 965OD UT WOS:000231959100039 ER PT J AU Cliver, EW Laurenza, M Storini, M Thompson, BJ AF Cliver, EW Laurenza, M Storini, M Thompson, BJ TI On the origins of solar EIT waves SO ASTROPHYSICAL JOURNAL LA English DT Article DE sun : corona; sun : coronal mass ejections (CMEs); sun : flares ID CORONAL MASS EJECTION; WIND SPACECRAFT DATA; GOPALSWAMY,N. ET-AL; II RADIO-BURSTS; FLARE WAVES; INTERPLANETARY SHOCKS; SOHO/EIT OBSERVATIONS; LASCO OBSERVATIONS; MORETON WAVES; CMES AB Approximately half of the large-scale coronal waves identified in images obtained by the Extreme-Ultraviolet Imaging Telescope (EIT) on the Solar and Heliospheric Observatory from 1997 March to 1998 June were associated with small solar flares with soft X-ray intensities below C class. The probability of a given flare of this intensity having an associated EIT wave is low. For example, of similar to 8,000 B-class flares occurring during this 15 month period, only similar to 1% were linked to EIT waves. These results indicate the need for a special condition that distinguishes flares with EIT waves from the vast majority of flares that lack wave association. Various lines of evidence, including the fact that EIT waves have recently been shown to be highly associated with coronal mass ejections (CMEs), suggest that this special condition is a CME. A CME is not a sufficient condition for a detectable EIT wave, however, because we calculate that similar to 5 times as many front-side CMEs as EIT waves occurred during this period, after taking the various visibility factors for both phenomena into account. In general, EIT wave association increases with CME speed and width. C1 USAF, Res Lab, Space Vehicles Directorate, Hanscom AFB, MA 01731 USA. INAF, Ist Fis Spazio Interplanetario, I-00133 Rome, Italy. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Cliver, EW (reprint author), USAF, Res Lab, Space Vehicles Directorate, Hanscom AFB, MA 01731 USA. RI Thompson, Barbara/C-9429-2012 NR 64 TC 62 Z9 64 U1 1 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2005 VL 631 IS 1 BP 604 EP 611 DI 10.1086/432250 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 965OD UT WOS:000231959100047 ER PT J AU McAteer, RTJ Gallagher, PT Ireland, J AF McAteer, RTJ Gallagher, PT Ireland, J TI Statistics of active region complexity: A large-scale fractal dimension survey SO ASTROPHYSICAL JOURNAL LA English DT Article DE sun : activity; sun : flares; sun : magnetic fields ID PHOTOSPHERIC MAGNETIC-FIELD; MICHELSON DOPPLER IMAGER; PERCOLATION THEORY; SOLAR GRANULATION; FLARES; FLUX; SUN; DEPENDENCE; DIFFUSION; POLARITY AB A quantification of the magnetic complexity of active regions using a fractal dimension measure is presented. This fully automated approach uses full-disk MDI magnetograms of active regions from a large data set ( 2742 days of the SOHO mission, 9342 active region images) to compare the calculated fractal dimension of each region to both its Mount Wilson classification and flare rate. Each Mount Wilson class exhibits a similar fractal dimension frequency distribution, possibly suggesting a self-similar nature of all active regions. Solar flare productivity exhibits an increase in both the frequency and GOES X-ray magnitude of flares from regions with higher fractal dimension. Specifically, a lower threshold fractal dimension of 1.2 and 1.25 exists as a necessary, but not sufficient, requirement for an active region to produce M- and X-class flares, respectively, within 24 hr of the observation. C1 NASA, Goddard Space Flight Ctr, L3 Commun GSI, Greenbelt, MD 20771 USA. Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. RP McAteer, RTJ (reprint author), NASA, Goddard Space Flight Ctr, L3 Commun GSI, Greenbelt, MD 20771 USA. EM j.mcateer@grasshopper.gsfc.nasa.gov RI McAteer, R. T. James/D-3736-2011; Gallagher, Peter/C-7717-2011 OI Gallagher, Peter/0000-0001-9745-0400 NR 44 TC 59 Z9 60 U1 1 U2 6 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2005 VL 631 IS 1 BP 628 EP 635 DI 10.1086/432412 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 965OD UT WOS:000231959100050 ER PT J AU Khan, SA Shafer, RA Benford, DJ Staguhn, JG Chanial, P Le Floc'h, E Babbedge, TSR Farrah, D Moseley, SH Dwek, E Clements, DL Sumner, TJ Ashby, MLN Brand, K Brodwin, M Eisenhardt, PR Elston, R Gonzalez, AH McKenzie, E Murray, SS AF Khan, SA Shafer, RA Benford, DJ Staguhn, JG Chanial, P Le Floc'h, E Babbedge, TSR Farrah, D Moseley, SH Dwek, E Clements, DL Sumner, TJ Ashby, MLN Brand, K Brodwin, M Eisenhardt, PR Elston, R Gonzalez, AH McKenzie, E Murray, SS TI On the discovery of the first galaxy selected at 350 microns SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : high-redshift; galaxies : starburst; infrared : galaxies; submillimeter ID DEEP SUBMILLIMETER SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; STAR-FORMATION HISTORY; HIGH-REDSHIFT GALAXIES; EXTREMELY RED OBJECTS; STELLAR MASS DENSITY; LUMINOSITY DENSITY; INFRARED GALAXIES; SHARC-II; FIELD AB We report the detection of a 3.6 sigma source selected at 350 mm in the Bootes Deep Field. The source, the first short-wavelength submillimeter-selected galaxy (SSG1), was discovered as part of a blank-field extragalactic survey using the 350 mu m-optimized Submillimeter High Angular Resolution Camera (SHARC II) at the Caltech Submillimeter Observatory. With multiwavelength photometry from the NOAO Deep Wide-Field Survey (R and I band), FLAMEX (J and K-s), Spitzer (IRAC and MIPS), and the Westerbork 1.4 GHz deep survey (radio upper limit), we are able to constrain the photometric redshift using different methods, all of which suggest a redshift of similar to 1. In the absence of long-wavelength submillimeter data, we use SED templates to infer that this source is an ultraluminous infrared galaxy with a dust temperature of 30 +/- 5 K, occupying a region of luminosity-temperature space shared by moderate-redshift ISO-selected ULIRGs (rather than high-redshift SCUBA-selected submillimeter galaxies). SHARC II can thus select galaxies with moderately "warm" dust that might be missed in submillimeter surveys at longer wavelengths. C1 Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. Sci Syst & Applicat Inc, Lanham, MD 20706 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Florida, Dept Astron, Gainesville, FL 32611 USA. RP Khan, SA (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, Prince Consort Rd, London SW7 2AZ, England. RI Benford, Dominic/D-4760-2012 OI Benford, Dominic/0000-0002-9884-4206 NR 49 TC 6 Z9 6 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 SEP 20 PY 2005 VL 631 IS 1 BP L9 EP L12 DI 10.1086/497111 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 965OG UT WOS:000231959400003 ER PT J AU Wang, JX Wang, TG Tozzi, P Giacconi, R Hasinger, G Kewley, L Mainieri, V Nonino, M Norman, C Streblyanska, A Szokoly, G Yaqoob, T Zirm, A AF Wang, JX Wang, TG Tozzi, P Giacconi, R Hasinger, G Kewley, L Mainieri, V Nonino, M Norman, C Streblyanska, A Szokoly, G Yaqoob, T Zirm, A TI Relativistic outflow in CXOCDFS J033260.0-274748 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; quasars : individual (CXOCDFS J033260.0-274748); X-rays : galaxies ID DEEP FIELD-SOUTH; LIKELIHOOD RATIO; SOURCE CATALOGS; ACCRETION DISK; EMISSION-LINE; NORTH SURVEY; X-RAYS; GALAXY AB In this Letter we report the detection of a strong and extremely blueshifted X-ray absorption feature in the 1 Ms Chandra spectrum of CXOCDFS J033260.0-274748, a quasar at z = 2.579 with L2-10 keV similar to 4 x 10(44) ergs s(-1). The broad absorption feature at similar to 6.3 keV in the observed frame can be fitted either as an absorption edge at 20.9 keV or as a broad absorption line at 22.2 keV rest frame. The absorber has to be extremely ionized with an ionization parameter xi similar to 10(4) and a high column density, NH > 5 x 10(23) cm(-2). We reject the possibility of a statistical or instrumental artifact. The most likely interpretation is an extremely blueshifted broad absorption line or absorption edge, due to H or He-like iron in a relativistic jetlike outflow with bulk velocity of similar to 0.7c-0.8c. Similar relativistic outflows have been reported in the X-ray spectra of several other AGNs in the past few years. C1 Univ Sci & Technol China, Ctr Astrophys, Hefei 230026, Anhui, Peoples R China. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. Space Telescope Sci Inst, Baltimore, MD 21218 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Leiden Observ, Dept Astron, NL-2300 RA Leiden, Netherlands. RP Wang, JX (reprint author), Univ Sci & Technol China, Ctr Astrophys, Hefei 230026, Anhui, Peoples R China. EM jxw@ustc.edu.cn RI 王, 挺贵/B-8293-2013 NR 24 TC 5 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 SEP 20 PY 2005 VL 631 IS 1 BP L33 EP L36 DI 10.1086/496970 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 965OG UT WOS:000231959400009 ER PT J AU Palm, SP Benedetti, A Spinhirne, J AF Palm, SP Benedetti, A Spinhirne, J TI Validation of ECMWF global forecast model parameters using GLAS atmospheric channel measurements SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID BOUNDARY-LAYER; LIDAR; OCEAN; CLOUD; MISSION; ICE AB Satellite lidar (Light Detection And Ranging) data from GLAS is used to ascertain the performance of the European Center for Medium Range Weather Forecasts model predictions of cloud fraction, cloud vertical distribution, and boundary layer height. Results show that the model is reasonably accurate for low and middle clouds, but often misses the location and amount of high cirrus clouds. The model tends to overestimate high cloud fraction and this error grows with forecast length. The GLAS-derived boundary layer height over the oceans is generally 200 - 400 m higher than the model predictions, but small-scale and global patterns of PBL height show similar features. C1 Sci Syst & Applicat Inc, Lanham, MD 20706 USA. European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Palm, SP (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA. EM spp@virl.gsfc.nasa.gov; angela.benedetti@ecmwf.int; jspin@virl.gsfc.nasa.gov NR 10 TC 30 Z9 30 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 20 PY 2005 VL 32 IS 22 AR L22S09 DI 10.1029/2005GL023535 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 968QT UT WOS:000232177900002 ER PT J AU Palm, SP Fromm, M Spinhirne, J AF Palm, SP Fromm, M Spinhirne, J TI Observations of antarctic polar stratospheric clouds by the Geoscience Laser Altimeter System (GLAS) SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SAM-II; WINTER AB We present the first satellite lidar observations of Polar Stratospheric Clouds (PSCs). During late September and early October 2003, GLAS frequently observed type I and II PSCs over western Antarctica. At the peak of this activity on September 29 and 30 we investigate the vertical structure, horizontal coverage and general characteristics of the PSCs using the GLAS data. The PSCs were found to cover a relatively large area in a region where enhanced PSC frequency has been noted by previous PSC climatology studies. We also show near simultaneous measurements from the POAM III and SAGE II satellites that confirm the presence of type I and II PSCs in the same region. The area of PSC formation was found to coincide with the coldest temperatures and highest geopotential height in the lower stratosphere. In addition, extensive cloudiness was seen within the troposphere below the PSCs indicating that tropospheric disturbances played a role in their formation. C1 Sci Syst & Applicat Inc, Lanham, MD 20706 USA. USN, Res Lab, Washington, DC 20375 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Fromm, M (reprint author), Sci Syst & Applicat Inc, 10210 Greenbelt Rd,Suite 600, Lanham, MD 20706 USA. EM spp@virl.gsfc.nasa.gov; mike.fromm@nrl.navy.mil; jspin@virl.gsfc.nasa.gov RI Fromm, Michael/F-4639-2010 NR 13 TC 20 Z9 20 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 SEP 20 PY 2005 VL 32 IS 22 AR L22S04 DI 10.1029/2005GL023524 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 968QT UT WOS:000232177900001 ER PT J AU Wu, LG Wang, B Geng, SQ AF Wu, LG Wang, B Geng, SQ TI Growing typhoon influence on east Asia SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID WESTERN NORTH PACIFIC; TROPICAL CYCLONE ACTIVITY; EL-NINO; INTERDECADAL CHANGES; CLIMATE-CHANGE; PRECIPITATION; OSCILLATION; INTENSITY; MOVEMENT; VORTICES AB Numerical model studies have suggested that the ongoing global climate change will likely affect tropical cyclone activity. Since the global warming has been underway, it is meaningful to ask: Are there evidences of observed changes in tropical cyclone activity? Using best-track data from 1965 to 2003, we show for the first time that over the past four decades the two prevailing typhoon tracks in the western North Pacific (WNP) have shifted westward significantly; thus the subtropical East Asia has experienced increasing typhoon influence; but the typhoon influence over the South China Sea has considerably decreased. Our trajectory model simulation indicates that the long-term shifts in the typhoon tracks result primarily from the changes in the mean translation velocity of typhoons or the large-scale steering flow, which is associated with the westward expansion and strengthening of the WNP subtropical high. C1 Univ Maryland Baltimore Cty, Goddard Earth & Technol Ctr, Baltimore, MD 21228 USA. NASA, Atmospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD 20071 USA. Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Dept Meteorol, Honolulu, HI 96822 USA. Natl Marine Environm Res & Forecast Ctr, Beijing 100081, Peoples R China. RP Wu, LG (reprint author), Univ Maryland Baltimore Cty, Goddard Earth & Technol Ctr, Baltimore, MD 21228 USA. EM liguang@agnes.gsfc.nasa.gov NR 27 TC 115 Z9 129 U1 2 U2 29 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 20 PY 2005 VL 32 IS 18 AR L18703 DI 10.1029/2005GL022937 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 968QL UT WOS:000232177100001 ER PT J AU Yang, G Tang, J Kato, S Zhang, Q Qin, LC Woodson, M Liu, J Kim, JW Littlehei, PT Park, C Zhou, O AF Yang, G Tang, J Kato, S Zhang, Q Qin, LC Woodson, M Liu, J Kim, JW Littlehei, PT Park, C Zhou, O TI Magnetic nanowire based high resolution magnetic force microscope probes SO APPLIED PHYSICS LETTERS LA English DT Article ID DIELECTROPHORESIS; FABRICATION; ALUMINA; ARRAYS AB We report an efficient process for controlled fabrication of high-resolution magnetic force microscope probes using preformed magnetic nanowires. Nickel and cobalt nanowires produced by electrodeposition were directly assembled onto the tip of a commercial atomic force microscope cantilever with controlled orientation and length by dielectrophoresis. The properties of these nanowire-based probes are characterized. (c) 2005 American Institute of Physics. C1 Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. Natl Inst Mat Sci, Tsukuba, Ibaraki 3050047, Japan. Univ N Carolina, Curriculum Appl & Mat Sci, Chapel Hill, NC 27599 USA. Duke Univ, Dept Chem, Res Triangle Pk, NC 27709 USA. Sci & Technol Corp, Hampton, VA 23666 USA. NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA. NASA, Langley Res Ctr, Natl Inst Aerosp, Hampton, VA 23681 USA. RP Zhou, O (reprint author), Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. EM zhou@physics.unc.edu RI Kim, Jae-Woo/A-8314-2008; Lillehei, Peter/C-9196-2009; Liu, Jie/B-4440-2010 OI Lillehei, Peter/0000-0001-8183-9980; Liu, Jie/0000-0003-0451-6111 NR 14 TC 18 Z9 19 U1 2 U2 12 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 SEP 19 PY 2005 VL 87 IS 12 AR 123507 DI 10.1063/1.2043237 PG 3 WC Physics, Applied SC Physics GA 964UT UT WOS:000231907200066 ER PT J AU Tedesco, M Kim, EJ Gasiewski, A Klein, M Stankov, B AF Tedesco, M Kim, EJ Gasiewski, A Klein, M Stankov, B TI Analysis of multiscale radiometric data collected during the Cold Land Processes Experiment-1 (CLPX-1) SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SNOW WATER EQUIVALENT; SOIL-MOISTURE; DEPTH; VARIABILITY; RETRIEVAL; ALGORITHM AB Histograms of brightness temperatures collected at 18.7 and 37 GHz over the Fraser and North Park Meso-Scale Areas during the Cold Land Processes Experiment by the NOAA Polarimetric Scanning Radiometer (PSR/A) airborne sensor are modelled by a log-normal distribution (Fraser, forested area) and by a bi-modal distribution (North Park, patchy-snow, non-forested area). The brightness temperatures are re-sampled over a range of resolutions to study the effects of sensor resolution on the shape of the distribution, on the values of the average brightness temperatures and standard deviations. The histograms become more uniform and the spatial information in the initial distribution is lost for a resolution larger than 5000 m, in both areas. The values of brightness temperatures obtained by re-sampling the PSR-A data at 25 km resolution are consistent with those recorded by the Advanced Microwave Scanning Radiometer (AMSR-E) and Special Sensor Microwave/Imager (SSM/I) satellite radiometers at similar resolutions. C1 NASA, Goddard Space Flight Ctr, Goddard Earth Sci Technol Ctr, UMBC, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Instrumentat Sci Branch, Greenbelt, MD 20771 USA. NOAA, Environm Technol Lab, Boulder, CO 80305 USA. RP Tedesco, M (reprint author), NASA, Goddard Space Flight Ctr, Goddard Earth Sci Technol Ctr, UMBC, Code 614-6, Greenbelt, MD 20771 USA. EM mtedesco@umbc.edu NR 17 TC 10 Z9 10 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 17 PY 2005 VL 32 IS 18 AR L18501 DI 10.1029/2005GL023006 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 967SB UT WOS:000232110400001 ER PT J AU Gopalswamy, N Yashiro, S Liu, Y Michalek, G Vourlidas, A Kaiser, ML Howard, RA AF Gopalswamy, N Yashiro, S Liu, Y Michalek, G Vourlidas, A Kaiser, ML Howard, RA TI Coronal mass ejections and other extreme characteristics of the 2003 October-November solar eruptions SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ENERGETIC PARTICLE EVENTS; FORCE-FREE; RADIO; FLARES; SHOCKS; SPACECRAFT; CYCLE-23; WIND; SUN AB Fast coronal mass ejections (CMEs), X-class flares, solar energetic particle (SEP) events, and interplanetary shocks were abundantly observed during the episode of intense solar activity in late October and early November 2003. Most of the 80 CMEs originated from three active regions (NOAA ARs 484, 486, and 488). We compare the statistical properties of these CMEs with those of the general population of CMEs observed during cycle 23. We find that (1) the 2003 October-November CMEs were fast and wide on the average and hence were very energetic, (2) nearly 20 percent of the ultrafast CMEs (speed >= 2000 km s(-1)) of cycle 23 occurred during the October-November interval, including the fastest CME of the study period (similar to 2700 km s(-1) on 4 November 2003 at 1954 UT), (3) the rate of full-halo CMEs was nearly four times the average rate during cycle 23, (4) at least sixteen shocks were observed near the Sun, while eight of them were intercepted by spacecraft along the Sun-Earth line, (5) the CMEs were highly geoeffective: the resulting geomagnetic storms were among the most intense of cycle 23, (6) the CMEs were associated with very large SEP events, including the largest event of cycle 23. These extreme properties were commensurate with the size and energy of the associated active regions. This study suggests that the speed of CMEs may not be much higher than similar to 3000 km s(-1), consistent with the free energy available in active regions. An important practical implication of such a speed limit is that the Sun-Earth travel times of CME-driven shocks may not be less than similar to 0.5 day. Two of the shocks arrived at Earth in <24 hours, the first events in similar to 30 years and only the 14th and 15th documented cases of such events since 1859. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Catholic Univ Amer, Washington, DC 20064 USA. Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. USN, Res Lab, Solar Phys Branch, Div Space Sci, Washington, DC 20375 USA. RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM gopals@fugee.gsfc.nasa.gov; yashiro@cdaw.gsfc.nasa.gov; yliu@quake.stanford.edu; michalek@oa.uj.edu.pl; vourlidas@nrl.navy.mil; russ.howard@nrl.navy.mil RI Vourlidas, Angelos/C-8231-2009; Gopalswamy, Nat/D-3659-2012 OI Vourlidas, Angelos/0000-0002-8164-5948; NR 52 TC 37 Z9 37 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 SEP 17 PY 2005 VL 110 IS A9 AR A09S15 DI 10.1029/2004JA010958 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 967SW UT WOS:000232112500006 ER PT J AU Wu, CC Wu, ST Dryer, M Fry, CD Berdichevsky, D Smith, Z Detman, T Gopalswamy, N Skoug, R Zurbuchen, T Smith, C AF Wu, CC Wu, ST Dryer, M Fry, CD Berdichevsky, D Smith, Z Detman, T Gopalswamy, N Skoug, R Zurbuchen, T Smith, C TI Flare-generated shock evolution and geomagnetic storms during the ''Halloween 2003 epoch'': 29 October to 2 November SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID CORONAL MASS EJECTIONS; INTERPLANETARY SHOCKS; 1 AU; MHD; HELIOSPHERE; EARTH; TIME AB The October/November 2003 ("Halloween 2003'') epoch of intense solar flares provided an opportunity to test the results of earlier parametric 1.5 MHD studies of interacting interplanetary shock waves. These preliminary studies used an adaptive numerical grid that made it possible to identify products of these interactions. During 28 October to 2 November 2003, three shocks generated by four solar flares were observed at the L1 libration point by ACE/SWEPAM/SWICS/MAG. Two very distinct geomagnetic storms, associated with two of these flares (X17/4B and X10/2B), rank as two of the largest storms of solar cycle 23. The purpose of this paper is to present the use of an adaptive grid 1.5-dimensional MHD model that is initiated at the solar surface to study in detail the three shocks observed at L1 that were generated by the four solar flares. Accordingly, four separate pressure pulses, at the appropriate times and with different strengths and duration, determined via a trial and error procedure, are introduced on the Sun to mimic the four flares. The results show that the simulated solar wind velocity temporal profiles successfully matched the observations at L1. The major objective, to demonstrate the detailed nature of interacting shocks and some of their products after origination from closely spaced solar events, is achieved. In addition, the MHD model is able to suggest the solar sources that are associated with specific geomagnetic storms at Earth. C1 Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. NOAA, Space Environm Ctr, Boulder, CO USA. Explorat Phys Int Inc, Huntsville, AL 35806 USA. L3 Commun EER Syst Inc, Largo, MD 20774 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. Univ New Hampshire, Inst Earth Oceans & Space, Durham, NH 03824 USA. RP Wu, CC (reprint author), Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. EM wuc@cspar.uah.edu; wus@cspar.uah.edu; murray.dryer@noaa.gov; gfry@expi.com; xrdbb@lepvax.gsfc.nasa.gov; zdenka.smith@noaa.gov; thomas.detman@noaa.gov; gopals@fugee.nasa.gov; rskoug@lanl.gov; thomasz@umich.edu; chuck@briaxa.sr.unh.edu RI xue, yansheng/A-9712-2012; Gopalswamy, Nat/D-3659-2012 NR 25 TC 14 Z9 14 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD SEP 17 PY 2005 VL 110 IS A9 AR A09S17 DI 10.1029/2005JA011011 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 967SW UT WOS:000232112500007 ER PT J AU Racette, P Lang, RH AF Racette, P Lang, RH TI Radiometer design analysis based upon measurement uncertainty SO RADIO SCIENCE LA English DT Article ID AIRBORNE MICROWAVE RADIOMETER; INSTRUMENT DESCRIPTION; NOISE STANDARDS; WATER-VAPOR; CALIBRATION; SENSITIVITY; PERFORMANCE; IMPROVEMENT AB [ 1] This paper introduces a method for predicting the performance of a radiometer design based on calculating the measurement uncertainty. The variety in radiometer designs and the demand for improved radiometric measurements justify the need for a more general and comprehensive method to assess system performance. Radiometric resolution, or sensitivity, is a figure of merit that has been commonly used to characterize the performance of a radiometer. However, when evaluating the performance of a calibration design for a radiometer, the use of radiometric resolution has limited application. These limitations are overcome by considering instead the measurement uncertainty. A method for calculating measurement uncertainty for a generic radiometer design including its calibration algorithm is presented. The result is a generalized technique by which system calibration architectures and design parameters can be studied to optimize instrument performance for given requirements and constraints. Example applications demonstrate the utility of using measurement uncertainty as a figure of merit. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. George Washington Univ, Dept Elect Engn & Comp Sci, Washington, DC 20052 USA. RP Racette, P (reprint author), NASA, Goddard Space Flight Ctr, Code 555, Greenbelt, MD 20771 USA. EM paul.e.racette@nasa.gov; lang@gwu.edu NR 42 TC 7 Z9 7 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0048-6604 EI 1944-799X J9 RADIO SCI JI Radio Sci. PD SEP 17 PY 2005 VL 40 IS 5 AR RS5004 DI 10.1029/2004RS003132 PG 22 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications GA 967TC UT WOS:000232113100001 ER PT J AU Lancaster, RS Spinhirne, JD Palm, SP AF Lancaster, RS Spinhirne, JD Palm, SP TI Laser pulse reflectance of the ocean surface from the GLAS satellite lidar SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID WIND-SPEED; SCATTERING AB The world's oceans can potentially be used as an extended target for achieving a radiometric calibration of space borne lidar if the reflective properties of the surface can be accurately predicted from available environmental data such as wind speed. To test current understanding of ocean reflectance we compare surface pulse returns measured with the 1064 nm altimetry channel of the Geoscience Laser Altimeter System (GLAS) on the Ice, Cloud and land Elevation Satellite (ICESat) with the predictions of near-IR reflectance from current ocean models. Measurements of wind speed retrieved from the SeaWinds database of the QuikSCAT satellite provide the model input. We find that while ocean models do not provide a full description of the nadir lidar observations this calibration technique yields a precision that exceeds that accomplished using White Sands as a target and that does not require the coordination that accompanies specialized calibration experiments. C1 UMBC, Goddard Earth Sci & Technol Ctr, Greenbelt, MD 20771 USA. Sci Syst & Applicat Inc, Lanham, MD 20706 USA. NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Lancaster, RS (reprint author), UMBC, Goddard Earth Sci & Technol Ctr, Code 613-1, Greenbelt, MD 20771 USA. EM lancaster@virl.gsfc.nasa.gov NR 13 TC 12 Z9 14 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 16 PY 2005 VL 32 IS 22 AR L22S10 DI 10.1029/2005GL023732 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 967SC UT WOS:000232110500001 ER PT J AU Burrows, DN Romano, P Falcone, A Kobayashi, S Zhang, B Moretti, A O'Brien, PT Goad, MR Campana, S Page, KL Angelini, L Barthelmy, S Beardmore, AP Capalbi, M Chincarini, G Cummings, J Cusumano, G Fox, D Giommi, P Hill, JE Kennea, JA Krimm, H Mangano, V Marshall, F Meszaros, P Morris, DC Nousek, JA Osborne, JP Pagani, C Perri, M Tagliaferri, G Wells, AA Woosley, S Gehrels, N AF Burrows, DN Romano, P Falcone, A Kobayashi, S Zhang, B Moretti, A O'Brien, PT Goad, MR Campana, S Page, KL Angelini, L Barthelmy, S Beardmore, AP Capalbi, M Chincarini, G Cummings, J Cusumano, G Fox, D Giommi, P Hill, JE Kennea, JA Krimm, H Mangano, V Marshall, F Meszaros, P Morris, DC Nousek, JA Osborne, JP Pagani, C Perri, M Tagliaferri, G Wells, AA Woosley, S Gehrels, N TI Bright X-ray flares in gamma-ray burst afterglows SO SCIENCE LA English DT Article ID SUPERNOVAE; COLLAPSARS; EMISSION; SHOCKS AB Gamma-ray burst (GRB) afterglows have provided important clues to the nature of these massive explosive events, providing direct information on the nearby environment and indirect information on the central engine that powers the burst. We report the discovery of two bright x-ray flares in GRB afterglows, including a giant flare comparable in total energy to the burst itself, each peaking minutes after the burst. These strong rapid x-ray flares imply that the central engines of the bursts have long periods of activity, with strong internal shocks continuing for hundreds of seconds after the gamma-ray emission has ended. C1 Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. Osserv Astron Brera, INAF, I-23807 Merate, Italy. Penn State Univ, Ctr Gravitat Wave Phys, Davey Lab 104, University Pk, PA 16802 USA. Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Agenzia Spaziale Italiana Sci Data Ctr, I-00044 Frascati, Italy. Univ Milano Bicocca, Dipartimento Fis, I-20126 Milan, Italy. INAF Ist Astrofis Spaziale & Fis Cosm, Sez Palermo, I-90146 Palermo, Italy. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Burrows, DN (reprint author), Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. EM burrows@astro.psu.edu RI Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; OI moretti, alberto/0000-0002-9770-0315 NR 29 TC 367 Z9 373 U1 0 U2 3 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD SEP 16 PY 2005 VL 309 IS 5742 BP 1833 EP 1835 DI 10.1126/science.1116168 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 965ZN UT WOS:000231989500042 PM 16109845 ER PT J AU Vancil, BK Wintucky, EG AF Vancil, BK Wintucky, EG TI Weld techniques for reservoir cathodes SO APPLIED SURFACE SCIENCE LA English DT Article; Proceedings Paper CT 5th Internatioal Vacuum Electron Sources Conference CY SEP 06-10, 2004 CL Beijing, PEOPLES R CHINA SP Chinese Inst Elect, IEEE Elect Dev Soc, IEEE Beijing Sect, IEEE Beijing Branch, IEEE EDS Beijing Chapter, Natl Nat Sci Fdn China, BVERI, Beijing Univ Technol, SE Univ DE thermionic cathodes; reservoir cathodes; dispenser cathodes AB We report improvements in weld technology in support of our efforts to produce a commercial, long-life, miniature reservoir cathode. We have found that the laser weld between sintered tungsten pellet and reservoir sleeve can be made reliably hermetic if we apply a subsequent coating of molybdenum-ruthenium brazing alloy to the sides of the pellet and especially to the weld region. The emissive material is then inserted in the open end of the reservoir sleeve, which is then closed by a secondary weld. This secondary weld is reliably hermetic without the Mo-Ru coating, because it does not involve the porous tungsten matrix. Moreover, we have discovered an inspection procedure that allows us to check weld hermeticity at each assembly step. Thermal cycling tests indicate good weld integrity. Emission life testing is proceeding. (c) 2005 Elsevier B.V. All rights reserved.. C1 E Beam Inc, Beaverton, OR 97007 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Vancil, BK (reprint author), E Beam Inc, 21070 SW Tile Flat Rd, Beaverton, OR 97007 USA. EM bernie@ebeaminc.com; edwin.g.wintucky@grc.nasa.gov NR 2 TC 0 Z9 0 U1 1 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0169-4332 J9 APPL SURF SCI JI Appl. Surf. Sci. PD SEP 15 PY 2005 VL 251 IS 1-4 BP 101 EP 105 DI 10.1016/j.apsusc.2005.03.150 PG 5 WC Chemistry, Physical; Materials Science, Coatings & Films; Physics, Applied; Physics, Condensed Matter SC Chemistry; Materials Science; Physics GA 965ZD UT WOS:000231988500016 ER PT J AU Kwok, R AF Kwok, R TI Ross Sea ice motion, area flux, and deformation SO JOURNAL OF CLIMATE LA English DT Article ID SOUTHERN-OCEAN; SURFACE PRESSURE; WEDDELL SEA; ANTARCTICA; VARIABILITY; THICKNESS; POLYNYA; TRENDS; SHELF; OSCILLATION AB The sea ice motion, area export, and deformation of the Ross Sea ice cover are examined with satellite passive microwave and RADARSAT observations. The record of high-resolution synthetic aperture radar (SAR) data, from 1998 and 2000, allows the estimation of the variability of ice deformation at the small scale (similar to 10 km) and to assess the quality of the longer record of passive microwave ice motion. Daily and subdaily deformation fields and RADARSAT imagery highlight the variability of motion and deformation in the Ross Sea. With the passive microwave ice motion, the area export at a flux gate positioned between Cape Adare and Land Bay is estimated. Between 1992 and 2003, a positive trend can be seen in the winter (March-November) ice area flux that has a mean of 990 X 10(3) km(2) and ranges from a low of 600 X 1 03 km(2) in 1992 to a peak of 1600 X 10(3) km(2) in 2001. In the mean, the southern Ross Sea produces almost twice its own area of sea ice during the winter. Cross-gate sea level pressure (SLP) gradients explain similar to 60% of the variance in the ice area flux. A positive trend in this gradient, from reanalysis products, suggests a "spinup" of the Ross Sea Gyre over the past 12 yr. In both the NCEP-NCAR and ERA-40 surface pressure fields, longer-term trends in this gradient and mean SLP between 1979 and 2002 are explored along with positive anomalies in the monthly cross-gate SLP gradient associated with the positive phase of the Southern Hemisphere annular mode and the extrapolar Southern Oscillation. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kwok, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ron.kwok@jpl.nasa.gov RI Kwok, Ron/A-9762-2008 OI Kwok, Ron/0000-0003-4051-5896 NR 43 TC 18 Z9 19 U1 1 U2 6 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 J9 J CLIMATE JI J. Clim. PD SEP 15 PY 2005 VL 18 IS 18 BP 3759 EP 3776 DI 10.1175/JCLI3507.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 975BI UT WOS:000232635600004 ER PT J AU Lee, TJ Mejia, CN Beran, GJO Head-Gordon, M AF Lee, TJ Mejia, CN Beran, GJO Head-Gordon, M TI Search for stratospheric bromine reservoir species: Theoretical study of the photostability of mono-, tri-, and pentacoordinated bromine compounds SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID ABSORPTION CROSS-SECTIONS; OZONE DEPLETION POTENTIALS; DENSITY-FUNCTIONAL THEORY; ATMOSPHERIC BROMINE; EXCITED-STATES; CHEMISTRY; HOBR; RADICALS; SPECTRA; BR2O AB Previous work has shown that pentacoordinated bromine compounds have their lowest excited electronic states shifted to the blue relative to monocoordinated bromine molecules, and that this shift may be large enough to render them photostable in the lower stratosphere. Our earlier work has also shown that certain pentacoordinated bromine compounds are thermodynamically stable relative to their mono- or tricoordinated isomers, suggesting that if a bromine stratospheric reservoir species exists, it may be a pentacoordinated compound. In this study we have examined the singlet and triplet excited electronic states of several bromine compounds, using time dependent density functional theory, to assess their photostability under stratospheric conditions and in order to elucidate the nature of lowest excited states in mono-, tri-, and pentacoordinated bromine molecules. The triplet states have been included due to the strong spin-orbit mixing in bromine. We have found several pentacoordinated bromine/oxygen compounds that could be photostable in the lower stratosphere, but we have also found that monovalent bromine compounds where the bromine atom is bonded to an atom with no lone-pair p-electrons is far and away the most photostable. Attachment/detachment electron density plots have been useful in ascertaining the nature of the excited electronic states and their likely path to photodissociation. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Calif Berkeley, Dept Chem, Berkeley, CA 94563 USA. Lawrence Berkeley Natl Lab, Div Chem Sci, Berkeley, CA 94563 USA. RP Lee, TJ (reprint author), NASA, Ames Res Ctr, MS245-6, Moffett Field, CA 94035 USA. EM tjlee@mail.arc.nasa.gov RI Beran, Gregory/B-8684-2011; Lee, Timothy/K-2838-2012 OI Beran, Gregory/0000-0002-2229-2580; NR 32 TC 5 Z9 6 U1 0 U2 3 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 J9 J PHYS CHEM A JI J. Phys. Chem. A PD SEP 15 PY 2005 VL 109 IS 36 BP 8133 EP 8139 DI 10.1021/jp050997y PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 963MW UT WOS:000231809400009 PM 16834199 ER PT J AU Dargaville, TR Celina, M Martin, JW Banks, BA AF Dargaville, TR Celina, M Martin, JW Banks, BA TI Evaluation of piezoelectric PVDF polymers for use in space environments. II. Effects of atomic oxygen and vacuum UV exposure SO JOURNAL OF POLYMER SCIENCE PART B-POLYMER PHYSICS LA English DT Article DE atomic oxygen; space environment; vacuum ultraviolet radiation; vinylidene fluoride ID POLY(VINYLIDENE FLUORIDE); TEMPERATURE; DEGRADATION; RADIATION; EROSION; FILMS; FEP AB The effects of atomic oxygen (AO) and vacuum UV radiation simulating low Earth orbit conditions on two commercially available piezoelectric polymer films, poly(vinylidene fluoride) (PVDF) and poly(vinylidene fluoride-trifluoroethylene) P(VDF-TrFE), have been studied. Surface erosion and pattern development are significant for both polymers. Erosion yields were determined as 2.8 x 10(-24) cm(3)/atom for PVDF and 2.5 x 10-24 cm3/atom for P(VDF-TrFE). The piezoelectric properties of the residual material of both polymers were largely unchanged after exposure, although a slight shift in the Curie transition of the P(VDF-TrFE) was observed. A lightly cross-linked network was formed in the copolymer presumably because of penetrating vacuum ultraviolet (VUV) radiation, while the homopolymer remained uncross-linked. These differences were attributed to varying degrees of crystallinity and potentially greater absorption, and hence damage, of VUV radiation in P(VDF-TrFE) compared with PVDF. (c) 2005 Wiley Periodicals, Inc. C1 Sandia Natl Labs, Albuquerque, NM 87185 USA. NASA, Glenn Res Ctr, Cleveland, OH USA. RP Dargaville, TR (reprint author), Sandia Natl Labs, POB 5800, Albuquerque, NM 87185 USA. EM trdarga@sandia.gov OI Dargaville, Tim/0000-0003-4665-9508 NR 32 TC 11 Z9 11 U1 0 U2 7 PU JOHN WILEY & SONS INC PI HOBOKEN PA 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0887-6266 J9 J POLYM SCI POL PHYS JI J. Polym. Sci. Pt. B-Polym. Phys. PD SEP 15 PY 2005 VL 43 IS 18 BP 2503 EP 2513 DI 10.1002/polb.20549 PG 11 WC Polymer Science SC Polymer Science GA 959OH UT WOS:000231527000009 ER PT J AU Diner, DJ Braswell, BH Davies, R Gobron, N Hu, JN Jin, YF Kahn, RA Knyazikhin, Y Loeb, N Muller, JP Nolin, AW Pinty, B Schaaf, CB Seiz, G Stroeve, J AF Diner, DJ Braswell, BH Davies, R Gobron, N Hu, JN Jin, YF Kahn, RA Knyazikhin, Y Loeb, N Muller, JP Nolin, AW Pinty, B Schaaf, CB Seiz, G Stroeve, J TI The value of multiangle measurements for retrieving structurally and radiatively consistent properties of clouds, aerosols, and surfaces SO REMOTE SENSING OF ENVIRONMENT LA English DT Review DE multiangle remote sensing; terra; MISR; CERES; ASTER; MODIS ID GREENLAND ICE-SHEET; REFLECTANCE DISTRIBUTION FUNCTION; IMAGING SPECTRORADIOMETER MISR; ANGULAR-DISTRIBUTION MODELS; ENERGY SYSTEM INSTRUMENT; REMOTE-SENSING DATA; ARCTIC SEA-ICE; SPACEBORNE THERMAL EMISSION; MEASURING MISSION SATELLITE; VEGETATION LEAF-AREA AB Passive optical multiangle observations make possible the retrieval of scene structural characteristics that cannot be obtained with, or require fewer underlying assumptions than, single-angle sensors. Retrievable quantities include aerosol amount over a wide variety of surfaces (including bright targets); aerosol microphysical properties such as particle shape; geometrically-derived cloud-top heights and 3-D cloud morphologies; distinctions between polar clouds and ice; and textural measures of sea ice, ice sheets, and vegetation. At the same time, multiangle data are necessary for accurate retrievals of radiative quantities such as surface and top-of-atmosphere albedos, whose magnitudes are governed by structural characteristics of the reflecting media and which involve angular integration over intrinsically anisotropic intensity fields. Measurements of directional radiation streams also provide independent checks on model assumptions conventionally used in satellite retrievals, such as the application of 1-D radiative transfer theory, and provide data required to constrain more sophisticated, 3-D approaches. In this paper, the value of multiangle remote sensing in establishing physical correspondence and self-consistency between scene structural and radiative characteristics is demonstrated using simultaneous observations from instruments aboard NASA's Terra satellite (MISR, CERES, ASTER, and MODIS). Illustrations pertaining to the remote sensing of clouds, aerosols, ice, and vegetation properties are presented. (C) 2005 Elsevier Inc. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ New Hampshire, Durham, NH 03824 USA. Commiss European Communities, Joint Res Ctr, I-21020 Ispra, Italy. Boston Univ, Boston, MA 02215 USA. Univ Calif Irvine, Irvine, CA USA. NASA, Langley Res Ctr, Hampton, VA 23665 USA. UCL, London, England. Oregon State Univ, Corvallis, OR 97331 USA. Swiss Fed Inst Technol, Zurich, Switzerland. Univ Colorado, Boulder, CO 80309 USA. RP Diner, DJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM David.J.Diner@jpl.nasa.gov RI Stroeve, Julienne/D-1525-2010; Davies, Roger/D-4296-2009; Kahn, Ralph/D-5371-2012; Braswell, Bobby/D-6411-2016; OI Davies, Roger/0000-0002-2991-0409; Kahn, Ralph/0000-0002-5234-6359; Braswell, Bobby/0000-0002-4061-9516; Muller, Jan-Peter/0000-0002-5077-3736 NR 168 TC 97 Z9 102 U1 1 U2 21 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD SEP 15 PY 2005 VL 97 IS 4 BP 495 EP 518 DI 10.1016/j.rse.2005.06.006 PG 24 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 965RK UT WOS:000231967800007 ER PT J AU Petelina, SV Degenstein, DA Llewellyn, EJ Lloyd, ND Mertens, CJ Mlynczak, MG Russell, JM AF Petelina, SV Degenstein, DA Llewellyn, EJ Lloyd, ND Mertens, CJ Mlynczak, MG Russell, JM TI Thermal conditions for PMC existence derived from Odin/OSIRIS and TIMED/SABER data SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID NOCTILUCENT CLOUDS; MESOSPHERIC CLOUDS; MESOPAUSE REGION; 78-DEGREES-N; LATITUDE; LIDAR AB We study a relationship between Polar Mesospheric Cloud (PMC) brightness and coincident mesospheric Kinetic Temperatures (KT) measured by two satellite instruments, the Optical Spectrograph and Infrared Imager System and Sounding of the Atmosphere using Broadband Emission Radiometry respectively. Two fifteen-day periods in July 2002 and 2003 have been analyzed. For coincidences <= 3 hours and <= 200 km PMCs with a peak at 82-84 km were observed for the mean KT in this height range <= 142 K. Bright PMCs, at least twice brighter than the seasonal mean, were detected only for KT <= 134 K. The average KT for PMCs at 80 degrees-82.2 degrees N was lower than that at 60 degrees-75 degrees N by 5-8 K. The average KT coincident with PMCs was 1.4 to 7.9 K lower than that for non-PMC cases. There was up to 7% of non-PMC detections for the very low KT, <= 130 K. The total random and systematic uncertainty of this analysis was 9 K. C1 Univ Saskatchewan, Inst Space & Atmospher Studies, Saskatoon, SK S7N 5E2, Canada. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. RP Petelina, SV (reprint author), Univ Saskatchewan, Inst Space & Atmospher Studies, 116 Sci Pl, Saskatoon, SK S7N 5E2, Canada. EM svetlana@osirus.usask.ca RI Mlynczak, Martin/K-3396-2012 NR 17 TC 13 Z9 13 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 14 PY 2005 VL 32 IS 17 AR L17813 DI 10.1029/2005GL023099 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 967RX UT WOS:000232110000002 ER PT J AU Yang, P Wei, HL Huang, HL Baum, BA Hu, YX Kattawar, GW Mishchenko, MI Fu, Q AF Yang, P Wei, HL Huang, HL Baum, BA Hu, YX Kattawar, GW Mishchenko, MI Fu, Q TI Scattering and absorption property database for nonspherical ice particles in the near- through far-infrared spectral region SO APPLIED OPTICS LA English DT Article ID CLOUD OPTICAL-THICKNESS; CIRRUS CLOUDS; RADIATIVE PROPERTIES; LIGHT-SCATTERING; SINGLE-SCATTERING; CRYSTALS; PARAMETERIZATION; EXTINCTION; SENSITIVITY; WAVELENGTHS AB The single-scattering properties of ice particles in the near- through far-infrared spectral region are computed from a composite method that is based on a combination of the finite-difference time-domain technique, the T-matrix method, an improved geometrical-optics method, and Lorenz-Mie theory. Seven nonspherical ice crystal habits (aggregates, hexagonal solid and hollow columns, hexagonal plates, bullet rosettes, spheroids, and droxtals) are considered. A database of the single-scattering properties for each of these ice particles has been developed at 49 wavelengths between 3 and 100 mu m and for particle sizes ranging from 2 to 10,000 mu m specified in terms of the particle maximum dimension. The spectral variations of the single-scattering properties are discussed, as well as their dependence on the particle maximum dimension and effective particle size. The comparisons show that the assumption of spherical ice particles in the near-IR through far-IR region is generally not optimal for radiative transfer computation. Furthermore, a parameterization of the bulk optical properties is developed for mid-latitude cirrus clouds based on a set of 21 particle size distributions obtained from various field campaigns. (c) 2005 Optical Society of America. C1 Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. Univ Wisconsin, Cooperat Inst Meteorol Satellite Studies, Madison, WI 53706 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. RP Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. EM pyang@ariel.met.tamu.edu RI Yang, Ping/B-4590-2011; Baum, Bryan/B-7670-2011; Hu, Yongxiang/K-4426-2012; Mishchenko, Michael/D-4426-2012 OI Baum, Bryan/0000-0002-7193-2767; NR 47 TC 177 Z9 182 U1 1 U2 21 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD SEP 10 PY 2005 VL 44 IS 26 BP 5512 EP 5523 DI 10.1364/AO.44.005512 PG 12 WC Optics SC Optics GA 963GG UT WOS:000231791300022 PM 16161667 ER PT J AU Meister, G Kwiatkowska, EJ Franz, BA Patt, FS Feldman, GC McClain, CR AF Meister, G Kwiatkowska, EJ Franz, BA Patt, FS Feldman, GC McClain, CR TI Moderate-resolution imaging spectroradiometer ocean color polarization correction SO APPLIED OPTICS LA English DT Article ID ATMOSPHERIC CORRECTION; SURFACE-ROUGHNESS; SEAWIFS; MODIS; CALIBRATION; ALGORITHM; SENSITIVITY; SENSORS; EOS-AM1; MISSION AB The polarization correction for the Moderate-Resolution Imaging Spectroradiometer (MODIS) instruments on the Terra and Aqua satellites is described. The focus is on the prelaunch polarization characterization and on the derivation of polarization correction coefficients for the processing of ocean color data. The effect of the polarization correction is demonstrated. The radiances at the top of the atmosphere need to be corrected by as much as 3.2% in the 412 nm band. The effect on the water-leaving radiances can exceed 50%. The polarization correction produces good agreement of the MODIS Aqua water-leaving radiance time series with data from another, independent satellite-based ocean color sensor, the Sea-Viewing Wide Field-of-View Sensor (SeaWiFS). (c) 2005 Optical Society of America. C1 Futuretech Corp, Greenbelt, MD 20770 USA. Sci Applicat Int Corp, Beltsville, MD 20707 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Futuretech Corp, Greenbelt, MD 20770 USA. EM meister@simbios.gsfc.nasa.gov RI Franz, Bryan/D-6284-2012; Meister, Gerhard/F-7159-2012 OI Franz, Bryan/0000-0003-0293-2082; NR 25 TC 41 Z9 43 U1 0 U2 3 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD SEP 10 PY 2005 VL 44 IS 26 BP 5524 EP 5535 DI 10.1364/AO.44.005524 PG 12 WC Optics SC Optics GA 963GG UT WOS:000231791300023 PM 16161668 ER PT J AU Grady, CA Woodgate, BE Bowers, CW Gull, TR Sitko, ML Carpenter, WJ Lynch, DK Russell, RW Perry, RB Williger, GM Roberge, A Bouret, JC Sahu, M AF Grady, CA Woodgate, BE Bowers, CW Gull, TR Sitko, ML Carpenter, WJ Lynch, DK Russell, RW Perry, RB Williger, GM Roberge, A Bouret, JC Sahu, M TI Coronagraphic imaging of pre-main-sequence stars with the Hubble Space Telescope space telescope imaging spectrograph. I. The Herbig Ae stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; ISM : Herbig-Haro objects; ISM : jets and outflows; stars : pre-main-sequence ID T-TAURI STARS; INTERMEDIATE-MASS STARS; AE/BE STARS; CIRCUMSTELLAR DISK; HIGH-RESOLUTION; AB-AURIGAE; PROTOPLANETARY DISKS; BETA-PICTORIS; VEGA-TYPE; FUSE OBSERVATIONS AB STIS white-light coronagraphic imaging has been carried out for 14 nearby, lightly reddened Herbig Ae stars, providing data on the environments and disks associated with these stars. No disks are detected in our data when the Herbig Ae star is accompanied by a stellar companion at r <= 2 ''. We find that the optical visibility of protoplanetary disks associated with Herbig Ae stars at r >= 50 70 AU from the star is correlated with the strength of the mid-IR PAH features, particularly 6.2 mu m. These features, like the FUV fluorescent H-2 emission, trace the presence of material sufficiently far above the disk midplane that it is directly illuminated by the star's FUV radiation. In contrast, measures of the bulk properties of the disk, including ongoing accretion activity, mass, and the submillimeter slope of the SED, do not correlate with the surface brightness of the optical nebulosity. Modelers have interpreted the appearance of the IR SED and the presence of emission from warm silicate grains at 10 mu m as a measure of geometrical shadowing by material in the disk near the dust sublimation radius of 0.5 AU. Geometrical shadowing sufficient to render a disk dark to distances as large as 500 AU from a star would require that the star be optically visible only if viewed essentially pole-on, in disagreement with our program star system inclinations. Rather than invoking shadowing to account for the optically dark disks, the correlation of the STIS detections with PAH emission features suggests a correlation with disk flaring and an anticorrelation with the degree of dust settling toward the midplane. If this correlation continues to lower levels, the STIS data suggest that improvements in coronagraph performance that suppress the residual scattered and diffracted stellar light by an additional factor of >= 10 should render the majority of disks associated with nearby Herbig Ae stars detectable. C1 NASA, Goddard Space Flight Ctr, Explorat Universe Div, Exo Planets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA. Aerosp Corp, Los Angeles, CA 90009 USA. NASA, Langley Res Ctr, Sci Support Off, Hampton, VA 23681 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. Lab Astrophys Marseille, F-13376 Marseille, France. NASA, Goddard Space Flight Ctr, JWST Project, Greenbelt, MD 20771 USA. RP Grady, CA (reprint author), 2452 Delmer St,Suite 100, Oakland, CA 94602 USA. EM cgrady@echelle.gsfc.nasa.gov; williger@pha.jhu.edu RI Roberge, Aki/D-2782-2012; Gull, Theodore/D-2753-2012; Woodgate, Bruce/D-2970-2012 OI Roberge, Aki/0000-0002-2989-3725; Gull, Theodore/0000-0002-6851-5380; NR 84 TC 48 Z9 48 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 SEP 10 PY 2005 VL 630 IS 2 BP 958 EP 975 DI 10.1086/430731 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 961LR UT WOS:000231664400027 ER PT J AU Sterling, AC Moore, RL AF Sterling, AC Moore, RL TI Slow-rise and fast-rise phases of an erupting solar filament, and flare emission onset SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : coronal mass ejections (CMEs); Sun : filaments; Sun : flares; Sun : UV radiation; Sun : X-rays; gamma rays ID CORONAL MASS EJECTIONS; X-RAY TELESCOPE; A MISSION; RECONNECTION; REGION; MODEL AB We observe the eruption of an active-region solar filament on 1998 July 11 using high time cadence and high spatial resolution EUV observations from the TRACE satellite, along with soft X-ray images from the soft X-ray telescope ( SXT) on the Yohkoh satellite, hard X-ray fluxes from the BATSE instrument on the CGRO satellite and from the hard X-ray telescope ( HXT) on Yohkoh, and ground-based magnetograms. We concentrate on the initiation of the eruption in an effort to understand the eruption mechanism. Prior to eruption the filament undergoes a slow upward movement in a slow-rise phase with an approximately constant velocity of approximate to 15 km s(-1) that lasts about 10 minutes. It then erupts in a fast-rise phase, accelerating to a velocity of approximate to 200 km s(-1) in about 5 minutes and then decelerating to approximate to 150 km s(-1) over the next 5 minutes. EUV brightenings begin about concurrently with the start of the filament's slow rise and remain immediately beneath the rising filament during the slow rise; initial soft X-ray brightenings occur at about the same time and location. Strong hard X-ray emission begins after the onset of the fast rise and does not peak until the filament has traveled to a substantial altitude ( to a height about equal to the initial length of the erupting filament) beyond its initial location. Our observations are consistent with the slow-rise phase of the eruption resulting from the onset of "tether cutting" reconnection between magnetic fields beneath the filament, and the fast rise resulting from an explosive increase in the reconnection rate or by catastrophic destabilization of the overlying filament-carrying fields. About 2 days prior to the event, new flux emerged near the location of the initial brightenings, and this recently emerged flux could have been a catalyst for initiating the tether-cutting reconnection. With the exception of the sudden transition from the slow-rise phase to the fast-rise phase in our event, our filament's height-time profile is qualitatively similar to the plot of the erupting flux rope height as a function of time recently computed by Chen and Shibata for a model in which the eruption is triggered by reconnection between an emerging field and another field under the flux rope. C1 NASA, George C Marshall Space Flight Ctr, Space Sci Branch, Huntsville, AL 35812 USA. RP Sterling, AC (reprint author), NASA, George C Marshall Space Flight Ctr, Space Sci Branch, Huntsville, AL 35812 USA. EM alphonse.sterling@nasa.gov; ron.moore@nasa.gov NR 25 TC 78 Z9 79 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 SEP 10 PY 2005 VL 630 IS 2 BP 1148 EP 1159 DI 10.1086/432044 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 961LR UT WOS:000231664400044 ER PT J AU Balasubramaniam, KS Pevtsov, AA Neidig, DF Cliver, EW Thompson, BJ Young, CA Martin, SF Kiplinger, A AF Balasubramaniam, KS Pevtsov, AA Neidig, DF Cliver, EW Thompson, BJ Young, CA Martin, SF Kiplinger, A TI Sequential chromospheric brightenings beneath a transequatorial halo coronal mass ejection SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : activity; stars : magnetic fields; Sun : activity; Sun : coronal mass ejections ( CMEs); Sun : flares; Sun : magnetic fields; Sun : photosphere; sunspots ID SOLAR-FLARE WAVES; SOHO/EIT OBSERVATIONS; MORETON WAVES; LOOPS; EIT; MULTIWAVELENGTH; OSCILLATIONS AB Analyses of multiwavelength data sets for a solar eruption at similar to 21: 30 UT on 2002 December 19 show evidence for the disappearance of a large-scale, transequatorial coronal loop ( TL). In addition, coronal manifestations of the eruption ( based on SOHO EIT and LASCO images) include large-scale coronal dimming, flares in each associated active region in the northern and southern hemispheres, and a halo CME. We present detailed observations of the chromospheric aspects of this event based on H alpha images obtained with the ISOON telescope. The ISOON images reveal distant flare precursor brightenings, sympathetic flares, and, of most interest herein, four nearly cospatial propagating chromospheric brightenings. The speeds of the propagating disturbances causing these brightenings are 600 - 800 km s(-1). The inferred propagating disturbances have some of the characteristics of H alpha and EIT flare waves ( e. g., speed, apparent emanation from the flare site, subsequent filament activation). However, they differ from typical H alpha chromospheric flare waves ( also known as Moreton waves) because of their absence in off-band H alpha images, small angular arc of propagation (< 30 degrees), and their multiplicity. Three of the four propagating disturbances consist of a series of sequential chromospheric brightenings of network points that suddenly brighten in the area beneath the TL that disappeared earlier. SOHO MDI magnetograms show that the successively brightened points that define the inferred propagating disturbances were exclusively of one polarity, corresponding to the dominant polarity of the affected region. We speculate that the sequential chromospheric brightenings represent footpoints of field lines that extend into the corona, where they are energized in sequence by magnetic reconnection as coronal fields tear away from the chromosphere during the eruption of the transequatorial CME. We report briefly on three other events with similar narrow propagating disturbances that were confined to a single hemisphere. C1 Natl Solar Observ, Sunspot, NM 88349 USA. AFRL Space Vehicle Directorate, Space Weather Ctr Excellence, Bedford, MA 01731 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Helio Res, La Crescenta, CA 91214 USA. Univ Colorado, Ctr Integrated Plasma Studies, Boulder, CO 80309 USA. NOAA, Space Environm Ctr, Boulder, CO 80303 USA. RP Balasubramaniam, KS (reprint author), Natl Solar Observ, Sunspot, NM 88349 USA. EM bala@nso.edu; apevtsov@nso.edu RI Thompson, Barbara/C-9429-2012; OI Balasubramaniam, Krishnan/0000-0003-2221-0933; Pevtsov, Alexei/0000-0003-0489-0920 NR 34 TC 31 Z9 31 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2005 VL 630 IS 2 BP 1160 EP 1167 DI 10.1086/432030 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 961LR UT WOS:000231664400045 ER PT J AU Smith, SJ Djuric, N Lozano, JA Berrington, KA Chutjian, A AF Smith, SJ Djuric, N Lozano, JA Berrington, KA Chutjian, A TI Measurement of absolute cross sections for excitation of the 2s(2) S-1 -> 2s2p P-1 degrees transition in O+4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic data; atomic processes; stars : abundances; Sun : abundances ID ELECTRON-IMPACT-EXCITATION; ENERGY-LOSS; COLLISIONAL EXCITATION; LINE RATIOS; C-III; O-V; SPECTRA; REGIONS; IONS AB Experimental cross sections are reported for the 1s(2)2s(2) S-1 -> 1s(2)2s2p P-1(o) transition in O+4 located at 19.689 eV. Use is made of the electron energy-loss method, using a merged electron-ion beam geometry. The center-of-mass interaction energies for the measurements in the S-1 -> P-1(o) transition are in the range 18 eV ( below the threshold) to 30 eV. Data are compared with other previous electron energy-loss measurements and with results of a 26 term R-matrix calculation that includes fine structure explicitly via the Breit-Pauli Hamiltonian. Clear resonance enhancement is observed in all experimental and theoretical results near the threshold for this S-1 -> P-1(o) transition. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Sheffield Hallam Univ, Sch Sci & Math, Sheffield S1 1WB, S Yorkshire, England. RP Smith, SJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 26 TC 5 Z9 5 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 SEP 10 PY 2005 VL 630 IS 2 BP 1213 EP 1216 DI 10.1086/431752 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 961LR UT WOS:000231664400050 ER PT J AU Dow-Hygelund, CC Holden, BP Bouwens, RJ van der Wel, A Illingworth, GD Zirm, A Franx, M Rosati, P Ford, H van Dokkum, PG Stanford, SA Eisenhardt, P Fazio, GG AF Dow-Hygelund, CC Holden, BP Bouwens, RJ van der Wel, A Illingworth, GD Zirm, A Franx, M Rosati, P Ford, H van Dokkum, PG Stanford, SA Eisenhardt, P Fazio, GG TI UV continuum spectroscopy of a 6L(*) z=5.5 starburst galaxy SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : high-redshift; galaxies : individual (J1252-5224-4599); galaxies : starburst ID LYMAN-BREAK GALAXIES; FRAME ULTRAVIOLET-SPECTRA; ULTRA-DEEP-FIELD; STAR-FORMATION; SPACE-TELESCOPE; ADVANCED CAMERA; Z-APPROXIMATE-TO-6; RDCS-1252.9-2927; Z-SIMILAR-TO-6; DENSITY AB We have obtained a high S/ N ( 22.3 hr integration) UV continuum VLT FORS2 spectrum of an extremely bright (z(850) = 24.3) z = 5.515 +/- 0.003 star- forming galaxy ( BD38) in the field of the z = 1.24 cluster RDCS 1252.9 - 2927. From HST Advanced Camera for Surveys imaging, this object was selected as a potential z similar to 6 Lyman break galaxy ( LBG) based on its red i(775) -z(850) = 1.5 color. This object shows substantial continuum ( 0.41 +/- 0.02 mu Jy at 1300 angstrom) and low- ionization interstellar absorption features typical of LBGs at lower redshift A ( z similar to 3); this is the highest redshift LBG confirmed via metal- absorption spectral features. The equivalent widths of the absorption features are similar to z similar to 3 strong Ly alpha absorbers. No noticeable Ly alpha emission was detected (F <= 1.4 x 10(-18) ergs cm (-2) s (-1), 3 sigma). This object is at most amplified 0.3 mag from gravitational lensing by the foreground cluster. The delensed half- light radius of this object is 1.6 kpc ( 0 ".25), and the star formation rate derived from the rest- frame UV luminosity is SFRUV = 38h(0.7)(-2) M-circle dot yr (-1) corrected for dust extinction). In terms of recent determinations of the z similar to 6 UV luminosity function, this object appears to be 6L(*). The Spitzer IRAC fluxes for this object are 23.3 and 23.2 AB mag ( delensed) in the 3.6 and 4.5 mu m channels, respectively, implying a mass of ( 1 - 6) x 10(10) M-circle dot from population synthesis models. This galaxy is brighter than any confirmed z similar to 6 i- dropout to date in the band, and in the 3.6 and 4.5 mu m channels, and is the most z (850) massive starbursting galaxy known at z > 5. C1 Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 96064 USA. Univ Calif Santa Cruz, Dept Astron, Santa Cruz, CA 96062 USA. Leiden Observ, NL-2300 RA Leiden, Netherlands. European So Observ, D-85748 Garching, Germany. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Yale Univ, Dept Astron, New Haven, CT 06520 USA. Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dow-Hygelund, CC (reprint author), Univ Calif Santa Cruz, Dept Phys, 211 Interdisciplinary Sci Bldg,1156 High St, Santa Cruz, CA 96064 USA. EM cdow@scipp.ucsc.edu; holden@ucolick.org; bouwens@ucolick.org; vdwel@strw.leidenuniv.nl; gdi@ucolick.org; azirm@strw.leidenuniv.nl; franx@strw.leidenuniv.nl; prosati@eso.org; ford@pha.jhu.edu; dokkum@astro.yale.edu RI van der Wel, Arjen/G-8365-2011 NR 30 TC 28 Z9 28 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2005 VL 630 IS 2 BP L137 EP L140 DI 10.1086/491700 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 961LT UT WOS:000231664600009 ER PT J AU Hjorth, J Sollerman, J Gorosabel, J Granot, J Klose, S Kouveliotou, C Melinder, J Ramirez-Ruiz, E Starling, R Thomsen, B Andersen, MI Fynbo, JPU Jensen, BL Vreeswijk, PM Ceron, JMC Jakobsson, P Levan, A Pedersen, K Rhoads, JE Tanvir, NR Watson, D Wijers, RAMJ AF Hjorth, J Sollerman, J Gorosabel, J Granot, J Klose, S Kouveliotou, C Melinder, J Ramirez-Ruiz, E Starling, R Thomsen, B Andersen, MI Fynbo, JPU Jensen, BL Vreeswijk, PM Ceron, JMC Jakobsson, P Levan, A Pedersen, K Rhoads, JE Tanvir, NR Watson, D Wijers, RAMJ TI GRB 050509B: Constraints on short gamma-ray burst models SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts; supernovae : general ID NEUTRON-STAR MERGERS; SHORT-DURATION; OPTICAL AFTERGLOW; SUPERNOVA; EMISSION; PHOTOMETRY; COLLAPSARS; DISCOVERY; FLASHES; SEARCH AB We have obtained deep optical images with the Very Large Telescope at ESO of the first well-localized short-duration gamma-ray burst, GRB 050509B. From V and R imaging, initiated similar to 2 days after the GRB trigger and lasting up to three weeks, we detect no variable object inside the small Swift XRT X-ray error circle down to 2 sigma limits of V = 26.5 and R = 25.1. The X-ray error circle includes a giant elliptical galaxy at z = 0.225, which has been proposed as the likely host of this GRB. Our limits indicate that if the GRB originated at, z = 0.225 any supernova-like event accompanying the GRB would have to be over 100 times fainter than normal Type Ia SNe or Type Ic hypernovae, 5 times fainter than the faintest known Ia or Ic SNe, and fainter than the faintest known Type II SNe. Moreover, we use the optical limits to constrain the energetics of the GRB outflow. Simple models indicate that unless the intrinsic energy in the outflow from GRB 050509B was <= 10(51) ergs, there was very little radioactive material with efficient decay timescales for generating a large luminosity. These limits strongly constrain progenitor models for this short GRB. C1 Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. Inst Astrofis Andalucia, CSIC, E-18080 Granada, Spain. Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94309 USA. Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. NASA, George C Marshall Space Flight Ctr, Natl Space Sci Technol Ctr, Huntsville, AL 35805 USA. Inst Adv Study, Princeton, NJ 08540 USA. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus, Denmark. Astrophys Inst Potsdam, D-14482 Potsdam, Germany. European So Observ, Santiago 19, Chile. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. RP Hjorth, J (reprint author), Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark. EM jens@astro.ku.dk; josemari@alumni.nd.edu; jgu@iaa.es; granot@slac.stanford.edu; klose@tls-tautenburg.de; chryssa.kouveliotou-1@nasa.gov; jesper@astro.su.se; enrico@ias.edu; starling@science.uva.nl; bt@phys.au.dk; mandersen@aip.de; jfynbo@astro.ku.dk; jens@astro.ku.dk; pvreeswi@eso.org; brian_j@astro.ku.dk; pallja@astro.ku.dk; anl@star.le.ac.uk; kp@astro.ku.dk; rhoads@stsci.edu; nrt@star.herts.ac.uk; darach@astro.ku.dk; rwijers@science.uva.nl RI Hjorth, Jens/M-5787-2014; Watson, Darach/E-4521-2015; Jensen, Brian Lindgren/E-1275-2015; Jakobsson, Pall/L-9950-2015; OI Hjorth, Jens/0000-0002-4571-2306; Watson, Darach/0000-0002-4465-8264; Jensen, Brian Lindgren/0000-0002-0906-9771; Jakobsson, Pall/0000-0002-9404-5650; Wijers, Ralph/0000-0002-3101-1808; Sollerman, Jesper/0000-0003-1546-6615 NR 46 TC 95 Z9 97 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 SEP 10 PY 2005 VL 630 IS 2 BP L117 EP L120 DI 10.1086/491733 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 961LT UT WOS:000231664600004 ER PT J AU Bauer, SE Koch, D AF Bauer, SE Koch, D TI Impact of heterogeneous sulfate formation at mineral dust surfaces on aerosol loads and radiative forcing in the Goddard Institute for Space Studies general circulation model SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SEA-SALT SULFATE; VOLCANIC SULFUR EMISSIONS; AIR-POLLUTION; PARTICLES; NITRATE; SIZE; CHEMISTRY; TRANSPORT; OXIDATION; OZONE AB [1] Heterogeneous chemical reactions between sulfate precursors on the surface of mineral dust aerosols affect the atmospheric aerosol cycle and the Earth radiation budget. Heterogeneous reactions of sulfur dioxide with mineral dust particles enhance sulfate formation by producing internally mixed sulfate dust aerosols. The anthropogenic sulfate forcing is estimated to be reduced to - 0.18 W/m(2) because of the reduced load of externally mixed sulfate aerosols, compared to - 0.25 W/m(2) when heterogeneous surface reactions are excluded. Sulfate coating on mineral dust particles increases wet deposition of dust, causing a positive anthropogenic forcing due to less sulfate coating at preindustrial times. However, heterogeneous reaction pathways are highly uncertain, which is reflected in the wide spread of reaction pathways and uptake probability coefficients in the literature. We undertake a series of sensitivity experiments with the Goddard Institute for Space Studies climate model to investigate the impact of the uncertainty in uptake mechanisms and dust aerosol size distributions on the simulated sulfate cycle. The results of this study are very sensitive to both tested variables. For example, doubling the clay emissions ( particles whose radii are less than 1 mm) leads to a sevenfold increase in heterogeneous sulfate production. C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Columbia Univ, Earth Inst, New York, NY 10027 USA. RP NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM sbauer@giss.nasa.gov RI Bauer, Susanne/P-3082-2014 NR 54 TC 69 Z9 70 U1 3 U2 18 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP 10 PY 2005 VL 110 IS D17 AR D17202 DI 10.1029/2005JD005870 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 963TF UT WOS:000231828100004 ER PT J AU Gao, ST Cui, XP Zhou, YS Li, XF Tao, WK AF Gao, ST Cui, XP Zhou, YS Li, XF Tao, WK TI A modeling study of moist and dynamic vorticity vectors associated with two-dimensional tropical convection SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID POTENTIAL VORTICITY; FRONTAL RAINBANDS; CLOUD SYSTEMS; PHASE-III; EXTRATROPICAL CYCLONES; MICROSCALE STRUCTURE; MESOSCALE PROCESSES; SURFACE PROCESSES; TOGA COARE; PART II AB [1] Moist ((xi) over right arrow x del q(v)/rho, MVV) and dynamic ((xi) over right arrow x (V) over right arrow/rho, DVV) vorticity vectors are introduced to study 2-D tropical convection with 2-D cloud-resolving simulation data. The cloud model is forced by vertical velocity, zonal wind, horizontal advection, and sea surface temperature data obtained from TOGA COARE and is integrated for a selected 10-day period. The MVV and DVV have zonal and vertical components in the 2-D x-z frame. Analysis of zonally averaged and mass-integrated quantities shows that the vertical ( zonal) component of the MVV and the sum of the cloud hydrometeor mixing ratios are in phase with a correlation coefficient of 0.78 (0.32), and the vertical ( zonal) component of the DVV and the sum of the mixing ratios are in ( out of) phase with a correlation coefficient of 0.52 ( - 0.62), indicating that the vertical component of the MVV and both zonal and vertical component of the DVV are closely associated with tropical convection. The tendency equations for the MVV and DVV are derived, and the zonally averaged and mass-integrated tendency budgets are analyzed. The tendency of the vertical component of the MVV is mainly determined by the interaction between the vorticity and the zonal gradient of condensational/depositional heating. The tendency of the zonal component of the DVV is controlled by the interaction between the vorticity, buoyancy, and vertical pressure gradient, whereas the tendency of the vertical component is determined by the interaction between the vorticity and zonal pressure gradient. C1 Chinese Acad Sci, Inst Atmospher Phys, Lab Cloud Precipitat Phys & Severe Storms, Beijing 100029, Peoples R China. Joint Ctr Satellite Data Assimilat, Camp Springs, MD 20746 USA. NOAA, NESDIS, Off Res & Applicat, Camp Springs, MD 20746 USA. NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Chinese Acad Sci, Inst Atmospher Phys, Lab Cloud Precipitat Phys & Severe Storms, Beijing 100029, Peoples R China. EM gst@lasg.iap.ac.cn RI Li, Xiaofan/F-5605-2010; Li, Xiaofan/G-2094-2014 NR 45 TC 77 Z9 94 U1 2 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP 10 PY 2005 VL 110 IS D17 AR D17104 DI 10.1029/2004JD005675 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 963TF UT WOS:000231828100003 ER PT J AU Sittler, EC Hartle, RE Vinas, AF Johnson, RE Smith, HT Mueller-Wodarg, I AF Sittler, EC Hartle, RE Vinas, AF Johnson, RE Smith, HT Mueller-Wodarg, I TI Titan interaction with Saturn's magnetosphere: Voyager 1 results revisited SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID TOTAL CROSS-SECTIONS; ELECTRON-CAPTURE; PLANETARY EXOSPHERES; MOLECULAR-HYDROGEN; UPPER-ATMOSPHERE; POSITIVE-IONS; MHD MODEL; NITROGEN; COLLISIONS; IONOSPHERE AB We investigate the details of Titan's interaction with Saturn's magnetosphere, which includes formation and location of an ionopause, mass loading via ion pickup, and the effects of finite gyroradii. We present new interpretations of the Voyager 1 plasma instrument measurements not addressed by Hartle et al. (1982). Pickup ions H+ and H-2(+) dominate in the outermost region with respect to Titan's "ionopause," followed by CH4+ at intermediate distances and N-2(+) just outside the "ionopause." Mass loading and slowing down of the ambient plasma is observed to increase as the pickup ion mass increases with decreasing radial distance from Titan's ionosphere. H-2 and CH4 are molecules not originally included in the exosphere of Titan by Hartle and coworkers, and the pickup ions of H-2(+) and CH4+ are a new feature of our model calculations and should be present in Titan's exospheric region. Therefore Titan could be an important source of carbon to Saturn's magnetosphere. Finite gyroradius effects are identified in the plasma interaction with Titan's atmosphere, which results in an asymmetric removal of ambient plasma from Titan's exosphere region. The finite gyroradius effects also show that the observed hot keV ion component of the ambient plasma is a heavy ion such as N+/O+. A minimum "ionopause" altitude of 4800 km is estimated by a new approach using mass loading. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Virginia, Dept Engn Phys, Charlottesville, VA 22904 USA. Univ London Imperial Coll Sci Technol & Med, Space & Atmospher Phys Grp, London SW7 2BW, England. RP Sittler, EC (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM edward.c.sittler@nasa.gov; richard.e.hartle@nasa.gov; adolfo.f.vinas@nasa.gov; rej@virginia.edu; i.mueller-wodarg@imperial.ac.uk RI Mueller-Wodarg, Ingo/M-9945-2014; Smith, Howard/H-4662-2016 OI Mueller-Wodarg, Ingo/0000-0001-6308-7826; Smith, Howard/0000-0003-3537-3360 NR 55 TC 26 Z9 26 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 SEP 10 PY 2005 VL 110 IS A9 AR A09302 DI 10.1029/2004JA010759 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 963TS UT WOS:000231829500001 ER PT J AU Fricker, HA Borsa, A Minster, B Carabajal, C Quinn, K Bills, B AF Fricker, HA Borsa, A Minster, B Carabajal, C Quinn, K Bills, B TI Assessment of ICESat performance at the Salar de Uyuni, Bolivia SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB The primary goal of the Ice, Cloud and land Elevation Satellite (ICESat) mission is ice sheet elevation change detection. Confirmation that ICESat is achieving its stated scientific requirement of detecting spatially-averaged changes as small as 1.5 cm/year requires continual assessment of ICESat-derived elevations throughout the mission. We use a GPS-derived digital elevation model (DEM) of the salar de Uyuni, Bolivia for this purpose. Using all twelve ICESat passes over the salar survey area acquired to date, we show that the accuracy of ICESat-derived elevations is impacted by environmental effects (e.g., forward scattering and surface reflectance) and instrument effects (e.g., pointing biases, detector saturation, and variations in transmitted laser energy). We estimate that under optimal conditions at the salar de Uyuni, ICESat-derived elevations have an absolute accuracy of <2 cm and precision of <3 cm. C1 Univ Calif San Diego, Scripps Inst Oceanog, Inst Geophys & Planetary Phys, La Jolla, CA 92093 USA. NVI Inc, NASA, Goddard Space Flight Ctr, Space Geodesy Lab, Greenbelt, MD 20771 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. RP Fricker, HA (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Inst Geophys & Planetary Phys, 9500 Gilman Dr, La Jolla, CA 92093 USA. EM hafricker@ucsd.edu NR 4 TC 8 Z9 9 U1 4 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 SEP 9 PY 2005 VL 32 IS 21 AR L21S06 DI 10.1029/2005GL023423 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 963TB UT WOS:000231827700001 ER PT J AU Hlavka, DL Palm, SP Hart, WD Spinhirne, JD McGill, MJ Welton, EJ AF Hlavka, DL Palm, SP Hart, WD Spinhirne, JD McGill, MJ Welton, EJ TI Aerosol and cloud optical depth from GLAS: Results and verification for an October 2003 California fire smoke case SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID LIDAR; NETWORK AB Data from the satellite lidar Geoscience Laser Altimeter System (GLAS) has provided a new means to retrieve height and optical depth of transmissive cloud and aerosol layers globally. We compare data sets from GLAS and an airborne under-flight of the Cloud Physics Lidar (CPL) during a unique smoke opportunity as part of a validation experiment in October 2003. The CPL has known layer identification and optical retrieval performance. GLAS data products, including calibrated attenuated backscatter profiles, layer identification, and optical depth, are compared to simultaneous aircraft lidar retrievals with similar model assumptions with a goal toward discovering algorithm biases in GLAS. The case described here involves heavy smoke layers from large-scale fires in southern California and thin cirrus clouds. The GLAS optical retrievals agree with the CPL data when the GLAS aerosol lidar ratio, S, is reset from default maritime to smoke and in inland urban pollution localities. C1 NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Hlavka, DL (reprint author), NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Code 613-1, Greenbelt, MD 20771 USA. EM sgdlh@virl.gsfc.nasa.gov RI Welton, Ellsworth/A-8362-2012; McGill, Matthew/D-8176-2012; OI Hlavka, Dennis/0000-0002-2976-7243 NR 7 TC 21 Z9 21 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 9 PY 2005 VL 32 IS 22 AR L22S07 DI 10.1029/2005GL023413 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 963TC UT WOS:000231827800001 ER PT J AU Ofman, L Davila, JM Nakariakov, VM Vinas, AF AF Ofman, L Davila, JM Nakariakov, VM Vinas, AF TI High-frequency Alfven waves in multi-ion coronal plasma: Observational implications SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID SOLAR-WIND ACCELERATION; ION-CYCLOTRON WAVES; TEMPERATURE ANISOTROPY; PARTICLE INTERACTIONS; MINOR IONS; OMEGA-HE; INSTABILITIES; DRIVEN; MODEL; HOLES AB [1] We investigate the effects of high-frequency ( of order ion gyrofrequency) Alfven and ion-cyclotron waves on ion emission lines by studying the dispersion of these waves in a multi-ion coronal plasma. For this purpose we solve the dispersion relation of the linearized multifluid and Vlasov equations in a magnetized multi-ion plasma with coronal abundances of heavy ions. We also calculate the dispersion relation using nonlinear one-dimensional hybrid kinetic simulations of the multi-ion plasma. When heavy ions are present the dispersion relation of parallel propagating Alfven cyclotron waves exhibits the following branches ( in the positive Omega - k quadrant): right-hand polarized nonresonant and left-hand polarized resonant branch for protons and each ion. We calculate the ratio of ion to proton velocities perpendicular to the direction of the magnetic field for each wave modes for typical coronal parameters and find strong enhancement of the heavy ion perpendicular fluid velocity compared with proton perpendicular fluid velocity. The linear multifluid cold plasma results agree with linear warm plasma Vlasov results and with the nonlinear hybrid simulation model results. In view of our findings we discuss how the observed nonthermal line broadening of minor ions in coronal holes may relate to the high-frequency wave motions. C1 Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. RP Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. EM leon.ofman@gsfc.nasa.gov; joseph.m.davila@nasa.gov; v.nakariakov@warwick.ac.uk; adolfo.vinas@gsfc.nasa.gov RI Nakariakov, Valery/E-2375-2013; Lee, SungHwan/O-2563-2013 OI Nakariakov, Valery/0000-0001-6423-8286; NR 64 TC 17 Z9 17 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD SEP 9 PY 2005 VL 110 IS A9 AR A09102 DI 10.1029/2004JA010969 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 963TR UT WOS:000231829300002 ER PT J AU Bansal, NP Gamble, EA AF Bansal, NP Gamble, EA TI Crystallization kinetics of a solid oxide fuel cell seal glass by differential thermal analysis SO JOURNAL OF POWER SOURCES LA English DT Article DE solid oxide fuel cell; seals; glass; devitrification; activation energy; differential thermal analysis ID CRYSTAL-GROWTH KINETICS; SOFCS; DTA AB Crystallization kinetics of a barium-calcium aluminosilicate glass (BCAS), a sealant material for planar solid oxide fuel cells (SOFC), have been investigated by differential thermal analysis (DTA). From variation of DTA peak maximum temperature with heating rate, the activation energy for glass crystallization was calculated to be 259 kJ/mol using a kinetic model. Development of crystalline phases on thermal treatments of the glass at various temperatures has been followed by powder X-ray diffraction. Microstructure and chemical composition of the crystalline phases were investigated by scanning electron microscopy and energy dispersive spectroscopic (EDS) analysis. BaSiO3 and hexacelsian (BaAl2Si2O8) were the primary crystalline phases whereas monoclinic celsian (BaAl2Si2O8) and (BaxCay)SiO4 were also detected as minor phases. Needle-shaped BaSiO3 crystals are formed first. followed by the formation of other phases at longer times of heat treatments. The glass does not fully crystallize even after long-term heat treatments at 750-900 degrees C. Devitrification of the glass seal over a long period of time during operation of the SOFC would generate thermal stresses in the seal and may have adverse effects on its mechanical performance. This may lead to cracking of the seal, resulting in mixing of the fuel and the oxidant gases. Crown Copyright (c) 2005 Published by Elsevier B.V. All rights reserved. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Bansal, NP (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM Narottam.P.Bansal@nasa.gov NR 20 TC 82 Z9 90 U1 3 U2 32 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-7753 J9 J POWER SOURCES JI J. Power Sources PD SEP 9 PY 2005 VL 147 IS 1-2 BP 107 EP 115 DI 10.1016/j.jpowsour.2005.01.010 PG 9 WC Chemistry, Physical; Electrochemistry; Energy & Fuels; Materials Science, Multidisciplinary SC Chemistry; Electrochemistry; Energy & Fuels; Materials Science GA 969NQ UT WOS:000232241400009 ER PT J AU Limpasuvan, V Wu, DL Schwartz, MJ Waters, JW Wu, Q Killeen, TL AF Limpasuvan, V Wu, DL Schwartz, MJ Waters, JW Wu, Q Killeen, TL TI The two-day wave in EOS MLS temperature and wind measurements during 2004-2005 winter SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID RESOLUTION DOPPLER IMAGER; MIDDLE ATMOSPHERE; QUASI-2-DAY WAVE; STRATOSPHERIC ANALYSES; INSTABILITY; UARS AB Two-day wave observations during January - March 2005 are reported using the recently launched Microwave Limb Sounder (MLS) aboard NASA's Earth Observing System Aura mission. Wave-induced disturbances in temperature, water vapor, carbon monoxide, and MLS line-of-sight wind appear in early January, peak near the end of January, and persist until late February. Temperature and wind amplitudes as large as 9 K and 50 m/s are observed near 90 km. The wave disturbance is initially confined in the mid to low summer latitudes where the climatological summer easterly jet exhibits strong shear. The wave then develops features akin to the third Rossby-gravity global normal mode, with a weak temperature disturbance in the winter hemisphere (anti-symmetric about the equator) and wind disturbance over the equator. Strong wind perturbation episode around 17 - 23 January 2005 in the mid-latitude Southern hemisphere coincides with a particularly intense solar proton event. C1 Coastal Carolina Univ, Dept Chem & Phys, Conway, SC 29528 USA. CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. RP Limpasuvan, V (reprint author), Coastal Carolina Univ, Dept Chem & Phys, POB 261954, Conway, SC 29528 USA. EM var@coastal.edu; dwu@mls.jpl.nasa.gov; michael@mls.jpl.nasa.gov; joe@mls.jpl.nasa.gov; qwu@ucar.edu; killeen@ucar.edu RI Limpasuvan, Varavut/K-6266-2013; Schwartz, Michael/F-5172-2016; Wu, Dong/D-5375-2012 OI Schwartz, Michael/0000-0001-6169-5094; NR 19 TC 34 Z9 34 U1 1 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 8 PY 2005 VL 32 IS 17 AR L17809 DI 10.1029/2005GL023396 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 963SY UT WOS:000231827400002 ER PT J AU Gettelman, A Webster, CR AF Gettelman, A Webster, CR TI Simulations of water isotope abundances in the upper troposphere and lower stratosphere and implications for stratosphere troposphere exchange SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID TROPICAL TROPOPAUSE LAYER; VAPOR; TRANSPORT; RATIOS; CLOUD; PRECIPITATION; AIRCRAFT; MODEL AB [1] An analytic model of transport and microphysics in the tropical tropopause layer (TTL) is extended to include stable isotopes of water. The model, running along trajectories, is tested against in situ and satellite observations of HDO and (H2O)-O-18 in the Upper Troposphere and Lower Stratosphere (UT/LS). The model is able to reproduce the range of isotopic depletions observed in the data, and reproduce individual episodes that mirror or depart from Rayleigh fractionation processes. The results indicate that water substance in the upper troposphere does not follow a Rayleigh distillation model due to the presence of condensed phase water. Stratospheric abundances of stable isotopes of water can be understood based on known isotopic physics, convective transport of ice, and gradual dehydration. C1 Natl Ctr Atmospher Res, Boulder, CO 80307 USA. CALTECH, Jet Prop Lab, Div Earth & Space Sci, Pasadena, CA 91109 USA. RP Gettelman, A (reprint author), Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. EM andrew@ucar.edu NR 28 TC 18 Z9 18 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP 8 PY 2005 VL 110 IS D17 AR D17301 DI 10.1029/2004JD004812 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 963TE UT WOS:000231828000001 ER PT J AU Hoogenboom, T Houseman, G Martin, P AF Hoogenboom, T Houseman, G Martin, P TI Elastic thickness estimates for coronae associated with chasmata on Venus SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID CONTINENTAL LITHOSPHERE; BETA-REGIO; TECTONICS; EVOLUTION; GRAVITY; SUBDUCTION; FEATURES; FLEXURE; ORIGIN; TOPOGRAPHY AB [1] In this study we investigate the relationship between the local elastic lithospheric thickness and the relative ages of coronae on Venus in an attempt to further understand corona and chasmata formation/evolution. We use Magellan gravity and topography data to estimate the elastic lithospheric thickness in the vicinity of coronae associated with chasmata. The relative timing of corona formation with respect to chasmata formation is classified using superposition relationships between fractures and flows associated with the corona, and the regional fracture sets associated with the chasmata. For the 31 coronae that we here examine ( limited by low resolution of the Magellan gravity field in some regions of interest), estimates of elastic thickness appear to be related to the relative timing of corona formation. Coronae that formed after chasmata exhibit smaller values of elastic thickness ( 0 to 19 km), which may result from their formation on relatively warm and weak lithosphere due to lithospheric extension associated with chasmata formation. Coronae that formed prior to chasmata formation display greater elastic thickness values ( 0 to 56 km). These coronae are interpreted to have formed on lithosphere that was stronger (colder). However, examples of coronae with small elastic thickness (< 5 km) are found in all relative timing groups. C1 Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England. Univ Cambridge, Dept Phys, Cambridge CB3 0HE, England. RP Hoogenboom, T (reprint author), Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 183-501, Pasadena, CA 91106 USA. EM trudi@jpl.nasa.edu NR 51 TC 9 Z9 9 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD SEP 8 PY 2005 VL 110 IS E9 AR E09003 DI 10.1029/2004JE002394 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 963TM UT WOS:000231828800001 ER PT J AU Kim, HI Johnson, PV Beegle, LW Beauchamp, JL Kanik, I AF Kim, HI Johnson, PV Beegle, LW Beauchamp, JL Kanik, I TI Electrospray ionization ion mobility spectrometry of carboxylate anions: Ion mobilities and a mass-mobility correlation SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID ORGANIC-COMPOUNDS; AMINO-ACIDS; DRIFT-GAS; MARS; SURFACE; SEARCH AB A number of carboxylate anions spanning a mass range of 87-253 amu (pyruvate, oxalate, malonate, maleate, succinate, malate, tartarate, glutarate, adipate, phthalate, citrate, gluconate, 1,2,4-benzenetricarboxylate, and 1,2,4,5-benzenetetracarboxylate) were investigated using electrospray ionization ion mobility spectrometry. Measured ion mobilities demonstrated a high correlation between mass and mobility in both N-2 and CO2 drift gases. Such a strong mass-mobility correlation among structurally dissimilar ions suggests that the carboxylate functional group that these ions have in common is the source of the correlation. Computational analysis was performed to determine the most stable conformation of the studied carboxylate anions in the gas phase under the current experimental conditions. This analysis indicated that the most stable conformations for multicarboxylate anions included intramolecular hydrogen-bonded ring structures formed between the carboxylate group and the neutral carboxyl group. The carboxylate anions that form ring confirmations generally show higher ion mobility values than those that form extended conformations. This is the first observation of intramolecular hydrogen-bonded ring conformation of carboxylate anions in the gas phase at atmospheric pressure. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CALTECH, Noyes Lab Chem Phys, Pasadena, CA 91125 USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Paul.V.Johnson@jpl.nasa.gov RI Beegle, Luther/A-6354-2010; Kim, Hugh/G-4476-2011; Johnson, Paul/D-4001-2009 OI Johnson, Paul/0000-0002-0186-8456 NR 26 TC 13 Z9 13 U1 0 U2 15 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 J9 J PHYS CHEM A JI J. Phys. Chem. A PD SEP 8 PY 2005 VL 109 IS 35 BP 7888 EP 7895 DI 10.1021/jp051274h PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 961UK UT WOS:000231687100009 PM 16834170 ER PT J AU Hill, D Lin, Y Qu, LW Kitaygorodskiy, A Connell, JW Allard, LF Sun, YP AF Hill, D Lin, Y Qu, LW Kitaygorodskiy, A Connell, JW Allard, LF Sun, YP TI Functionalization of carbon nanotubes with derivatized polyimide SO MACROMOLECULES LA English DT Article ID ELECTROSTATIC CHARGE MITIGATION; TRANSFER RADICAL POLYMERIZATION; DISPERSION; LUMINESCENCE; CHEMISTRY; FILMS; NMR AB Single-walled and multiple-walled carbon nanotubes were functionalized with derivatized polyimide for the homogeneous dispersion of the nanotubes. For the functionalization, the nanotubebound carboxylic acids derived from the surface defects were targeted for esterification reactions with pendant hydroxyl groups in the derivatized polyimide. The functionalized nanotube samples, readily soluble in several common organic solvents, were thoroughly characterized by a series of instrumental techniques including NMR in both solution phase and solid state, optical absorption, Raman, thermogravimetric analysis, and microscopy methods. The results were consistent with well-dispersed nanotubes functionalized by the polyimide, and also with the expectation that the nanotube electronic properties were largely preserved in the specific mode of functionalization. The presumed formation of ester linkages in the functionalized samples was supported by the results from chemical defunctionalization. The potential applications of the polyimide-functionalized carbon nanotubes and the demonstrated functionalization strategy are discussed. C1 Clemson Univ, Dept Chem, Clemson, SC 29634 USA. Clemson Univ, Lab Emerging Mat & Technol, Clemson, SC 29634 USA. NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA. Oak Ridge Natl Lab, High Temp Mat Lab, Oak Ridge, TN 37831 USA. RP Sun, YP (reprint author), Clemson Univ, Dept Chem, Clemson, SC 29634 USA. NR 42 TC 82 Z9 83 U1 2 U2 21 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0024-9297 J9 MACROMOLECULES JI Macromolecules PD SEP 6 PY 2005 VL 38 IS 18 BP 7670 EP 7675 DI 10.1021/ma0509210 PG 6 WC Polymer Science SC Polymer Science GA 960RX UT WOS:000231612000019 ER PT J AU Kaufman, YJ Boucher, O Tanre, D Chin, M Remer, LA Takemura, T AF Kaufman, YJ Boucher, O Tanre, D Chin, M Remer, LA Takemura, T TI Aerosol anthropogenic component estimated from satellite data SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID OPTICAL-PROPERTIES; AIR-POLLUTION; CLIMATE; RETRIEVALS; THICKNESS; ALBEDO; MODEL; RAIN AB Satellite instruments do not measure the aerosol chemical composition needed to discriminate anthropogenic from natural aerosol components. However the ability of new satellite instruments to distinguish fine (submicron) from coarse (supermicron) aerosols over the oceans, serves as a signature of the anthropogenic component and can be used to estimate the fraction of anthropogenic aerosols with an uncertainty of +/-30%. Application to two years of global MODIS data shows that 21 +/- 7% of the aerosol optical thickness over the oceans has an anthropogenic origin. We found that three chemical transport models, used for global estimates of the aerosol forcing of climate, calculate a global average anthropogenic optical thickness over the ocean between 0.030 and 0.036, in line with the present MODIS assessment of 0.033. This increases our confidence in model assessments of the aerosol direct forcing of climate. The MODIS estimated aerosol forcing over cloud free oceans is therefore -1.4 +/- 0.4 W/m(2). C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Met Off, Climate Chem & Ecosyst Team, Exeter EX1 3PB, Devon, England. Kyushu Univ, Appl Mech Res Inst, Fukuoka 8168580, Japan. Univ Lille 1, Opt Atmospher Lab, CNRS, F-59655 Villeneuve Dascq, France. RP NASA, Goddard Space Flight Ctr, Code 613, Greenbelt, MD 20771 USA. EM yoram.j.kaufman@nasa.gov RI Takemura, Toshihiko/C-2822-2009; Boucher, Olivier/J-5810-2012; Chin, Mian/J-8354-2012; Boucher, Olivier/K-7483-2012; Kyushu, RIAM/F-4018-2015; U-ID, Kyushu/C-5291-2016 OI Takemura, Toshihiko/0000-0002-2859-6067; Boucher, Olivier/0000-0003-2328-5769; Boucher, Olivier/0000-0003-2328-5769; NR 23 TC 128 Z9 133 U1 1 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 3 PY 2005 VL 32 IS 17 AR L17804 DI 10.1029/2005GL023125 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 962JG UT WOS:000231727000002 ER PT J AU Gross, RS Fukumori, I Menemenlis, D AF Gross, RS Fukumori, I Menemenlis, D TI Atmospheric and oceanic excitation of decadal-scale Earth orientation variations SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID POLAR MOTION; ANGULAR-MOMENTUM; ROTATION; MODEL; CORE; TIDES; ICE; REPRESENTATION; FLUCTUATIONS; REANALYSIS AB The contribution of atmospheric wind and surface pressure and oceanic current and bottom pressure variations during 1949-2002 to exciting changes in the Earth's orientation on decadal timescales is investigated using an atmospheric angular momentum series computed from the National Centers for Environmental Prediction/National Center for Atmospheric Research (NCEP/NCAR) reanalysis project and an oceanic angular momentum series computed from a near-global ocean model that was forced by surface fluxes from the NCEP/NCAR reanalysis project. Not surprisingly, since decadal-scale variations in the length of day are caused mainly by interactions between the mantle and core, the effect of the atmosphere and oceans is found to be only about 14% of that observed. More surprisingly, it is found that the effect of atmospheric and oceanic processes on decadal-scale changes in polar motion is also only about 20% (x component) and 38% (y component) of that observed. Therefore redistribution of mass within the atmosphere and oceans does not appear to be the main cause of the Markowitz wobble. It is also found that on timescales between 10 days and 4 years the atmospheric and oceanic angular momentum series used here have very little skill in explaining Earth orientation variations before the mid to late 1970s. This is attributed to errors in both the Earth orientation observations prior to 1976 when measurements from the accurate space-geodetic techniques became available and to errors in the modeled atmospheric fields prior to 1979 when the satellite era of global weather observing systems began. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Gross, RS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 238-600, Pasadena, CA 91109 USA. EM richard.gross@jpl.nasa.gov NR 58 TC 31 Z9 31 U1 1 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD SEP 3 PY 2005 VL 110 IS B9 AR B09405 DI 10.1029/2004JB003565 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 962JY UT WOS:000231728900002 ER PT J AU Wygant, JR Cattell, CA Lysak, R Song, Y Dombeck, J McFadden, J Mozer, FS Carlson, CW Parks, G Lucek, EA Balogh, A Andre, M Reme, H Hesse, M Mouikis, C AF Wygant, JR Cattell, CA Lysak, R Song, Y Dombeck, J McFadden, J Mozer, FS Carlson, CW Parks, G Lucek, EA Balogh, A Andre, M Reme, H Hesse, M Mouikis, C TI Cluster observations of an intense normal component of the electric field at a thin reconnecting current sheet in the tail and its role in the shock-like acceleration of the ion fluid into the separatrix region SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID COLLISIONLESS MAGNETIC RECONNECTION; LATITUDE DAYSIDE MAGNETOPAUSE; GEOTAIL OBSERVATIONS; PLASMA SHEET; MAGNETOTAIL RECONNECTION; PARTICLE SIMULATIONS; EARTHS MAGNETOPAUSE; KINK INSTABILITY; BOUNDARY-LAYER; FULL PARTICLE AB Measurements from the Cluster spacecraft of electric fields, magnetic fields, and ions are used to study the structure and dynamics of the reconnection region in the tail at distances of similar to 18 R-E near 22.4 MLT on 1 October 2001. This paper focuses on measurements of the large amplitude normal component of the electric field observed in the ion decoupling region near the reconnection x-line, the structure of the associated potential drops across the current sheet, and the role of the electrostatic potential structure in the ballistic acceleration of ions across the current sheet. The thinnest current sheet observed during this interval was bifurcated into a pair of current sheets and the measured width of the individual current sheet was 60-100 km (3-5 c/omega(pe)). Coinciding with the pair of thin current sheets is a large-amplitude (+/-60 mV/m) bipolar electric field structure directed normal to the current sheets toward the midplane of the plasma sheet. The potential drop between the outer boundary of the thin current sheet and the neutral sheet due to this electric field is 4-6 kV. This electric field structure produces a 4-6 kV electric potential well centered on the separatrix region. Measured H+ velocity space distributions obtained inside the current layers provide evidence that the H+ fluids from the northern and southern tail lobes are accelerated into the potential well, producing a pair of counterstreaming, monoenergetic H+ beams. These beams are directed within 20 degrees of the normal direction with energies of 4-6 keV. The data also suggest there is ballistic acceleration of O+ in a similar larger-scale potential well of 10-30 kV spatially coinciding with the larger scale size (similar to 1000-3000 km) portions of current sheet surrounding the thin current sheet. Distribution functions show counterstreaming O+ populations with energies of similar to 20 keV accelerated along the average normal direction within this large-scale potential structure. The normal component of the electric field in the thin current sheet layer is large enough to drive an E x B drift of the electrons similar to 10,000 km/s (0.25 x electron Alfven velocity), which can account for the magnitude of the cross-tail current associated with the thin current sheet. C1 Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2B7, England. Swedish Inst Space Phys, Uppsala Div, Uppsala, Sweden. Ctr Etud Spatiale Rayonnements, Toulouse, France. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ New Hampshire, Durham, NH 03824 USA. RP Wygant, JR (reprint author), Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. EM wygant@ham.space.umn.edu RI Hesse, Michael/D-2031-2012; OI Cattell, Cynthia/0000-0002-3805-320X NR 68 TC 163 Z9 167 U1 1 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD SEP 3 PY 2005 VL 110 IS A9 AR A09206 DI 10.1029/2004JA010708 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 962KD UT WOS:000231729400003 ER PT J AU Alpert, P Kishcha, P Kaufman, YJ Schwarzbard, R AF Alpert, P Kishcha, P Kaufman, YJ Schwarzbard, R TI Global dimming or local dimming?: Effect of urbanization on sunlight availability SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SURFACE SOLAR-RADIATION; AIR-POLLUTION; IRRADIANCE; TRENDS AB From the 1950s to the 1980s, a significant decrease of surface solar radiation has been observed at different locations throughout the world. Here we show that this phenomenon, widely termed global dimming, is dominated by the large urban sites. The global-scale analysis of year-to-year variations of solar radiation fluxes shows a decline of 0.41 W/m(2)/yr for highly populated sites compared to only 0.16 W/m(2)/yr for sparsely populated sites (<0.1 million). Since most of the globe has sparse population, this suggests that solar dimming is of local or regional nature. The dimming is sharpest for the sites at 10 degrees N to 40 degrees N with great industrial activity. In the equatorial regions even the opposite trend to dimming is observed for sparsely populated sites. C1 Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Alpert, P (reprint author), Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel. EM kishcha@gmail.com RI Namikawa, Laercio/C-5559-2013 OI Namikawa, Laercio/0000-0001-7847-1804 NR 13 TC 89 Z9 98 U1 1 U2 21 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 2 PY 2005 VL 32 IS 17 AR L17802 DI 10.1029/2005GL023320 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 962JF UT WOS:000231726900001 ER PT J AU Wahlund, JE Bostrom, R Gustafsson, G Gurnett, DA Kurth, WS Averkamp, T Hospodarsky, GB Persoon, AM Canu, P Pedersen, A Desch, MD Eriksson, AI Gill, R Morooka, MW Andre, M AF Wahlund, JE Bostrom, R Gustafsson, G Gurnett, DA Kurth, WS Averkamp, T Hospodarsky, GB Persoon, AM Canu, P Pedersen, A Desch, MD Eriksson, AI Gill, R Morooka, MW Andre, M TI The inner magnetosphere of Saturn: Cassini RPWS cold plasma results from the first encounter SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID VOYAGER-2; ELECTRONS; RADIO AB We present new results from the inner magnetosphere of Saturn obtained by the Radio and Plasma Wave Science (RPWS) investigation onboard Cassini around the period of the Saturn orbit injection ( July 1, 2004). Plasma wave electric field emissions, voltage sweeps by the Langmuir probe ( LP) and radio sounder data were used to infer the cold plasma (< 100 eV) characteristics within 20 R(S) of Saturn. A dense (< 150 cm(-3)) and cold (< 7 eV) plasma torus was found just outside the visible F-ring. This torus of partly dusty plasma does not perfectly co-rotate with Saturn, which suggests the cold plasma is electro-dynamically coupled to the charged ring-dust particles. The spacecraft potential was a few volts negative above the E- and G-rings, indicating the dust-particles were likewise negatively charged. The cold ion characteristics changed near the magnetically conjugate position of Dione, indicating release of volatile material from this icy moon. C1 Swedish Inst Space Phys, Uppsala Div, SE-75121 Uppsala, Sweden. Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. Ctr Etud Environm Terr & Planetaires, F-78140 Velizy Villacoublay, France. Univ Oslo, Dept Phys, N-0316 Oslo, Norway. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Wahlund, JE (reprint author), Swedish Inst Space Phys, Uppsala Div, POB 537, SE-75121 Uppsala, Sweden. EM jwe@irfu.se; rb@irfu.se; gg@irfu.se; dag@space.physics.uiowa.edu; wsk@space.physics.uiowa.edu; wtr@space.physics.uiowa.edu; gbh@space.physics.uiowa.edu; amp@space.physics.uiowa.edu; patrick.canu@cetp.ipsl.fr; arne.pedersen@fys.uio.no; mdesch@pop600.gsfc.nasa.gov; aie@irfu.se; rg@irfu.se; michiko@irfu.se; ma@irfu.se NR 15 TC 42 Z9 42 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 2 PY 2005 VL 32 IS 20 AR L20S09 DI 10.1029/2005GL022699 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 962JH UT WOS:000231727100001 ER PT J AU Whaler, KA Purucker, ME AF Whaler, KA Purucker, ME TI A spatially continuous magnetization model for Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID SPHERICAL HARMONIC MODEL; MERIDIANI-PLANUM; CRUSTAL MAGNETIZATION; SATELLITE DATA; HIGH-ALTITUDE; FIELD; ANOMALIES; MAGNETISM; HEMATITE; GRAVITY AB Using a three-component magnetic field data set at over 100,000 satellite points previously compiled for spherical harmonic analysis, we have produced a continuously varying magnetization model for Mars. The magnetized layer was assumed to be 40 km thick, an average value based on previous studies of the topography and gravity field. The severe nonuniqueness in magnetization modeling is addressed by seeking the model with minimum root-mean-square (RMS) magnetization for a given fit to the data, with the trade-off between RMS magnetization and fit controlled by a damping parameter. Our preferred model has magnetization amplitudes up to 20 A/m. It is expressed as a linear combination of the Green's functions relating each observation to magnetization at the point of interest within the crust, leading to a linear system of equations of dimension the number of data points. Although this is impractically large for direct solution, most of the matrix elements relating data to model parameters are negligibly small. We therefore apply methods applicable to sparse systems, allowing us to preserve the resolution of the original data set. Thus we produce more detailed models than any previously published, although they share many similarities. We find that tectonism in the Valles Marineris region has a magnetic signature, and we show that volcanism south of the dichotomy boundary has both a magnetic and gravity signature. The method can also be used to downward continue magnetic data, and a comparison with other leveling techniques at Mars' surface is favorable. C1 Univ Edinburgh, Sch Geosci, Inst Earth Sci, Edinburgh EH9 3JW, Midlothian, Scotland. NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Raytheon ITSS, Greenbelt, MD 20771 USA. RP Whaler, KA (reprint author), Univ Edinburgh, Sch Geosci, Inst Earth Sci, W Mains Rd, Edinburgh EH9 3JW, Midlothian, Scotland. EM kathy.whaler@ed.ac.uk; purucker@geomag.gsfc.nasa.gov NR 60 TC 30 Z9 31 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 SEP 2 PY 2005 VL 110 IS E9 AR E09001 DI 10.1029/2004JE002393 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 962JR UT WOS:000231728200001 ER PT J AU Prezeau, G Kurylov, A AF Prezeau, G Kurylov, A TI Neutrino mass constraints on mu decay and pi(0)->nu(nu)over-bar SO PHYSICAL REVIEW LETTERS LA English DT Article ID PARAMETERS AB In this Letter, we show that upper limits on the neutrino mass translate into upper limits on the class of neutrino-matter interactions that can generate loop corrections to the neutrino mass matrix. We apply our results to mu and pi decays and derive model-independent limits on six of the ten parameters used to parametrize contributions to mu decay that do not belong to the standard model. These upper limits provide improved constraints on the five Michel parameters, rho,xi',xi '',alpha,alpha', that exceed Particle Data Group constraints by at least one order of magnitude. For pi(0)->nu(nu) over bar we find, for the branching ratio, B(pi(0)->nu(nu) over bar)< 10(-10). C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CALTECH, Kellogg Radiat Lab, Pasadena, CA 91125 USA. RP Prezeau, G (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 16 TC 16 Z9 16 U1 0 U2 0 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD SEP 2 PY 2005 VL 95 IS 10 AR 101802 DI 10.1103/PhysRevLett.95.101802 PG 4 WC Physics, Multidisciplinary SC Physics GA 960TI UT WOS:000231615700007 PM 16196918 ER PT J AU Santer, BD Wigley, TML Mears, C Wentz, FJ Klein, SA Seidel, DJ Taylor, KE Thorne, PW Wehner, MF Gleckler, PJ Boyle, JS Collins, WD Dixon, KW Doutriaux, C Free, M Fu, Q Hansen, JE Jones, GS Ruedy, R Karl, TR Lanzante, JR Meehl, GA Ramaswamy, V Russell, G Schmidt, GA AF Santer, BD Wigley, TML Mears, C Wentz, FJ Klein, SA Seidel, DJ Taylor, KE Thorne, PW Wehner, MF Gleckler, PJ Boyle, JS Collins, WD Dixon, KW Doutriaux, C Free, M Fu, Q Hansen, JE Jones, GS Ruedy, R Karl, TR Lanzante, JR Meehl, GA Ramaswamy, V Russell, G Schmidt, GA TI Amplification of surface temperature trends and variability in the tropical atmosphere SO SCIENCE LA English DT Article ID SATELLITE; TROPOSPHERE; RADIOSONDE AB The month-to-month variability of tropical temperatures is larger in the troposphere than at Earth's surface. This amplification behavior is similar in a range of observations and climate model simulations and is consistent with basic theory. On multidecadal time scales, tropospheric amplification of surface warming is a robust feature of model simulations, but it occurs in only one observational data set. Other observations show weak, or even negative, amplification. These results suggest either that different physical mechanisms control amplification processes on monthly and decadal time scales, and models fail to capture such behavior or (more plausibly) that residual errors in several observational data sets used here affect their representation of long-term trends. C1 Lawrence Livermore Natl Lab, Program Climate Model Diag & Intercomparison, Livermore, CA 94550 USA. Natl Ctr Atmospher Res, Boulder, CO 80303 USA. Remote Syst Sensing, Santa Rosa, CA 95401 USA. NOAA, Air Resources Lab, Silver Spring, MD 20910 USA. UK Met Off, Hadlet Ctr Climate Predict & Res, Exeter EX1 3PB, Devon, England. Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. NOAA, Geophys Fluid Dynam Lab, Princeton, NJ 08542 USA. Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. NASA, Goddard Inst Space Studies, New York, NY 10025 USA. NOAA, Natl Climat Data Ctr, Asheville, NC 28801 USA. RP Santer, BD (reprint author), Lawrence Livermore Natl Lab, Program Climate Model Diag & Intercomparison, Livermore, CA 94550 USA. EM santer1@llnl.gov RI Wigley, Tom/B-4705-2008; Taylor, Karl/F-7290-2011; Santer, Benjamin/F-9781-2011; Schmidt, Gavin/D-4427-2012; Gleckler, Peter/H-4762-2012; Jones, Gareth/H-8022-2013; Thorne, Peter/F-2225-2014; Collins, William/J-3147-2014; Dixon, Keith/L-7120-2015; Klein, Stephen/H-4337-2016 OI Taylor, Karl/0000-0002-6491-2135; Schmidt, Gavin/0000-0002-2258-0486; Gleckler, Peter/0000-0003-2816-6224; Thorne, Peter/0000-0003-0485-9798; Collins, William/0000-0002-4463-9848; Dixon, Keith/0000-0003-3044-326X; Klein, Stephen/0000-0002-5476-858X NR 30 TC 175 Z9 177 U1 2 U2 32 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD SEP 2 PY 2005 VL 309 IS 5740 BP 1551 EP 1556 DI 10.1126/science.1114867 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 962EY UT WOS:000231715000047 PM 16099951 ER PT J AU D'Antoni, HL AF D'Antoni, HL TI Astrobiology, the origin of life and global change SO ACTA BIOQUIMICA CLINICA LATINOAMERICANA LA Spanish DT Article ID IRRADIANCE; CLIMATE C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP D'Antoni, HL (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Hector.L.Dantoni@nasa.gov NR 20 TC 0 Z9 0 U1 1 U2 9 PU FEDERACION BIOQUIMICA PROVINCIA BUENOS AIRES PI LA PLATA, BUENOS AIRES PA CALLE 6, NO. 1344, 1900 LA PLATA, BUENOS AIRES, ARGENTINA SN 0325-2957 J9 ACTA BIOQUIM CLIN L JI Acta Bioquim. Clin. Latinoam. PD SEP PY 2005 VL 39 IS 3 BP 381 EP 394 PG 14 WC Medical Laboratory Technology SC Medical Laboratory Technology GA 001XP UT WOS:000234576300013 ER PT J AU Sukumar, V Alahmad, M Buck, K Hess, H Li, H Cox, D Zghoul, FN Jackson, J Terry, S Blalock, B Mojarradi, MM West, WC Whitacre, JF AF Sukumar, V Alahmad, M Buck, K Hess, H Li, H Cox, D Zghoul, FN Jackson, J Terry, S Blalock, B Mojarradi, MM West, WC Whitacre, JF TI High voltage MOSFET gate/bulk driver controller for a microbattery switch matrix in a 0.35 mu m microwave SOI technology SO ANALOG INTEGRATED CIRCUITS AND SIGNAL PROCESSING LA English DT Article DE LDMOSFET; micropower; microbattery; SOI AB Integrated microbatteries are being currently developed to act as a "micropower" source in microsatellites. The current and voltage rating of the microbattery is fixed. Certain highly miniaturized systems require higher voltages and currents. A switching matrix is designed to achieve the same. The switching matrix is designed using High Voltage Metal Oxide Semiconductor (MOS) structures and bulk isolated H gate transistors. This paper presents a design approach to help attain any random grouping pattern between the microbatteries. In this case, the result is an ability to charge microbatteries in parallel and to discharge microbatteries in parallel or pairs of microbatteries in series. This is achieved by providing the appropriate gate/bulk voltages to the matrix. High Voltage MOS structures are developed which can take higher drain-to-source voltages in a 3.3 V process. The designs are built using Microwave Silicon-on-Insulator process. C1 Univ Idaho, Microelect Res & Commun Inst, Moscow, ID 83844 USA. Univ Tennessee, Integrated Circuits & Syst Lab, Knoxville, TN USA. CALTECH, Jet Propuls Lab, Pasadena, CA USA. RP Sukumar, V (reprint author), Univ Idaho, Microelect Res & Commun Inst, Moscow, ID 83844 USA. EM vinesh@mrc.uidaho.edu NR 7 TC 3 Z9 3 U1 1 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0925-1030 J9 ANALOG INTEGR CIRC S JI Analog Integr. Circuits Process. PD SEP PY 2005 VL 44 IS 3 BP 203 EP 211 DI 10.1007/s10470-005-2999-6 PG 9 WC Computer Science, Hardware & Architecture; Engineering, Electrical & Electronic SC Computer Science; Engineering GA 959KO UT WOS:000231516800002 ER PT J AU Rebollo, TC Gomez, DR AF Rebollo, TC Gomez, DR TI A numerical solver for the primitive equations of the ocean using term-by-term stabilization SO APPLIED NUMERICAL MATHEMATICS LA English DT Article DE oceanography; primitive equations; mixed finite elements; stabilized finite elements ID NAVIER-STOKES EQUATIONS; FINITE-ELEMENT METHODS; SHALLOW-WATER FLOW; HYDROSTATIC APPROXIMATION; OCEANOGRAPHY; SYSTEM AB In this work we introduce and analyze a numerical approximation of the primitive equations of the ocean by means of stabilized finite elements. We use a reduced formulation of these equations which only includes the (3D) horizontal velocity and the (2D) surface pressure. This, combined with the use of stabilized finite elements, provides a large reduction of degrees of freedom in comparison with previous mixed methods. The use of isoparametric prismatic finite elements provides good geometric adaptability to the topography. We perform an analysis of stability and convergence using the concept of static condensation on bubble spaces. Finally, we test our stabilized approximations in flows with complex 3D structure, including a real-life application. Specifically, we simulate the wind-driven circulation in Lake Neuchatel. (c) 2004 IMACS. Published by Elsevier B.V. All rights reserved. C1 NASA, Ames Res Ctr, Exobiol Branch, Stanford, CA 94305 USA. Univ Sevilla, Dept Ecuaciones Diferenciales & Anal Numer, E-41080 Seville, Spain. RP Gomez, DR (reprint author), NASA, Ames Res Ctr, Exobiol Branch, MS 239-4, Stanford, CA 94305 USA. EM chacon@us.es; dgomez@templar.arc.nasa.gov OI Chacon Rebollo, Tomas/0000-0002-0784-1174 NR 43 TC 1 Z9 1 U1 0 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9274 J9 APPL NUMER MATH JI Appl. Numer. Math. PD SEP PY 2005 VL 55 IS 1 BP 1 EP 31 DI 10.1016/j.apum.2004.08.007 PG 31 WC Mathematics, Applied SC Mathematics GA 949YU UT WOS:000230825600001 ER PT J AU Veselovskii, I Kolgotin, A Muller, D Whiteman, DN AF Veselovskii, I Kolgotin, A Muller, D Whiteman, DN TI Information content of multiwavelength lidar data with respect to microphysical particle properties derived from eigenvalue analysis SO APPLIED OPTICS LA English DT Article ID SIZE DISTRIBUTION; AEROSOL; BACKSCATTER; EXTINCTION; RETRIEVAL AB The multiwavelength Raman lidar technique in combination with sophisticated inversion algorithms has been recognized as a new tool for deriving information about the microphysical properties of atmospheric aerosols. The input optical parameter sets, provided by respective aerosol Raman lidars, are at the theoretical lower limit at which these inversion algorithms work properly. For that reason there is ongoing intense discussion of the accuracy of these inversion methods and the possibility of simultaneous retrieval of the particle size distribution and the complex refractive index. We present results of the eigenvalue analysis, used to study the information content of multiwavelength lidar data with respect to microphysical particle properties. Such an analysis provides, on a rather mathematical basis, more insight into the limitations of these inversion algorithms regarding the accuracy of the retrieved parameters. We show that the effective radius may be retrieved to 50% accuracy and the real and imaginary part of the complex refractive index to +/- 0.05 and +/- 0.005i, if the imaginary part is < 0.02i. These results are in accordance with the classic approach of simulation studies with synthetic particle size distributions. Major difficulties are found with a particle effective radius of < 0.15 mu m. In that case the complex refractive index may not be derived with sufficient accuracy. The eigenvalue analysis also shows that the accuracy of the derived parameters degrades if the imaginary part is > 0.02i, Furthermore it shows the importance of the simultaneous use of backscatter and extinction coefficients for the retrieval of microphysical parameters. (c) 2005 Optical Society of America. C1 Phys Instrumentat Ctr, Moscow 142190, Russia. Inst Tropospher Res, D-04318 Leipzig, Germany. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Veselovskii, I (reprint author), Phys Instrumentat Ctr, Moscow 142190, Russia. EM irgorv@pic.troitsk.ru; detlef@tropos.de; david.n.whiteman@nasa.gov RI MUELLER, DETLEF/F-1010-2015 OI MUELLER, DETLEF/0000-0002-0203-7654 NR 19 TC 37 Z9 43 U1 0 U2 4 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD SEP 1 PY 2005 VL 44 IS 25 BP 5292 EP 5303 DI 10.1364/AO.44.005292 PG 12 WC Optics SC Optics GA 960FH UT WOS:000231575100017 PM 16149352 ER PT J AU Das, V Crenshaw, DM Hutchings, JB Deo, RP Kraemer, SB Gull, TR Kaiser, ME Nelson, CH Weistrop, D AF Das, V Crenshaw, DM Hutchings, JB Deo, RP Kraemer, SB Gull, TR Kaiser, ME Nelson, CH Weistrop, D TI Mapping the kinematics of the narrow-line region in the Seyfert galaxy NGC 4151 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : individual ( NGC 4151); galaxies : kinematics and dynamics; galaxies : Seyfert; ISM : jets and outflows; ultraviolet : galaxies ID NGC 4151; EMISSION; SPECTROSCOPY; NGC-1068 AB Using the Hubble Space Telescope (HST) Space Telescope Imaging Spectrograph (STIS), observations of the [O III] emission from the narrow-line region (NLR) of NGC 4151 were obtained and radial velocities determined. Five orbits of HST time were used to obtain spectra at five parallel slit configurations at a position angle of 58 degrees, with spatial resolution 0.''2 across and 0."1 along each slit. A spectral resolving power (Delta lambda/lambda) of similar to 9000 with the G430M grating gave velocity measurements accurate to similar to 34 km s(-1). A kinematic model was generated to match the radial velocities for comparison to previous kinematic models of biconical radial outflow developed for low-dispersion spectra at two slit positions. The new high-resolution spectra permit the measurement of accurate velocity dispersions for each radial velocity component. The FWHM reaches a maximum of 1000 km s(-1) near the nucleus and generally decreases with increasing distance to about 100 km s(-1) in the extended NLR, starting at about 600 from the nucleus. In addition to the bright emission knots, which generally fit our model, there are faint high-velocity clouds that do not fit the biconical outflow pattern of our kinematic model. These faint clouds occur at the turnover points of the outflowing bright clouds. We suggest possible scenarios that could explain these rogue clouds: ( 1) backflow resulting from shocks and ( 2) outflow outside of the bicones, although the latter does not explain how the knots are ionized and accelerated. A comparison of our observations with a high-resolution radio map shows that there is no evidence that the kinematics of the NLR clouds are affected by the radio lobes that comprise the inner jet. C1 Georgia State Univ, Dept Phys & Astron, Astron Off, Atlanta, GA 30303 USA. Natl Res Council Canada, Herzberg Inst Astrophys, Dominion Astrophys Observ, Victoria, BC V9E 2E7, Canada. NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. Catholic Univ Amer, Washington, DC 20064 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA. Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. RP Georgia State Univ, Dept Phys & Astron, Astron Off, 1 Pk Pl South SE,Suite 700, Atlanta, GA 30303 USA. EM das@chara.gsu.edu; crenshaw@chara.gsu.edu; john.hutchings@nrc-cnrc.gc.ca; deo@chara.gsu.edu; stiskraemer@yancey.gsfc.nasa.gov; theodore.r.gull@nasa.gov; kaiser@pha.jhu.edu; charles.nelson@drake.edu; weistrop@physics.unlv.edu RI Gull, Theodore/D-2753-2012 OI Gull, Theodore/0000-0002-6851-5380 NR 14 TC 88 Z9 89 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD SEP PY 2005 VL 130 IS 3 BP 945 EP 956 DI 10.1086/432255 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958LX UT WOS:000231450900006 ER PT J AU Fitzpatrick, EL Massa, D AF Fitzpatrick, EL Massa, D TI An analysis of the shapes of ultraviolet extinction curves. IV. Extinction without standards SO ASTRONOMICAL JOURNAL LA English DT Article DE dust, extinction; methods : data analysis; stars : abundances; stars : atmospheres ID INTERSTELLAR EXTINCTION; UV EXTINCTION; PHYSICAL-PROPERTIES; B-STARS; FAR-UV; H-I; CLOUD; DUST; RECALIBRATION; ABSORPTION AB In this paper we present a new method for deriving UV through IR extinction curves, based on the use of stellar atmosphere models to provide estimates of the intrinsic (i.e., unreddened) stellar spectral energy distributions ( SEDs), rather than unreddened ( or lightly reddened) standard stars. We show that this ''extinction without standards'' technique greatly increases the accuracy of the derived extinction curves and allows realistic estimations of the uncertainties. An additional benefit of the technique is that it simultaneously determines the fundamental properties of the reddened stars themselves, making the procedure valuable for both stellar and interstellar studies. Given the physical limitations of the models we currently employ, the technique is limited to main-sequence and mildly evolved B stars. However, in principle, it can be adapted to any class of star for which accurate model SEDs are available and for which the signatures of interstellar reddening can be distinguished from those of the stellar parameters. We demonstrate how the extinction without standards curves make it possible to ( 1) study the uniformity of curves in localized spatial regions with unprecedented precision, ( 2) determine the relationships between different aspects of curve morphology, ( 3) produce high-quality extinction curves from low color excess sight lines, and ( 4) derive reliable extinction curves for mid to late B stars, thereby increasing spatial coverage and allowing the study of extinction in open clusters and associations dominated by such stars. The application of this technique to the available database of UV through IR SEDs, and to future observations, will provide valuable constraints on the nature of interstellar grains and on the processes that modify them, and it will enhance our ability to remove the multiwave-length effects of extinction from astronomical energy distributions. C1 Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA. NASA, Goddard Space Flight Ctr, SGT Inc, Greenbelt, MD 20771 USA. RP Fitzpatrick, EL (reprint author), Villanova Univ, Dept Astron & Astrophys, 800 Lancaster Ave, Villanova, PA 19085 USA. EM fitz@astronomy.villanova.edu; massa@derckmassa.net NR 31 TC 34 Z9 34 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 2005 VL 130 IS 3 BP 1127 EP 1140 DI 10.1086/431900 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958LX UT WOS:000231450900017 ER PT J AU Doppmann, GW Greene, TP Covey, KR Lada, CJ AF Doppmann, GW Greene, TP Covey, KR Lada, CJ TI The physical natures of Class I and flat-spectrum protostellar photospheres: A near-infrared spectroscopic study SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared : stars; stars : formation; stars : fundamental parameters; stars : late-type; stars : low-mass, brown dwarfs; stars : pre-main-sequence; stars : rotation; techniques : spectroscopic ID YOUNG STELLAR OBJECTS; T-TAURI STARS; AURIGA MOLECULAR CLOUD; MAIN-SEQUENCE STARS; MAGNETOSPHERIC ACCRETION MODELS; SCORPIUS OB ASSOCIATION; INITIAL MASS FUNCTION; CO EMISSION; RADIAL-VELOCITIES; IRAS OBSERVATIONS AB We present high-resolution (R similar or equal to 18,000), high signal-to-noise ratio, 2 mu m spectra of 52 IR-selected Class I and flat-spectrum young stellar objects in the Taurus-Auriga, rho Ophiuchi, Serpens, Perseus, and Corona Australis dark clouds. We detect key absorption lines in 41 objects and fit synthetic spectra generated from pre-main-sequence models to deduce the effective temperatures, surface gravities, near-IR veilings, rotation velocities, and radial velocities of each of these 41 sources. We find these objects to span ranges in effective temperature, surface gravity, and stellar luminosity that appear similar to those of late spectral type Class II sources and classical T Tauri stars. However, because of significant but uncertain corrections for scattering and extinction, the derived luminosities for the embedded protostellar objects must be regarded as being highly uncertain. We determine that the mean 2 mu m veiling of Class I and flat-spectrum objects is significantly higher than that of Class II objects in the same region where both types of objects are extensively observed (rho Oph). We find that a significant fraction of our protostellar sample also exhibits emission lines. Twenty-three objects show H-2 emission, which is usually indicative of the presence of energetic outflows. Thirty-four sources show H I Br gamma emission, and a number of these exhibit profile asymmetries consistent with infall. Eight sources show significant Delta(v) = 2 CO emission suggestive of emission from a circumstellar disk. Overall, these observations indicate that Class I and flat-spectrum objects are self-embedded protostars undergoing significant mass accretion, although the objects appear to span a broad range of mass accretion activity. C1 NASA, Ames Res Ctr, Moffett Field, CA USA. Univ Washington, Dept Astron, Seattle, WA 98195 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Assoc Univ Res Astron Inc, Gemini Observ, So Operat Ctr, Casilla 603, La Serena, Chile. EM doppmann@gemini.edu; thomas.p.greene@nasa.gov; covey@.astro.washington.edu; clada@cfa.harvard.edu OI Covey, Kevin/0000-0001-6914-7797 NR 90 TC 69 Z9 69 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD SEP PY 2005 VL 130 IS 3 BP 1145 EP 1170 DI 10.1086/431954 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958LX UT WOS:000231450900019 ER PT J AU Carson, JC Eikenberry, SS Brandl, BR Wilson, JC Hayward, TL AF Carson, JC Eikenberry, SS Brandl, BR Wilson, JC Hayward, TL TI The Cornell High-Order Adaptive Optics Survey for brown dwarfs in stellar systems. I. Observations, data reduction, and detection analyses SO ASTRONOMICAL JOURNAL LA English DT Article DE instrumentation : adaptive optics; instrumentation : high angular resolution; methods : data analysis; stars : low-mass, brown dwarfs; surveys; techniques : high angular resolution ID DIGITAL SKY SURVEY; SURVEY COMMISSIONING DATA; EXTRASOLAR GIANT PLANETS; T-DWARFS; SPECTRAL CLASSIFICATION; INFRARED CAMERA; DISCOVERY; METHANE; COMPANIONS; SEARCH AB In this first of a two-paper sequence, we report techniques and results of the Cornell High-Order Adaptive Optics Survey ( CHAOS) for brown dwarf companions. At the time of this writing, this study represents the most sensitive published population survey of brown dwarf companions to main-sequence stars for separations akin to our own outer solar system. The survey, conducted using the Palomar 200 inch ( 5 m) Hale Telescope, consists of K-s coronagraphic observations of 80 main-sequence stars out to 22 pc. At 100 separation from a typical target system, the survey achieves median sensitivities 10 mag fainter than the parent star. In terms of companion mass, the survey achieves typical sensitivities of 25M(J) (1 Gyr), 50M(J) ( solar age), and 60M(J) ( 10 Gyr), using the evolutionary models of Baraffe and coworkers. Using common proper motion to distinguish companions from field stars, we find that no systems show positive evidence of a substellar companion (searchable separation similar to 1'' - 15''; projected separation similar to 10 - 155 AU at the median target distance). In the second paper of the series we will present our Monte Carlo population simulations. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 183-900, Pasadena, CA 91109 USA. NR 35 TC 21 Z9 21 U1 0 U2 1 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 SEP PY 2005 VL 130 IS 3 BP 1212 EP 1220 DI 10.1086/432604 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958LX UT WOS:000231450900024 ER PT J AU Debes, JH Sigurdsson, S Woodgate, BE AF Debes, JH Sigurdsson, S Woodgate, BE TI Cool customers in the stellar graveyard. II. Limits to substellar objects around nearby DAZ white dwarfs SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; infrared : stars; planetary systems; stars : low-mass, brown dwarfs; white dwarfs ID METAL ABUNDANCE PATTERNS; LOW-MASS STARS; EXTRASOLAR GIANT PLANETS; BROWN DWARF; EVOLUTIONARY MODELS; LUMINOSITY FUNCTION; T-DWARFS; COMPANION; ACCRETION; SYSTEMS AB Results from a concerted Hubble Space Telescope (HST) survey of nearby white dwarfs for substellar objects are presented. A total of seven DAZ white dwarfs with distances of < 50 pc had high-contrast and high spatial resolution NICMOS coronagraphic images taken to search for candidate substellar objects at separations <= 10'' away. Limits to unresolved companions are derived through analysis of Two Micron All Sky Survey photometry of the white dwarfs compared to expected fluxes based on the white dwarf's effective temperature, distance, and gravity. Our HST survey of seven DAZ white dwarfs identified candidate companions for four of the white dwarfs. For three of these, HST and ground-based second-epoch observations showed the candidates to be background stars. The fourth white dwarf, which is close to the Galactic plane, has seven candidate companions at distances of 2''-4'', which remain to be followed up. We find that for four of the white dwarfs we are sensitive to planetary companions of >= 10M(J). For all the targets, we are sensitive to companions of > 18M(J). The lack of significant near-IR excesses for our targets limits any kind of unresolved companions present to be substellar. In light of these results we make several comments on the possibility of determining the origin of metals in the atmospheres of these white dwarfs. C1 Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. RI Woodgate, Bruce/D-2970-2012; OI Sigurdsson, Steinn/0000-0002-8187-1144 NR 60 TC 20 Z9 20 U1 0 U2 1 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 SEP PY 2005 VL 130 IS 3 BP 1221 EP 1230 DI 10.1086/432660 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958LX UT WOS:000231450900025 ER PT J AU Pandey, JC Singh, KP Drake, SA Sagar, R AF Pandey, JC Singh, KP Drake, SA Sagar, R TI Optical and X-ray studies of chromospherically active stars: FR Cancri, HD 95559, and LO Pegasi SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : general; stars : activity; stars : individual ( FR Cancri, LO Pegasi, HD 95559); X-rays : stars ID RS-CANUM-VENATICORUM; EINSTEIN SLEW SURVEY; ALL-SKY SURVEY; DRACONIS VARIABLES; RADIO-CONTINUUM; BINARY-SYSTEMS; SOURCE CATALOG; CVN BINARIES; AB-DORADUS; VLA SURVEY AB We present a multiwavelength study of three chromospherically active stars, namely, FR Cnc (BD + 16 degrees 1753), HD 95559, and LO Peg ( BD + 22 degrees 4409), including newly obtained optical photometry and low-resolution optical spectroscopy for FR Cnc, as well as archival IR and X-ray observations. The BVR photometry carried out from 2001 to 2004 has found significant photometric variability to be present in all three stars. For FR Cnc, a photometric period of 0: 8267 +/- 0.0004 days has been established. The strong variation in the phase and amplitude of the FR Cnc light curves when folded on this period implies the presence of evolving and migrating spots or spot groups on its surface. Two independent spots with migration periods of 0.97 and 0.93 yr, respectively, are inferred. The photometry of HD 95559 suggests the formation of a spot ( group) during the interval of our observations. We infer the existence of two independent spots or groups in the photosphere of LO Peg, one of which has a migration period of 1.12 yr. The optical spectroscopy of FR Cnc carried out during 2002 - 2003 reveals the presence of strong and variable Ca II H and K, H beta, and H alpha emission features indicative of a high level of chromospheric activity. The value of 5.3 for the ratio of the excess emission in H alpha to H beta, E-H alpha/E-H beta, suggests that the chromospheric emission may arise from an extended off-limb region. We have searched for the presence of color excesses in the near-IR JHK bands of these stars using Two Micron All Sky Survey data, but none of them appear to have any significant color excess. We have also analyzed archival X-ray observations of HD 95559 and LO Peg carried out with the ROSAT observatory. The best-fit models to their X-ray spectra imply the presence of two coronal plasma components of differing temperatures and with subsolar metal abundances. The inferred emission measures and temperatures of these systems are similar to those found for other active dwarf stars. The kinematics of FR Cnc suggest that it is a very young ( 35 - 55 Myr) main-sequence star and a possible member of the IC 2391 supercluster. LO Peg also has young disk-type kinematics and has been previously suggested to be a member of the 100 Myr old Local Association (Pleiades moving group). The kinematics of HD 95559 indicate it is a possible member of the 600 Myr old Hyades supercluster. C1 Aryabhatta Res Inst Observat Sci, Naini Tal 263129, India. Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. Univ Space Res Assoc, Lanham, MD 20706 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Aryabhatta Res Inst Observat Sci, Naini Tal 263129, India. NR 60 TC 9 Z9 10 U1 0 U2 1 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 SEP PY 2005 VL 130 IS 3 BP 1231 EP 1246 DI 10.1086/432539 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958LX UT WOS:000231450900026 ER PT J AU Rigopoulou, D Vacca, WD Berta, S Franceschini, A Aussel, H AF Rigopoulou, D Vacca, WD Berta, S Franceschini, A Aussel, H TI FORS spectroscopy of galaxies in the Hubble Deep Field-South SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology : observations; surveys; galaxies : luminosity function, mass function; galaxies : starburst ID LUMINOSITY FUNCTION; STAR-FORMATION; REDSHIFT SURVEY; HDF-S; IR; EVOLUTION; REGION; COUNTS AB We present low resolution multi-object spectroscopy of an I-band magnitude limited (I-AB similar or equal to 23-23.5) sample of galaxies located in an area centered on the Hubble Deep Field-South (HDFS). The observations were obtained using the Focal Reducer/low dispersion Spectrograph ( FORS) on the ESO Very Large Telescope. Thirty-two primary spectroscopic targets in the HST-WFPC2 HDFS were supplemented with galaxies detected in the Infrared Space Observatory's survey of the HDFS and the ESO Imaging Deep Survey to comprise a sample of 100 galaxies for spectroscopic observations. Based on detections of several emission lines, such as [OII]lambda 3727, H-beta and [OIII]lambda 5007, or of other spectroscopic features, we measured accurate redshifts for 50 objects in the central HDFS and flanking fields. The redshift range of the current sample of galaxies is 0.6-1.2, with a median redshift of 1.13 (at I similar or equal to 23.5 not corrected for completeness). The sample is dominated by starburst galaxies with only a small fraction of ellipticals (similar to 10%). For the emission line objects, the extinction corrected [OII]lambda 3727 line strengths yield estimates of star formation rates in the range 0.5-30 M circle dot yr(-1). We used the present data to derive the [OII]lambda 3727 luminosity function up to redshift of 1.2. When combined with [OII]lambda 3727 luminosity densities for the local and high redshift Universe, our results confirm the steep rise in the star formation rate (SFR) to z similar or equal to 1.3. C1 Univ Oxford, Oxford OX1 3RH, England. MPE, D-85741 Garching, Germany. NASA, Ames Res Ctr, USRA, Moffett Field, CA 94035 USA. Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. Inst Astron, Honolulu, HI 96822 USA. RP Rigopoulou, D (reprint author), Univ Oxford, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England. EM dar@astro.ox.ac.uk NR 30 TC 10 Z9 10 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2005 VL 440 IS 1 BP 61 EP U32 DI 10.1051/0004-6361:20034109 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 957GO UT WOS:000231358000012 ER PT J AU Ruiterkamp, R Peeters, Z Moore, MH Hudson, RL Ehrenfreund, P AF Ruiterkamp, R Peeters, Z Moore, MH Hudson, RL Ehrenfreund, P TI A quantitative study of proton irradiation and UV photolysis of benzene in interstellar environments SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM : molecules; ISM : abundances; ISM : clouds ID POLYCYCLIC AROMATIC-HYDROCARBONS; ULTRAVIOLET PHOTOLYSIS; MOLECULAR CLOUDS; MATRIX-ISOLATION; RADIATION-FIELD; ION IRRADIATION; ICE MIXTURES; RELEVANT; TEMPERATURES; ENVELOPES AB Benzene is an essential intermediate in the formation pathways of polycyclic aromatic hydrocarbons (PAHs) and carbon dust. Therefore, it is important to understand the interplay of formation and destruction in order to assess the lifetime of benzene in space. We performed UV photolysis and proton (0.8 MeV) bombardment experiments on benzene (C6H6) isolated in inert argon matrices and in oxygen-rich solid mixtures in the laboratory. The destruction of benzene in different chemical environments was measured for both methods of energetic processing. Additionally, we quantitatively determined the absorbed photon fraction in the sample layers when exposed to our UV lamp with actinometry. This enabled us to derive destruction cross sections for benzene for both UV photolysis and proton bombardment allowing us to compare these two ways of energetic processing. The laboratory data were extrapolated to different interstellar environments and we found that benzene is efficiently destroyed in diffuse interstellar clouds, but could survive dense cloud environments longer than the average lifetime of the cloud. Benzene is likely to survive in the dense parts of circumstellar envelopes around carbon-rich AGB stars but only in a very finite region where UV photons are attenuated. C1 Leiden Observ, NL-2300 RA Leiden, Netherlands. Leiden Inst Chem, Astrobiol Lab, NL-2300 RA Leiden, Netherlands. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Eckerd Coll, Dept Chem, St Petersburg, FL 33733 USA. RP Ruiterkamp, R (reprint author), Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM ruiterka@strw.leidenuniv.nl RI Hudson, Reggie/E-2335-2012 NR 41 TC 24 Z9 25 U1 0 U2 7 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2005 VL 440 IS 1 BP 391 EP 402 DI 10.1051/0004-6361:20042090 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 957GO UT WOS:000231358000041 ER PT J AU Smith, IA Tilanus, RPJ Tanvir, N Wijers, RAMJ Vreeswijk, P Rol, E Kouveliotou, C AF Smith, IA Tilanus, RPJ Tanvir, N Wijers, RAMJ Vreeswijk, P Rol, E Kouveliotou, C TI SCUBA sub-millimeter observations of gamma-ray bursts - III. GRB 030329: the brightest sub-millimeter afterglow to date SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma rays : bursts; submillimeter ID 29 MARCH 2003; IC HYPERNOVA SN-2003DH/GRB-030329; BROAD-BAND AFTERGLOW; OPTICAL AFTERGLOW; FIREBALL MODEL; HOST GALAXIES; LIGHT-CURVE; SUPERNOVA 2003DH; GRB 970508; EVOLUTION AB We present all the Target of Opportunity (ToO) sub-millimeter observations of GRB 030329 taken by the millimetre Common-User Bolometer Array ( SCUBA) on the James Clerk Maxwell Telescope (JCMT). This was by far the brightest sub-millimeter afterglow seen to date. The flux density at 850 mu m was approximately constant up to a break that took place similar to 7 days after the burst. This was consistent with being a jet break. The 850 mu m results agree with those at longer wavelengths that show a brighter flux similar to 7 days after the burst, right at the time of the break. No short-lived large-scale brightenings were detected in the sub-millimeter light curve. However, the 850 mu m light curve may have had a drop less than or similar to 16 days after the burst. The peak of the afterglow emission was at similar to 90 GHz in the days before the break in the light curve. A simple modeling is consistent with the spectral indices remaining the same as the afterglow evolved, with the breaks in the spectrum moving to longer wavelengths at later times and the flux at the peak falling. No significant sub-millimeter emission was detected from the host galaxy. C1 Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA. Joint Astron Ctr, Hilo, HI 96720 USA. Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Ctr High Energy Astrophys, NL-1098 SJ Amsterdam, Netherlands. European So Observ, Santiago 19001, Chile. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. NASA, Marshall Space Flight Ctr, NSSTC, Huntsville, AL 35805 USA. Univ Space Res Assoc, Columbia, MD 21044 USA. RP Smith, IA (reprint author), Rice Univ, Dept Phys & Astron, 6100 S Main,MS-108, Houston, TX 77005 USA. EM iansmith@rice.edu OI Wijers, Ralph/0000-0002-3101-1808 NR 64 TC 9 Z9 9 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2005 VL 439 IS 3 BP 981 EP 986 DI 10.1051/0004-6361:20053106 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 955EA UT WOS:000231206900017 ER PT J AU Smith, IA Tilanus, RPJ Tanvir, N Barnard, VE Moriarty-Schieven, GH Frail, DA Wijers, RAMJ Vreeswijk, P Rol, E Kouveliotou, C AF Smith, IA Tilanus, RPJ Tanvir, N Barnard, VE Moriarty-Schieven, GH Frail, DA Wijers, RAMJ Vreeswijk, P Rol, E Kouveliotou, C TI SCUBA sub-millimeter observations of gamma-ray bursts - IV. GRB 021004, 021211, 030115, 030226, 041006 SO ASTRONOMY & ASTROPHYSICS LA English DT Review DE gamma rays : bursts; submillimeter ID WIND-INTERACTION-MODELS; EARLY OPTICAL-EMISSION; BROAD-BAND AFTERGLOW; STAR-FORMATION; HOST GALAXIES; FIREBALL MODEL; GRB 970508; RADIO AFTERGLOWS; DISCOVERY; REDSHIFT AB We discuss our ongoing program of Target of Opportunity (ToO) sub-millimeter observations of gamma-ray bursts (GRBs) using the Sub-millimetre Common-User Bolometer Array ( SCUBA) on the James Clerk Maxwell Telescope (JCMT). In this paper, we present the ToO observations of GRBs 021004, 021211, 030115, 030226, and 041006. The observations of GRBs 021004, 021211, 030226, and 041006 all started within similar to 1 day of the burst, but did not detect any significant sub-millimeter emission from the reverse shock and/or afterglow. These observations put some constraints on the models for the early emission, although the generally poor observing conditions and/or the faintness of these afterglows at other wavelengths limit the inferences that can be drawn from these lack of detections. However, these observations demonstrate that SCUBA can perform rapid observations of GRBs, and provide encouragement for future observations in the Swift era. None of these GRBs had significant sub-millimeter emission from their host galaxies. This adds to the indication that GRBs are not closely linked to the most luminous dusty star-forming galaxies. C1 Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA. Joint Astron Ctr, Hilo, HI 96720 USA. Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. Natl Radio Astron Observ, Socorro, NM 87801 USA. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Ctr High Energy Astrophys, NL-1098 SJ Amsterdam, Netherlands. European So Observ, Santiago 19001, Chile. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. NASA, Marshall Space Flight Ctr, NSSTC, Huntsville, AL 35805 USA. Univ Space Res Assoc, Columbia, MD 21044 USA. RP Smith, IA (reprint author), Rice Univ, Dept Phys & Astron, 6100 S Main,MS-108, Houston, TX 77005 USA. EM iansmith@rice.edu OI Wijers, Ralph/0000-0002-3101-1808 NR 125 TC 16 Z9 16 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2005 VL 439 IS 3 BP 987 EP 996 DI 10.1051/0004-6361:20053107 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 955EA UT WOS:000231206900018 ER PT J AU Zirm, AW Overzier, RA Miley, GK Blakeslee, JP Clampin, M De Breuck, C Demarco, R Ford, HC Hartig, GF Homeier, N Illingworth, GD Martel, AR Rottgering, HJA Venemans, B Ardila, DR Bartko, F Benitez, NB Bouwens, RJ Bradley, LD Broadhurst, TJ Brown, RA Burrows, CJ Cheng, ES Cross, NJG Feldman, PD Franx, M Golimowski, DA Goto, T Gronwall, C Holden, B Infante, L Kimble, RA Krist, JE Lesser, MP Mei, S Menanteau, F Meurer, GR Motta, V Postman, M Rosati, P Sirianni, M Sparks, WB Tran, HD Tsvetanov, ZI White, RL Zheng, W AF Zirm, AW Overzier, RA Miley, GK Blakeslee, JP Clampin, M De Breuck, C Demarco, R Ford, HC Hartig, GF Homeier, N Illingworth, GD Martel, AR Rottgering, HJA Venemans, B Ardila, DR Bartko, F Benitez, NB Bouwens, RJ Bradley, LD Broadhurst, TJ Brown, RA Burrows, CJ Cheng, ES Cross, NJG Feldman, PD Franx, M Golimowski, DA Goto, T Gronwall, C Holden, B Infante, L Kimble, RA Krist, JE Lesser, MP Mei, S Menanteau, F Meurer, GR Motta, V Postman, M Rosati, P Sirianni, M Sparks, WB Tran, HD Tsvetanov, ZI White, RL Zheng, W TI Feedback and brightest cluster galaxy formation: ACS observations of the radio galaxy TNJ J1338-1942 AT z=4.1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : halos; galaxies : high-redshift; galaxies : individual (TN J1338-1942) ID LYMAN-BREAK GALAXIES; EMISSION-LINE PROPERTIES; JET-CLOUD INTERACTIONS; LY-ALPHA EMITTERS; X-RAY SURVEY; K-Z RELATION; HIGH-REDSHIFT; STAR-FORMATION; GALACTIC SUPERWINDS; KECK SPECTROPOLARIMETRY AB We present deep optical imaging of the z 4: 1 radio galaxy TN J1338 - 1942, obtained using the Advanced Camera for Surveys ( ACS) on board the Hubble Space Telescope, as well as ground- based near- infrared imaging data from the European Southern Observatory ( ESO) Very Large Telescope ( VLT). The radio galaxy is known to reside within a large galaxy overdensity ( both in physical extent and density contrast). There is good evidence that this `` protocluster'' region is the progenitor of a present- day rich galaxy cluster. TN J1338 is the dominant galaxy in the protocluster in terms of size and luminosity ( in both the optical and near- infrared) and therefore seems destined to evolve into the brightest cluster galaxy. The high spatial resolution ACS images reveal several kiloparsec- scale features within and around the radio galaxy. The continuum light is aligned with the radio axis and is resolved into two clumps in the i(775) and z(850) bands. These components have luminosities similar to 10(9) L-circle dot and sizes of a few kpc. The estimated nebular continuum, scattered light, synchrotron- and inverse Compton - scattering contributions to the aligned continuum light are only a few percent of the observed total, indicating that the observed flux is likely dominated by forming stars. The estimated star formation rate for the whole radio galaxy is similar to 200M(circle dot) yr(-1). A simple model in which the jet has triggered star formation in these continuum knots is consistent with the available data. A striking, but small, linear feature is evident in the z850 aligned light and may be indicative of a large- scale shock associated with the advance of the radio jet. The rest of the aligned light also seems morphologically consistent with star formation induced by shocks associated with the radio source, as seen in other high- z radio galaxies ( e. g., 4C 41.17). An unusual feature is seen in Ly alpha emission. A wedge- shaped extension emanates from the radio galaxy perpendicularly to the radio axis. This `` wedge'' naturally connects to the surrounding asymmetric, large- scale (similar to 100 kpc) Ly alpha halo. We posit that the wedge is a starburst- driven superwind associated with the first major epoch of formation of the brightest cluster galaxy. The shock and wedge are examples of feedback processes due to both active galactic nucleus and star formation in the earliest stages of massive galaxy formation. C1 Leiden Observ, NL-2300 RA Leiden, Netherlands. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. European So Observ, D-85748 Garching, Germany. Space Telescope Sci Inst, Baltimore, MD 21218 USA. CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. Conceptual Analyt LLC, Glenn Dale, MD 20769 USA. Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. WM Keck Observ, Kamuela, HI 96743 USA. RP Leiden Observ, Postbus 9513, NL-2300 RA Leiden, Netherlands. RI White, Richard/A-8143-2012; Clampin, mark/D-2738-2012; Kimble, Randy/D-5317-2012 NR 96 TC 32 Z9 32 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2005 VL 630 IS 1 BP 68 EP 81 DI 10.1086/431921 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958JD UT WOS:000231439700006 ER PT J AU Barsony, M Ressler, ME Marsh, KA AF Barsony, M Ressler, ME Marsh, KA TI A mid-infrared imaging survey of embedded young stellar objects in the p Ophiuchi cloud core SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; ISM : individual (p Ophiuchi cloud); planetary systems : protoplanetary disks; stars : formation; stars : pre; main-sequence; surveys ID MAIN-SEQUENCE STARS; T-TAURI STARS; SPECTRAL ENERGY-DISTRIBUTIONS; INFRARED MULTIPLICITY SURVEY; TRIPLE SYSTEM WL-20; HERBIG AE/BE STARS; X-RAY SOURCES; RHO-OPHIUCHI; DARK CLOUD; IRAS OBSERVATIONS AB Results of a comprehensive, new, ground-based mid-infrared imaging survey of the young stellar population of the rho Ophiuchi cloud are presented. Data were acquired at the Palomar 5 m and at the Keck 10 m telescopes with the MIRLIN and LWS instruments, at 0".5 and 0".25 resolutions, respectively. Of 172 survey objects, 85 were detected. Among the 22 multiple systems observed, 15 were resolved and their individual component fluxes determined. A plot of the frequency distribution of the detected objects with SED spectral slope shows that YSOs spend similar to 4 x 10(5) yr in the flat-spectrum phase, clearing out their remnant infall envelopes. Mid-infrared variability is found among a significant fraction of the surveyed objects and is found to occur for all SED classes with optically thick disks. Large-amplitude near-infrared variability, also found for all SED classes with optically thick disks, seems to occur with somewhat higher frequency at the earlier evolutionary stages. Although a general trend of mid-infrared excess and near-infrared veiling exists progressing through SED classes, with Class I objects generally exhibiting r(K) >= 1, flat-spectrum objects with r(K) >= 0.58, and Class III objects with r(K) = 0, Class II objects exhibit the widest range of r(K) values, ranging from 0 <= r(K) <= 4: 5. However, the highly variable value of veiling that a single source can exhibit in any of the SED classes in which active disk accretion can take place is striking and is direct observational evidence for highly time-variable accretion activity in disks. Finally, by comparing mid-infrared versus near-infrared excesses in a subsample with well-determined effective temperatures and extinction values, disk-clearing mechanisms are explored. The results are consistent with disk clearing proceeding from the inside out. C1 Univ Calif San Francisco, Dept Phys & Astron, San Francisco, CA 94121 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA. EM mbarsony@stars.sfsu.edu; michael.e.ressler@jpl.nasa.gov; michael.e.ressler@jpl.nasa.gov NR 51 TC 39 Z9 39 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 SEP 1 PY 2005 VL 630 IS 1 BP 381 EP 399 DI 10.1086/431351 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958JD UT WOS:000231439700029 ER PT J AU Baring, MG Gonthier, PL Harding, AK AF Baring, MG Gonthier, PL Harding, AK TI Spin-dependent cyclotron decay rates in strong magnetic fields SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : theory; magnetic fields; pulsars : general; radiation mechanisms : nonthermal; relativity; stars : neutron ID ELECTRON SELF-ENERGY; COMPTON-SCATTERING; QUANTUM ELECTRODYNAMICS; SYNCHROTRON RADIATION; EMISSION; LINE; TRANSITIONS; ABSORPTION AB Cyclotron decay and absorption rates have been well studied in the literature, focusing primarily on spectral, angular, and polarization dependence. Astrophysical applications usually do not require retention of information on the electron spin state, and these are normally averaged in obtaining the requisite rates. In magnetic fields, higher order quantum processes such as Compton scattering become resonant at the cyclotron frequency and its harmonics, with the resonances being formally divergent. Such divergences are usually eliminated by accounting for the finite lifetimes of excited Landau states. This practice requires the use of spin-dependent cyclotron rates in order to obtain accurate determinations of process rates very near cyclotronic resonances, the phase-space domain most relevant for certain applications to pulsar models. This paper develops previous results in the literature to obtain compact analytic expressions for cyclotron decay rates/widths in terms of a series of Legendre functions of the second kind; these expressions can be used expediently in astrophysical models. The rates are derived using two popular eigenstate formalisms, namely, that due to Sokolov & Ternov and that due to Johnson & Lippmann. These constitute two sets of eigenfunctions of the Dirac equation that diagonalize different operators and accordingly yield different spin-dependent cyclotron rates. This paper illustrates the attractive Lorentz transformation characteristics of the Sokolov & Ternov formulation, which is another reason why it is preferable when electron spin information must be explicitly retained. C1 Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA. Hope Coll, Dept Phys & Engn, Holland, MI 49422 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Baring, MG (reprint author), Rice Univ, Dept Phys & Astron, MS 108,POB 1892, Houston, TX 77251 USA. EM baring@rice.edu; gonthier@physics.hope.edu; harding@twinkie.gsfc.nasa.gov RI Harding, Alice/D-3160-2012 NR 34 TC 26 Z9 26 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 SEP 1 PY 2005 VL 630 IS 1 BP 430 EP 440 DI 10.1086/431895 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958JD UT WOS:000231439700033 ER PT J AU Muslimov, AG Harding, AK AF Muslimov, AG Harding, AK TI Effects of rotation and relativistic charge flow on pulsar magnetospheric structure SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars : general; stars : neutron ID RADIO-EMISSION GEOMETRY; PARTICLE-ACCELERATION; POLAR CAPS; SLOT GAPS; MODEL; PLASMA; POLARIZATION; SYSTEM; ELECTRODYNAMICS; RADIATION AB We propose an analytical three-dimensional model of the open field line region of a neutron star (NS) magnetosphere. We construct an explicit analytic solution for arbitrary obliquity ( angle between the rotation and magnetic axes) incorporating the effects of magnetospheric rotation, relativistic flow of charges ( e. g., primary electron beam) along the open field lines, and E x B drift of these charges. Our solution employs the space-charge-limited longitudinal current calculated in the electrodynamic model of Muslimov and Tsygan and is valid up to very high altitudes nearly approaching the light cylinder. We assume that in the innermost magnetosphere, the NS magnetic field can be well represented by a static magnetic dipole configuration. At high altitudes the open magnetic field lines significantly deviate from those of a static dipole and tend to focus into a cylindrical bundle, swept back in the direction opposite the rotation and bent toward the rotational equator. We briefly discuss some implications of our study to spin-powered pulsars. C1 NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Muslimov, AG (reprint author), ManTech Int Corp, 46610 Expedit Dr,Suite 101, Lexington Pk, MD 20653 USA. RI Harding, Alice/D-3160-2012 NR 44 TC 11 Z9 12 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 SEP 1 PY 2005 VL 630 IS 1 BP 454 EP 464 DI 10.1086/431735 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958JD UT WOS:000231439700035 ER PT J AU Long, KS Froning, CS Knigge, C Blair, WP Kallman, TR Ko, YK AF Long, KS Froning, CS Knigge, C Blair, WP Kallman, TR Ko, YK TI Far-ultraviolet spectroscopy of the dwarf novae SS cygni and WX Hydri in quiescence SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion; accretion disks; binaries : close; novae, cataclysmic variables; stars : individual ( SS Cygni, WX Hydri); ultraviolet : stars ID HIGH-RESOLUTION SPECTROGRAPH; DISC INSTABILITY MODEL; ROTATING WHITE-DWARF; LONG-TERM BEHAVIOR; U-GEMINORUM; CATACLYSMIC VARIABLES; X-RAY; ACCRETION DISK; VW-HYDRI; OPTICAL OBSERVATIONS AB We present time-resolved FUV spectra of the dwarf novae SS Cyg and WX Hyi in quiescence from observations using the Hopkins Ultraviolet Telescope on the Astro-1 and Astro-2 space shuttle missions and the Goddard High Resolution Spectrograph on the Hubble Space Telescope. Both dwarf novae are characterized by blue continua that extend to the Lyman limit punctuated by broad emission lines including transitions of O VI, N V, Si IV, andC IV. The continuum of WX Hyi can be fitted with a white dwarf model with physically reasonable model parameters, but neither system actually shows unambiguous signatures of white dwarf emission. The shape and flux of the spectrum of SS Cyg cannot be self-consistently reconciled with a white dwarf providing all of the FUV continuum flux. Combination white dwarf/disk or white dwarf/optically thin plasma models improve the fit but still do not give physically reasonable model parameters for a quiescent dwarf nova. Assuming that the UV emission lines arise from the disk, the line shapes indicate that surface fluxes fall roughly as R-2 in both systems. Fits to the double-peaked line profiles in SS Cyg indicate that the FUV line-forming region is concentrated closer to the white dwarf than that of the optical lines and provide no evidence of a hole in the inner disk. Although the flux from SS Cyg was relatively constant during all of our observations, WX Hyi showed significant variability during the GHRS observations. In WX Hyi, the line and continuum fluxes are (with the exception of He II) highly correlated, indicating a link between the formation mechanisms of the line and continuum regions. C1 Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM long@stsci.edu; cfroning@casa.colorado.edu; christian@astro.soton.ac.uk; wpb@pha.jhu.edu; tim@xstar.gsfc.nasa.gov; yko@cfa.harvard.edu NR 66 TC 19 Z9 19 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2005 VL 630 IS 1 BP 511 EP 527 DI 10.1086/432088 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958JD UT WOS:000231439700040 ER PT J AU Pravdo, SH Shaklan, SB Lloyd, J AF Pravdo, SH Shaklan, SB Lloyd, J TI Astrometric discovery of GJ 802b: In the brown dwarf oasis? SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : low-mass, brown dwarfs ID MASS-LUMINOSITY-RELATION; T-DWARFS; SPECTROSCOPIC SURVEY; SOLAR NEIGHBORHOOD; BINARY-SYSTEMS; STARS; SPECTRA; CATALOG; PARALLAXES; SEQUENCE AB The Stellar Planet Survey is an ongoing astrometric search for giant planets and brown dwarfs around a sample of similar to 30 M dwarfs. We have discovered several low-mass companions by measuring the motion of our target stars relative to their reference frames. The lowest mass discovery thus far is GJ 802b, a companion to the M5 dwarf GJ 802A. The orbital period is 3.14 +/- 0.03 yr, the system mass is 0.214 +/- 0.045 M-circle dot, and the semimajor axis is 1.28 +/- 0.10 AU or 81 +/- 6 mas. Imaging observations indicate that GJ 802b is likely to be a brown dwarf with the astrometrically determined mass 0.058 +/- 0.021 M-circle dot (1 sigma limits). The remaining uncertainty in the orbit is the eccentricity that is now loosely constrained. We discuss how the system age limits the mass and the prospects of further narrowing the mass range when e is more precisely determined. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP CALTECH, Jet Prop Lab, 306-431,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM spravdo@jpl.nasa.gov; shaklan@huey.jpl.nasa.gov; jpl@astro.cornell.edu RI Lloyd, James/B-3769-2011 NR 41 TC 25 Z9 25 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 SEP 1 PY 2005 VL 630 IS 1 BP 528 EP 534 DI 10.1086/431967 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958JD UT WOS:000231439700041 ER PT J AU Friedel, DN Remijan, AJ Snyder, LE A'Hearn, MF Blake, GA De Pater, I Dickel, HR Forster, JR Hogerheijde, MR Kraybill, C Looney, LW Palmer, P Wright, MCH AF Friedel, DN Remijan, AJ Snyder, LE A'Hearn, MF Blake, GA De Pater, I Dickel, HR Forster, JR Hogerheijde, MR Kraybill, C Looney, LW Palmer, P Wright, MCH TI BIMA array detections of HCN in comets linear C/2002 T7) and neat (C/2001 Q4) SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets : individual (C/2002 T7 (LINEAR), NEAT; (C/2001 Q4)); molecular processes; radio lines : solar system; techniques : interferometric ID BOPP C/1995 O1; HALE-BOPP; B2 HYAKUTAKE; HYDROGEN-CYANIDE; SPECTROSCOPY; RATES; WATER AB We present interferometric detections of HCN in comets LINEAR (C/2002 T7) and NEAT (C/2001 Q4) with the Berkeley-Illinois-Maryland Association (BIMA) array. With a 25.'' 4 X 20.'' 3 synthesized beam around comet LINEAR and using a variable temperature and outflow velocity (VTOV) model, we found an HCN column density of < N-T> = ( 6.4 +/- 2.1) X 10(12) cm(-2) and a production rate of Q( HCN) (6.5 +/- 2.2) X 10(26) s(-1), giving a production rate ratio of HCN relative to H2O of similar to( 3.3 +/- 1.1) X 10(-3) and relative to CN of similar to 4.6 +/- 1.5. With a 21.'' 3 X 17.'' 5 synthesized beam around comet NEAT and using a VTOV model, we found an HCN column density of < N-T> = (8.5 +/- 4.5) X 10(11) cm(-2) and a production rate of Q(HCN) (8.9 +/- 4.7) X 10(25) s(-1), giving a production rate ratio of HCN relative to H2O of similar to(7.4 +/- 3.9) X 10(-4) and relative to CN of similar to 0.3 +/- 0.2. For both comets, the production rates relative to H2O are similar to those found in previous comet observations. For comet LINEAR, the production rate relative to CN is consistent with HCN being the primary parent species of CN, while for comet NEAT it is too low for this to be the case. C1 Univ Illinois, Dept Astron, Urbana, IL 61801 USA. NASA Goddard Space Flight Ctr, Computat & Informat Sci & Technol Off, Greenbelt, MD 20771 USA. Univ Maryland, Dept Astron, College Pk, MD USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Leiden Observat, NL-2300 RA Leiden, Netherlands. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. RP Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. EM friedel@astro.uiuc.edu; aremijan@pop900.gsfc.nasa.gov; snyder@astro.uiuc.edu; ma@astro.umd.edu; gab@gps.caltech.edu; imke@floris.berkeley.edu; lanie@astrouiuc.edu; rforster@astro.berkeley.edu; michiel@strw.leidenuniv.nl; ckraybill@astro.berkeley.edu; lanie@astro.uiuc.edu; ppalmer@oskar.uchicago.edu; wright@astro.berkeley.edu NR 31 TC 15 Z9 15 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 SEP 1 PY 2005 VL 630 IS 1 BP 623 EP 630 DI 10.1086/432107 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958JD UT WOS:000231439700050 ER PT J AU Kimura, Y Nuth, JA AF Kimura, Y Nuth, JA TI Laboratory synthesized calcium oxide and calcium hydroxide grains: A candidate to explain the 6.8 mu m band SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM : molecules; methods : laboratory; molecular data ID ABSORPTION FEATURES; PROTOSTELLAR SOURCES; SPECTRUM; PROTOSTARS; ICE; SPECTROSCOPY; CHONDRITES; ORIGIN AB We demonstrate that CaO and Ca(OH)(2) are excellent candidates to explain the 6.8 mu m feature, which is one of the most obscure features in young stellar objects. We discuss the condensation of CaO grains and the potential formation of a Ca(OH)(2) surface layer. The infrared spectra of these grains are compared with the spectra of 15 young stellar objects. We note that CaO-rich grains are seen in all meteoritic CAIs (calcium-aluminum-rich inclusions) and that the 6.8 mu m feature has only been observed in young stellar objects. Therefore, we consider CaO grains to be a plausible candidate to explain the 6.8 mu m feature and hypothesize that they are produced in the hot interiors of young stellar environments. C1 NASA Goddard Space Flight Ctr, Solar Syst Exlplorat Div, Astrochem Lab, Greenbelt, MD 20771 USA. RP Kimura, Y (reprint author), NASA Goddard Space Flight Ctr, Solar Syst Exlplorat Div, Astrochem Lab, Code 691, Greenbelt, MD 20771 USA. RI Nuth, Joseph/E-7085-2012; Kimura, Yuki/J-9635-2014 OI Kimura, Yuki/0000-0002-9218-7663 NR 26 TC 6 Z9 6 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2005 VL 630 IS 1 BP 637 EP 641 DI 10.1086/431965 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958JD UT WOS:000231439700052 ER PT J AU Cannon, JM Walter, F Bendo, GJ Calzetti, D Dale, DA Draine, BT Engelbracht, CW Gordon, KD Helou, G Kennicutt, RC Murphy, EJ Thornley, MD Armus, L Hollenbach, DJ Leitherer, C Regan, MW Roussel, H Sheth, K AF Cannon, JM Walter, F Bendo, GJ Calzetti, D Dale, DA Draine, BT Engelbracht, CW Gordon, KD Helou, G Kennicutt, RC Murphy, EJ Thornley, MD Armus, L Hollenbach, DJ Leitherer, C Regan, MW Roussel, H Sheth, K TI Spitzer observations of the supergiant shell region in IC 2574 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : dwarf; galaxies : individual ( IC 2574); galaxies : irregular; galaxies : ISM; infrared : galaxies ID GROUP DWARF GALAXIES; H-II REGIONS; IC 2574; INTERSTELLAR-MEDIUM; MAGELLANIC-CLOUD; STAR-FORMATION; KINEMATICS; HOLES AB We present spatially resolved Spitzer Space Telescope imaging of the supergiant shell region of the M81 group dwarf galaxy IC 2574 obtained as part of the Spitzer Infrared Nearby Galaxies Survey. This region harbors one of the best nearby examples of a kinematically distinct H I shell, with an associated remnant stellar cluster; the shell is initiating sequential star formation as it interacts with the surrounding interstellar medium. This region dominates the infrared luminosity of IC 2574 and is spatially resolved in all Spitzer imaging bands. We study the differences in dust temperature as a function of local environment and compare local star formation rates as inferred from Ha and total infrared luminosities. We find that the strong Ha sources are associated with regions of warm dust; however, the most luminous infrared and Ha sources are not necessarily cospatial. The coolest dust is found in the regions farthest from the rim of the shell; these regions show the best agreement between star formation rates derived from Ha and from total infrared luminosities (although discrepancies at the factor of 3 - 4 level still exist). There is considerable variation in the radio-far-infrared correlation in different regions surrounding the shell. The low dust content of the region may influence the scatter seen in these relations; these data demonstrate that the expanding shell is dramatically affecting its surroundings by triggering star formation and altering the dust temperature. C1 Max Planck Inst Astron, D-69117 Heidelberg, Germany. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. Princeton Univ Observ, Princeton, NJ 08544 USA. CALTECH, Pasadena, CA 91101 USA. Yale Univ, Dept Astron, New Haven, CT 06520 USA. Bucknell Univ, Dept Phys, Lewisburg, PA 17837 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Cannon, JM (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM cannon@mpia.de; walter@mpia.de; gbendo@as.arizona.edu; calzetti@stsci.edu; ddale@uwyo.edu; draine@astro.princeton.edu; chad@as.arizona.edu; kgordon@as.arizona.edu; gxh@ipac.caltech.edu; robk@as.arizona.edu; murphy@astro.yale.edu; mthornle@bucknell.edu; lee@ipac.caltech.edu; hollenba@ism.arc.nasa.gov; leitherer@stsci.edu; mregan@stsci.edu; hroussel@irastro.caltech.edu; kartik@astro.caltech.edu OI Draine, Bruce/0000-0002-0846-936X NR 21 TC 29 Z9 29 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 SEP 1 PY 2005 VL 630 IS 1 BP L37 EP L40 DI 10.1086/491671 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958JG UT WOS:000231440000010 ER PT J AU Silverberg, RF Cheng, ES Aguirre, JE Bezaire, JJ Crawford, TM Meyer, SS Bier, A Campano, B Chen, TC Cottingham, DA Sharp, EH Christensen, PR Cordone, S Timbie, PT Dame, RE Fixsen, DJ Kristensen, RJK Norgaard-Nielsen, HU Wilson, GW AF Silverberg, RF Cheng, ES Aguirre, JE Bezaire, JJ Crawford, TM Meyer, SS Bier, A Campano, B Chen, TC Cottingham, DA Sharp, EH Christensen, PR Cordone, S Timbie, PT Dame, RE Fixsen, DJ Kristensen, RJK Norgaard-Nielsen, HU Wilson, GW TI The TopHat experiment: A balloon-borne instrument for mapping millimeter and submillimeter emission SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE balloons; cosmic microwave background; cosmology : observations; galaxies : general ID GALACTIC DUST EMISSION; BACKGROUND-RADIATION; ANISOTROPY; SPECTRUM; MAPS; BOOMERANG; NOISE AB The TopHat experiment was designed to measure the anisotropy in the cosmic microwave background radiation on angular scales from 0.degrees 3 to 30 degrees and the thermal emission from both Galactic and extragalactic dust. The balloon-borne instrument had five spectral bands spanning frequencies from 175 to 630 GHz. The telescope was a compact, 1 m, on-axis Cassegrain telescope designed to scan the sky at a fixed elevation of 78 degrees. The radiometer used cryogenic bolometers coupled to a single feed horn via a dichroic filter system. The observing strategy was intended to efficiently cover a region 48 degrees in diameter centered on the south polar cap with a highly cross-linked and redundant pattern with nearly uniform sky coverage. The Long Duration Balloon flight over Antarctica in 2001 January surveyed about 6% of the sky. Here we describe the design of the instrument and the achieved in-flight performance and provide a brief discussion of the data analysis. C1 NASA, Astron & Solar Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. NASA, GST, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. Mega Engn, Silver Spring, MD 20901 USA. NASA, SSAI, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Danish Space Res Inst, Copenhagen, Denmark. Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. RP Silverberg, RF (reprint author), NASA, Astron & Solar Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 20 TC 3 Z9 3 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 SEP PY 2005 VL 160 IS 1 BP 59 EP 75 DI 10.1086/432117 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958LY UT WOS:000231451000003 ER PT J AU Landi, E Phillips, KJH AF Landi, E Phillips, KJH TI Spectral atlas of X-ray lines emitted during solar flares based on Chianti SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE line : identification; plasmas; Sun : flares; Sun : X-rays, gamma rays ID DIELECTRONIC SATELLITE SPECTRA; OPTICALLY THIN PLASMAS; MAXIMUM-MISSION; ATOMIC DATABASE; EMISSION-LINES; IONS; DIAGNOSTICS; IRON; TEMPERATURE; RADIATION AB A spectral atlas of X-ray lines in the wavelength range 7.47-18.97 angstrom is presented, based on high-resolution spectra obtained during two M-class solar flares ( on 1980 August 25 and 1985 July 2) with the Flat Crystal Spectrometer on board the Solar Maximum Mission. The physical properties of the flaring plasmas are derived as a function of time using strong, unblended lines. From these properties, predicted spectra using the CHIANTI database have been obtained, which were then compared with wavelengths and fluxes of lines in the observed spectra to establish line identifications. Identifications for nearly all the observed lines in the resulting atlas are given, with some significant corrections to previous analyses of these flare spectra. Line ratios allowed us to determine temperature and density; in the 1985 July 2 flare, very high densities (N-e similar or equal to 10(13) cm(-3)) were measured. C1 Artep Inc, Ellicott City, MD 21042 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 21042 USA. RI Landi, Enrico/H-4493-2011 NR 30 TC 29 Z9 29 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 2005 VL 160 IS 1 BP 286 EP 311 DI 10.1086/431953 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958LY UT WOS:000231451000013 ER PT J AU Koscheyev, VS Coca, A Leon, GR Trevino, RC AF Koscheyev, VS Coca, A Leon, GR Trevino, RC TI Redirection of biological heat from head to hands to support finger comfort in the cold SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE biological heat redirection; head hand heat bypass; finger comfort ID TEMPERATURE; HYPERTHERMIA; EXPOSURE; EVA AB Introduction: Maintaining hand comfort in the cold while sustaining optimal performance is still a challenge. There has been little research on the efficacy of transporting biological heat from the head to the hands to stabilize finger comfort, although there are notable temperature differences between these two areas in the cold. Method: A tubing bypass between the head and the hands was designed as an independent component in a liquid cooling/warming garment (LCWG). Seven subjects (four men, three women) were studied, comparing finger temperature (T-fing) change in two conditions: LCWG with additional bypass; and LCWG without bypass. The protocol consisted of three stages: 1) comfort stabilization, LCWG inlet water temperature 33 degrees C, water in loop in bypass condition 23 degrees C; 2) body cooling, LCWG inlet water temperature 20 degrees C; and 3) rewarming, LCWG inlet water temperature 45 degrees C. Results: The time to reach the 25 degrees C Tfing discomfort criterion was significantly longer in the bypass condition (p < 0.01); Tfing was significantly higher at the same time point when T-fing of 25 degrees C was reached in the control condition (p < 0.01). Conclusion: The incorporation of a bypass transferring biological heat from a high to a low skin temperature area has potential to improve local finger comfort and thus increase the time personnel can work in cold environments. C1 Univ Minnesota, Dept Kinesiol, Lab Hlth & Human Performance Extreme Environm, Minneapolis, MN 55455 USA. Univ Minnesota, Dept Psychol, Minneapolis, MN 55455 USA. NASA, Johnston Space Ctr, Houston, TX USA. RP Koscheyev, VS (reprint author), Univ Minnesota, Dept Kinesiol, Lab Hlth & Human Performance Extreme Environm, 111 Cooke Hall,1900 Univ Ave SE, Minneapolis, MN 55455 USA. EM kosch002@tc.umn.edu NR 20 TC 0 Z9 0 U1 0 U2 3 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 SEP PY 2005 VL 76 IS 9 BP 828 EP 832 PG 5 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 962XZ UT WOS:000231768100002 PM 16173678 ER PT J AU Jayaraman, M Radhika, V Bamne, MN Ramos, R Briggs, R Dhanasekaran, DN AF Jayaraman, M Radhika, V Bamne, MN Ramos, R Briggs, R Dhanasekaran, DN TI Engineered Saccharomyces cerevisiae strain BioS-OS1/2, for the detection of oxidative stress SO BIOTECHNOLOGY PROGRESS LA English DT Article ID YEAST; YAP1; GLUTATHIONE; PROTECTION; CELLS; GENE AB One of the major stress factors during space and high-altitude flight is the oxidative damage caused by the release of reactive oxygen intermediates (ROIs) in human tissues. ROIs are released in response to several stress factors including radiation in space. Since ROIs contribute to several pathological conditions, there has been a great interest in developing a biosensor that can monitor the impact of ROIs on biological systems. Toward this goal, we sought to engineer a yeast stain that can monitor oxidative stress and be easily integrated into a biosensor platform. Saccharomyces cerevisiae respond to hyperoxidative stress by activating the expression of many proteins including the transcription factor, Yap1. Activated Yap1 primarily binds to the Yap-1 response elements in the promoters of genes that combat oxidative stress. Based on these observations, we genetically altered the Yap-1 pathway in the YCR094W BY4742 strain of S. cerevisiae by fusing the YREs in the promoter region of TRX2 gene to a cDNA-insert encoding green fluorescent protein (GFP). Exposure of this engineered yeast strain BioS-OS1 to varying levels of oxidative stress, as generated by different concentrations of H2O2 or diamide, elicits robust expression of GFP that can be monitored by the fluorescence of GFP by as early as 1 h. BioS-OS1 can detect a H2O2 concentration from 300 mu M onward. We also show that the signaling strength of the strain can be increased by engineering multiple YREs in the upstream of the cDNA-insert encoding GFP. Thus, the results presented here demonstrate that the engineered BioS-OS yeast strain can detect ROI-generating oxidative stress and validate the use of this prototypic strain for the development of a biosensor to detect and monitor oxidative stress factors during space and high altitude flights. C1 Temple Univ, Sch Med, Fels Inst Canc Res & Mol Biol, Philadelphia, PA 19140 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Radhika, V (reprint author), Temple Univ, Sch Med, Fels Inst Canc Res & Mol Biol, 3307 N Broad St, Philadelphia, PA 19140 USA. EM vradhika@temple.edu; danny001@temple.edu RI Bamne, Mikhil/A-9519-2010; OI Jayaraman, Muralidharan/0000-0003-3274-877X NR 23 TC 6 Z9 6 U1 1 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 8756-7938 J9 BIOTECHNOL PROGR JI Biotechnol. Prog. PD SEP-OCT PY 2005 VL 21 IS 5 BP 1373 EP 1379 DI 10.1021/bp050104j PG 7 WC Biotechnology & Applied Microbiology; Food Science & Technology SC Biotechnology & Applied Microbiology; Food Science & Technology GA 972NU UT WOS:000232461300003 PM 16209540 ER PT J AU Tripoli, GJ Medaglia, CM Dietrich, S Mugnai, A Panegrossi, G Pinori, S Smith, EA AF Tripoli, GJ Medaglia, CM Dietrich, S Mugnai, A Panegrossi, G Pinori, S Smith, EA TI The 9-10 November 2001 Algerian flood - A numerical study SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID MODEL C1 Univ Wisconsin, Dept Atmospher & Ocean Sci, Madison, WI 53706 USA. CNR, Inst Atmospher Sci & Climate, Rome, Italy. Univ Ferrara, Dept Phys, I-44100 Ferrara, Italy. NASA, Goddard Space Flight Ctr, Off GPM Project Scientist, Greenbelt, MD 20771 USA. RP Tripoli, GJ (reprint author), Univ Wisconsin, Dept Atmospher & Ocean Sci, Madison, WI 53706 USA. EM tripoli@aos.wisc.edu RI Panegrossi, Giulia/C-5702-2015; OI Panegrossi, Giulia/0000-0002-5170-7087; Dietrich, Stefano/0000-0003-3808-365X NR 11 TC 32 Z9 32 U1 0 U2 3 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD SEP PY 2005 VL 86 IS 9 BP 1229 EP 1235 DI 10.1175/BAMS-86-9-1229 PG 7 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 971DV UT WOS:000232362500018 ER PT J AU Negri, AJ Burkardt, N Golden, JH Halverson, JB Huffman, GJ Larsen, MC McGinley, JA Updike, RG Verdin, JP Wieczorek, GF AF Negri, AJ Burkardt, N Golden, JH Halverson, JB Huffman, GJ Larsen, MC McGinley, JA Updike, RG Verdin, JP Wieczorek, GF TI The hurricane-flood-landslide continuum SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID PRECIPITATION; LAPS C1 NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. US Geol Survey, Policy Anal & Sci Assistance Program, Ft Collins, CO USA. NOAA, Forecast Syst Lab, Boulder, CO 80303 USA. Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Catonsville, MD USA. Sci Syst & Applicat Inc, Greenbelt, MD USA. US Geol Survey, Off Chief Sci Hydrol, Reston, VA 22092 USA. US Geol Survey, Denver, CO 80225 USA. US Geol Survey, EROS Data Ctr, Sioux Falls, SD USA. US Geol Survey, Menlo Pk, CA 94025 USA. RP Negri, AJ (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Bldg 33,Room C408,Code 613-3, Greenbelt, MD 20771 USA. EM andrew.j.negri@nasa.gov RI Huffman, George/F-4494-2014 OI Huffman, George/0000-0003-3858-8308 NR 12 TC 15 Z9 15 U1 0 U2 4 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD SEP PY 2005 VL 86 IS 9 BP 1241 EP 1247 DI 10.1175/BAMS-86-9-1241 PG 7 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 971DV UT WOS:000232362500020 ER PT J AU Al-Saadi, J Szykman, J Pierce, RB Kittaka, C Neil, D Chu, DA Remer, L Gumley, L Prins, E Weinstock, L MacDonald, C Wayland, R Dimmick, F Fishman, J AF Al-Saadi, J Szykman, J Pierce, RB Kittaka, C Neil, D Chu, DA Remer, L Gumley, L Prins, E Weinstock, L MacDonald, C Wayland, R Dimmick, F Fishman, J TI Improving national air quality forecasts with satellite aerosol observations SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID RESOLUTION IMAGING SPECTRORADIOMETER; POLLUTION; SYSTEM; MODIS; LAND AB Accurate air quality forecasts can allow for mitigation of the health risks associated with high levels of air pollution. During September 2003, a team of NASA NOAA and EPA researchers demonstrated a prototype tool for improving fine particulate matter (PM2.5) air quality forecasts using satellite aerosol observations. Daily forecast products were generated from a near-real-time fusion of multiple input data products, including aerosol optical depth (AOD) from the Moderate Resolution Imaging Spectroradiometer (MODIS)/Earth Observing System (EOS) instrument on the NASA Terra satellite, PM 2.5 concentration from over 300 state/local/national surface monitoring stations, meteorological fields from the NOAA/NCEP Eta Model, and fire locations from the NOAA/National Environmental Satellite, Data, and Information Service (NESDIS) Geostationary Operational Environmental Satellite (GOES) Wildfire Automated Biomass Burning Algorithm (WFABBA) product. The products were disseminated via a Web interface to a small group of forecasters representing state and local air management agencies and the EPA. The MODIS data improved forecaster knowledge of synoptic-scale air pollution events, particularly over oceans and in regions devoid of surface monitors. Forecast trajectories initialized in regions of high AOD offered guidance for identifying potential episodes of poor air quality. The capability of this approach was illustrated with a case study showing that aerosol resulting from wildfires in the northwestern United States and southwestern Canada is transported across the continent to influence air quality in the Great Lakes region a few days later. The timing of this demonstration was selected to help improve the accuracy of the EPAs AIRNow (www.epa.gov/airnow/) next-day PM2.5, air quality index forecast, which began on 1 October 2003. Based on the positive response from air quality managers and forecasters, this prototype was expanded and transitioned to an operational provider during the summer of 2004. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. US EPA, Off Res & Dev, Res Triangle Pk, NC 27711 USA. SAIC, Hampton, VA USA. Univ Maryland Baltimore Cty, Joint Ctr Earth Sci Technol, Baltimore, MD 21228 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Wisconsin, SSEC CIMSS, Madison, WI USA. Univ Wisconsin, NOAA, NES DIS ORA, Madison, WI USA. US EPA, Off Air Qual Planning & Stand, Res Triangle Pk, NC 27711 USA. RP Al-Saadi, J (reprint author), NASA, Langley Res Ctr, MS 401B, Hampton, VA 23681 USA. EM j.a.al-saadi@nasa.gov RI Pierce, Robert Bradley/F-5609-2010 OI Pierce, Robert Bradley/0000-0002-2767-1643 NR 33 TC 181 Z9 184 U1 9 U2 49 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD SEP PY 2005 VL 86 IS 9 BP 1249 EP + DI 10.1175/BAMS-86-9-1249 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 971DV UT WOS:000232362500021 ER PT J AU Cahalan, RF Oreopoulos, L Marshak, A Evans, KF Davis, AB Pincus, R Yetzer, KH Mayer, B Davies, R Ackerman, TP Barker, HW Clothiaux, EE Ellingson, RG Garay, MJ Kassianov, E Kinne, S Macke, A O'Hirok, W Partain, PT Prigarin, SM Rublev, AN Stephens, GL Szczap, F Takara, EE Varnai, T Wen, GY Zhuravleva, TB AF Cahalan, RF Oreopoulos, L Marshak, A Evans, KF Davis, AB Pincus, R Yetzer, KH Mayer, B Davies, R Ackerman, TP Barker, HW Clothiaux, EE Ellingson, RG Garay, MJ Kassianov, E Kinne, S Macke, A O'Hirok, W Partain, PT Prigarin, SM Rublev, AN Stephens, GL Szczap, F Takara, EE Varnai, T Wen, GY Zhuravleva, TB TI The 13RC - Bringing together the most advanced radiative transfer tools for cloudy atmospheres SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID INDEPENDENT PIXEL APPROXIMATION; GENERAL-CIRCULATION MODELS; DISCRETE-ORDINATE-METHOD; AVERAGED SOLAR FLUXES; PART I; INHOMOGENEOUS CLOUDS; MULTIPLE-SCATTERING; CLIMATE FEEDBACK; PARAMETERIZATION; SIMULATION AB The interaction of clouds with solar and terrestrial radiation is one of the most important topics of climate research. In recent years it has been recognized that only a full three-dimensional (3D) treatment of this interaction can provide answers to many climate and remote sensing problems, leading to the worldwide development of numerous 3D radiative transfer (RT) codes. The international Intercomparison of 3D Radiation Codes (I3RC), described in this paper, sprung from the natural need to compare the performance of these 3D RT codes used in a variety of current scientific work in the atmospheric sciences. I3RC supports intercomparison and development of both exact and approximate 3D methods in its effort to 1) understand and document the errors/limits of 3D algorithms and their sources; 2) provide "baseline" cases for future code development for 3D radiation; 3) promote sharing and production of 3D radiative tools; 4) derive guidelines for 3D radiative tool selection; and 5) improve atmospheric science education in 3D RT. Results from the two completed phases of I3RC have been presented in two workshops and are expected to guide improvements in both remote sensing and radiative energy budget calculations in cloudy atmospheres. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA. Univ Colorado, Boulder, CO 80309 USA. Los Alamos Natl Lab, Los Alamos, NM USA. NOAA, CIRES, Climate Diagnost Ctr, Boulder, CO 80303 USA. Raytheon ITSS, Beltsville, MD USA. Deutsch Zentrum Luft & Raumfahrt, Oberpfaffenhofen, Germany. CALTECH, Jet Prop Lab, Pasadena, CA USA. Pacific NW Natl Lab, Richland, WA USA. Meteorol Serv Canada, Downsview, ON, Canada. Penn State Univ, University Pk, PA 16802 USA. Florida State Univ, Tallahassee, FL 32306 USA. Univ Calif Los Angeles, Los Angeles, CA USA. Max Planck Inst Meteorol, Hamburg, Germany. Univ Kiel, Liebniz Inst Marine Sci, IFM GEOMAR, Kiel, Germany. Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA. Colorado State Univ, Ft Collins, CO 80523 USA. Inst Computat Math & Math Geophys, Novosibirsk, Russia. Kurchatov Inst, Moscow, Russia. Univ Clermont Ferrand, Clermont Ferrand, France. Russian Acad Sci, Inst Atmospher Opt, Tomsk, Russia. RP Cahalan, RF (reprint author), NASA, Goddard Space Flight Ctr, Code 613-2, Greenbelt, MD 20771 USA. EM Robert.F.Cahalan@nasa.gov RI Mayer, Bernhard/B-3397-2011; Davies, Roger/D-4296-2009; Oreopoulos, Lazaros/E-5868-2012; Cahalan, Robert/E-3462-2012; Marshak, Alexander/D-5671-2012; Pincus, Robert/B-1723-2013 OI Mayer, Bernhard/0000-0002-3358-0190; Davies, Roger/0000-0002-2991-0409; Oreopoulos, Lazaros/0000-0001-6061-6905; Cahalan, Robert/0000-0001-9724-1270; Pincus, Robert/0000-0002-0016-3470 NR 59 TC 117 Z9 119 U1 3 U2 10 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD SEP PY 2005 VL 86 IS 9 BP 1275 EP + DI 10.1175/BAMS-86-9-1275 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 971DV UT WOS:000232362500023 ER PT J AU Ohring, G Wielicki, B Spencer, R Emery, B Datla, R AF Ohring, G Wielicki, B Spencer, R Emery, B Datla, R TI Satellite instrument calibration for measuring global climate change - Report of a Workshop SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Editorial Material AB Measuring the small changes associated with long-term global climate change from space is a daunting task. The satellite instruments must be capable of observing atmospheric and surface temperature trends as small as 0.1 degrees C decade(-1), ozone changes as little as 1% decade(-1), and variations in the sun's output as tiny as 0.1% decade(-1). To address these problems and recommend directions for improvements in satellite instrument calibration, the National Institute of Standards and Technology (NIST), National Polar-orbiting Operational Environmental Satellite System-Integrated Program Office (NPOESS-IPO), National Oceanic and Atmospheric Administration (NOAA), and National Aeronautics and Space Administration (NASA) organized a workshop at the University of Maryland Inn and Conference Center, College Park, Maryland, 12-14 November 2002. Some 75 scientists participated including researchers who develop and analyze long-term datasets from satellites; experts in the field of satellite instrument calibration, and physicists working on state-of-the-art calibration sources and standards. The workshop defined the absolute accuracies and long-term stabilities of global climate datasets that are needed to detect expected trends, translated these dataset accuracies and stabilities to required satellite instrument accuracies and stabilities, and evaluated the ability of current observing systems to meet these requirements. The workshop's recommendations include a set of basic axioms or overarching principles that must guide high quality climate observations in general, and a road map for improving satellite instrument characterization, calibration, intercalibration, and associated activities to meet the challenge of measuring global climate change. The workshop also recommended that a follow-up workshop be conducted to discuss implementation of the road map developed at this workshop. C1 NOAA, College Pk, MD USA. NIST, College Pk, MD USA. NASA, Langley Res Ctr, Hampton, VA 23665 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Univ Colorado, Boulder, CO 80309 USA. NIST, Gaithersburg, MD 20899 USA. RP Ohring, G (reprint author), 6100-712 Westchester Pk Dr, College Pk, MD 20740 USA. EM george.ohring@noaa.gov RI Ohring, George/F-5616-2010 NR 16 TC 108 Z9 110 U1 0 U2 5 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD SEP PY 2005 VL 86 IS 9 BP 1303 EP + DI 10.1175/BAMS-86-9-1303 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 971DV UT WOS:000232362500025 ER PT J AU Cullings, K Raleigh, C Vogler, DR AF Cullings, K Raleigh, C Vogler, DR TI Effects of severe dwarf mistletoe infection on the ectomycorrhizal community of a Pinus contorta stand in Yellowstone Park SO CANADIAN JOURNAL OF BOTANY-REVUE CANADIENNE DE BOTANIQUE LA English DT Article DE dwarf mistletoe; Yellowstone; ectomycorrhizae PCR; DNA sequencing ID ELEMENTAL ORGANIC-ANALYSIS; NATIONAL-PARK; MYCORRHIZAL COLONIZATION; ENVIRONMENTAL-STRESS; DIFFERENT AGE; PINYON PINES; FUNGI; DEFOLIATION; FOREST; SEEDLINGS AB Molecular methods were used to test the hypothesis that severe infection by dwarf mistletoe (Arceuthobium, a carbon-sink parasite) affects the ectomycorrhizal (EM) communities of its host, lodgepole pine. Results indicate significantly lower EM fungal species richness (2 +/- 0.2 SE species per core in uninfected and 1 +/- 0.2 species per core in infected blocks; P < 0.005), Shannon-Wiener diversity indices (1.1 in uninfected and 0.6 in infected; P < 0.05), and also differences in species EM fungal composition; uninfected blocks are dominated by a species of Cortinarius while the infected stand is dominated by species of Russula, and Piloderma (26%). By contrast, dwarf mistletoe infection has no apparent effect on evenness (0.65 in controls and 0.47 in infected; 0.05 < P < 0.1), or on EM infection levels (35 +/- 7 EM tips per core in uninfected and 21 +/- 5 in infected; P > 0.1). Thus, dwarf mistletoe infection may select for EM fungal species that impose a lower carbon demand on the host, or that possess carbon-degrading abilities to augment carbon lost to the parasite, enabling the trees in infected blocks to maintain relatively high EM infection levels. Our results indicate that effects of dwarf mistletoe infection occur not just in the crown of infected but extend into the soil as well, and hence may have much greater implications for ecosystem function than previously thought. C1 NASA, Ames Res Ctr, Mountain View, CA 94035 USA. US Forest Serv, USDA, Pacific SW Res Stn, Inst Forest Genet, Placerville, CA 95667 USA. RP Cullings, K (reprint author), NASA, Ames Res Ctr, Mountain View, CA 94035 USA. EM kcullings@mail.arc.nasa.gov NR 44 TC 10 Z9 10 U1 2 U2 13 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA, ONTARIO K1A 0R6, CANADA SN 0008-4026 J9 CAN J BOT JI Can. J. Bot.-Rev. Can. Bot. PD SEP PY 2005 VL 83 IS 9 BP 1174 EP 1180 DI 10.1139/b05-100 PG 7 WC Plant Sciences SC Plant Sciences GA 994RW UT WOS:000234049900013 ER PT J AU Koljonen, ML Pella, JJ Masuda, M AF Koljonen, ML Pella, JJ Masuda, M TI Classical individual assignments versus mixture modeling to estimate stock proportions in Atlantic salmon (Salmo salar) catches from DNA microsatellite data SO CANADIAN JOURNAL OF FISHERIES AND AQUATIC SCIENCES LA English DT Article ID MULTILOCUS GENOTYPE DATA; POPULATION-STRUCTURE; GENETIC-VARIATION; PHYLOGENETIC TREES; PACIFIC SALMON; BALTIC SEA; IDENTIFICATION; DIFFERENTIATION; PROGRAM; MANAGEMENT AB Mixture modeling is shown to outperform classical individual assignments for both estimating stock composition and identifying individuals' sources in a case study of an eight-locus DNA microsatellite database from 26 Atlantic salmon (Salmo salar) stocks of the Baltic Sea. Performance of the estimation methods was compared using self-assignment tests applied to each of the baseline samples and using independent repeat samples from two of the baseline stocks. The different theoretical underpinnings, hypothesis testing versus decision theory, of the methods explain their estimation capacities. In addition, actual catch samples from three northern Baltic Sea sites in 2000 were analysed by mixture modeling, and estimated compositions were consistent with previous knowledge. Baltic main basin and Gulf of Finland stocks were each minor components (< 1% at any site), and three groups of Gulf of Bothnia stocks, wild (36%-43% among sites), Finnish hatchery (15%-49%), and Swedish hatchery (11%-41%), were each important with the two hatchery contributions trending geographically. C1 Finnish Game & Fisheries Res Inst, FIN-00791 Helsinki, Finland. Natl Marine Fisheries Serv, Auke Bay Lab, Alaska Fisheries Sci Ctr, NOAA, Juneau, AK 99801 USA. RP Koljonen, ML (reprint author), Finnish Game & Fisheries Res Inst, POB 2, FIN-00791 Helsinki, Finland. EM marja-liisa.koljonen@rktl.fi NR 58 TC 46 Z9 47 U1 0 U2 8 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA, ONTARIO K1A 0R6, CANADA SN 0706-652X J9 CAN J FISH AQUAT SCI JI Can. J. Fish. Aquat. Sci. PD SEP PY 2005 VL 62 IS 9 BP 2143 EP 2158 DI 10.1139/F05-128 PG 16 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 964OG UT WOS:000231889800020 ER PT J AU Pitcher, KW Rehberg, MJ Pendleton, GW Raum-Suryan, KL Gelatt, TS Swain, UG Sigler, MF AF Pitcher, KW Rehberg, MJ Pendleton, GW Raum-Suryan, KL Gelatt, TS Swain, UG Sigler, MF TI Ontogeny of dive performance in pup and juvenile Steller sea lions in Alaska SO CANADIAN JOURNAL OF ZOOLOGY-REVUE CANADIENNE DE ZOOLOGIE LA English DT Article ID DIMORPHIC CAPITAL BREEDER; EUMETOPIAS-JUBATUS; DIVING BEHAVIOR; LEPTONYCHOTES WEDDELLII; POPULATION-DYNAMICS; WALLEYE POLLOCK; BODY-SIZE; FUR-SEAL; PATTERNS; GULF AB Development of competent diving ability is critical to obtaining nutritional independence in marine mammals such as Steller sea lions (SSLs), Eumetopias jubatus (Schreber, 1776). We studied diving performance in pup (75) and juvenile (36) SSLs using satellite data recorders. In general, dives by SSLs were brief and shallow. Overall, 82.3% of dives were < 2 min long and 86.9% of dives were < 10 m deep. Long ( > 5 min) and deep dives ( > 100 m) constituted only 2.49% and 0.77%, respectively, of total dives. We used linear mixed-effects models to investigate the relationships between the response variables maximum-daily-depth, time-at-depth, mean-dive-duration, dive rate, and time-at-sea and the predictor variables age, sex, population (eastern and western Alaska populations), time-of-day, and month-of-year. All response variables except dive rate were positively related (P < 0.05) to age. Dive rate declined (P < 0.001) with age. Time-of-day, month, population, sex, and some first-order interactions were all significantly (P < 0.05) related to some measure of diving performance. With large samples we were able to identify significant relationships between the response variables and the predictor variables, even though the total amount of variation explained by the models was low, because most dives were short and shallow regardless of age, sex, population, time-of-day, or month-of-year. Depths and durations of dives by juvenile animals increased throughout the range of ages studied and were similar to or greater than those previously reported for juveniles and adult females. We expect maximum depths and durations to continue to increase with age until body mass plateaus at about 10 years of age. Therefore, we expect older animals to be more efficient foragers, as they would have greater aerobic dive limits as well as more experience locating and capturing prey. C1 Alaska Dept Fish & Game, Div Wildlife Conservat, Anchorage, AK 99518 USA. Alaska Dept Fish & Game, Div Wildlife Conservat, Douglas, AK 99824 USA. Natl Marine Fisheries Serv, Alsaka Fisheries Sci Ctr, Auke Bay Lab, Juneau, AK 99801 USA. RP Pitcher, KW (reprint author), Alaska Dept Fish & Game, Div Wildlife Conservat, 525 W 67th Ave, Anchorage, AK 99518 USA. EM ken_pitcher@fishgame.state.ak.us NR 51 TC 35 Z9 39 U1 1 U2 13 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA, ONTARIO K1A 0R6, CANADA SN 0008-4301 J9 CAN J ZOOL JI Can. J. Zool.-Rev. Can. Zool. PD SEP PY 2005 VL 83 IS 9 BP 1214 EP 1231 DI 10.1139/Z05-098 PG 18 WC Zoology SC Zoology GA 984KM UT WOS:000233303800008 ER PT J AU Wang, M Shen, ZK Dong, DN AF Wang, M Shen, ZK Dong, DN TI Effects of non-tectonic crustal deformation on continuous GPS position time series and correction to them SO CHINESE JOURNAL OF GEOPHYSICS-CHINESE EDITION LA Chinese DT Article DE crustal motion; non-tectonic deformation; mass loading; CPS ID CHINA; SYSTEM AB A crustal deformation field observed by GPS usually includes both tectonic and non-tectonic deformation signals, and it is vitally important to remove the non-tectonic deformation signals from the data in order to effectively use GPS observations to study tectonic deformation. Using the Earth satellite data and geophysical models, we calculate non-tectonic crustal deformation caused by ocean tide loading, atmospheric mass loading, snow and soil moisture mass loading, and non-tidal ocean mass loading. Based on the quantitative analyses, the effects of non-tectonic crustal deformation on the position time series of GPS fiducial stations from the Crustal Movement Observation Network of China are studied and corrected. Our study shows that these effects on the vertical components of station positions are remarkable, especially those resulted from the atmospheric mass loading and snow and soil moisture mass loading. Using these models to correct for the non-tectonic deformation, we have reduced the RMS of the station vertical position by about I turn, which is about 11 % of the total RMS. The amplitudes of annual vertical position variations are also reduced by about 37%. Moreover, we find that the position time series corrected using geophysical models followed by an empirical fitting of annual and semi-annual variations are smoother than that corrected using the empirical fitting of annual and semi-annual variations only, indicating that geophysical model corrections can not be substituted by pure empirical fitting in removing the non-tectonic deformation effects. C1 China Earthquake Adm, Inst Geol, State Key Lab Earthquake Dynam, Beijing 100029, Peoples R China. China Earthquake Adm, Inst Earthquake Sci, Beijing 100036, Peoples R China. Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Wang, M (reprint author), China Earthquake Adm, Inst Geol, State Key Lab Earthquake Dynam, Beijing 100029, Peoples R China. EM mwang@gps.gov.cn NR 16 TC 19 Z9 74 U1 1 U2 6 PU SCIENCE PRESS PI BEIJING PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA SN 0001-5733 J9 CHINESE J GEOPHYS-CH JI Chinese J. Geophys.-Chinese Ed. PD SEP PY 2005 VL 48 IS 5 BP 1045 EP 1052 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 969KG UT WOS:000232232400010 ER PT J AU Forth, SC Staroselsky, A AF Forth, SC Staroselsky, A TI A hybrid FEM/BEM approach for designing an aircraft engine structural health monitoring SO CMES-COMPUTER MODELING IN ENGINEERING & SCIENCES LA English DT Article DE hybrid numerical method; health monitoring; finite element; boundary element; aircraft engine; crack propagation ID SURFACE CRACKS; GROWTH AB A new hybrid surface-integral-finite-element numerical scheme has been developed to model a three-dimensional crack propagating through a thin, multi-layered coating. The finite element method was used to model the physical state of the coating, and the surface integral method was used to model the fatigue crack growth. The two formulations are coupled through the need to satisfy boundary conditions on the crack and external surface. The coupling is sufficiently weak that the surface integral mesh of the crack surface and the finite element mesh of the uncracked volume can be set up independently. Thus, when modeling crack growth, the finite element mesh can remain fixed for the duration of the simulation as the crack mesh is advanced. This method was developed to evaluate the feasibility of fabricating a structural health monitoring system for real-time detection of surface cracks propagating in aircraft engine components. In this work, the authors formulate the hybrid surface-integral-finite-element method and discuss the mechanical issues of implementing a structural health monitoring system in an aircraft engine environment. C1 NASA, Langley Res Ctr, Hampton, VA 23665 USA. United Technol Res Ctr, E Hartford, CT 06108 USA. RP Forth, SC (reprint author), NASA, Langley Res Ctr, 2 W Reid St,MS 188E, Hampton, VA 23665 USA. NR 40 TC 12 Z9 12 U1 0 U2 1 PU TECH SCIENCE PRESS PI ENCINO PA 4924 BALBOA BLVD, # 488, ENCINO, CA 91316 USA SN 1526-1492 J9 CMES-COMP MODEL ENG JI CMES-Comp. Model. Eng. Sci. PD SEP PY 2005 VL 9 IS 3 BP 287 EP 298 PG 12 WC Engineering, Multidisciplinary; Mathematics, Interdisciplinary Applications SC Engineering; Mathematics GA 976PA UT WOS:000232744400006 ER PT J AU Nezlin, NP DiGiacomo, PM AF Nezlin, NP DiGiacomo, PM TI Satellite ocean color observations of stormwater runoff plumes along the San Pedro Shelf (southern California) during 1997-2003 SO CONTINENTAL SHELF RESEARCH LA English DT Article DE ocean color; freshwater discharge; plumes; precipitation; San pedro shelf; 33.47-33.79 degrees N; 118.4-117.7 W ID RIVER PLUME; MONICA BAY; COASTAL WATERS; SEASONAL VARIABILITY; HUNTINGTON BEACH; BARBARA CHANNEL; CURRENT SYSTEM; TEMPERATURE; IMPACTS; QUALITY AB Knowledge of freshwater runoff plume dynamics in southern California is important for management of coastal water quality, because river discharge associated with episodic winter rainstorms can be a major source of pollutants and pathogens to coastal waters. The purpose of this study was to analyze the spatio-temporal dynamics of plumes at the San Pedro Shelf in southern California and identify factors influencing the incidence and dispersal patterns of plumes. We used 1.1-km spatial resolution satellite images collected in 1997-2003 by the SeaWiFS optical radiometer. The area of each plume was detected by the backscattering characteristics of surface waters in the vicinity of the mouths of four rivers that discharge to the San Pedro Basin. The rainstorm magnitude was estimated from atmospheric precipitation averaged over the total area of local watersheds. The plume size estimated from the backscattering coefficient nLw555 > 1.3 mW cm(-2) mu m(-1) sr(-1) was highly correlated with the amount of rainwater precipitated over the watershed area and accumulated during the period preceding the plume. The relation between rainstorm and plume area was linear with zero intercept: that means that the minimum rainstorm magnitude under which no plume occurred in the study area was almost zero, and even small precipitation resulted in a plume. The persistence of the plumes was estimated by fitting the coefficients of the model of plume water dissipation to achieve maximum correlation between the plume area and rainstorm: Twenty-five percent of rainwater dissipated daily, which gradually decreased the plume size. The size, alongshore and cross-shelf translocation of the plumes were modulated slightly by the local circulation, forced remotely by the equatorward wind a few hundred km to the south (along the coast of Baja California). The influence of tidal circulation on the plume area was slight and statistically insignificant. (c) 2005 Elsevier Ltd. All rights reserved. C1 So Calif Coastal Water Res Project, Westminster, CA 92683 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Nezlin, NP (reprint author), So Calif Coastal Water Res Project, 7171 Fenwick Lane, Westminster, CA 92683 USA. EM nikolayn@sccwrp.org RI DiGiacomo, Paul/F-5584-2010 OI DiGiacomo, Paul/0000-0003-4550-1899 NR 59 TC 45 Z9 47 U1 1 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0278-4343 J9 CONT SHELF RES JI Cont. Shelf Res. PD SEP PY 2005 VL 25 IS 14 BP 1692 EP 1711 DI 10.1016/j.csr.2005.05.001 PG 20 WC Oceanography SC Oceanography GA 966DP UT WOS:000232000100003 ER PT J AU Yuan, JC Dagg, MJ Del Castillo, CE AF Yuan, JC Dagg, MJ Del Castillo, CE TI In-pixel variations of chl a fluorescence in the Northern Gulf of Mexico and their implications for calibrating remotely sensed chl a and other products SO CONTINENTAL SHELF RESEARCH LA English DT Article DE remote sensing; calibration; valiclation; SeaWiFS; MODIS; chl a ID OCEAN COLOR; SEAWIFS; VALIDATION AB Remote sensing instruments such as SeaWiFS and MODIS are often calibrated or tested by comparison with in situ data. These comparisons are based on the premise that there is uniform in-pixel variation of the standard deviation of in situ properties. To evaluate some of the errors resulting from this assumption, we conducted an analysis of in-pixel variation of chl a fluorescence by examining fluorescence data from a flow-through system on an underway vessel mapping surface properties for 10 days on the continental shelf in the vicinity of the Mississippi River delta. Significant variations of in-pixel standard deviation of chl a fluorescence were observed, which indicate that this uniformity assumption is not valid in the Northern Gulf of Mexico. Furthermore, our analysis indicates that a large apparent error by the remote sensor is generated if uniformity of standard deviation is assumed. Our results suggest that one should take into account both in-pixel mean and standard deviation, when comparing remotely sensed ocean color data with in situ measurements. Similar measures should be taken when comparing other remotely sensed products with field determinations. (c) 2005 Elsevier Ltd. All rights reserved. C1 Univ So Mississippi, Dept Marine Sci, Stennis Space Ctr, MS 39529 USA. Louisiana Univ Marine Consortium, Chauvin, LA 70344 USA. NASA, Earth Sci Applicat Directorate, Stennis Space Ctr, MS 39529 USA. RP Yuan, JC (reprint author), Univ So Mississippi, Dept Marine Sci, Stennis Space Ctr, MS 39529 USA. EM jinchun.yuan@usm.edu RI Del Castillo, Carlos/N-2601-2013 NR 11 TC 7 Z9 7 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0278-4343 J9 CONT SHELF RES JI Cont. Shelf Res. PD SEP PY 2005 VL 25 IS 15 BP 1894 EP 1904 DI 10.1016/j.csr.2005.06.003 PG 11 WC Oceanography SC Oceanography GA 973EY UT WOS:000232506900008 ER PT J AU Vaisberg, OL Avanov, LA Leibov, AV Smirnov, VN Keller, J Moore, T Chornay, D Collier, M Troshin, VS Myagkikh, VD AF Vaisberg, OL Avanov, LA Leibov, AV Smirnov, VN Keller, J Moore, T Chornay, D Collier, M Troshin, VS Myagkikh, VD TI A panoramic plasma spectrometer: An all-sky camera for charged particles SO COSMIC RESEARCH LA English DT Article C1 Russian Acad Sci, Space Res Inst, Moscow, Russia. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Vaisberg, OL (reprint author), Russian Acad Sci, Space Res Inst, Moscow, Russia. RI Moore, Thomas/D-4675-2012; Keller, John/I-5097-2013 OI Moore, Thomas/0000-0002-3150-1137; NR 7 TC 2 Z9 2 U1 2 U2 3 PU MAIK NAUKA/INTERPERIODICA PI NEW YORK PA C/O KLUWER ACADEMIC-PLENUM PUBLISHERS, 233 SPRING ST, NEW YORK, NY 10013-1578 USA SN 0010-9525 J9 COSMIC RES+ JI Cosmic Res. PD SEP-OCT PY 2005 VL 43 IS 5 BP 373 EP 376 DI 10.1007/s10604-005-0058-9 PG 4 WC Engineering, Aerospace; Astronomy & Astrophysics SC Engineering; Astronomy & Astrophysics GA 982HL UT WOS:000233148600009 ER PT J AU Choi, SR Zhu, D Miller, RA AF Choi, SR Zhu, D Miller, RA TI Fracture behavior under mixed-mode loading of ceramic plasma-sprayed thermal barrier coatings at ambient and elevated temperatures SO ENGINEERING FRACTURE MECHANICS LA English DT Article DE ceramic thermal barrier coatings; mixed modes I and II loading; asymmetric four-point flexure; fracture toughness testing; plasma-sprayed ZrO(2-)8wt%Y2O3 ID II FRACTURE; BRITTLE-FRACTURE; TOUGHNESS; ENERGY AB The fracture behavior under modes I and II loading of ceramic plasma-sprayed thermal barrier coatings was determined in air at 25 and 1316 degrees C in asymmetric four-point flexure. The mode I fracture toughness was found to be K-Ic = 1.15 +/- 0.07 and 0.98 +/- 0.13 MPa root m, respectively, at 25 and 1316 degrees C. The respective 'nominal' mode II fracture toughness values were K-IIc = 0.73 +/- 0.10 and 0.65 +/- 0.04 MPa root m. The empirical mixed-mode fracture criterion best described the coatings' fracture behavior under mixed-mode loading. The angle of crack propagation was in reasonable agreement with the minimum strain energy density criterion. (c) 2005 Elsevier Ltd. All rights reserved. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Choi, SR (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM sung.r.choi@grc.nasa.gov NR 41 TC 23 Z9 23 U1 0 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0013-7944 J9 ENG FRACT MECH JI Eng. Fract. Mech. PD SEP PY 2005 VL 72 IS 13 BP 2144 EP 2158 DI 10.1016/j.engfracmech.2005.01.010 PG 15 WC Mechanics SC Mechanics GA 952NO UT WOS:000231011300007 ER PT J AU Milesi, C Running, SW Elvidge, CD Dietz, JB Tuttle, BT Nemani, RR AF Milesi, C Running, SW Elvidge, CD Dietz, JB Tuttle, BT Nemani, RR TI Mapping and modeling the biogeochemical cycling of turf grasses in the United States SO ENVIRONMENTAL MANAGEMENT LA English DT Article DE turf grasses; BIOME-BGC; impervious surface area; carbon budget; carbon sequestration potential; water use ID FOREST ECOSYSTEM PROCESSES; REGIONAL APPLICATIONS; CARBON SEQUESTRATION; GENERAL-MODEL; AMERICAN LAWN; TURFGRASS; BGC; SIMULATIONS; MANAGEMENT; EXCHANGE AB Turf grasses are ubiquitous in the urban landscape of the United States and are often associated with various types of environmental impacts, especially on water resources, yet there have been limited efforts to quantify their total surface and ecosystem functioning, such as their total impact on the continental water budget and potential net ecosystem exchange (NEE). In this study, relating turf grass area to an estimate of fractional impervious surface area, it was calculated that potentially 163,800 km(2) (+/- 35,850 km(2)) of land are cultivated with turf grasses in the continental United States, an area three times larger than that of any irrigated crop. Using the Biome-BGC ecosystem process model, the growth of warm-season and cool-season turf grasses was modeled at a number of sites across the 48 conterminous states under different management scenarios, simulating potential carbon and water fluxes as if the entire turf surface was to be managed like a well-maintained lawn. The results indicate that well-watered and fertilized turf grasses act as a carbon sink. The potential NEE that could derive from the total surface potentially under turf (up to 17 Tg C/yr with the simulated scenarios) would require up to 695 to 900 liters of water per person per day, depending on the modeled water irrigation practices, suggesting that outdoor water conservation practices such as xeriscaping and irrigation with recycled waste-water may need to be extended as many municipalities continue to face increasing pressures on freshwater. C1 Univ Montana, Coll Forestry & Conservat, Numerical Terradynam Simulat Grp, Missoula, MT 59812 USA. NOAA, Natl Geophys Data Ctr, Boulder, CO 80303 USA. Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA. Univ Colorado, NOAA, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Milesi, C (reprint author), Univ Montana, Coll Forestry & Conservat, Numerical Terradynam Simulat Grp, Missoula, MT 59812 USA. EM milesi@ntsg.umt.edu RI Elvidge, Christopher/C-3012-2009 NR 44 TC 223 Z9 239 U1 17 U2 126 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0364-152X J9 ENVIRON MANAGE JI Environ. Manage. PD SEP PY 2005 VL 36 IS 3 BP 426 EP 438 DI 10.1007/s00267-004-0316-2 PG 13 WC Environmental Sciences SC Environmental Sciences & Ecology GA 965OC UT WOS:000231959000008 PM 16086109 ER PT J AU Goffredi, SK Orphan, VJ Rouse, GW Jahnke, L Embaye, T Turk, K Lee, R Vrijenhoek, RC AF Goffredi, SK Orphan, VJ Rouse, GW Jahnke, L Embaye, T Turk, K Lee, R Vrijenhoek, RC TI Evolutionary innovation: a bone-eating marine symbiosis SO ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID POLYUNSATURATED FATTY-ACIDS; TARGETED OLIGONUCLEOTIDE PROBES; 16S RIBOSOMAL-RNA; BACTERIA; MICROORGANISMS; IDENTIFICATION; HYBRIDIZATION; CHOLESTEROL; ISOTOPES; ANIMALS AB Symbiotic associations between microbes and invertebrates have resulted in some of the most unusual physiological and morphological adaptations that have evolved in the animal world. We document a new symbiosis between marine polychaetes of the genus Osedax and members of the bacterial group Oceanospirillales, known for heterotrophic degradation of complex organic compounds. These organisms were discovered living on the carcass of a grey whale at 2891 m depth in Monterey Canyon, off the coast of California. The mouthless and gutless worms are unique in their morphological specializations used to obtain nutrition from decomposing mammalian bones. Adult worms possess elaborate posterior root-like extensions that invade whale bone and contain bacteriocytes that house intracellular symbionts. Stable isotopes and fatty acid analyses suggest that these unusual endosymbionts are likely responsible for the nutrition of this locally abundant and reproductively prolific deep-sea worm. C1 Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. S Australian Museum, Adelaide, SA 5000, Australia. Univ Adelaide, Adelaide, SA 5005, Australia. Washington State Univ, Pullman, WA 99164 USA. RP Goffredi, SK (reprint author), CALTECH, Pasadena, CA 91125 USA. EM goffredi@caltech.edu RI Rouse, Greg/F-2611-2010; Orphan, Victoria/K-1002-2014 OI Rouse, Greg/0000-0001-9036-9263; Orphan, Victoria/0000-0002-5374-6178 NR 35 TC 84 Z9 86 U1 19 U2 51 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 1462-2912 J9 ENVIRON MICROBIOL JI Environ. Microbiol. PD SEP PY 2005 VL 7 IS 9 BP 1369 EP 1378 DI 10.1111/j.1462-2920.2005.00824.x PG 10 WC Microbiology SC Microbiology GA 952RU UT WOS:000231024000010 PM 16104860 ER PT J AU Han, YH Kumar, AN Reschke, MF Somers, JT Dell'Osso, LF Leigh, RJ AF Han, YH Kumar, AN Reschke, MF Somers, JT Dell'Osso, LF Leigh, RJ TI Vestibular and non-vestibular contributions to eye movements that compensate for head rotations during viewing of near targets SO EXPERIMENTAL BRAIN RESEARCH LA English DT Article DE vestibulo-ocular reflex; retinal image slip; prediction; vergence ID HORIZONTAL VESTIBULOOCULAR REFLEX; SMOOTH-PURSUIT; OCULAR REFLEX; RESPONSES; ACCELERATION; DISTANCE; BEHAVIOR; FIXATION; VERGENCE; LATENCY AB Geometry dictates that when subjects view a near target during head rotation the eyes must rotate more than the head. The relative contribution to this compensatory response by adjustment of the vestibulo-ocular reflex gain (Gvor), visual tracking mechanisms including prediction, and convergence is debated. We studied horizontal eye movements induced by sinusoidal 0.2-2.8 Hz, en-bloc yaw rotation as ten normal humans viewed a near target that was either earth-fixed (EFT) or head-fixed (HFT). For EFT, group median gain was 1.49 at 0.2 Hz declining to 1.08 at 2.8 Hz. For HFT, group median gain was 0.03 at 0.2 Hz increasing to 0.71 at 2.8 Hz. By applying transient head perturbations (peak acceleration > 1,000 degrees s(-2)) during sinusoidal rotation, we determined that Gvor was similar during either EFT or HFT conditions, and contributed only similar to 75% to the compensatory response. We confirmed that retinal image slip contributed to the compensatory response by demonstrating reduced gain during EFT viewing under strobe illumination. Gain also declined during sum-of-sines head rotations, confirming the contribution of predictive mechanisms. The gain of compensatory eye movements was similar during monocular or binocular viewing, although vergence angle was greater during binocular viewing. Comparison with previous studies indicates that mechanisms for generation of eye rotations during near viewing depend on head stimulus type (rotation or translation), waveform (transient or sinusoidal), and the species being tested. C1 Case Western Reserve Univ, Dept Neurol, Dept Vet Affairs Med Ctr, Cleveland, OH 44106 USA. Case Western Reserve Univ, Univ Hosp, Cleveland, OH 44106 USA. Case Western Reserve Univ, Dept Biomed Engn, Dept Vet Affairs Med Ctr, Cleveland, OH 44106 USA. NASA, Lyndon B Johnson Space Ctr, Neurosci Lab, Houston, TX 77058 USA. NASA, Lyndon B Johnson Space Ctr, Wyle Labs, Houston, TX 77058 USA. RP Leigh, RJ (reprint author), Case Western Reserve Univ, Dept Neurol, Dept Vet Affairs Med Ctr, 11100 Euclid Ave, Cleveland, OH 44106 USA. EM rjl4@po.cwru.edu RI Somers, Jeffrey/N-4168-2014 OI Somers, Jeffrey/0000-0003-3347-6614 FU NEI NIH HHS [EY06717] NR 40 TC 7 Z9 7 U1 0 U2 1 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0014-4819 J9 EXP BRAIN RES JI Exp. Brain Res. PD SEP PY 2005 VL 165 IS 3 BP 294 EP 304 DI 10.1007/s00221-005-2305-y PG 11 WC Neurosciences SC Neurosciences & Neurology GA 958OZ UT WOS:000231458900003 PM 15889244 ER PT J AU Busby, MS Mier, KL Brodeur, RD AF Busby, MS Mier, KL Brodeur, RD TI Habitat associations of demersal fishes and crabs in the Pribilof Islands region of the Bering Sea SO FISHERIES RESEARCH LA English DT Article DE fishes; crabs; habitat; ROV; Bering Sea; Pribilof Islands ID CONTINENTAL-SHELF; LOPHOLATILUS-CHAMAELEONTICEPS; ANOMALOUS CONDITIONS; SOUTHEASTERN ALASKA; COMMUNITY STRUCTURE; PACIFIC-OCEAN; DEEP-REEF; SEBASTES; ROCKFISH; BEHAVIOR AB Habitat associations of demersal fishes and crabs were determined from observations of videotapes recorded by a camera-equipped remotely operated vehicle (ROV) in the Bering Sea near the Pribilof Islands in September 1995 and 1997. We identified 42 taxa representing 16 families of fishes and 8 taxa from 3 families of crabs. Families Pleuronectidae (righteye flounders) and Cottidae (sculpins) were represented by the greatest number of taxa. Lepidopsetta polyxystra and Chionoecetes opilio were the most frequently observed fish and crab species. Other fish species in the families Pleuronectidae, Gadidae, Scorpaenidae, Agonidae, and Bathymasteridae were also encountered frequently. Six classifications based on substrate and cover were used to describe the habitat where each fish and crab was observed. Agonids and pleuronectids were typically observed on silt, mud, or sand substrate with no cover while other taxa, particularly cottids and bathymasterids, were encountered in more varieties of habitat including areas covered with rocks and boulders. Significant differences in species composition were found among habitats and stratified depth ranges. Similarity analyses showed that different taxa were responsible for these differences, but within each habitat type and depth range, two to five species contributed to 90% of the average similarity. Some ROV dives were paired with bottom trawls in the same general locations. Species compositions of the ROV observations were significantly correlated with that of the corresponding bottom trawl catch compositions. Overall, we believe that in situ observations provide useful information on fish habitats and behaviors not readily available from conventional trawling surveys. Published by Elsevier B.V. C1 NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Resource Assessment & Conservat Engn Div, Seattle, WA 98115 USA. NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr,Hatfield Marine Sci Ctr, Estuarine & Ocean Ecol Program, Newport, OR 97365 USA. RP Busby, MS (reprint author), NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Resource Assessment & Conservat Engn Div, 7600 Sand Point Way NE,Bldg 4, Seattle, WA 98115 USA. EM morgan.busby@noaa.gov NR 38 TC 10 Z9 11 U1 0 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0165-7836 J9 FISH RES JI Fish Res. PD SEP PY 2005 VL 75 IS 1-3 BP 15 EP 28 DI 10.1016/j.fishres.2005.05.012 PG 14 WC Fisheries SC Fisheries GA 956MP UT WOS:000231304300002 ER PT J AU Chen, C Yokota, R Hasegawa, M Kochi, M Horie, K Hergenrother, P AF Chen, C Yokota, R Hasegawa, M Kochi, M Horie, K Hergenrother, P TI Isomeric biphenyl polyimides. (I) Chemical structure-property relationships SO HIGH PERFORMANCE POLYMERS LA English DT Article; Proceedings Paper CT 5th International Meeting on Step Polymerization or Polycondensation CY SEP 26-30, 2004 CL Roanoke, VA DE polyimides; s-BPDA; a-BPDA; i-BPDA; 3,3 '-ODA; dynamic mechanical thermal analysis; tensile properties ID HIGH THERMOOXIDATIVE STABILITY; THERMO-PROCESSABLE POLYIMIDES; 2,3,3',4'-BIPHENYLTETRACARBOXYLIC DIANHYDRIDE; HIGH-STRENGTH; HIGH-MODULUS; COMPOSITES; FILMS AB A series of polyimides (PIs) were prepared from three biphenyltetracarboxylic dianhydrides (BPDA) isomers, i.e., 3,3',4,4'-BPDA (s-BPDA), 2,3,3',4'-BPDA (a-BPDA), and 2,2",3,3"-BPDA (iBPDA) with various diamines through the conventional two step process. Polymerization reactivity, solubility, and dynamic mechanical properties (T-g, softening behavior, and storage modulus at glassy state) were compared between PIs derived from these BPDA isomers and para/meta diamine isomers. The solubility in NMP increased as follows: i-BPDA-PI > a-BPDA-PI > s-BPDA-PI. The order is attributed to semi-crystalline and fully amorphous morphologies of s-BPDA-PI and other isomeric BPDA-PIs, respectively. The use of meta-diamines lowered the T-g whereas the use of bent/distorted BPDA isomers enhanced the T-g (s-BPDA-PI < a-BPDA-PI < i-BPDA-PI). The BPDA isomer effect on T-g is based on the difficulty of obtaining internal rotation around the biphenyl linkages. The width of the DMA rubbery plateau region decreased in the order of i-BPDA < a-BPDA-PI < s-BPDA-PI, depending on the crystallinity and the extent of chain entanglement. In a-BPDA- and i-BPDA-PI systems, PIs from meta-diamines led to higher modulus than the corresponding PIs from para-diamines. C1 Shizuoka Inst Sci & Technol, Dept Mat & Life Sci, Fac Sci & Engn, Shizuoka 4378555, Japan. Inst Space & Astronaut Sci, Kanagawa 2290022, Japan. Toho Univ, Dept Chem, Fac Sci, Chiba 2748510, Japan. Tokyo Univ Agr & Technol, Fac Engn, Dept Organ & Polymer Mat Chem, Tokyo 1848588, Japan. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Kochi, M (reprint author), Shizuoka Inst Sci & Technol, Dept Mat & Life Sci, Fac Sci & Engn, 2200-2 Toyosawa, Shizuoka 4378555, Japan. EM kochi4096@ybb.ne.jp NR 31 TC 29 Z9 34 U1 6 U2 23 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 SEP PY 2005 VL 17 IS 3 BP 317 EP 333 DI 10.1177/0954008305055556 PG 17 WC Polymer Science SC Polymer Science GA 961ZK UT WOS:000231700600002 ER PT J AU Kochi, M Chen, CH Yokota, R Hasegawa, M Hergenrother, P AF Kochi, M Chen, CH Yokota, R Hasegawa, M Hergenrother, P TI Isomeric biphenyl polyimides. (II) Glass transitions and secondary relaxation processes SO HIGH PERFORMANCE POLYMERS LA English DT Article; Proceedings Paper CT 5th International Meeting on Step Polymerization or Polycondensation CY SEP 26-30, 2004 CL Roanoke, VA DE asymmetric polyimide; BPDA isomer; DMA; WAXD; glass transition; beta relaxation process ID MECHANICAL-PROPERTIES; BLENDS AB Dynamic mechanical analysis was performed on a series of the isomeric polymides (PIs) made from the reaction of s-, a-, and i-BPDA each with 4,4'-ODA, 3,3'-ODA, 1,3,3-APB and 1,4,4-APB. The glass transitions (T(g)s) moved towards higher temperatures in the order of s-, a-, and i-BPDA for the para diamine-based Pls whereas the T-g values showed little change for meta diamine-based PI regardless of the BPDA isomer. Conversely, the temperature of the beta relaxation process increased in the order of i-, a-, and s-BPDA with any diamine. These behaviors can be interpreted in terms of the steric hindrance effects due to the configuration of BPDA isomers and diamines. C1 Shizuoka Inst Sci & Technol, Shizuoka 4378555, Japan. Jilin Univ, Alan G MacDiarmid Inst, Changchun 130023, Peoples R China. Inst Space & Astronaut Sci, Kanagawa 2290022, Japan. Toho Univ, Fac Sci, Dept Chem, Chiba 2748510, Japan. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Kochi, M (reprint author), Shizuoka Inst Sci & Technol, Shizuoka 4378555, Japan. EM kochi4096@ybb.ne.jp NR 16 TC 24 Z9 27 U1 3 U2 19 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 SEP PY 2005 VL 17 IS 3 BP 335 EP 347 DI 10.1177/0954008305055557 PG 13 WC Polymer Science SC Polymer Science GA 961ZK UT WOS:000231700600003 ER PT J AU Dery, SJ Salomonson, VV Stieglitz, M Hall, DK Appel, I AF Dery, SJ Salomonson, VV Stieglitz, M Hall, DK Appel, I TI An approach to using snow areal depletion curves inferred from MODIS and its application to land surface modelling in Alaska SO HYDROLOGICAL PROCESSES LA English DT Article DE Alaska; snow depletion curve; land surface modelling; MODIS; snow ID ATMOSPHERIC BOUNDARY-LAYER; CATCHMENT-BASED APPROACH; BLOWING SNOW; ARCTIC ALASKA; HIGH-LATITUDES; CLIMATE CHANGE; RIVER-BASIN; COVER MAPS; CLEAR-SKY; SIMULATION AB Snowcover areal depletion curves inferred from the moderate resolution imaging spectroradiometer (MODIS) are validated and then applied in NASA ' s catchment-based land surface model (CLSM) for numerical simulations of hydrometeorological processes in the Kuparuk River basin (KRB) of Alaska. The results demonstrate that the MODIS snowcover fraction f derived from a simple relationship in terms of the normalized difference snow index compares well with Landsat values over the range 20 <= f <= 100%. For f < 20%, however, MODIS 500 m subpixel data underestimate the amount of snow by up to 13% compared with Landsat at spatial resolutions of 30 m binned to equivalent 500 m pixels. After a bias correction, MODIS snow areal depletion curves during the spring transition period of 2002 for the KRB exhibit similar features to those derived from surface-based observations. These results are applied in the CLSM subgrid-scale snow parameterization that includes a deep and a shallow snowcover fraction. Simulations of the evolution of the snowpack and of freshwater discharge rates for the KRB over a period of I I years are then analysed with the inclusion of this feature. It is shown that persistent snowdrifts on the arctic landscape, associated with a secondary plateau in the snow areal depletion curves, are hydrologically important. An automated method is developed to generate the shallow and deep snowcover fractions from MODIS snow areal depletion curves. This provides the means to apply the CLSM subgrid-scale snow parameterization in all watersheds subject to seasonal snowcovers. Improved simulations and predictions of the global surface energy and water budgets are expected with the incorporation of the MODIS snow data into the CLSM. Copyright (c) 2005 John Wiley & Sons, Ltd. C1 Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. NASA, Goddard Space Flight Ctr, Earth Sci Directorate, Greenbelt, MD 20771 USA. Georgia Inst Technol, Sch Civil & Environm Engn, Atlanta, GA 30332 USA. Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. Raytheon ITSS, Upper Marlboro, MD USA. RP Dery, SJ (reprint author), Princeton Univ, Program Atmospher & Ocean Sci, 307 GFDL, Princeton, NJ 08544 USA. EM sdery@princeton.edu RI Appel, Igor/E-7940-2011; Hall, Dorothy/D-5562-2012 OI Appel, Igor/0000-0003-0907-3807; NR 60 TC 57 Z9 61 U1 0 U2 11 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND SN 0885-6087 J9 HYDROL PROCESS JI Hydrol. Process. PD SEP PY 2005 VL 19 IS 14 BP 2755 EP 2774 DI 10.1002/hyp.5784 PG 20 WC Water Resources SC Water Resources GA 969CE UT WOS:000232210200007 ER PT J AU Friedson, AJ AF Friedson, AJ TI Water, ammonia, and H2S mixing ratios in Jupiter's five-micron hot spots: A dynamical model SO ICARUS LA English DT Article DE Jupiter; atmosphere; dynamics; composition ID ATMOSPHERIC GRAVITY-WAVES; PROBE MASS-SPECTROMETER; MEAN ZONAL FLOW; GALILEO PROBE; CLOUD STRUCTURE; VERTICAL STRUCTURE; EQUATORIAL REGION; GIANT PLANETS; ENTRY SITE; CONVECTION AB The Galileo probe entered the jovian atmosphere at the southern edge of a 5-micron hot spot, one of typically 8-10 quasi-evenly-spaced longitudinal areas of anomalously high 5-micron IR emission that reside in a narrow latitude band centered on +7.5 degrees. These hot spots are characterized primarily by a low abundance of the cloud particles that dominate the 5-micron opacity at other locations on the planet, and by significant desiccation of ammonia, water and hydrogen sulfide in the upper layers of the troposphere. Ortiz et al. [1998. Evolution and persistence of 5-micron hot spots at the Galileo probe entry latitude. J. Geophys. Res. 103, 23,051-23,069] found that the latitude and drift rate of the hot spots could be explained if they are formed by an equatorially trapped Rossby wave of meridional degree 1 moving with a phase speed between 99 and 103 m s(-1) relative to System III. Here we model additional properties of the hot spots in terms of the amplitude saturation of such a wave propagating in the weakly stratified deep troposphere. We identify the hot spots with locations where the wave plus mean thermal stratification becomes marginally stable. In these locations, potential temperature isotherms stretch downward to very deep levels in the troposphere. Since fluid parcels follow these isotherms under adiabatic flow conditions, the parcels dive downward when they enter the portion of the wave associated with the hot spot and soar upward upon leaving the spot. We show that this model can account for the anomalous vertical profiles of NH3, H2O, and H2S mixing ratio measured by the Galileo probe. Pressures vary by as much as 20 bar over potential temperature isotherms in solutions that produce sufficient desiccation of water and H2S in hot spots. Approximately 6 x 10(-2) of Jupiter's internal heat flux must be tapped to maintain the wave over the mean hot spot lifetime of 10(7) s. The results suggest that the phenomenon that causes hot spots may occur widely, although in less dramatic form, across Jupiter's surface, and consequently NH3, H2S, and H2O mixing ratio profiles may vary significantly from location to location in Jupiter's troposphere. (c) 2005 Elsevier Inc. All rights reserved. C1 CALTECH, Jet Prop Lab, Div Earth & Space Sci, Pasadena, CA 91109 USA. RP Friedson, AJ (reprint author), CALTECH, Jet Prop Lab, Div Earth & Space Sci, MS 169-237, Pasadena, CA 91109 USA. EM andrew.j.friedson@jpl.nasa.gov NR 42 TC 19 Z9 19 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 SEP PY 2005 VL 177 IS 1 BP 1 EP 17 DI 10.1016/j.icarus.2005.03.004 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958XL UT WOS:000231481400001 ER PT J AU Williams, DA Keszthelyi, LP Schenk, PM Milazzo, MP Lopes, RMC Rathbun, JA Greeley, R AF Williams, DA Keszthelyi, LP Schenk, PM Milazzo, MP Lopes, RMC Rathbun, JA Greeley, R TI The Zamama-Thor region of Io: Insights from a synthesis of mapping, topography, and Galileo spacecraft data SO ICARUS LA English DT Article DE satellites of Jupiter Io; geological processes; volcanism; surfaces (satellite) ID JUPITERS MOON IO; SILICATE VOLCANISM; PHOTOPOLARIMETER-RADIOMETER; ACTIVE VOLCANISM; SATELLITE IO; IMAGING DATA; SULFUR FLOW; LAVA FLOWS; SO2 FROST; HOT-SPOTS AB We have studied data from the Galileo spacecraft's three remote sensing instruments (Solid-State Imager (SSI), Near-Infrared Mapping Spectrometer (NIMS), and Photopolarimeter-Radiometer (PPR)) covering the Zamama-Thor region of Io's antijovian hemisphere, and produced a geomorphological map of this region. This is the third of three regional maps we are producing from the Galileo spacecraft data. Our goal is to assess the variety of volcanic and tectonic materials and their interrelationships on Io using planetary mapping techniques, supplemented with all available Galileo remote sensing data. Based on the Galileo data analysis and our mapping, we have determined that the most recent geologic activity in the Zamama-Thor region has been dominated by two sites of large-scale volcanic surface changes. The Zamama Eruptive Center is a site of both explosive and effusive eruptions, which emanate from two relatively steep edifices (Zamama Tholi A and B) that appear to be built by both silicate and sulfur volcanism. A similar to 100-km long flow field formed sometime after the 1979 Voyager flybys, which appears to be a site of promethean-style compound flows, flow-front SO2 plumes, and adjacent sulfur flows. Larger, possibly stealthy, plumes have on at least one occasion during the Galileo mission tapped a source that probably includes S and/or Cl to produce a red pyroclastic deposit from the same vent from which silicate lavas were erupted. The Thor Eruptive Center, which may have been active prior to Voyager, became active again during the Galileo mission between May and August 2001. A pillanian-style eruption at Thor included the tallest plume observed to date on to (at least 500 km high) and new dark lava flows. The plume produced a central dark pyroclastic deposit (probably silicate-rich) and an outlying white diffuse ring that is SO2-rich. Mapping shows that several of the new dark lava flows around the plume vent have reoccupied sites of earlier flows. Unlike most of the other pillanian eruptions observed during the Galileo mission, the 2001 Thor eruption did not produce a large red ring deposit, indicating a relative lack of S and/or Cl gases interacting with the magma during that eruption. Between these two eruptive centers are two paterae, Thomagata and Reshef. Thomagata Patera is located on a large shield-like mesa and shows no signs of activity. In contrast, Reshef Patera is located on a large, irregular mesa that is apparently undergoing degradation through erosion (perhaps from SO2-sapping or chemical decomposition of sulfur-rich material) from multiple secondary volcanic centers. (c) 2005 Elsevier Inc. All rights reserved. C1 Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. US Geol Survey, Astrogeol Team, Flagstaff, AZ 86001 USA. Lunar & Planetary Inst, Houston, TX 77058 USA. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ USA. NASA, Jet Propuls Lab, Pasadena, CA USA. Univ Redlands, Dept Phys, Redlands, CA 92373 USA. RP Williams, DA (reprint author), Arizona State Univ, Dept Geol Sci, Box 871404, Tempe, AZ 85287 USA. EM david.williams@asu.edu RI Lopes, Rosaly/D-1608-2016 OI Lopes, Rosaly/0000-0002-7928-3167 NR 76 TC 12 Z9 12 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 SEP PY 2005 VL 177 IS 1 BP 69 EP 88 DI 10.1016/j.icarus.2005.03.005 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958XL UT WOS:000231481400005 ER PT J AU Kimura, Y Tamura, K Koike, C Chihara, H Kaito, C AF Kimura, Y Tamura, K Koike, C Chihara, H Kaito, C TI Laboratory production of monophase pyrrhotite grains using solid-solid reaction and their characteristic infrared spectra SO ICARUS LA English DT Article DE infrared observations; interplanetary dust; solar nebula ID INTERPLANETARY DUST PARTICLE; IRON-NICKEL SULFIDES; CARBON-RICH STARS; PLANETARY-NEBULAE; SOLAR NEBULA; KINETICS AB A new method of producing pyrrhotite grains, which are most commonly found in cometary material and interplanetary dust particles, was developed. Pyrrhotite grains in the monophase having a 7C structure were predominately produced using a solid-solid reaction between iron and sulfur grains at room temperature. The characteristic infrared peaks were observed at 602, 563, and 397 cm(-1) (16.6, 17.8, and 25.2 mu m). (c) 2005 Elsevier Inc. All rights reserved. C1 Ritsumeikan Univ, Dept Phys, Shiga 5258577, Japan. Kyoto Pharmaceut Univ, Phys Lab, Kyoto 6078414, Japan. Osaka Univ, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. RP Kimura, Y (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Astrochem Lab, Code 691, Greenbelt, MD 20771 USA. EM ykimura@lepvax.gsfc.nasa.gov RI Kimura, Yuki/J-9635-2014 OI Kimura, Yuki/0000-0002-9218-7663 NR 20 TC 2 Z9 2 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD SEP PY 2005 VL 177 IS 1 BP 280 EP 285 DI 10.1016/j.icarus.2005.03.003 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958XL UT WOS:000231481400021 ER PT J AU Han, CM Huang, J Chang, K AF Han, CM Huang, J Chang, K TI A high efficiency offset-fed X/Ka-dual-band reflectarray using thin membranes SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION LA English DT Article DE circular polarization; inflatable membrane; microstrip ring; reflectarray antenna; variable rotation ID CIRCULARLY-POLARIZED REFLECTARRAY; VARIABLE ROTATION ANGLES; MICROSTRIP RING ELEMENTS; ANTENNA; PATCHES; DESIGN; SIZE AB Modern space-borne applications require large-aperture antennas having capabilities of low mass and high packaging efficiency to overcome the launch vehicle size and weight restrictions. This paper presents a dual-band reflectarray antenna developed for future space inflatable structures with thin membranes. To offset the effects of the thin-membrane substrates required in the inflatable structure, foam layers are inserted below the X and Ka band membranes, allowing broadband CP performance at both bands. More than 50% efficiencies are achieved at both frequency bands, showing potential for even larger high-gain inflatable antennas for future space applications. C1 Texas A&M Univ, Dept Elect Engn, College Stn, TX 77843 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Han, CM (reprint author), Texas A&M Univ, Dept Elect Engn, College Stn, TX 77843 USA. EM hcj-fals@ee.tamu.edu; jhuang@pop.jpl.nasa.gov; chang@ee.tamu.edu NR 16 TC 29 Z9 33 U1 1 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-926X J9 IEEE T ANTENN PROPAG JI IEEE Trans. Antennas Propag. PD SEP PY 2005 VL 53 IS 9 BP 2792 EP 2798 DI 10.1109/TAP.2005.854531 PG 7 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 963TY UT WOS:000231830100002 ER PT J AU Lall, P Singh, N Suhling, JC Strickland, M Blanche, J AF Lall, P Singh, N Suhling, JC Strickland, M Blanche, J TI Thermo-mechanical reliability tradeoffs for deployment of area array packages in harsh environments SO IEEE TRANSACTIONS ON COMPONENTS AND PACKAGING TECHNOLOGIES LA English DT Article; Proceedings Paper CT 9th Intersociety Conference on Thermal and Thermomechanical Phenomena in Electronic Systems CY JUN 01-04, 2004 CL Las Vegas, NV SP IEEE, CPMT, Amer Soc Mech Engineers, 50th ECTC, Int Microelect & Packaging Soc DE ball grid array (BGA); design guidelines; solder joint fatigue; statistical model; thermal reliability prediction ID FATIGUE; LIFE; BGA AB Fine-pitch ball grid arrays (BGAs) and underfills have been used in benign office environments and wireless applications for a number of years, however their reliability in harsh environments is not well understood. In this work, the design guidelines development effort for deployment of fine-pitch ball-grid array packages in the harsh environments have been presented. Guidelines are targeted toward government contractors, OEMs, and third party contract manufacturers who intend to select part architectures and board designs based on specified mission requirements. The guidelines are intended as an aid for understanding the sensitivity of component reliability to geometry, package architecture, material properties and board attributes in different thermal environments in order to quantitatively evaluate the impact of these parameters on the component reliability. The intent is to develop a tool for doing tradeoffs between geometry, materials and quantitatively evaluating the impact on reliability. Sensitivity relations for geometry, materials, and architectures based on statistical models and failure mechanics based closed form models have been developed. Convergence between statistical model sensitivities and failure mechanics based sensitivities has been demonstrated. Predictions of sensitivities have been validated against experimental test data. C1 Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA. Auburn Univ, NSF, CAVE, Auburn, AL 36849 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Lall, P (reprint author), Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA. EM lall@eng.auburn.edu RI Suhling, Jeffrey/M-8391-2014 NR 25 TC 15 Z9 15 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1521-3331 J9 IEEE T COMPON PACK T JI IEEE Trans. Compon. Packaging Technol. PD SEP PY 2005 VL 28 IS 3 BP 457 EP 466 DI 10.1109/TCAPT.2005.854162 PG 10 WC Engineering, Manufacturing; Engineering, Electrical & Electronic; Materials Science, Multidisciplinary SC Engineering; Materials Science GA 960GG UT WOS:000231577700010 ER PT J AU Cooper, MS AF Cooper, MS TI Investigation of Arrhenius acceleration factor for integrated circuit early life failure region with several failure mechanisms SO IEEE TRANSACTIONS ON COMPONENTS AND PACKAGING TECHNOLOGIES LA English DT Article; Proceedings Paper CT 9th Intersociety Conference on Thermal and Thermomechanical Phenomena in Electronic Systems CY JUN 01-04, 2004 CL Las Vegas, NV SP IEEE, CPMT, Amer Soc Mech Engineers, 50th ECTC, Int Microelect & Packaging Soc DE Arrhenius activation energy; Arrhenius equation; infant mortality failure characteristics; mixed population failure mechanisms; Weibull distribution AB Use of the Arrhenius equation for analysis of burn-in and life test data has been called into question in recent years. Validity of the Arrhenius activation energy is asserted to be restricted to only one failure mechanism. Therefore, if multiple failure mechanisms apply to an integrated circuit type, the temperature acceleration factor must be complex. In this study a model is constructed using the Weibull distribution for the failure rate applicable when there are multiple failure mechanisms. In this model a different Arrhenius activation energy corresponds to each failure mechanism. It is shown that under conditions expected to be valid for most integrated circuits, an empirical effective Arrhenius activation energy can be computed that is valid for life test data taken under typical conditions to better than 10%. This provides some justification for the continued usage of a simple Arrhenius equation as an empirical model to analyze life test data. C1 Jet Prop Lab, Pasadena, CA 91109 USA. RP Cooper, MS (reprint author), Jet Prop Lab, Pasadena, CA 91109 USA. EM mark.s.cooper@jpl.nasa.gov NR 8 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 1521-3331 J9 IEEE T COMPON PACK T JI IEEE Trans. Compon. Packaging Technol. PD SEP PY 2005 VL 28 IS 3 BP 561 EP 563 DI 10.1109/TCAPT.2005.848581 PG 3 WC Engineering, Manufacturing; Engineering, Electrical & Electronic; Materials Science, Multidisciplinary SC Engineering; Materials Science GA 960GG UT WOS:000231577700023 ER PT J AU Hook, SJ Clodius, WB Balick, L Alley, RE Abtahi, A Richards, RC Schladow, SG AF Hook, SJ Clodius, WB Balick, L Alley, RE Abtahi, A Richards, RC Schladow, SG TI In-flight validation of mid- and thermal infrared data from the Multispectral Thermal Imager (MTI) using an automated high-altitude validation site at Lake Tahoe CA/NV, USA SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE calibration; radiance; temperature; thermal infrared; validation ID SEA-SURFACE TEMPERATURE; TRACK SCANNING RADIOMETER; COOL-SKIN; CALIBRATION; TRANSPORT; BULK; RETRIEVAL; SHEAR; WATER AB The Multispectral Thermal Imager (MTI) is a 15-band satellite-based imaging system. Two of the bands (J, K) are located in the mid-infrared (3-5 mu m) wavelength region: J, 3.5-4.1 mu m and K, 4.9-5.1 mu m, and three of the bands (L, M, N) are located in the thermal infrared (8-12 mu m) wavelength region: L, 8.0-8.4 mu m; M, 8.4-8.8 mu m; and N, 10.2-10.7 mu m. The absolute radiometric accuracy of the MTI data acquired in bands J-N was assessed over a period of approximately three years using data from the Lake Tahoe, CA/NV, automated validation site. Assessment involved using a radiative transfer model to propagate surface skin temperature measurements made at the time of the MTI overpass to predict the vicarious at-sensor radiance. The vicarious at-sensor radiance was convolved with the MTI system response functions to obtain the vicarious at-sensor MTI radiance in bands J-N. The vicarious radiances were then compared with the instrument measured radiances. In order to avoid any reflected solar contribution in the mid-infrared bands, only nighttime scenes were used in the analysis of bands J and K. Twelve cloud-free scenes were used in the analysis of the data from the mid-infrared bands (J, K), and 23 cloud-free scenes were used in the analysis of the thermal infrared bands (L, M, N). The scenes had skin temperatures ranging between 4.4 and 18.6 degrees C. The skin temperature was found to be, on average, 0.18 +/- 0.36 degrees C cooler than the bulk temperature during the day and 0.65 +/- 0.31 degrees C cooler than the bulk temperature at night. The smaller skin effect during the day was attributed to solar heating. The mean and standard deviation of the percent differences between the vicarious (predicted) at-sensor radiance convolved to the MTI bandpasses and the MTI measured radiances were -1.38 +/- 2.32, -2.46 +/- 1.96, -0.04 +/- 0.78, -1.97 +/- 0.62, -1.59 +/- 0.55 for bands J-N, respectively. The results indicate that, with the exception of band L, the instrument measured radiances are warmer than expected. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Univ Calif Davis, Dept Environm Sci & Policy, Tahoe Res Grp, Davis, CA 95616 USA. Univ Calif Davis, Dept Civil & Environm Engn, Davis, CA 95616 USA. RP Hook, SJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 26 TC 14 Z9 14 U1 4 U2 7 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD SEP PY 2005 VL 43 IS 9 BP 1991 EP 1999 DI 10.1109/TGRS.2005.853191 PG 9 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 959TM UT WOS:000231542200006 ER PT J AU Le Vine, DM Abraham, S Kerr, YH Wilson, WJ Skou, N Sobjaerg, SS AF Le Vine, DM Abraham, S Kerr, YH Wilson, WJ Skou, N Sobjaerg, SS TI Comparison of model prediction with measurements of galactic background noise at L-band SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE galactic background; microwave radiometry; remote sensing ID RADIO-CONTINUUM SURVEY; SEA-SURFACE SALINITY; SOUTHERN SKY; 1420 MHZ; SPACE AB The spectral window at L-band (1.413 GHz) is important for passive remote sensing of surface parameters such as soil moisture and sea surface salinity that are needed to understand the hydrological cycle and ocean circulation. Radiation from celestial sources (mostly galactic) is strong in this window, and an accurate accounting of this background radiation is often needed for calibration. This paper presents a comparison of the background radiation predicted by a model developed from modern radio astronomy measurements with measurements made with several modern L-band remote sensing radiometers. The comparison validates the model and illustrates the magnitude of the correction necessary in remote sensing applications. C1 Goddard Space Flight Ctr, Instrumentat Sci Branch, Greenbelt, MD 20771 USA. CESBIO, F-31401 Toulouse, France. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Tech Univ Denmark, DK-2800 Lyngby, Denmark. RP Le Vine, DM (reprint author), Goddard Space Flight Ctr, Instrumentat Sci Branch, Greenbelt, MD 20771 USA. EM David.M.LeVine@nasa.gov; Saji.Abraham@gsfc.nasa.gov; Yann.Kerr@cesbio.cnes.fr; william.j.wilson@jpl.nasa.gov NR 25 TC 6 Z9 6 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD SEP PY 2005 VL 43 IS 9 BP 2018 EP 2023 DI 10.1109/TGRS.2005.853190 PG 6 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 959TM UT WOS:000231542200009 ER PT J AU Merlin, O Chehbouni, AG Kerr, YH Njoku, EG Entekhabi, D AF Merlin, O Chehbouni, AG Kerr, YH Njoku, EG Entekhabi, D TI A combined modeling and multipectral/multiresolution remote sensing approach for disaggregation of surface soil moisture: Application to SMOS configuration SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE disaggregation; multispectral remote sensing; Soil Moisture and Ocean Salinity (SMOS) mission; surface soil moisture; synergy ID DIRECTIONAL RADIOMETRIC TEMPERATURES; MICROWAVE EMISSION; HIGH-RESOLUTION; COMPONENT TEMPERATURES; VEGETATION; PARAMETERIZATION; RETRIEVAL; CANOPY; SCHEME; VARIABILITY AB A new physically based disaggregation method is developed to improve the spatial resolution of the surface soil moisture extracted from the Soil Moisture and Ocean Salinity (SMOS) data. The approach combines the 40-km resolution SMOS multiangular brightness temperatures and 1-km resolution auxiliary data composed of visible, near-infrared, and thermal infrared remote sensing data and all the surface variables involved in the modeling of land surface-atmosphere interaction available at this scale (soil texture, atmospheric forcing, etc.). The method successively estimates a relative spatial distribution of soil moisture with fine-scale auxiliary data, and normalizes this distribution at SMOS resolution with SMOS data. The main assumption relies on the relationship between the radiometric soil temperature inverted from the thermal infrared and the microwave soil moisture. Based on synthetic data generated with a land surface model, it is shown that the radiometric soil temperature can be used as a tracer of the spatial variability of the 0-5 cm soil moisture. A sensitivity analysis shows that the algorithm remains stable for big uncertainties in auxiliary data and that the uncertainty in SMOS observation seems to be the limiting factor. Finally, a simple application to the SGP97/AVHRR data illustrates the usefulness of the approach. C1 CESBIO, F-31401 Toulouse, France. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. MIT, Dept Civil & Environm Engn, Cambridge, MA 02139 USA. RP Merlin, O (reprint author), CESBIO, F-31401 Toulouse, France. EM olivier.merlin@cesbio.cnes.fr; Yann.Kerr@cesbio.cnes.fr NR 44 TC 45 Z9 47 U1 3 U2 13 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD SEP PY 2005 VL 43 IS 9 BP 2036 EP 2050 DI 10.1109/TGRS.2005.853192 PG 15 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 959TM UT WOS:000231542200011 ER PT J AU Mundt, CW Montgomery, KN Udoh, UE Barker, VN Thonier, GC Tellier, AM Ricks, RD Darling, RB Cagle, YD Cabrol, NA Ruoss, SJ Swain, JL Hines, JW Kovacs, GTA AF Mundt, CW Montgomery, KN Udoh, UE Barker, VN Thonier, GC Tellier, AM Ricks, RD Darling, RB Cagle, YD Cabrol, NA Ruoss, SJ Swain, JL Hines, JW Kovacs, GTA TI A multiparameter wearable physiologic monitoring system for space and terrestrial applications SO IEEE TRANSACTIONS ON INFORMATION TECHNOLOGY IN BIOMEDICINE LA English DT Article; Proceedings Paper CT International Workshop on New Generation of Smart Wearable Health Systems and Applications CY DEC 11-14, 2003 CL Lucca, ITALY DE ambulatory physiologic monitoring; bluetooth crew physiologic observation device (CPOD); electrocardiogram (ECG); high altitude; LifeGuard; respiration; vital-signs; wearable ID TELEMEDICINE; ECG AB A novel, unobtrusive and wearable, multiparameter ambulatory physiologic monitoring system for space and terrestrial applications, termed LifeGuard, is presented. The core element is a wearable monitor, the crew physiologic observation device (CPOD), that provides the capability to continuously record two standard electrocardiogram leads, respiration rate via impedance plethysmography, heart rate, hemoglobin oxygen saturation, ambient or body temperature, three axes of acceleration, and blood pressure. These parameters can be digitally recorded with high fidelity over a 9-h period with precise time stamps and user-defined event markers. Data can be continuously streamed to a base station using a built-in Bluetooth RF link or stored in 32 MB of on-board flash memory and downloaded to a personal computer using a serial port. The device is powered by two AAA batteries. The design, laboratory, and field testing of the wearable monitors are described. C1 Stanford Univ, Stanford, CA 94304 USA. NASA, Ames Res Ctr, Moffett Field, CA 94305 USA. Univ Washington, Seattle, WA 98195 USA. RP Mundt, CW (reprint author), Stanford Univ, Stanford, CA 94304 USA. EM cmundt@mail.arc.nasa.gov; kovacs@cis.stanford.edu NR 21 TC 84 Z9 86 U1 3 U2 15 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1089-7771 J9 IEEE T INF TECHNOL B JI IEEE T. Inf. Technol. Biomed. PD SEP PY 2005 VL 9 IS 3 BP 382 EP 391 DI 10.1109/TITB.2005.854509 PG 10 WC Computer Science, Information Systems; Computer Science, Interdisciplinary Applications; Mathematical & Computational Biology; Medical Informatics SC Computer Science; Mathematical & Computational Biology; Medical Informatics GA 962QO UT WOS:000231747500010 PM 16167692 ER PT J AU Kuhn, WB Mojarradi, MM Moussessian, A AF Kuhn, WB Mojarradi, MM Moussessian, A TI A resonant switch for LNA protection in watt-level CMOS transceivers SO IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES LA English DT Article; Proceedings Paper CT 16th Asia-Pacific Microwave Conference CY DEC 15-18, 2004 CL New Delhi, INDIA DE CMOS transceivers; low-noise amplifier (LNA); transmit/receive (T/R) switch ID AMPLIFIER; 2.4-GHZ AB An integrated resonant switch designed to protect low-noise amplifier (LNA) circuits in CMOS transceivers is reported. The design implements the receive-path portion of a transmit/receive switch protecting 3-V-process transistors from 5 W (22-V peak) transmit signals while simultaneously helping to achieve a good LNA noise figure on receive and low power loss on transmit. Since the approach is to combine an LNA's matching, network and switch functions, the design has no traditional insertion loss on receive. The effective loss to the transmitted signal is less than 0.5 dB using moderate quality inductors (Q > 6) and 0.1 dB using Q = 12 inductors achievable in most RF-aware CMOS silicon-on-insulator foundries at UHF through S-band frequencies. C1 Kansas State Univ, Dept Elect & Comp Engn, Manhattan, KS 66506 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kuhn, WB (reprint author), Kansas State Univ, Dept Elect & Comp Engn, Manhattan, KS 66506 USA. EM wkuhn@ksu.edu NR 11 TC 6 Z9 7 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9480 J9 IEEE T MICROW THEORY JI IEEE Trans. Microw. Theory Tech. PD SEP PY 2005 VL 53 IS 9 SI SI BP 2819 EP 2825 DI 10.1109/TMTT.2005.854176 PG 7 WC Engineering, Electrical & Electronic SC Engineering GA 962HI UT WOS:000231721300022 ER PT J AU Maestrini, A Ward, JS Gill, JJ Javadi, HS Schlecht, E Tripon-Canseliet, C Chattopadhyay, G Mehdi, I AF Maestrini, A Ward, JS Gill, JJ Javadi, HS Schlecht, E Tripon-Canseliet, C Chattopadhyay, G Mehdi, I TI A 540-640-GHz high-efficiency four-anode frequency tripler SO IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES LA English DT Article; Proceedings Paper CT 16th Asia-Pacific Microwave Conference CY DEC 15-18, 2004 CL New Delhi, INDIA DE balanced tripler; frequency multiplier; frequency tripler; local oscillator; planar diode; Schottky diode; sextupler; submillimeter wavelengths; varactor ID SUBMILLIMETER WAVELENGTHS; LOCAL OSCILLATOR; SCHOTTKY VARACTOR; MILLIMETER-WAVE; TUNNEL-JUNCTIONS; MULTIPLIERS; GHZ; DIODES; THZ; PERFORMANCE AB We report on the design and performance of a broad-band, high-power 540-640-GHz fix-tuned balanced frequency tripler chip that utilizes four planar Schottky anodes. The suspended strip-line circuit is fabricated with a 12-mu m-thick support frame and is mounted in a split waveguide block. The chip is supported by thick beam leads that are also used to provide precise RF grounding. At room temperature, the tripler delivers 0.9-1.8 mW across the band with an estimated efficiency of 4.5%-9%. When cooled to 120 K, the tripler provides 2.0-4.2 mW across the band with an estimated efficiency of 8%-12%. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Observ Paris, Lab Etude Rayonnement & Mat Astrophys, F-75014 Paris, France. RP Maestrini, A (reprint author), Univ Paris 06, Lab Instruments & Syst Ile France, F-75252 Paris, France. EM alain.maestrini@lisif.jussieu.fr NR 58 TC 70 Z9 75 U1 1 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9480 J9 IEEE T MICROW THEORY JI IEEE Trans. Microw. Theory Tech. PD SEP PY 2005 VL 53 IS 9 SI SI BP 2835 EP 2843 DI 10.1109/TMTT.2005.854174 PG 9 WC Engineering, Electrical & Electronic SC Engineering GA 962HI UT WOS:000231721300024 ER PT J AU Svizhenko, A Anantram, MP Govindan, TR AF Svizhenko, A Anantram, MP Govindan, TR TI Ballistic transport and electrostatics in metallic carbon nanotubes SO IEEE TRANSACTIONS ON NANOTECHNOLOGY LA English DT Article DE ballistic transport; carbon nanotubes; inter-connects; modeling; nanowires ID CURRENT-CARRYING CAPACITY; ELECTRICAL-TRANSPORT; CURRENT SATURATION; CONTACT AB We calculate the current and electrostatic potential drop in metallic carbon nanotube wires self-consistently by solving the Green's function and electrostatics equations in the ballistic case. About one-tenth of the applied voltage drops across the bulk of a nanowire, independent of the lengths considered here. The remaining nine-tenths of the bias drops near the contacts, thereby creating a nonlinear potential drop. The scaling of the electric field at the center of the nanotube with length (L) is faster than 1/L (roughly 1/L1.25-1.75). At room temperature, the low bias conductance of larger-diameter nanotubes is larger than 4e(2)/h due to occupation of noncrossing subbands. The physics of conductance evolution with bias due to Zener tunneling in noncrossing subbands is discussed. C1 NASA, Ames Res Ctr, Ctr Nanotechnol Natl Aeronaut & Space Adm, Moffett Field, CA 94035 USA. RP Svizhenko, A (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol Natl Aeronaut & Space Adm, Moffett Field, Moffett Field, CA 94035 USA. EM svizhenk@nas.nasa.gov; anant@nas.nasa.gov; govindan@nas.nasa.gov NR 24 TC 32 Z9 32 U1 2 U2 12 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1536-125X J9 IEEE T NANOTECHNOL JI IEEE Trans. Nanotechnol. PD SEP PY 2005 VL 4 IS 5 BP 557 EP 562 DI 10.1109/TNANO.2005.851409 PG 6 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Science & Technology - Other Topics; Materials Science; Physics GA 963MX UT WOS:000231809500012 ER PT J AU Thomson, F Asmar, S Oudrhiri, K AF Thomson, F Asmar, S Oudrhiri, K TI Limitations on the use of the power-law form of S-y(f) to compute Allan variance SO IEEE TRANSACTIONS ON ULTRASONICS FERROELECTRICS AND FREQUENCY CONTROL LA English DT Article AB An exact solution to the well-known integral transform that relates the spectral density of the instantaneous fractional frequency deviation, S-y(f), to the Allan variance, sigma(y)(2)(Tau), is presented for the case of a power-law representation of S-y(f). The approximate solution to this integral transform, which is found. throughout the literature, also is derived. A graphical convergence analysis is presented, showing the range of applicability of the approximate solution. The results reinforce the use of the approximate solution, which converges quickly to the exact solution under virtually all reasonable measurement conditions. C1 Stanford Univ, Stanford, CA 94305 USA. CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Thomson, F (reprint author), Stanford Univ, Stanford, CA 94305 USA. EM fthomson@stanford.edu NR 4 TC 1 Z9 1 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0885-3010 J9 IEEE T ULTRASON FERR JI IEEE Trans. Ultrason. Ferroelectr. Freq. Control PD SEP PY 2005 VL 52 IS 9 BP 1468 EP 1472 DI 10.1109/TUFFC.2005.1516018 PG 5 WC Acoustics; Engineering, Electrical & Electronic SC Acoustics; Engineering GA 971YD UT WOS:000232420000005 PM 16285444 ER PT J AU Draper, SL Lerch, BA Locci, IE Shazly, M Prakash, V AF Draper, SL Lerch, BA Locci, IE Shazly, M Prakash, V TI Effect of exposure on the mechanical properties of Gamma MET PX SO INTERMETALLICS LA English DT Article; Proceedings Paper CT 2nd IRC International TiAl Workshop CY JUL 05-07, 2004 CL Univ Birmingham, Birmingham, ENGLAND SP IRC HO Univ Birmingham DE titanium aluminides; based on TiAl; brittleness and ductility; environmental embrittlement; fracture toughness; oxidation ID TEMPERATURE EXPOSURE; ALLOY AB The effect of a service environment exposure on the mechanical properties of a high Nb content TiAl alloy, Gamma MET PX1, was assessed. Gamma MET PX, like other TiAl alloys, experiences a reduction of ductility following high temperature exposure. Exposure in Ar, air, and high-purity oxygen all resulted in a loss of ductility with the ductility reduction increasing with oxygen content in the exposure atmosphere. Embrittling mechanisms, including bulk microstructural changes, moisture induced environmental embrittlement, and near surface effects were investigated. The embrittlement has been shown to be a near-surface effect, most likely due to the diffusion of oxygen into the alloy. (c) 2005 Elsevier Ltd. All rights reserved. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. Case Western Reserve Univ, Cleveland, OH 44106 USA. RP Draper, SL (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. NR 14 TC 17 Z9 19 U1 2 U2 4 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0966-9795 J9 INTERMETALLICS JI Intermetallics PD SEP PY 2005 VL 13 IS 9 SI SI BP 1014 EP 1019 DI 10.1016/j.intermet.2004.12.015 PG 6 WC Chemistry, Physical; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Chemistry; Materials Science; Metallurgy & Metallurgical Engineering GA 936PS UT WOS:000229868500017 ER PT J AU Wang, XF Zhang, NL AF Wang, XF Zhang, NL TI Numerical analysis of heat transfer in pulsating turbulent flow in a pipe SO INTERNATIONAL JOURNAL OF HEAT AND MASS TRANSFER LA English DT Article DE convection heat transfer; pulsating flow; turbulent modeling; large velocity amplitude; Womersley number; numerical calculation ID COMBUSTOR TAIL-PIPE; WALL SHEAR-STRESS; OSCILLATING FLOW; TRANSFER COEFFICIENT; 2-EQUATION MODEL; ENHANCEMENT; PREDICTION AB Convection heat transfer in pulsating turbulent flow with large velocity oscillating amplitudes in a pipe at constant wall temperature is numerically studied. A low-Reynolds-number (LRN) k-epsilon turbulent model is used in the turbulence modeling. The model analysis indicates that Womersley number is a very important parameter in the study of pulsating flow and heat transfer. Flow and heat transfer in a wide range of process parameters are investigated to reveal the velocity and temperature characteristics of the flow. The numerical calculation results show that in a pulsating turbulent flow there is an optimum Womersley number at which heat transfer is maximally enhanced. Both larger amplitude of velocity oscillation and flow reversal in the pulsating turbulent flow also greatly promote the heat transfer enhancement. (c) 2005 Elsevier Ltd. All rights reserved. C1 NASA, Glenn Res Ctr Lewis Field, Micrograv Sci Div, Cleveland, OH 44135 USA. Univ Nebraska, Dept Mech Engn, Lincoln, NE 68588 USA. RP NASA, Glenn Res Ctr Lewis Field, Micrograv Sci Div, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM nengli.zhang@grc.nasa.gov NR 49 TC 41 Z9 47 U1 3 U2 18 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0017-9310 EI 1879-2189 J9 INT J HEAT MASS TRAN JI Int. J. Heat Mass Transf. PD SEP PY 2005 VL 48 IS 19-20 BP 3957 EP 3970 DI 10.1016/j.ijheatmasstransfer.2005.04.011 PG 14 WC Thermodynamics; Engineering, Mechanical; Mechanics SC Thermodynamics; Engineering; Mechanics GA 959AU UT WOS:000231490100005 ER PT J AU Putman, WM Lin, SJ Shen, BW AF Putman, WM Lin, SJ Shen, BW TI Cross-platform performance of a portable communication module and the NASA finite volume general circulation model SO INTERNATIONAL JOURNAL OF HIGH PERFORMANCE COMPUTING APPLICATIONS LA English DT Article DE finite-volume GCM; communication library; scalability; portability; benchmark; MPI-1; MPI-2; SHMEM; MLP AB The National Aeronautics and Space Administration (NASA) finite-volume general circulation model (fvGCM) is a global atmospheric model, originally developed for long-term climate simulations. Recently, the NASA fvGCM has been applied in a variety of weather prediction applications, including hurricane and winter storm forecasts. Achieving efficient throughput on a variety of computational platforms is essential to meet the needs of the climate and weather prediction community. We have developed a scalable and portable climate/weather prediction system by applying a portable communication module within a fast numerical algorithm that exceeds the current community demands for computational performance on a variety of high performance computing platforms. The low-level communication module, Mod-Comm, simplifies interprocess communication within GCMs and provides an efficient means of communicating between decomposed global domains using a variety of single-threaded and multithreaded data communication paradigms (MPI-1, MPI-2, SHMEM, and MLP). Mod_Comm has been implemented within the NASA fvGCM and the Community Atmosphere Model (CAM) at the National Center for Atmospheric Research. It is shown that the optimal choice of data communication paradigm varies from system to system, and can have a significant impact on the overall model performance. Performance studies with the NASA fvGCM reveal substantial improvements in the computational performance when using this low-level communication module, throughput improvements of 40% or more have been observed on various platforms including the SGI Altix 3700, SGI Origin 3000, Compaq AIphaServerSC, IBM SP, and Cray. C1 NASA, Software Integrat & Visualizat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA. NASA, Sci Applicat Int Corp, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Putman, WM (reprint author), NASA, Software Integrat & Visualizat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM WILLIAM.M.PUTMAN@NASA.GOV NR 12 TC 10 Z9 10 U1 0 U2 0 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1094-3420 J9 INT J HIGH PERFORM C JI Int. J. High Perform. Comput. Appl. PD FAL PY 2005 VL 19 IS 3 BP 213 EP 223 DI 10.1177/1094342005056101 PG 11 WC Computer Science, Hardware & Architecture; Computer Science, Interdisciplinary Applications; Computer Science, Theory & Methods SC Computer Science GA 957RR UT WOS:000231391500005 ER PT J AU Collins, N Theurich, G DeLuca, C Suarez, M Trayanov, A Balaji, V Li, P Yang, WY Hill, C da Silva, A AF Collins, N Theurich, G DeLuca, C Suarez, M Trayanov, A Balaji, V Li, P Yang, WY Hill, C da Silva, A TI Design and implementation of components in the Earth system modeling framework SO INTERNATIONAL JOURNAL OF HIGH PERFORMANCE COMPUTING APPLICATIONS LA English DT Article DE framework; high performance computing; climate modeling AB The Earth System Modeling Framework is a component-based architecture for developing and assembling climate and related models. A virtual machine underlies the component-level constructs in ESMF, providing both a foundation for performance portability and mechanisms for resource allocation and component sequencing. C1 Natl Ctr Atmospher Res, Earth Syst Modeling Framework Implementat Team, Boulder, CO 80307 USA. Silicon Graph Inc, Profess Serv, Mountain View, CA 94043 USA. Goddard Space Flight Ctr, NCCS, Applicat Team, Greenbelt, MD 20771 USA. NOAA, Modeling Syst Grp, Geophys Fluid Dynam Lab, Greenbelt, MD 20771 USA. Jet Prop Lab, Pasadena, CA 91125 USA. MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Collins, N (reprint author), Natl Ctr Atmospher Res, Earth Syst Modeling Framework Implementat Team, Boulder, CO 80307 USA. RI da Silva, Arlindo/D-6301-2012 OI da Silva, Arlindo/0000-0002-3381-4030 NR 5 TC 37 Z9 37 U1 1 U2 10 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1094-3420 J9 INT J HIGH PERFORM C JI Int. J. High Perform. Comput. Appl. PD FAL PY 2005 VL 19 IS 3 BP 341 EP 350 DI 10.1177/1094342005056120 PG 10 WC Computer Science, Hardware & Architecture; Computer Science, Interdisciplinary Applications; Computer Science, Theory & Methods SC Computer Science GA 957RR UT WOS:000231391500014 ER PT J AU Tabiei, A Yia, WT Goldberg, R AF Tabiei, A Yia, WT Goldberg, R TI Non-linear strain rate dependent micro-mechanical composite material model for finite element impact and crashworthiness simulation SO INTERNATIONAL JOURNAL OF NON-LINEAR MECHANICS LA English DT Article DE crashworthiness of composites; impact of composite; strain effect of composites; impact simulation of composites AB The present study aims at implementation of a strain rate dependent, non-linear, micro-mechanics material model for laminated, unidirectional polymer matrix composites into the explicit finite element code LSDYNA. The objective is to develop an accurate and simple micro-mechanical, rate dependent material model, which is computationally efficient. Within the model a representative volume cell is assumed. The stress-strain relation including rate dependent effects for the micro-model is derived for both shell elements and solid elements. Micro-failure criterion is presented for each material constituent and failure mode. The implemented model can deal with problems such as impact, crashworthiness, and failure analysis under quasi-static loads. The developed material model has a wide range of applications such as jet engine jackets, armor plates, and structural crashworthiness simulation. The deformation response of two representative composite materials with varying fiber orientation is presented using the described technique. The predicted results compare favorably to experimental values. (c) 2004 Published by Elsevier Ltd. C1 Univ Cincinnati, Ctr Excellence DYNA3D Anal, Dept Aerosp Engn & Engn Mech, Cincinnati, OH 45221 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Tabiei, A (reprint author), Univ Cincinnati, Ctr Excellence DYNA3D Anal, Dept Aerosp Engn & Engn Mech, Cincinnati, OH 45221 USA. EM ala.tabiei@uc.edu NR 10 TC 16 Z9 17 U1 1 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0020-7462 J9 INT J NONLINEAR MECH JI Int. J. Non-Linear Mech. PD SEP PY 2005 VL 40 IS 7 BP 957 EP 970 DI 10.1016/j.ijnonlinmec.2004.10.004 PG 14 WC Mechanics SC Mechanics GA 940ZD UT WOS:000230183500002 ER PT J AU Hilburger, MW Starnes, JH AF Hilburger, MW Starnes, JH TI Buckling behavior of compression-loaded composite cylindrical shells with reinforced cutouts SO INTERNATIONAL JOURNAL OF NON-LINEAR MECHANICS LA English DT Article DE buckling; composite shells; reinforced cutouts AB Results from a numerical study of the response of thin-walled compress ion-loaded quasi-isotropic laminated composite cylindrical shells with unreinforced and reinforced square cutouts are presented. The effects of cutout reinforcement orthotropy, size, and thickness on the non-linear response of the shells are described. A high-fidelity non-linear analysis procedure has been used to predict the non-linear response of the shells. The analysis procedure includes a non-linear static analysis that predicts stable response characteristics of the shells and a non-linear transient analysis that predicts unstable dynamic buckling response characteristics. The results illustrate the complex non-linear response of a compression-loaded shell with an unreinforced cutout. In particular, a local buckling response occurs in the shell near the cutout and is caused by a complex non-linear coupling between local shell-wall deformations and in-plane destabilizing compression stresses near the cutout. In general, reinforcement around a cutout in a compression-loaded shell can retard or eliminate the local buckling response near the cutout and increase the buckling load of the shell. However, results are presented that show how certain reinforcement configurations can cause an unexpected increase in the magnitude of local deformations and stresses in the shell and cause a reduction in the buckling load. Specific cases are presented that suggest that the orthotropy, thickness, and size of a cutout reinforcement in a shell can be tailored to achieve improved buckling response characteristics. (c) Published by Elsevier Ltd. C1 NASA, Langley Res Ctr, Mech & Durabil Branch, Hampton, VA 23681 USA. RP Hilburger, MW (reprint author), NASA, Langley Res Ctr, Mech & Durabil Branch, MS 190, Hampton, VA 23681 USA. EM mark.w.hilburger@nasa.gov NR 16 TC 20 Z9 21 U1 0 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0020-7462 J9 INT J NONLINEAR MECH JI Int. J. Non-Linear Mech. PD SEP PY 2005 VL 40 IS 7 BP 1005 EP 1021 DI 10.1016/j.ijnonlinmec.2005.02.001 PG 17 WC Mechanics SC Mechanics GA 940ZD UT WOS:000230183500005 ER PT J AU Oterkus, E Barut, A Madenci, E Ambur, DR AF Oterkus, E Barut, A Madenci, E Ambur, DR TI Nonlinear analysis of a composite panel with a cutout repaired by a bonded tapered composite patch SO INTERNATIONAL JOURNAL OF SOLIDS AND STRUCTURES LA English DT Article AB This study presents a solution method to analyze the geometrically nonlinear response of a patch-repaired flat panel (skin) with a cutout under general loading conditions. The effect of induced stiffening due to tensile loading on the in-plane and, particularly, the out-of-plane behaviors of the patch-repaired skin are investigated. The damage to the skin is represented in the form of a cutout under the patch. The patch with tapered edges is free of external tractions. The skin is subjected to general boundary and loading conditions along its external edge. The solution method provides the transverse shear and normal stresses in the adhesive between the skin and the patch, and in-plane and bending stresses in the patch and skin. Both the patch and skin are made of linearly elastic composite laminates, and the adhesive between them is homogeneous and isotropic, exhibiting a bi-linear elastic behavior. Modified Green's strain-displacement relations in conjunction with von Karman assumptions are employed in determining the in-plane strains in the skin and patch; however, the transverse shear strains in the adhesive are determined based on the shear-lag theory. The present solution method utilizes the principle of virtual work in conjunction with complex potential functions. (c) 2005 Elsevier Ltd. All rights reserved. C1 Univ Arizona, Tucson, AZ 85721 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Madenci, E (reprint author), Univ Arizona, Tucson, AZ 85721 USA. EM madenci@email.arizona.edu NR 12 TC 8 Z9 9 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0020-7683 J9 INT J SOLIDS STRUCT JI Int. J. Solids Struct. PD SEP PY 2005 VL 42 IS 18-19 BP 5274 EP 5306 DI 10.1016/j.ijsolstr.2005.02.024 PG 33 WC Mechanics SC Mechanics GA 939EF UT WOS:000230054500021 ER PT J AU Landis, GA AF Landis, GA TI Analysis of a lunar sling launcher SO JBIS-JOURNAL OF THE BRITISH INTERPLANETARY SOCIETY LA English DT Article DE tether; lunar launch; mass-driver AB A method of launching from the lunar surface is analyzed, in which the payload launched is swung on a high-strength cable until it reaches the desired launch speed. For a moderate acceleration limit of 11.5 g, a cable length of 50 km would be sufficient to launch into a lunar escape trajectory. If lower accelerations are desired, the cable length must be proportionately longer. Analysis shows that the concept will be feasible with existing materials, and will be simple to implement using advanced materials. C1 NASA, John Glenn Res Ctr, Cleveland, OH 44135 USA. RP Landis, GA (reprint author), NASA, John Glenn Res Ctr, 302-1,21000 Brookpk Rd, Cleveland, OH 44135 USA. EM geoffrey.a.landis@nasa.gov NR 14 TC 1 Z9 1 U1 0 U2 0 PU BRITISH INTERPLANETARY SOC PI LONDON PA 27-29 S LAMBETH RD, LONDON SW8 1SZ, ENGLAND SN 0007-084X J9 JBIS-J BRIT INTERPLA JI JBIS-J. Br. Interplanet. Soc. PD SEP-OCT PY 2005 VL 58 IS 9-10 BP 294 EP 297 PG 4 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Engineering; Astronomy & Astrophysics; Geology GA 960MM UT WOS:000231597800002 ER PT J AU Johnson, L Harris, D Trausch, A Matloff, GL Taylor, T Cutting, K AF Johnson, L Harris, D Trausch, A Matloff, GL Taylor, T Cutting, K TI A strategic roadmap to Centauri SO JBIS-JOURNAL OF THE BRITISH INTERPLANETARY SOCIETY LA English DT Article DE interplanetary propulsion; space manufacturing; space fabrication; space resources; space colonization; interstellar travel ID INTERSTELLAR TRAVEL; PROPULSION; SPACE AB This paper discusses the connectivity between in-space propulsion and in-space fabrication/repair and is based upon a workshop presentation by Les Johnson, manager of the In-Space Propulsion (ISP) Technology Project at NASA's Marshall Space Flight Center (MSFC) in Huntsville, Alabama. Technologies under study by ISP include aerocapture, advanced solar-electric propulsion, solar-thermal propulsion, advanced chemical propulsion, tethers and solar-photon sails. These propulsion systems are all approaching technology readiness levels (TRLs) at which they can be considered for application in space-science and exploration missions. Historically, human frontiers have expanded as people have learned to "live-off-the-land" in new environments and to exploit local resources. With this expansion, frontier settlements have required development of transportation improvements to carry tools and manufactured products to and from the frontier. It is demonstrated how ISP technologies will assist in the development of the solar-system frontier. In-space fabrication and repair will both require and assist the development of ISP propulsion systems, whether humans choose to settle planetary surfaces or to exploit resources of small Solar System bodies. As was true for successful terrestrial pioneers, in-space settlement and exploitation will require sophisticated surveys of inner and outer Solar System objects. ISP technologies will contribute to the success of these surveys, as well as to the efforts to retrieve Solar System resources. In a similar fashion, the utility of ISP products will be greatly enhanced by the technologies of in-space repair and fabrication. As in-space propulsion, fabrication and repair develop, human civilization may expand well beyond the Earth. In the future, small human communities (preceded by robotic explorers) may utilize these techniques to set sail for the nearest stars. C1 NASA, George C Marshall Space Flight Ctr, In Space Propuls Technol Project, Huntsville, AL 35812 USA. CUNY, New York City Coll Technol, Dept Phys & Biol Sci, Brooklyn, NY 11201 USA. Gray Res, Huntsville, AL 35806 USA. BAE Syst, Huntsville, AL 35806 USA. RP Johnson, L (reprint author), NASA, George C Marshall Space Flight Ctr, In Space Propuls Technol Project, NP40, Huntsville, AL 35812 USA. EM C.Les.Johnson@nasa.gov NR 59 TC 0 Z9 0 U1 1 U2 6 PU BRITISH INTERPLANETARY SOC PI LONDON PA 27-29 S LAMBETH RD, LONDON SW8 1SZ, ENGLAND SN 0007-084X J9 JBIS-J BRIT INTERPLA JI JBIS-J. Br. Interplanet. Soc. PD SEP-OCT PY 2005 VL 58 IS 9-10 BP 316 EP 325 PG 10 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Engineering; Astronomy & Astrophysics; Geology GA 960MM UT WOS:000231597800006 ER PT J AU Lazos, BS AF Lazos, BS TI Biologically inspired fixed-wing configuration studies SO JOURNAL OF AIRCRAFT LA English DT Article AB Through the evolution of natural flight systems, it is expected that many have been optimized to provide enhanced efficiency. With this in mind the current study was conducted to determine whether flight configurations found in nature might be appropriately applied to fixed-wing mechanical flight systems to provide performance improvements through energy savings. Four different biologically inspired wings were designed and experimentally tested against a planar elliptic configuration used as a baseline. Two of the configurations show performance improvements over the baseline, using two different comparison techniques. Surface oil flow visualizations at the wingtips highlight differences that provide insight into the flow physics of the improvements. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Lazos, BS (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 22 TC 9 Z9 9 U1 1 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 SEP-OCT PY 2005 VL 42 IS 5 BP 1089 EP 1098 DI 10.2514/1.10496 PG 10 WC Engineering, Aerospace SC Engineering GA 972KG UT WOS:000232452100001 ER PT J AU Ruzicka, GC Strawn, RC Meadowcroft, ET AF Ruzicka, GC Strawn, RC Meadowcroft, ET TI Discrete-blade, Navier-Stokes computational fluid dynamics analysis of ducted-fan flow SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT AIAA 42nd Aerospace Sciences Meeting and Exhibit CY JAN 05-08, 2004 CL Reno, NV SP Amer Inst Aeronaut & Astronaut AB The application of overset grid methods to studying the flowfield of the FANTAIL (TM) antitorque system of the RAH-66 rotorcraft is described. The FANTAIL itself and the experimental program used to design it are described first. Then, OVERFLOW-D, an overset grid-based, Navier-Stokes computational fluid dynamics code is reviewed, and its adaptation to the ducted fan geometry of the FANTAIL is explained. The modeling of the FANTAIL using OVERFLOW-D, including grids and boundary conditions, is explained in detail. The results of numerical studies of the hovering FANTAIL are presented and are shown to compare well with experiment. Flowfield visualizations are presented and are used to explain how the blade tip vortices combine with the adverse pressure gradient beneath the rotor disk to impact flow along the duct wall beneath the disk. C1 Boeing Co, Boeing US Arm Program & Mil Rotorcraft, Ridley Pk, PA 19142 USA. USA, NASA, Ames Res Ctr, Rotorcraft Div,Aeroflight Dynam Directorate, Moffett Field, CA 94035 USA. RP Ruzicka, GC (reprint author), USA, NASA, Ames Res Ctr, Rotorcraft Div,Aeroflight Dynam Directorate, Mail Stop N258-1, Moffett Field, CA 94035 USA. NR 12 TC 3 Z9 4 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 SEP-OCT PY 2005 VL 42 IS 5 BP 1109 EP 1117 DI 10.2514/1.8731 PG 9 WC Engineering, Aerospace SC Engineering GA 972KG UT WOS:000232452100003 ER PT J AU Melton, LP Schaeffler, NW Yao, CS Seifert, A AF Melton, LP Schaeffler, NW Yao, CS Seifert, A TI Active control of flow separation from supercritical airfoil leading-edge flap shoulder SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT AIAA 1st Flow Control Conference CY JUN 24-26, 2002 CL ST LOUIS, MO SP AIAA ID HIGH REYNOLDS-NUMBERS; ACTUATORS AB Zero-net mass-flux periodic excitation was applied at the leading-edge flap shoulder of a simplified high-lift airfoil to delay flow separation. The term simplified infers that no slat or Fowler flaps are used. The NASA energy efficient transport supercritical airfoil was fitted with a 15% chord simply hinged leading-edge flap and a 25% chord simply hinged trailing-edge flap. Initially, the cruise configuration data from previous experiments were reproduced. The effects of leading- and trailing-edge flap deflections on the airfoil integral parameters were quantified. Detailed flow features were measured to identify optimal actuator placement. The measurements included steady and unsteady model and tunnel wall pressures, wake surveys, arrays of surface hot films, flow visualization, and particle image velocimetry. Eventually, high-frequency periodic excitation was applied to delay the occurrence of leading-edge flap shoulder stall and increased the maximum lift by 10-15%. Low-frequency amplitude modulation was used to reduce the oscillatory momentum coefficient by roughly 50% with similar aerodynamic performance gains. It is demonstrated that the efficacy of the amplitude-modulated excitation is due to the generation of low-frequency motion, which is amplified by the separating shear layer. C1 NASA, Langley Res Ctr, Flow Phys & Control Branch, Hampton, VA 23681 USA. Tel Aviv Univ, Fac Engn, Sch Mech Engn, Dept Fluid Mech & Heat Transfer, IL-69978 Tel Aviv, Israel. Natl Inst Aerosp, Hampton, VA USA. RP Melton, LP (reprint author), NASA, Langley Res Ctr, Flow Phys & Control Branch, MS 170, Hampton, VA 23681 USA. EM l.p.melton@lare.nasa.gov; n.w.schaeffler@larc.nasa.gov; c.s.yao@larc.nasa.gov; seifert@eng.tau.ac.il NR 16 TC 14 Z9 14 U1 0 U2 1 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD SEP-OCT PY 2005 VL 42 IS 5 BP 1142 EP 1149 PG 8 WC Engineering, Aerospace SC Engineering GA 972KG UT WOS:000232452100007 ER PT J AU Laflin, KR Klausmeyer, SM Zickuhr, T Vassberg, JC Wahls, RA Morrison, JH Brodersen, OP Rakowitz, ME Tinoco, EN Godard, JL AF Laflin, KR Klausmeyer, SM Zickuhr, T Vassberg, JC Wahls, RA Morrison, JH Brodersen, OP Rakowitz, ME Tinoco, EN Godard, JL TI Data summary from second AIAA computational fluid dynamics drag prediction workshop SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT AIAA 42nd Aerospace Sciences Meeting and Exhibit CY JAN 05-08, 2004 CL Reno, NV SP Amer Inst Aeronaut & Astronaut ID CONFIGURATION; GRIDS AB Results from the Second AIAA Drag Prediction Workshop are summarized. The workshop focused on absolute and configuration delta drag prediction of the DLR, German Aerospace Research Center F6 geometry, which is representative of transport aircraft designed for transonic flight. Both wing-body and wing-body-nacelle-pylon configurations are considered. Comparisons are made using industry relevant test cases that include single-point conditions, drag polars, and drag-rise curves. Drag, lift, and pitching moment predictions from several different Reynolds averaged Navier-Stokes computational fluid dynamics codes are presented and compared to experimental data. Solutions on multiblock structured, unstructured, and overset structured grids using a variety of turbulence models are considered. Results of a grid-refinement study and a comparison of tripped transition vs fully turbulent boundary-layer computations are reported. C1 Cessna Aircraft Co, Dept Aerodynam & Prod Anal, Wichita, KS 67218 USA. Boeing Co, Huntington Beach, CA 92647 USA. NASA, Langley Res Ctr, Configurat Aerodynam Branch, Hampton, VA 23681 USA. NASA, Langley Res Ctr, Dept Computat Aerosci, Hampton, VA 23681 USA. DLR, German Aerosp Ctr, Inst Aerodynam & Flow Technol, D-38108 Braunschweig, Germany. Boeing Co, Seattle, WA 98124 USA. Off Natl Etud & Rech Aerosp, F-92322 Chatillon, France. RP Laflin, KR (reprint author), Cessna Aircraft Co, Dept Aerodynam & Prod Anal, Wichita, KS 67218 USA. NR 40 TC 42 Z9 47 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 SEP-OCT PY 2005 VL 42 IS 5 BP 1165 EP 1178 DI 10.2514/1.10771 PG 14 WC Engineering, Aerospace SC Engineering GA 972KG UT WOS:000232452100009 ER PT J AU Yeo, H Johnson, W AF Yeo, H Johnson, W TI Assessment of comprehensive analysis calculation of airloads on helicopter rotors SO JOURNAL OF AIRCRAFT LA English DT Article AB Blade section normal force and pitching moment were investigated for six rotors operating at transition and high speeds: H-34 in flight and wind tunnel, SA 330 (research Puma), SA 349/2, UH-60A full-scale, and BO-105 model (Higher-Harmonic Acoustics Rotor Test 1). The measured data from flight and wind-tunnel tests were compared with calculations obtained using the comprehensive analysis CANIRAD II. The calculations were made using two free-wake models: rolled up and multiple trailer with consolidation models. At transition speed, there is fair to good agreement for the blade section normal force between the test data and analysis for the H-34, research Puma, and SA 349/2 with the rolled-up wake. The calculated airloads differ significantly from the measurements for the UH-60A and BO-105. Better correlation is obtained for the UH-60A and BO-105 by using the multiple trailer with consolidation wake model. In the high-speed condition, the analysis shows generally good agreement with the research Puma flight data in both magnitude and phase. However, poor agreement is obtained for the other rotors examined. The analysis shows that the aerodynamic tip design (chord length and quarter-chord location) of the, research Puma has an important influence on the phase correlation. C1 USA, NASA, Ames Res Ctr, Rotocraft Div,Aeroflightdynam Directorate, Milpitas, CA 95035 USA. RP Yeo, H (reprint author), USA, NASA, Ames Res Ctr, Rotocraft Div,Aeroflightdynam Directorate, MS 243-12, Milpitas, CA 95035 USA. NR 11 TC 26 Z9 29 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 SEP-OCT PY 2005 VL 42 IS 5 BP 1218 EP 1228 DI 10.2514/1.11595 PG 11 WC Engineering, Aerospace SC Engineering GA 972KG UT WOS:000232452100014 ER PT J AU Jegley, DC AF Jegley, DC TI Structural efficiency of stitched composite panels with stiffener crippling SO JOURNAL OF AIRCRAFT LA English DT Article AB The structural efficiency of blade-stiffened stitched specimens is compared to determine their weight-saving potential if blades were allowed to buckle at less than or equal to design ultimate load. Analytical and experimental results from four configurations of crippling specimens are presented. Specimen skin and blades were held together with through-the-thickness stitches prior to curing. No mechanical fasteners were used for the assembly. Tests were conducted with and without low-speed impact damage. Failure modes are discussed. Finite element and experimental results agree for the response of the structures. For some specimen configurations, improved structural efficiency can be obtained by allowing stiffeners to buckle at design limit load rather than requiring that buckling not occur prior to design ultimate load. A parametric study is presented herein, which describes the possible weight savings with this approach. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Jegley, DC (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 8 TC 0 Z9 1 U1 0 U2 0 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD SEP-OCT PY 2005 VL 42 IS 5 BP 1273 EP 1280 DI 10.2514/1.11845 PG 8 WC Engineering, Aerospace SC Engineering GA 972KG UT WOS:000232452100020 ER PT J AU Patnaik, SN Coroneos, RM Guptill, JD Hopkins, DA AF Patnaik, SN Coroneos, RM Guptill, JD Hopkins, DA TI Subsonic aircraft design optimization with neural network and regression approximators SO JOURNAL OF AIRCRAFT LA English DT Article C1 Ohio Aerosp Inst, Brookpark, OH 44142 USA. NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA. RP Patnaik, SN (reprint author), Ohio Aerosp Inst, Brookpark, OH 44142 USA. NR 11 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 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD SEP-OCT PY 2005 VL 42 IS 5 BP 1347 EP 1349 DI 10.2514/1.11113 PG 3 WC Engineering, Aerospace SC Engineering GA 972KG UT WOS:000232452100031 ER PT J AU Grossman-Clarke, S Zehnder, JA Stefanov, WL Liu, YB Zoldak, MA AF Grossman-Clarke, S Zehnder, JA Stefanov, WL Liu, YB Zoldak, MA TI Urban modifications in a mesoscale meteorological model and the effects on near-surface variables in an arid metropolitan region SO JOURNAL OF APPLIED METEOROLOGY LA English DT Article ID OZONE AIR-QUALITY; LAND-USE; SIMULATION; VEGETATION; AREAS; BASIN; ROUGHNESS; IMPACTS; PHOENIX; FLUXES AB A refined land cover classification for the arid Phoenix (Arizona) metropolitan area and some simple modifications to the surface energetics were introduced in the fifth-generation Pennsylvania State University-National Center for Atmospheric Research Mesoscale Model (MM5). The single urban category in the existing 24-category U.S. Geological Survey land cover classification used in MM5 was divided into three classes to account for heterogeneity of urban land cover. Updated land cover data were derived from 1998 Landsat Thematic Mapper satellite images. The composition of the urban land use classes in terms of typical fractions of vegetation and anthropogenic surfaces was determined from ground-truth information, allowing a variety of moisture availability for evaporation by land cover class. Bulk approaches for characteristics of the urban surface energy budget, such as heat storage, the production of anthropogenic heat, and radiation trapping, were introduced in MM5's Medium Range Forecast boundary layer scheme and slab land surface model. A 72-h simulation was performed with MM5 on a 2 km X 2 km grid during June 1998. The new land cover classification had a significant impact on the turbulent heat fluxes and the evolution of the boundary layer and improved the capability of MM5 to simulate the daytime part of the diurnal temperature cycle in the urban area. The nighttime near-surface air temperatures were improved significantly by adding radiation trapping, heat storage, and anthropogenic heating to the model. C1 Arizona State Univ, Int Inst Sustainabil, Tempe, AZ 85287 USA. Arizona State Univ, Dept Geog, Tempe, AZ 85287 USA. Arizona State Univ, Dept Math, Tempe, AZ 85287 USA. NASA, Lyndon B Johnson Space Ctr, Image Sci & Anal Lab, Houston, TX 77058 USA. Natl Ctr Atmospher Res, Res Applicat Lab, Boulder, CO USA. RP Grossman-Clarke, S (reprint author), Arizona State Univ, Int Inst Sustainabil, POB 873211, Tempe, AZ 85287 USA. EM sg.clarke@asu.edu NR 41 TC 78 Z9 80 U1 2 U2 9 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 SEP PY 2005 VL 44 IS 9 BP 1281 EP 1297 DI 10.1175/JAM2286.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 977BB UT WOS:000232776300001 ER PT J AU McNider, RT Lapenta, WM Biazar, AP Jedlovec, GJ Suggs, RJ Pleim, J AF McNider, RT Lapenta, WM Biazar, AP Jedlovec, GJ Suggs, RJ Pleim, J TI Retrieval of model grid-scale heat capacity using geostationary satellite products. Part I: First case-study application SO JOURNAL OF APPLIED METEOROLOGY LA English DT Article ID ATMOSPHERIC MESOSCALE MODEL; GROUND SURFACE-TEMPERATURE; BOUNDARY-LAYER DEVELOPMENT; SIMPLE PHYSICAL MODEL; DATA ASSIMILATION; NUMERICAL-MODEL; ENERGY FLUXES; SOIL-MOISTURE; WETNESS DATA; PARAMETERIZATION AB In weather forecast and general circulation models the behavior of the atmospheric boundary layer, especially the nocturnal boundary layer, can be critically dependent on the magnitude of the effective model grid-scale bulk heat capacity. Yet, this model parameter is uncertain both in its value and in its conceptual meaning for a model grid in heterogeneous conditions. Current methods for estimating the grid-scale heat capacity involve the areal/volume weighting of heat capacity (resistance) of various, often ill-defined, components. This can lead to errors in model performance in certain parameter spaces. Here, a technique is proposed and tested for recovering bulk heat capacity using time tendencies in satellite-retrieved surface skin temperature (SST). The technique builds upon sensitivity studies that show that surface temperature is most sensitive to thermal inertia in the early evening hours. The retrievals are made within the context of a surface energy budget in a regional-scale model [the fifth-generation Pennsylvania State University National Center for Atmospheric Research Mesoscale Model (MM5)]. The retrieved heat capacities are used in the forecast model, and it is shown that the model predictions of temperature are improved in the nighttime during the forecast periods. C1 Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35899 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Natl Ocean & Atmospher Adm, Air Resources Lab, Atmospher Sci Modeling Div, Res Triangle Pk, NC USA. RP McNider, RT (reprint author), Natl Space & Sci Technol Ctr, 320 Sparkman Dr, Huntsville, AL 35605 USA. EM mcnider@nsstc.uah.edu RI Pleim, Jonathan Pleim/C-1331-2017 OI Pleim, Jonathan Pleim/0000-0001-6190-6082 NR 57 TC 13 Z9 13 U1 0 U2 1 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 SEP PY 2005 VL 44 IS 9 BP 1346 EP 1360 DI 10.1175/JAM2270.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 977BB UT WOS:000232776300005 ER PT J AU Heymsfield, AJ Wang, Z Matrosov, S AF Heymsfield, AJ Wang, Z Matrosov, S TI Improved radar ice water content retrieval algorithms using coincident microphysical and radar measurements SO JOURNAL OF APPLIED METEOROLOGY LA English DT Article ID DUAL-WAVELENGTH RADAR; CIRRUS CLOUDS; REFLECTIVITY; PRECIPITATION; SIZE; MASS AB Airborne radar reflectivity measurements at frequencies of 9.6 and 94 GHz, with collocated, in situ particle size distribution and ice water content measurements from the Cirrus Regional Study of Tropical Anvils and Cirrus Layers (CRYSTAL) Florida Area Cirrus Experiment (FACE) in Florida in July 2002, offer one of the first opportunities to evaluate and improve algorithms for retrieving ice water content from single-wavelength spaceborne radar measurements. Both ice water content and radar reflectivity depend on the distribution of particle mass with size. It is demonstrated that single, power-law, mass dimensional relationships are unable to adequately account for the dominating contribution of small particles at lower reflectivities and large particles at higher reflectivities. To circumvent the need for multiple, or complex, mass dimensional relationships, analytic expressions that use particle ensemble mean ice particle densities that are derived from the coincident microphysical and radar observations are developed. These expressions, together with more than 5000 CRYSTAL FACE size distributions, are used to develop radar reflectivity-ice water content relationships for the two radar wavelengths that appear to provide improvements over earlier relationships, at least,for convectively generated stratiform ice clouds. C1 NCAR, Boulder, CO 80301 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. NOAA, Environm Technol Lab, Boulder, CO USA. RP Heymsfield, AJ (reprint author), NCAR, 3450 Mitchell Lane, Boulder, CO 80301 USA. EM heyms1@ncar.ucar.edu RI Heymsfield, Andrew/E-7340-2011; Wang, Zhien/F-4857-2011 NR 25 TC 28 Z9 28 U1 0 U2 6 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 SEP PY 2005 VL 44 IS 9 BP 1391 EP 1412 DI 10.1175/JAM2282.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 977BB UT WOS:000232776300008 ER PT J AU Bogucki, DJ Jones, BH Carr, ME AF Bogucki, DJ Jones, BH Carr, ME TI Remote measurements of horizontal eddy diffusivity SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID RELEASE EXPERIMENTS AB The rate of horizontal diffusivity or lateral dispersion is key to understanding the dispersion of tracers and contaminants in the ocean, and it is an elusive, yet crucial, parameter in numerical models of circulation. However, the difficulty of parameterizing horizontal mixing is exacerbated in the shallow coastal ocean, which points to the need for more direct measurements. Here, a novel and inexpensive approach to remotely measure the rate of horizontal diffusivity is proposed. Current shipboard measurement techniques require repeated surveys and are thus time consuming and labor intensive. Furthermore, intensive in situ sampling is generally impractical for routine coastal management or for rapid assessment in the case of emergencies. A remote approach is particularly useful in shallow coastal regions or those with complex bathymetry. A time series of images from a dye-release experiment was obtained with a standard three-megapixel digital camera from a helicopter that hovered over the study area. The red-green-blue (RGB) images were then 1.) analyzed to distinguish the dye from the ambient color of the water and adjacent land features, 2) orthorectified, and 3) analyzed to obtain advection and diffusion rates of the thin subsurface dye layer. A horizontal current of the order of 6 cm s(-1) was found. The estimated horizontal eddy diffusivity rate for scales of O(10 m) in the harbor was 0.1 m(2) s(-1). The dye diffusivity and advection rate that are calculated from the images are consistent with independent calculations based on in situ measurements of current speed fluctuations. C1 Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Div Appl Marine Phys, Miami, FL 33149 USA. Univ So Calif, Dept Biol Sci, Los Angeles, CA 90089 USA. CALTECH, Jet Propuls Lab, Pasadena, CA USA. RP Bogucki, DJ (reprint author), Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Div Appl Marine Phys, 4600 Rickenbacker Causeway, Miami, FL 33149 USA. EM dbogucki@rsmas.miami.edu NR 14 TC 11 Z9 11 U1 0 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 SEP PY 2005 VL 22 IS 9 BP 1373 EP 1380 DI 10.1175/JTECH1794.1 PG 8 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 973XS UT WOS:000232556500005 ER PT J AU Tran, N Zanife, OZ Chapron, B Vandemark, D Vincent, P AF Tran, N Zanife, OZ Chapron, B Vandemark, D Vincent, P TI Absolute calibration of Jason-1 and Envisat altimeter Ku-band radar cross sections from cross comparison with TRMM precipitation radar measurements SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID MEASURING MISSION TRMM; SEA-STATE BIAS; WIND-SPEED ALGORITHM; SURFACE WIND; SATELLITE DATA; IN-SITU; BACKSCATTER; LEVEL; SLOPE; RAIN AB One year of collocated, rain-free nadir Ku-band backscatter cross-section measurements from the Tropical Rainfall Mapping Mission (TRMM) precipitation radar (PR) and both Jason-1 and Envisat RA-2 altimeter measurements have been compiled to compare these three sources of Ku-band radar cross section. With the exception of a +1.46 dB relative offset between Jason-1 and PR measurements and a -1.40 dB offset between Envisat and PR ones, all three Ku-band measurements compare very well in terms of dependencies upon model wind speed estimates and significant wave height measurements. The altimeter radars and the rain radar thus provide consistent measurements, and observed biases can be rationalized as differences in the radar calibration. The precipitation radar, which also covers off-nadir measurements, has been absolutely calibrated using an active radar calibrator. Consequently, the observed relative offsets can be used to indirectly calibrate both Jason-1 and Envisat altimeter Ku-band radar cross sections in an absolute sense. C1 CLS, DOS, Space Oceanog Div, F-31526 Ramonville St Agne, France. IFREMER, Brest, France. NASA, Goddard Space Flight Ctr, Wallops Isl, VA 23337 USA. CNES, Toulouse, France. RP CLS, DOS, Space Oceanog Div, 8-10 Rue Hermes, F-31526 Ramonville St Agne, France. EM tran@cls.fr RI Chapron, Bertrand/O-6527-2015; tournadre, jean/F-8402-2010 OI tournadre, jean/0000-0003-1159-4388 NR 50 TC 8 Z9 8 U1 0 U2 2 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD SEP PY 2005 VL 22 IS 9 BP 1389 EP 1402 DI 10.1175/JTECH1791.1 PG 14 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 973XS UT WOS:000232556500007 ER PT J AU Aikin, AC Grebowsky, JM Burrows, JP Correira, J Pesnell, WD AF Aikin, AC Grebowsky, JM Burrows, JP Correira, J Pesnell, WD TI Temporal evolution of the vertical content of metallic ion and neutral species SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article; Proceedings Paper CT AGU Meeting on Meteors and the Mesopause CY 2003 CL San Francisco, CA SP AGU DE atmospheric metals; micrometeoroids; leonid meteor shower ID SATELLITE MEASUREMENTS; METEORS; LIDAR; MG AB Temporal changes in the vertical column contents of the meteoric metals Mg+, Mg, Fe+, and Fe have been measured at similar to 1030 LT for all longitudes in the latitude zone of 10 degrees N-30 degrees N during November 1996, encompassing the period of the Leonid meteor shower. The column contents were obtained using UV radiances measured by the GOME instrument on the ERS-2 satellite. Throughout the month there are several interesting prominent content enhancements of all species. After the Leonid shower peak on 17 November the ion species contents increase before the contents of the neutrals. However, it is difficult to confirm that this is a shower effect given the other similar variations seen earlier in the contents and in the sporadic meteor flux enhancements. The peaks in visual meteors on 17 November are not observed in the total metal column amounts. The GOME instrument has been in continuous operation since April 1995 and is an excellent resource for studying the temporal behavior of meteoric metals on a global scale. (c) 2005 Elsevier Ltd. All rights reserved. C1 Catholic Univ Amer, Washington, DC 20064 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Bremen, IUP, D-2800 Bremen, Germany. Nomad Res Inc, Arnold, MD 21012 USA. RP Aikin, AC (reprint author), Catholic Univ Amer, Washington, DC 20064 USA. EM aikin@carioca.gsfc.nasa.gov; u5jmg@lepvax.gsfc.nasa.gov; 17correira@cua.edu RI Pesnell, William/D-1062-2012; Grebowsky, Joseph/I-7185-2013; Burrows, John/B-6199-2014 OI Pesnell, William/0000-0002-8306-2500; Burrows, John/0000-0002-6821-5580 NR 19 TC 1 Z9 1 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD SEP PY 2005 VL 67 IS 13 BP 1238 EP 1244 DI 10.1016/j.jastp.2005.06.012 PG 7 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 967GG UT WOS:000232078900010 ER PT J AU Rohlin, L Trent, JD Salmon, K Kim, U Gunsalus, RP Liao, JC AF Rohlin, L Trent, JD Salmon, K Kim, U Gunsalus, RP Liao, JC TI Heat shock response of Archaeoglobus fulgidus SO JOURNAL OF BACTERIOLOGY LA English DT Article ID DNA MICROARRAY ANALYSIS; GROUP-II CHAPERONIN; HYPERTHERMOPHILIC ARCHAEON; PYROCOCCUS-FURIOSUS; ESCHERICHIA-COLI; MOLECULAR CHAPERONE; HALOFERAX-VOLCANII; UNFOLDED PROTEINS; BACILLUS-SUBTILIS; GENE-EXPRESSION AB The heat shock response of the hyperthermophilic archaeon Archaeoglobus fulgidus strain VC-16 was studied using whole-genome microarrays. On the basis of the resulting expression profiles, approximately 350 of the 2,410 open reading frames (ORFs) (ca. 14%) exhibited increased or decreased transcript abundance. These span a range of cell functions, including energy production, amino acid metabolism, and signal transduction, where the majority are uncharacterized. One ORF called AF1298 was identified that contains a putative helix-turn-helix DNA binding motif. The gene product, HSR1, was expressed and purified from Escherichia coli and was used to characterize specific DNA recognition regions upstream of two A. fulgidus genes, AF1298 and AF1971. The results indicate that AF1298 is autoregulated and is part of an operon with two downstream genes that encode a small heat shock protein, Hsp20, and cdc48, an AAA(+) ATPase. The DNase I footprints using HSR1 suggest the presence of a cis-binding motif upstream of AF1298 consisting of CTAAC-N5-GTTAG. Since AF1298 is negatively regulated in response to heat shock and encodes a protein only distantly related to the N-terminal DNA binding domain of Phr of Pyrococcus furiosus, these results suggest that HSR1 and Phr may belong to an evolutionarily diverse protein family involved in heat shock regulation in hyperthermophilic and mesophilic Archaea organisms. C1 Univ Calif Los Angeles, Dept Chem Engn, Los Angeles, CA 90095 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Calif Los Angeles, Dept Microbiol Immunol & Mol Genet, Los Angeles, CA USA. RP Liao, JC (reprint author), Univ Calif Los Angeles, Dept Chem Engn, 5531 Boelter Hall, Los Angeles, CA 90095 USA. EM liaoj@ucla.edu RI Hsing-Yen, Su/G-9552-2014 NR 49 TC 38 Z9 42 U1 0 U2 1 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0021-9193 J9 J BACTERIOL JI J. Bacteriol. PD SEP PY 2005 VL 187 IS 17 BP 6046 EP 6057 DI 10.1128/JB.187.17.6046-6057.2005 PG 12 WC Microbiology SC Microbiology GA 957XF UT WOS:000231406000021 PM 16109946 ER PT J AU Gao, FG Fay, JM Mathew, G Jeevarajan, AS Anderson, MM AF Gao, FG Fay, JM Mathew, G Jeevarajan, AS Anderson, MM TI Optical sensor based on fluorescent quenching and pulsed blue LED excitation for long-term monitoring of dissolved oxygen in NASA space bioreactors SO JOURNAL OF BIOMEDICAL OPTICS LA English DT Article; Proceedings Paper CT 4th Inter Workshop on Optical Imaging from Bench to Bedside CY SEP, 2004 CL NIH, Bethesda, MD HO NIH DE sensors; fluorescence; cells; biology; photodiodes; optical devices ID LINEAR CALIBRATION FUNCTION; GLUCOSE BIOSENSOR; FIBER; RUTHENIUM; COMPLEXES; OPTRODE; TIME AB There is a need to monitor the concentration of dissolved oxygen (DO) present in the culture medium for NASA's space cell biology experiments, as well as in earth-based cell cultures. Continuous measurement of DO concentration in the cell culture medium in perfused bioreactors requires that the oxygen sensor provide adequate sensitivity and low toxicity to the cells, as well as maintain calibration over several weeks. Although there are a number of sensors for dis solved oxygen on the market and under development elsewhere, very few meet these stringent conditions. An in-house optical oxygen sensor (HOXY) based on dynamic fluorescent quenching of Tris(4,7diphenyl-1,10-phenanthroline)ruthenium(II) chloride and a pulsed blue LED light source was developed in our laboratory to address these requirements. The sensing element consisted of the fluorescent 1290 Drive dye embedded in a silicone matrix and coated onto a glass capillary. Photobleaching was minimized by a pulsed LED light source. The total noise in the sensor output is 2% and the sensor dynamic range is 0 to 200 mm Hg. The resolution of the sensor is 0.1 mm Hg at 50 mm Hg, and 0.25 mm Hg at 130 mm Hg, while the accuracy is 5%. The LED-based oxygen sensor exhibited stable performance and low drift, making it compatible for space-flight bioreactor systems. (c) 2005 Society of Photo-Optical Instrumentation Engineers. C1 NASA, Lyndon B Johnson Space Ctr, Cellular Biotechnol Program, Houston, TX 77058 USA. Wyle Life Sci, Houston, TX 77058 USA. Texas Tech Univ, Sch Med, Lubbock, TX 79409 USA. RP Jeevarajan, AS (reprint author), NASA, Lyndon B Johnson Space Ctr, Cellular Biotechnol Program, 2101 NASA Rd 1, Houston, TX 77058 USA. EM antony.s.jeevarajan@nasa.gov NR 29 TC 4 Z9 4 U1 2 U2 12 PU SPIE-INT SOCIETY OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 1083-3668 J9 J BIOMED OPT JI J. Biomed. Opt. PD SEP-OCT PY 2005 VL 10 IS 5 AR 054005 DI 10.1117/1.2062427 PG 6 WC Biochemical Research Methods; Optics; Radiology, Nuclear Medicine & Medical Imaging SC Biochemistry & Molecular Biology; Optics; Radiology, Nuclear Medicine & Medical Imaging GA 989YY UT WOS:000233711300030 PM 16292965 ER PT J AU Sibonga, JD Evans, HJ Sung, H Spector, ER Oganov, VS Bakulin, AV Shackelford, LC LeBlanc, AD AF Sibonga, JD Evans, HJ Sung, H Spector, ER Oganov, VS Bakulin, AV Shackelford, LC LeBlanc, AD TI Skeletal recovery following long-duration spaceflight missions as predicted by preflight and postflight dual X-ray absorptiometry (DXA) scans of 49 crewmembers. SO JOURNAL OF BONE AND MINERAL RESEARCH LA English DT Meeting Abstract CT 27th Annual Meeting of the American-Society-for-Bone-and-Mineral-Research CY SEP 23-27, 2005 CL Nashville, TN SP Amer Soc Bone & Mineral Res C1 Univ Space Res Assoc, Div Space Life Sci, Houston, TX USA. Wyle Labs, Houston, TX USA. Minist Publ Hlth Russia, Inst Biomed Problems, Moscow, Russia. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC BONE & MINERAL RES PI WASHINGTON PA 2025 M ST, N W, STE 800, WASHINGTON, DC 20036-3309 USA SN 0884-0431 J9 J BONE MINER RES JI J. Bone Miner. Res. PD SEP PY 2005 VL 20 IS 9 SU 1 BP S44 EP S44 PG 1 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 987FM UT WOS:000233503800172 ER PT J AU Loeb, NG Manalo-Smith, N AF Loeb, NG Manalo-Smith, N TI Top-of-atmosphere direct radiative effect of aerosols over global oceans from merged CERES and MODIS observations SO JOURNAL OF CLIMATE LA English DT Article ID ANGULAR-DISTRIBUTION MODELS; ENERGY SYSTEM INSTRUMENT; PART I; OPTICAL-PROPERTIES; FLUX ESTIMATION; SAHARAN DUST; CLOUDS; SATELLITE; RETRIEVALS; ALGORITHM AB The direct radiative effect of aerosols (DREA) is defined as the difference between radiative fluxes in the absence and presence of aerosols. In this study, the direct radiative effect of aerosols is estimated for 46 months (March 2000-December 2003) of merged Clouds and the Earth's Radiant Energy System (CERES) and Moderate Resolution Imaging Spectroradiometer (MODIS) Terra global measurements over ocean. This analysis includes the contribution from clear regions in both clear and partly cloudy CERES footprints. MODIS-CERES narrow-to-broadband regressions are developed to convert clear-sky MODIS narrowband radiances to broadband shortwave (SW) radiances, and CERES clear-sky angular distribution models (ADMs) are used to estimate the corresponding top-of-atmosphere (TOA) radiative fluxes that are needed to determine the DREA. Clear-sky MODIS pixels are identified using two independent cloud masks: (i) the NOAA/National Environmental Satellite, Data, and Information Service (NESDIS) algorithm that is used for inferring aerosol properties from MODIS on the CERES Single Scanner Footprint TOA/Surface Fluxes and Clouds (SSF) product (NOAA SSF); and (ii) the standard algorithm that is used by the MODIS aerosol group to produce the MODIS aerosol product (MOD04). Over global oceans, direct radiative cooling by aerosols for clear scenes that are identified from MOD04 is estimated to be 40% larger than for clear scenes from NOAA SSF (5.5 compared to 3.8 W m(-2)). Regionally, differences are largest in areas that are affected by dust aerosol, such as oceanic regions that are adjacent to the Sahara and Saudi Arabian deserts, and in northern Pacific Ocean regions that are influenced by dust transported from Asia. The net total-sky (clear and cloudy) DREA is negative (cooling) and is estimated to be -2.0 W m(-2) from MOD04, and -1.6 W m(-2) from NOAA SSF. The DREA is shown to have pronounced seasonal cycles in the Northern Hemisphere and large year-to-year fluctuations near deserts. However, no systematic trend in deseasonalized anomalies of the DREA is observed over the 46-month time series that is considered. C1 Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 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. EM n.g.loeb@larc.nasa.gov NR 40 TC 102 Z9 104 U1 3 U2 15 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 SEP 1 PY 2005 VL 18 IS 17 BP 3506 EP 3526 DI 10.1175/JCLI3504.1 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 972RJ UT WOS:000232470600006 ER PT J AU Rossow, WB Zhang, YC Wang, JH AF Rossow, WB Zhang, YC Wang, JH TI A statistical model of cloud vertical structure based on reconciling cloud layer amounts inferred from satellites and radiosonde humidity profiles SO JOURNAL OF CLIMATE LA English DT Article ID HIGH-LEVEL CLOUDS; ATMOSPHERE RADIATIVE FLUXES; UPPER-AIR OBSERVATIONS; GAS EXPERIMENT II; ISCCP DATA SETS; STRATOSPHERIC AEROSOL; SURFACE OBSERVATIONS; CIRCULATION SYSTEMS; OVERLAP STATISTICS; LIFE-CYCLE AB To diagnose how cloud processes feed back on weather- and climate-scale variations of the atmosphere requires determining the changes that clouds produce in the atmospheric diabatic heating by radiation and precipitation at the same scales of variation. In particular, not only the magnitude of these changes must be quantified but also their correlation with atmospheric temperature variations; hence, the space-time resolution of the cloud perturbations must be sufficient to account for the majority of these variations. Although extensive new global cloud and radiative flux datasets have recently become available, the vertical profiles of clouds and consequent radiative flux divergence have not been systematically measured covering weather-scale variations from about 100 km, 3 h up to climate-scale variations of 10000 km, decadal inclusive. By combining the statistics of cloud layer occurrence from the International Satellite Cloud Climatology Project (ISCCP) and an analysis of radiosonde humidity profiles, a statistical model has been developed that associates each cloud type, recognizable from satellite measurements, with a particular cloud vertical structure. Application of this model to the ISCCP cloud layer amounts produces estimates of low-level cloud amounts and average cloud-base pressures that are quantitatively closer to observations based on surface weather observations, capturing the variations with latitude and season and land and ocean (results are less good in the polar regions). The main advantage of this statistical model is that the correlations of cloud vertical structure with meteorology are qualitatively similar to "classical" information relating cloud properties to weather. These results can be evaluated and improved with the advent of satellites that can directly probe cloud vertical structures over the globe, providing statistics with changing meteorological conditions. C1 Columbia Univ, Goddard Inst Space Studies, NASA, New York, NY 10025 USA. Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. Natl Ctr Atmospher Res, Boulder, CO 80307 USA. RP Columbia Univ, Goddard Inst Space Studies, NASA, 2880 Broadway, New York, NY 10025 USA. EM wrossow@giss.nasa.gov RI Rossow, William/F-3138-2015 NR 64 TC 32 Z9 32 U1 1 U2 13 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD SEP 1 PY 2005 VL 18 IS 17 BP 3587 EP 3605 DI 10.1175/JCLI3479.1 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 972RJ UT WOS:000232470600011 ER PT J AU Boyd, JL Shah, V Du, B Vaksman, Z AF Boyd, JL Shah, V Du, B Vaksman, Z TI Absorption and pharmacokinetics of acetaminophen in astronauts SO JOURNAL OF CLINICAL PHARMACOLOGY LA English DT Meeting Abstract CT 34th Annual Meeting of the American-College-of-Clinical-Pharmacology CY SEP 11-13, 2005 CL Rockville, MD SP Amer Coll Clin Pharmacol C1 Univ Space Res Assoc, Houston, TX USA. Wyle Labs, Houston, TX USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NR 0 TC 0 Z9 0 U1 1 U2 2 PU SAGE PUBLICATIONS INC PI THOUSAND OAKS PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA SN 0091-2700 J9 J CLIN PHARMACOL JI J. Clin. Pharmacol. PD SEP PY 2005 VL 45 IS 9 MA 75 BP 1085 EP 1085 PG 1 WC Pharmacology & Pharmacy SC Pharmacology & Pharmacy GA 956OO UT WOS:000231309900079 ER PT J AU Rosenfeld, R Frieman, JA AF Rosenfeld, R Frieman, JA TI A simple model for quintessential inflation SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE dark energy theory; inflation; axions; cosmology of theories beyond the SM ID NAMBU-GOLDSTONE BOSONS; COSMOLOGICAL CONSTANT; DARK ENERGY; NATURAL INFLATION; CHAOTIC INFLATION; UNIVERSE; CONSTRAINTS; SUPERNOVAE; AXION AB We propose a simple toy model for quintessential inflation where a complex scalar field described by a Lagrangian with a U(1)(PQ) symmetry spontaneously broken at a high energy scale and explicitly broken by instanton effects at a much lower energy can account for both the early inflationary phase and the recent accelerated expansion of the Universe. The real part of the complex field plays the role of the in flaton whereas the imaginary part, the 'axion', is the quintessence field. C1 Univ Estadual Paulista, Inst Fis Theor, BR-01405900 Sao Paulo, Brazil. NASA, Fermi Natl Accelerator Lab, Fermilab Astrophys Ctr, Batavia, IL 60510 USA. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. RP Univ Estadual Paulista, Inst Fis Theor, Rua Pamplona,145, BR-01405900 Sao Paulo, Brazil. EM rosenfel@ift.unesp.br; frieman@fnal.gov RI Rosenfeld, Rogerio/L-5845-2016 NR 42 TC 14 Z9 14 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1475-7516 J9 J COSMOL ASTROPART P JI J. Cosmol. Astropart. Phys. PD SEP PY 2005 IS 9 AR 003 DI 10.1088/1475-7516/2005/09/003 PG 8 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 969AF UT WOS:000232205100013 ER PT J AU Volz, MP Walker, JS Schweizer, M Cobb, SD Szofran, FR AF Volz, MP Walker, JS Schweizer, M Cobb, SD Szofran, FR TI Bridgman growth of germanium crystals in a rotating magnetic field SO JOURNAL OF CRYSTAL GROWTH LA English DT Article DE rotating magnetic field; segregation; Bridgman technique; semiconducting germanium ID FLUID-FLOW; INSTABILITY; GAAS AB A series of (100)-oriented gallium-doped germanium crystals has been grown by the vertical Bridgman method and under the influence of a rotating magnetic field (RMF). Time-dependent flow instabilities occur when the critical magnetic Taylor number (T-m(c)) is exceeded, and this can be observed by noting the appearance of striations in the grown crystals. T-m(c) decreases as the aspect ratio of the melt increases, and approaches the theoretical limit expected for an infinite cylinder. Intentional interface demarcations are introduced by pulsing the RMF on and off. The RMF has a marked effect on the interface shape, changing it from concave to nearly flat as the RMF strength is increased. (c) 2005 Elsevier B.V. All rights reserved. C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Univ Illinois, Dept Mech & Ind Engn, Urbana, IL 61801 USA. NASA, George C Marshall Space Flight Ctr, USRA, Huntsville, AL 35812 USA. RP Volz, MP (reprint author), NASA, George C Marshall Space Flight Ctr, XD42, Huntsville, AL 35812 USA. EM martin.volz@nasa.gov NR 18 TC 17 Z9 20 U1 1 U2 6 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0248 J9 J CRYST GROWTH JI J. Cryst. Growth PD SEP 1 PY 2005 VL 282 IS 3-4 BP 305 EP 312 DI 10.1016/j.jcrysgro.2005.05.031 PG 8 WC Crystallography; Materials Science, Multidisciplinary; Physics, Applied SC Crystallography; Materials Science; Physics GA 958FG UT WOS:000231429500006 ER PT J AU Fei, JT Chen, SH Tho, G Joshi, SM AF Fei, JT Chen, SH Tho, G Joshi, SM TI Robust adaptive control scheme for discrete-time system with actuator failures SO JOURNAL OF DYNAMIC SYSTEMS MEASUREMENT AND CONTROL-TRANSACTIONS OF THE ASME LA English DT Article ID TRACKING CONTROL; FEEDBACK AB A robust adaptive control approach using output feedback for output tracking is developed for discrete-time linear time-invariant systems with uncertain failures of redundant actuators in the presence of the unmodeled dynamics and bounded output disturbance. Such actuator failures are characterized by some unknown inputs stuck at some unknown fixed values at unknown time instants. Technical issues such as plant-model output matching, adaptive controller structure, adaptive parameter update laws, stability and tracking analysis, and robustness of system performance are solved for the discrete-time adaptive actuator failure compensation problem. A case study is conducted for adaptive compensation of rudder servomechanism failures of a Boeing 747 dynamic model presented in discrete time, verifying the desired adaptive system performance in the. presence of uncertain actuator failures. C1 Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22903 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Fei, JT (reprint author), Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22903 USA. NR 16 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 0022-0434 J9 J DYN SYST-T ASME JI J. Dyn. Syst. Meas. Control-Trans. ASME PD SEP PY 2005 VL 127 IS 3 BP 520 EP 526 DI 10.1115/1.1978912 PG 7 WC Automation & Control Systems; Instruments & Instrumentation SC Automation & Control Systems; Instruments & Instrumentation GA 967DJ UT WOS:000232071400024 ER PT J AU Gallagher, DL Adrian, ML Liemohn, MW AF Gallagher, DL Adrian, ML Liemohn, MW TI Origin and evolution of deep plasmaspheric notches SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID EXTREME-ULTRAVIOLET IMAGER; RADIO PLASMA IMAGER; MAGNETOSPHERIC CONVECTION; KILOMETRIC CONTINUUM; ELECTRON-DENSITY; MAGNETIC STORM; FIELD; MODEL; DISTURBANCE; BOUNDARY AB Deep plasmaspheric notches can extend over more than 2 R-E in radial distance and 3 hours MLT in the magnetic equatorial plane, as observed by the extreme ultraviolet (EUV) imager on the IMAGE mission. They are among the largest evacuated features in the exterior plasmaspheric boundary. They can last for days and exhibit a variety of shapes. It appears that weak convection and limited erosion precedes notch formation at the westward, near-Earth edge of the convection plume. Eighteen clear notch events were found and analyzed in 2000. Among these events, notches were found to drift as slowly as 44% of corotation. In only one case was a notch found to drift at the corotation rate within measurement error. On average, these notches drift at about 21.5 h d(-1) or 90% of the corotational rate. Notches sometimes exhibit an interior structure that appears as an extended prominence of dense plasma, which forms a W- or M-like feature in IMAGE/EUV images, depending on viewing perspective. Initial modeling suggests that notches and notch prominences may be caused in part by intense small-scale potential structures that result from the localized injection of ring current plasma. Plasma filling rates during recovery are examined in three L shell ranges from L = 2 to L = 3.5 with rates ranging from 5 to 140 cm(-3) d(-1). Plasma loss during a minor substorm is found to extend to surprisingly low L shell with rates ranging from 100 to 130 cm(-3) d(-1) across the L shells examined. C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Michigan, Space Phys Res Lab, Ann Arbor, MI 48109 USA. RP Gallagher, DL (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. EM dennis.l.gallagher@nasa.gov RI Liemohn, Michael/H-8703-2012 OI Liemohn, Michael/0000-0002-7039-2631 NR 45 TC 42 Z9 42 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 SEP 1 PY 2005 VL 110 IS A9 AR A09201 DI 10.1029/2004JA010906 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 962KC UT WOS:000231729300003 ER PT J AU Tischler, MB Blanken, CL Cheung, KK Swei, SSM Sahasrabudhe, V Faynberg, A AF Tischler, MB Blanken, CL Cheung, KK Swei, SSM Sahasrabudhe, V Faynberg, A TI Modernized control laws for UH-60 BLACK HAWK optimization and flight-test results SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article; Proceedings Paper CT 4th Decennial Specialists Conference on Aeromechanics CY JAN 21-23, 2004 CL San Francisco, CA SP Amer Helicopter Soc ID CONTROL-SYSTEM DESIGN; ROTORCRAFT; IDENTIFICATION AB Modernized control laws were developed to provide an attitude-command/attitude-hold response type for the UH-60 BLACK HAWK helicopter and thereby afford improved handling qualities for near-Earth operation in night and poor weather. The inner-loop system modernized control laws were implemented using the 10% authority stability augmentation system actuators and was evaluated in an EH-60L helicopter. Central to addressing the significant resource and technical challenges of this project was the extensive use of a modern integrated tool set. System identification methods provided an accurate flight-identified aircraft response model and allowed the efficient isolation of discrepancies in the block diagram-based simulation model. Additional key tools were real-time rapid prototyping and a well-designed picture-to-code process. Control laws we're tuned to achieve the maximum design margin relative to handling qualities and control system performance requirements. The optimized design was seen to be robust to uncertainties in the identified physical parameters. A flight-test evaluation by three test pilots showed significant benefits of the optimized design compared to the BLACK HAWK standard flight control configuration. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Sikorsky Aircraft Corp, Stratford, CT 06601 USA. RP NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM mtischler@mail.arc.nasa.gov; cblanken@mail.arc.nasa.gov; kcheung@mail.arc.nasa.gov; sswei@mail.arc.nasa.gov; vsahasrabudhe@sikorsky.com; afaynberg@sikorsky.com NR 24 TC 3 Z9 3 U1 0 U2 6 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 EI 1533-3884 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD SEP-OCT PY 2005 VL 28 IS 5 BP 964 EP 978 DI 10.2514/1.8021 PG 15 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 964IE UT WOS:000231872200015 ER PT J AU Bayen, AM Meyer, G Tomlin, CJ AF Bayen, AM Meyer, G Tomlin, CJ TI Lagrangian delay predictive model for sector-based air traffic flow SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article ID MANAGEMENT AB A control theoretical model of sector-based air traffic flow is derived using hybrid automata theory. This model is Lagrangian, because it models the properties of the system along its trajectories. A subset of this model is used to generate analytic predictions of air traffic congestion: A dynamic sector capacity is defined and derived that is used for predicting the time it takes to overload a given portion of airspace. This result links the Lagrangian approach with Eulerian models, which account for temporal variations of parameters in a fixed volume. To determine the accuracy of predictions, an air traffic flow simulator is designed and validated. The simulator is then used to show that flow scheduling and conflict resolution may be decorrelated by reducing aircraft density. C1 Univ Calif Berkeley, Dept Civil & Environm Engn, Berkeley, CA 94720 USA. Swiss Fed Inst Technol, CH-8092 Zurich, Switzerland. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA. Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA. RP Bayen, AM (reprint author), Univ Calif Berkeley, Dept Civil & Environm Engn, 711 Davis Hall, Berkeley, CA 94720 USA. EM bayen@ce.berkeley.edu; pascal_grieder@mckinsey.com; tomlin@stanford.edu NR 31 TC 20 Z9 20 U1 1 U2 8 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD SEP-OCT PY 2005 VL 28 IS 5 BP 1015 EP 1026 DI 10.2514/1.15242 PG 12 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 964IE UT WOS:000231872200020 ER PT J AU Baldelli, DH Lind, R Brenner, M AF Baldelli, DH Lind, R Brenner, M TI Nonlinear aeroelastic/aeroservoelastic modeling by block-oriented identification SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article AB The investigation of aeroelastic/aeroservoelastic stability through flight testing is an essential part of aircraft certification. The stability boundary prediction is especially difficult when the instability is associated with nonlinearities in the dynamics. An approach is presented for the characterization of the nonlinear dynamics by noniterative identification algorithms. Two different block-oriented nonlinear models are considered to augment existing linear models with nonlinear operators derived by analyzing experimental data. Specifically, focuse is placed on the identification of Hammerstein or Wiener block-oriented models from a N-point data record {(u) over bar (k), (y) over bar (k)}(k)(N)=1 of observed input-output measurements from an aeroelastic/aeroservoelastic system. Central in the identification of block-oriented models is the use of an a priori set of orthonormal bases tuned with the dynamics of the aeroelastic/aeroservoelastic system. In both cases, a method is proposed to generate the orthonormal bases that is based on the cascade of input-normal balanced state-space realizations of all-pass filters. Case studies with a simulated structurally nonlinear prototypical two-dimensional wing section and actual F/A-18 active aeroelastic wing ground vibration test data are presented. C1 ZONA Technol Inc, Scottsdale, AZ 85251 USA. Univ Florida, Dept Mech & Aerosp Engn, Gainesville, FL 32611 USA. NASA, Dryden Flight Res Ctr, Edwards AFB, CA 93523 USA. RP ZONA Technol Inc, Scottsdale, AZ 85251 USA. NR 17 TC 15 Z9 21 U1 0 U2 6 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 EI 1533-3884 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD SEP-OCT PY 2005 VL 28 IS 5 BP 1056 EP 1064 DI 10.2514/1.11792 PG 9 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 964IE UT WOS:000231872200025 ER PT J AU Young, P Lu, YJ Terrill, R Li, J AF Young, P Lu, YJ Terrill, R Li, J TI High-sensitivity NO2 detection with carbon nanotube-gold nanoparticle composite films SO JOURNAL OF NANOSCIENCE AND NANOTECHNOLOGY LA English DT Article DE carbon nanotubes; alkanethiol monolayer protected gold nanoparticle; gas detection; nanosensors ID VAPOR DETECTION; SENSORS; CORE; GAS AB Composite films of single-walled carbon nanotube mesh doped with alkanethiol monolayer protected gold clusters (MPCs) have been investigated for ultrahigh sensitivity detection of nitrogen dioxide. The response to NO2 (measured as increased conductance) of the composite materials increased with MPC loading until a threshold MPC loading level was achieved, after which no further enhancement of sensor response is observed. The total of about ten droplets of MPC solution had been cast atop the SWNT mesh. The detection limit for NO2 has been improved 9.6-fold, to 4.6 ppb, compared with that obtained with pure SWNT sensors. Ultraviolet illumination helps to speed up the sensor recovery. All tests were done under ambient conditions. C1 NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. San Jose State Univ, Dept Chem, San Jose, CA 95192 USA. RP Li, J (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. NR 14 TC 24 Z9 24 U1 1 U2 11 PU AMER SCIENTIFIC PUBLISHERS PI STEVENSON RANCH PA 25650 NORTH LEWIS WAY, STEVENSON RANCH, CA 91381-1439 USA SN 1533-4880 J9 J NANOSCI NANOTECHNO JI J. Nanosci. Nanotechnol. PD SEP PY 2005 VL 5 IS 9 BP 1509 EP 1513 DI 10.1166/jnn.2005.323 PG 5 WC Chemistry, Multidisciplinary; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA 956IC UT WOS:000231292400020 PM 16193966 ER PT J AU Lakatos, P Shah, AS Knuth, KH Ulbert, I Karmos, G Schroeder, CE AF Lakatos, P Shah, AS Knuth, KH Ulbert, I Karmos, G Schroeder, CE TI An oscillatory hierarchy controlling neuronal excitability and stimulus processing in the auditory cortex SO JOURNAL OF NEUROPHYSIOLOGY LA English DT Article ID SOURCE-DENSITY ANALYSIS; TO-TRIAL VARIABILITY; GAMMA OSCILLATIONS; ENTORHINAL CORTEX; BEHAVING RAT; EVOKED-RESPONSES; LAMINAR PROFILE; MODULATION; SYNCHRONIZATION; MECHANISMS AB EEG oscillations are hypothesized to reflect cyclical variations in the neuronal excitability, with particular frequency bands reflecting differing spatial scales of brain operation. However, despite decades of clinical and scientific investigation, there is no unifying theory of EEG organization, and the role of ongoing activity in sensory processing remains controversial. This study analyzed laminar profiles of synaptic activity [ current source density CSD] and multiunit activity (MUA), both spontaneous and stimulus-driven, in primary auditory cortex of awake macaque monkeys. Our results reveal that the EEG is hierarchically organized; delta (1-4 Hz) phase modulates theta (4-10 Hz) amplitude, and theta phase modulates gamma (30-50 Hz) amplitude. This oscillatory hierarchy controls baseline excitability and thus stimulus-related responses in a neuronal ensemble. We propose that the hierarchical organization of ambient oscillatory activity allows auditory cortex to structure its temporal activity pattern so as to optimize the processing of rhythmic inputs. C1 Nathan S Kline Inst Psychiat Res, Cognit Neurosci & Schizophrenia Program, Orangeburg, NY 10962 USA. Hungarian Acad Sci, Inst Psychol, Budapest, Hungary. NASA, Ames Res Ctr, Computat Sci Div, Moffett Field, CA 94035 USA. Albert Einstein Coll Med, Dept Neurosci, Bronx, NY 10467 USA. RP Schroeder, CE (reprint author), Nathan S Kline Inst Psychiat Res, Cognit Neurosci & Schizophrenia Program, Orangeburg, NY 10962 USA. EM schrod@nki.rfmh.org RI Ulbert, Istvan/F-2213-2010; OI Lakatos, Peter/0000-0003-0221-4021 NR 44 TC 473 Z9 476 U1 4 U2 36 PU AMER PHYSIOLOGICAL SOC PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA SN 0022-3077 J9 J NEUROPHYSIOL JI J. Neurophysiol. PD SEP PY 2005 VL 94 IS 3 BP 1904 EP 1911 DI 10.1152/jn.00263.2005 PG 8 WC Neurosciences; Physiology SC Neurosciences & Neurology; Physiology GA 955WX UT WOS:000231259400026 PM 15901760 ER PT J AU Waugh, DW Hall, TM AF Waugh, DW Hall, TM TI Propagation of tracer signals in boundary currents SO JOURNAL OF PHYSICAL OCEANOGRAPHY LA English DT Article ID ATLANTIC DEEP-WATER; WESTERN NORTH-ATLANTIC; LABRADOR SEA-WATER; STRATOSPHERIC TRANSPORT; TEMPORAL EVOLUTION; TROPICAL ATLANTIC; TIME-SERIES; AGE; OCEAN; MODEL AB The propagation of a range of tracer signals in a simple model of the deep western boundary current is examined. Analytical expressions are derived in certain limits for the transit-time distributions and the propagation times (tracer ages) of tracers with exponentially growing or periodic concentration histories at the boundary current's origin. If mixing between the boundary current and the surrounding ocean is either very slow or very rapid, then all tracer signals propagate at the same rate. In contrast, for intermediate mixing rates tracer ages generally depend on the history of the tracer variations at the origin and range from the advective time along the current to the much larger mean age. Close agreement of the model with chlorofluorocarbon (CFC) and tritium observations in the North Atlantic deep western boundary current (DWBC) is obtained when the model is in the intermediate mixing regime, with current speed around 5 cm s(-1) and mixing time scale around 1 yr. In this regime anomalies in temperature and salinity of decadal or shorter period will propagate downstream at roughly the current speed, which is much faster than the spreading rate inferred from CFC or tritium-helium ages (approximately 5 cm s(-1) as compared with 2 cm s(-1)). This rapid propagation of anomalies is consistent with observations in the subpolar DWBC, but is at odds with inferences from measurements in the tropical DWBC. This suggests that observed tropical temperature and salinity anomalies are not simply propagated signals from the north. The sensitivity of the tracer spreading rates to tracer and mixing time scales in the model suggests that tight constraints on the flow and transport in real DWBCs may be obtained from simultaneous measurements of several different tracers-in particular, hydrographic anomalies and steadily increasing transient tracers. C1 Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Waugh, DW (reprint author), Johns Hopkins Univ, Dept Earth & Planetary Sci, 3400 N Charles, Baltimore, MD 21218 USA. EM waugh@jhu.edu RI Waugh, Darryn/K-3688-2016 OI Waugh, Darryn/0000-0001-7692-2798 NR 39 TC 12 Z9 12 U1 0 U2 1 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-3670 J9 J PHYS OCEANOGR JI J. Phys. Oceanogr. PD SEP PY 2005 VL 35 IS 9 BP 1538 EP 1552 DI 10.1175/JPO2779.1 PG 15 WC Oceanography SC Oceanography GA 972RG UT WOS:000232470300003 ER PT J AU Khazanov, G Delamere, P Kabin, K Linde, TJ AF Khazanov, G Delamere, P Kabin, K Linde, TJ TI Fundamentals of the plasma sail concept: Magnetohydrodynamic and kinetic studies SO JOURNAL OF PROPULSION AND POWER LA English DT Article ID 3-DIMENSIONAL MHD SIMULATION; HYBRID CODE; MAGNETOSPHERE; HELIOSPHERE; RELEASE AB The Mini-Magnetospheric Plasma Propulsion system (M2P2) was proposed by Winglee et al. to harness the kinetic energy of the solar wind by creating a large magnetic bubble around the spacecraft. This bubble would be supported by plasma injection into a strong magnetic field produced by an electromagnet onboard the spacecraft. In the case of M2P2, the size of the magnetic bubble is actually less than, or comparable to, the scale of these characteristic parameters. Therefore, a kinetic approach, which addresses the small-scale physical mechanisms, must be used. A two-component approach is adopted to determining a preliminary estimate of the momentum transfer to the plasma sail. The first component is a self-consistent MHD simulation of the plasma flow near the spacecraft. It is shown that the fluid treatment is valid to roughly 5 km from the source. The MHD solution is used at this boundary as initial conditions for the hybrid simulation. The hybrid simulations showed that the forces delivered to the innermost regions of the plasma sail are considerably smaller (similar to 10) than their MHD counterparts. Furthermore, these forces are roughly perpendicular to the solar wind flow, in contrast to the MHD forces that are essentially aligned with the solar wind direction. C1 NASA, George C Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. Univ Alberta, Dept Phys, Edmonton, AB T6G 2J1, Canada. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. RP Khazanov, G (reprint author), NASA, George C Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. NR 24 TC 12 Z9 12 U1 0 U2 4 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 J9 J PROPUL POWER JI J. Propul. Power PD SEP-OCT PY 2005 VL 21 IS 5 BP 853 EP 861 DI 10.2514/1.3737 PG 9 WC Engineering, Aerospace SC Engineering GA 963DS UT WOS:000231784100012 ER PT J AU Foster, JE Patterson, MJ AF Foster, JE Patterson, MJ TI Characterization of 40-centimeter microwave electron cyclotron resonance ion source and neutralizer SO JOURNAL OF PROPULSION AND POWER LA English DT Article; Proceedings Paper CT AIAA/ASME/SAE/ASEE 39th Joint Propulsion Conference CY JUL 20, 2003 CL Huntsville, AL SP AIAA, ASME, SAE, ASEE ID PLASMA AB Discharge characteristics of a 40-cm, 2.45-GHz electron cyclotron resonance ion thruster discharge chamber and neutralizer were acquired. Thruster bulk discharge plasma characteristics were assessed using a single Langmuir probe. An estimate of the total extractable ion current was measured as a function of input microwave power and flow rate. Additionally, radial ion current density profiles at the thruster's exit plane were characterized using five equally spaced Faraday probes. Distinct low- and high-density operating modes were observed as discharge input power was varied from 0 to 200 W. In the high mode, extractable ion currents as high as 0.82 A were measured. Neutralizer emission current was characterized as a function of flow rate and microwave power. Neutralizer extraction currents as high as 0.6 A were measured. C1 NASA, John H Glenn Res Ctr Lewis Field, On Board Propuls & Power Branch, Cleveland, OH 44135 USA. RP Foster, JE (reprint author), NASA, John H Glenn Res Ctr Lewis Field, On Board Propuls & Power Branch, Cleveland, OH 44135 USA. NR 22 TC 2 Z9 2 U1 1 U2 3 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 J9 J PROPUL POWER JI J. Propul. Power PD SEP-OCT PY 2005 VL 21 IS 5 BP 862 EP 869 DI 10.2514/1.4932 PG 8 WC Engineering, Aerospace SC Engineering GA 963DS UT WOS:000231784100013 ER PT J AU Turner, MW Hawk, CW Litchford, RJ AF Turner, MW Hawk, CW Litchford, RJ TI Inductive measurement of plasma jet electrical conductivity SO JOURNAL OF PROPULSION AND POWER LA English DT Article; Proceedings Paper CT AIAA/ASME/SAE/ASEE 36th Joint Propulsion Conference and Exhibit CY JUL 16-19, 2000 CL HUNTSVILLE, AL SP Amer Inst Aeronaut & Astronaut, ASME, SAE, ASEE ID VELOCITY; STREAMS AB An inductive probing scheme, originally developed for shock tube studies, has been adapted to measure explosive plasma jet conductivities. In this method, the perturbation of an applied magnetic field by a plasma-jet induces a voltage in a search coil, which, in turn, can be used to infer electrical conductivity through the inversion of a Fredholm integral equation of the first kind. A 1-in. (25.4-mm)-diam probe was designed and constructed, and calibration was accomplished by firing an aluminum slug through the probe using a light-gas gun. Exploratory laboratory experiments were carried out using plasma jets expelled from 15-g high-explosive shaped charges. Measured conductivities were in the range of 3 kS/m for unseeded octol charges and 20 Win for seeded octol charges containing 2% potassium carbonate by mass. C1 Univ Alabama, Huntsville, AL 35899 USA. NASA, George C Marshall Space Flight Ctr, Propuls Res Lab, Energet Res Grp, Huntsville, AL 35812 USA. RP Turner, MW (reprint author), Univ Alabama, S225 Technol Hall, Huntsville, AL 35899 USA. NR 19 TC 0 Z9 0 U1 2 U2 3 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 J9 J PROPUL POWER JI J. Propul. Power PD SEP-OCT PY 2005 VL 21 IS 5 BP 900 EP 907 DI 10.2514/1.12077 PG 8 WC Engineering, Aerospace SC Engineering GA 963DS UT WOS:000231784100018 ER PT J AU Mok, JS Helms, WJ Sisco, JC Anderson, WE AF Mok, JS Helms, WJ Sisco, JC Anderson, WE TI Thermal decomposition of hydrogen peroxide, Part 1: Experimental results SO JOURNAL OF PROPULSION AND POWER LA English DT Article; Proceedings Paper CT AIAA/ASME/SAE/ASEE 38th Joint Propulsion Conference CY JUL 07-10, 2002 CL Indianapolis, IN SP Amer Inst Aeronaut & Astronaut, ASME, SAE, ASEE ID PROPELLANTS; MICROEXPLOSION; COMBUSTION AB Thermal decomposition is an important process in propulsion systems that use hydrogen peroxide (HP). Neither a combined vaporization-decomposition model nor a fundamental understanding of the way liquid HP vaporizes and decomposes in these rocket applications exist. Results are presented from an experimental study of the combined thermal decomposition of HP at rocket-type conditions. A liquid spray of HP is injected into a cross stream of HP decomposition products at chamber pressures ranging from 2.0 to over 5.5 MPa. Two injectors with different orifice diameters are used. Experimental parameters include flow rates of the decomposition products and liquid injectant, HP concentration, chamber geometry, and momentum ratio between the liquid injectant and the decomposition stream. A decomposition efficiency of the liquid HP is determined based on the ratio between measured chamber pressure and chamber pressure calculated by equilibrium chemistry. An analysis of the crossflow injection is used to assess the effects of spray trajectory. Decomposition efficiencies ranging between 10 and 90% were measured. The results show that decomposition efficiency is inversely proportional to the fractional amount of liquid injectant How rate, linearly proportional to residence time, and that higher concentration HP decomposes at a faster rate. C1 Hyundai Motor Co, Emiss Res Team, Ctr Adv Technol, Hwaseong 7721, South Korea. Kia Motors Corp, Hwaseong 7721, South Korea. NASA, Lyndon B Johnson Space Ctr, Mission Operat Directorate,Shuttle Guidance & Con, Syst Div,Guidance & Propuls Branch, Houston, TX 77058 USA. Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA. RP Mok, JS (reprint author), Hyundai Motor Co, Emiss Res Team, Ctr Adv Technol, Hwaseong 7721, South Korea. NR 18 TC 1 Z9 1 U1 1 U2 8 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 J9 J PROPUL POWER JI J. Propul. Power PD SEP-OCT PY 2005 VL 21 IS 5 BP 942 EP 953 DI 10.2514/1.13284 PG 12 WC Engineering, Aerospace SC Engineering GA 963DS UT WOS:000231784100023 ER PT J AU Kojima, J Nguyen, QV AF Kojima, J Nguyen, QV TI Quantitative analysis of spectral interference of spontaneous Raman scattering in high-pressure fuel-rich H-2-air combustion SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE combustion diagnostics; high-pressure flame; Raman scattering; spectral interference; rotation-vibration spectral modeling ID HYDROGEN CARS THERMOMETRY; RAYLEIGH-LIF MEASUREMENTS; TEMPERATURE-MEASUREMENTS; EXCIMER-LASER; WATER-VAPOR; NARROW-BAND; FLAMES; BAR; H-2; INTENSITIES AB We present a theoretical study of the spectral interferences in the spontaneous Raman scattering spectra of major combustion products in 30-atm fuel-rich H-2-air flames. An effective methodology is introduced to choose an appropriate line-shape model for simulating Raman spectra in high-pressure combustion environments. The Voigt profile with the additive approximation assumption was found to provide a reasonable model of the spectral line shape for the present analysis. The rotational/vibrational Raman spectra of H-2, N-2, and H2O were calculated using an anharmonic-oscillator model using the latest collisional broadening coefficients. The calculated spectra were validated with data obtained in a 10-atm fuel-rich H-2-air flame and showed excellent agreement. Our quantitative spectral analysis for equivalence ratios ranging from 1.5 to 5.0 revealed substantial amounts of spectral cross-talk between the rotational H2 lines and the N-2 O-/Q-branch; and between the vibrational H-2 O(0,3) line and the vibrational H2O spectrum. We also address the temperature dependence of the spectral cross-talk and extend our analysis to include a cross-talk compensation technique that removes the interference arising from the H2 Raman spectra onto the N-2, or H2O spectra. (c) 2004 Elsevier Ltd. All rights reserved. C1 Ohio Aerosp Inst, Cleveland, OH 44142 USA. NASA, John H Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA. RP Kojima, J (reprint author), Ohio Aerosp Inst, 22800 Cedar Point Rd, Cleveland, OH 44142 USA. EM Jun.Kojima@grc.nasa.gov NR 35 TC 16 Z9 16 U1 0 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD SEP 1 PY 2005 VL 94 IS 3-4 BP 439 EP 466 DI 10.1016/j.jqsrt.2004.10.004 PG 28 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 912YN UT WOS:000228116300013 ER PT J AU Waller, J Reynolds, M Saulsberry, R Albright, J AF Waller, J Reynolds, M Saulsberry, R Albright, J TI Lessons learned during redesign of shuttle reaction control thruster pilot seat assembly SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article AB Current generation Space Shuttle Orbiter primary reaction control subsystem thrusters have been plagued by problems associated with oxidizer leakage, internal corrosion, and fuel valve pilot seal extrusion. In an effort to fix these problems, and thus improve thruster reliability and reduce life-cycle costs, the pilot-operated valve on the thruster was redesigned. Efforts to improve self-flushing characteristics and minimize oxidizer-induced corrosion within the pilot-operated valve were largely successful; however, a variety of problems stemming from the redesign of the pilot seat assembly within the valve were encountered. The lessons learned from the design, materials selection, and fabrication of the pilot seat assembly are addressed. For example, maximizing the likeness of prototype to final parts and exercising rigorous process control during seal fabrication were found to facilitate the transition from concept to finished hardware. Selection of a suitable polytetrafluoroethylene resin was found to be a predetermining factor in fabrication of viable pilot,seals with acceptable mechanical properties. Last, use of a correctly sized and shaped pilot seal preform was found to be essential in preventing excessive and unbalanced stress within the seal during fabrication and in minimizing seal extrusion or recession after fabrication. C1 NASA, Lyndon B Johnson Space Ctr, White Sands Test Facil, Mat Technol Grp, Las Cruces, NM 88004 USA. NASA, Lyndon B Johnson Space Ctr, White Sands Test Facil, Propellants & Hazardous Fluids Grp, Las Cruces, NM 88004 USA. NASA, Lyndon B Johnson Space Ctr, White Sands Test Facil, Labs Dept, Las Cruces, NM 88004 USA. NASA, Lyndon B Johnson Space Ctr, Div Energy Syst, Houston, TX 77058 USA. RP Waller, J (reprint author), NASA, Lyndon B Johnson Space Ctr, White Sands Test Facil, Mat Technol Grp, Las Cruces, NM 88004 USA. NR 11 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 SEP-OCT PY 2005 VL 42 IS 5 BP 928 EP 935 DI 10.2514/1.6314 PG 8 WC Engineering, Aerospace SC Engineering GA 973LF UT WOS:000232523400021 ER PT J AU Verrilli, MJ DiCarlo, JA Calomino, A Yun, H Barnett, TR AF Verrilli, MJ DiCarlo, JA Calomino, A Yun, H Barnett, TR TI Hoop tensile properties of ceramic matrix composite cylinders SO JOURNAL OF TESTING AND EVALUATION LA English DT Article DE ceramic matrix composite; silicon carbide fibers; composite structures; mechanical properties ID FIBER AB Tensile stress-strain properties in the hoop direction were obtained for 100-mm diameter ceramic matrix composite cylinders using ring specimens machined from the cylinder ends. The silicon carbide fiber-reinforced silicon carbide matrix composite (SiC/SiC) cylinders were fabricated from 2D balanced SiC fabric with several material variants, including wall thickness (6, 8, and 12 plies), SiC fiber type (Sylramic, Sylramic-iBN, Hi-Nicalon, and Hi-Nicalon S), fiber sizing type, and matrix type (full CVI SiC, and partial CVI SiC plus slurry cast + melt-infiltrated SiC-Si). Cloth ply splices existed in all the hoops. Tensile hoop measurements were made at room temperature and 1200 degrees C using hydrostatic ring test facilities. Room temperature hoop strengths for the various cylinders were generally similar and at 1200 degrees C, ultimate strengths and strains of the hoops were about 70 % of their room temperature values, and elastic moduli were about 90-100 % of their room temperature values. The hoop properties are compared with in-plane data measured on flat panels using same material variants, but containing no splices. A lower strength and failure strain of hoops compared to panels was observed and was due to a stress concentration associated with the cloth splice geometry. The failure mode of the hoops, determined through microstructural examination, revealed that a fracture surface always existed at the cloth ply splice on the inner diameter of the failed specimens. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. Cleveland State Univ, Cleveland, OH 44115 USA. So Res Inst, Birmingham, AL 35211 USA. RP Verrilli, MJ (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 19 TC 0 Z9 0 U1 0 U2 3 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 SEP PY 2005 VL 33 IS 5 BP 370 EP 376 PG 7 WC Materials Science, Characterization & Testing SC Materials Science GA 955NF UT WOS:000231231900011 ER PT J AU Shams, QA Zuckerwar, AJ Sealey, BS AF Shams, QA Zuckerwar, AJ Sealey, BS TI Compact nonporous windscreen for infrasonic measurements SO JOURNAL OF THE ACOUSTICAL SOCIETY OF AMERICA LA English DT Article AB Infrasonic windscreens, designed for service at frequencies below 20 Hz, were fabricated from a variety of materials having a low acoustic impedance, and tested against four specifications (the first three in a small wind tunnel): (1) wind-generated noise reduction ("insertion loss") at a free-stream wind speed of 9.3 m/s, (2) transmission of low-frequency sound from a known source (subwoofer), (3) spectrum of sound generated from trailing vortices (aeolian tones), and (4) water absorption (to determine suitability for all-weather service). The operating principle is based on the high penetrating capability of infrasound through solid barriers. Windscreen materials included three woods (pine, cedar, and balsa), closed-cell polyurethane foam, and Space Shuttle tile material. The windscreen inside diameter ranged from 0.0254 to 0.1016 m (1 to 4 in.), and wall thickness from 0.003175 to 0.01905 m ((1)/(8) to (3)/(4) in.). A windscreen made of closed-cell polyurethane foam revealed a wind noise reduction of 10-20 dB from 0.7 to 25 Hz, transmission coefficient near unity from 10 to 20 Hz, and spectral peaks beyond 20 Hz due to vortex-generated sound. Following a description of past methods, the principle of operation, and the experimental method, experimental data are presented for a variety of windscreens. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Shams, QA (reprint author), NASA, Langley Res Ctr, Mail Stop 238, Hampton, VA 23681 USA. EM qamar.a.shams@nasa.gov NR 13 TC 6 Z9 6 U1 0 U2 4 PU ACOUSTICAL SOC AMER AMER INST PHYSICS PI MELVILLE PA STE 1 NO 1, 2 HUNTINGTON QUADRANGLE, MELVILLE, NY 11747-4502 USA SN 0001-4966 J9 J ACOUST SOC AM JI J. Acoust. Soc. Am. PD SEP PY 2005 VL 118 IS 3 BP 1335 EP 1340 DI 10.1121/1.992707 PN 1 PG 6 WC Acoustics; Audiology & Speech-Language Pathology SC Acoustics; Audiology & Speech-Language Pathology GA 965PV UT WOS:000231963600011 ER PT J AU Steinberg, SL Kluitenberg, GJ Jones, SB Daidzic, NE Reddi, LN Xiao, M Tuller, M Newman, RM Or, D Alexander, JID AF Steinberg, SL Kluitenberg, GJ Jones, SB Daidzic, NE Reddi, LN Xiao, M Tuller, M Newman, RM Or, D Alexander, JID TI Physical and hydraulic properties of baked ceramic aggregates used for plant growth medium SO JOURNAL OF THE AMERICAN SOCIETY FOR HORTICULTURAL SCIENCE LA English DT Article DE bulk density; porosity; pore size distribution; water content; water retention; hydraulic conductivity; fritted clay; arcillite ID UNSATURATED POROUS-MEDIA; WATER; MICROGRAVITY; CONDUCTIVITY; MODEL; CLAY; FLOW; SOIL AB Baked ceramic aggregates (fritted clay, arcillite) have been used for plant research both on the ground and in microgravity. Optimal control of water and air within the root zone in any gravity environment depends on physical and hydraulic properties of the aggregate, which were evaluated for 0.25-1-mm and 1-2-mm particle size distributions. The maximum bulk densities obtained by any packing technique were 0.68 and 0.64 g(.)cm(-3) for 0.25-1-mm and 1-2-mm particles, respectively. Wettable porosity obtained by infiltration with water was approximate to 65%, substantially lower than total porosity of approximate to 74%. Aggregate of both particle sizes exhibited a bimodal pore size distribution consisting of inter-aggregate macropores and intra-aggregate micropores, with the transition from macro- to microporosity beginning at volumetric water content of approximate to 36% to 39%. For inter-aggregate water contents that support optimal plant growth there is 45% change in water content that occurs over a relatively small matric suction range of 0-20 cm H2O for 0.25-1-mm and 0 to -10 cm H2O for 1-2-mm aggregate. Hysteresis is substantial between draining and wetting aggregate, which results in as much as a approximate to 10% to 20% difference in volumetric water content for a given matric potential. Hydraulic conductivity was approximately an order of magnitude higher for 1-2-mm than for 0.25-1-mm aggregate until significant drainage of the inter-aggregate pore space occurred. The large change in water content for a relatively small change in matric potential suggests that significant differences in water retention may be observed in microgravity as compared to earth. C1 Univ Space Res Assoc, NASA, JSC, Houston, TX 77058 USA. Kansas State Univ, Dept Agron, Manhattan, KS 66506 USA. Utah State Univ, Dept Plants Soils & Biometeorol, Logan, UT 84322 USA. NASA, GLENN, Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA. Kansas State Univ, Dept Civil Engn, Manhattan, KS 66506 USA. Univ Idaho, Soils & Land Resources Div, Moscow, ID 83844 USA. Univ Connecticut, Dept Civil & Environm Engn, Storrs, CT 06269 USA. Case Western Reserve Univ, Cleveland, OH 44106 USA. RP Steinberg, SL (reprint author), Univ Space Res Assoc, NASA, JSC, Mail Code EC3, Houston, TX 77058 USA. RI Jones, Scott/A-9745-2010; Tuller, Markus/H-1822-2012; Or, Dani/D-8768-2012 OI Jones, Scott/0000-0002-3804-8785; Tuller, Markus/0000-0003-3659-2768; Or, Dani/0000-0002-3236-2933 NR 39 TC 10 Z9 10 U1 1 U2 9 PU AMER SOC HORTICULTURAL SCIENCE PI ALEXANDRIA PA 113 S WEST ST, STE 200, ALEXANDRIA, VA 22314-2851 USA SN 0003-1062 J9 J AM SOC HORTIC SCI JI J. Am. Soc. Hortic. Sci. PD SEP PY 2005 VL 130 IS 5 BP 767 EP 774 PG 8 WC Horticulture SC Agriculture GA 965DL UT WOS:000231930200018 PM 16173159 ER PT J AU Liess, S Waliser, DE Schubert, SD AF Liess, S Waliser, DE Schubert, SD TI Predictability studies of the intraseasonal oscillation with the ECHAM5 GCM SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID MADDEN-JULIAN OSCILLATION; ASIAN SUMMER MONSOON; EXTREME PRECIPITATION EVENTS; WESTERN UNITED-STATES; EL-NINO; TROPICAL CONVECTION; EQUATORIAL PACIFIC; NUMERICAL-MODEL; RANGE FORECASTS; KELVIN WAVES AB Our ability to predict active and break periods of the Asian summer monsoon is intimately tied to our ability to predict the intraseasonal oscillation (ISO). The present study analyzes the upper limit of potential predictability of the northern summer ISO, as it is simulated by the ECHAM5 atmospheric general circulation model forced with climatological SSTs. The leading extended empirical orthogonal functions of precipitation, computed from a 10-yr control simulation, are used to define four different phases of the ISO. Fourteen-member ensembles of 90-day hindcasts are run for each phase of the three strongest ISO events identified in the 10-yr control run. Initial conditions for each ensemble are created from the control simulation using a breeding method. The signal-to-noise ratio is analyzed over a region that covers the core of the Asian summer monsoon activity. Over Southeast Asia, the upper limit for predictability of precipitation and 200-hPa zonal wind is about 27 and 33 days, respectively. Over India, values of more than 15 days occur for both variables. A spatial analysis of the different phases of the ISO reveals that the predictability follows the eastward- and northward-propagating ISO during the active and break phases of the monsoon. Precipitation reveals increased predictability at the end of the convective phase. Analogous, 200-hPa zonal wind shows strongest predictability during low and easterly anomalies. This potential predictability is considerably higher than for numerical forecasts of typical weather variations, particularly for the Tropics, indicating that useful forecasts of monsoon active and break events may be possible with lead times of more than two weeks for precipitation and the dynamics. A closer look at the breeding method used here to initialize the hindcasts shows the importance of appropriate ensemble experiment designs. C1 SUNY Stony Brook, Inst Terr & Planetary Atmospheres, Stony Brook, NY 11794 USA. Jet Propuls Lab, Pasadena, CA USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Liess, S (reprint author), SUNY Stony Brook, Inst Terr & Planetary Atmospheres, Stony Brook, NY 11794 USA. EM stefan.liess@stonybrook.edu RI Liess, Stefan /C-9311-2013 OI Liess, Stefan /0000-0002-3544-8505 NR 57 TC 31 Z9 33 U1 0 U2 2 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 J9 J ATMOS SCI JI J. Atmos. Sci. PD SEP PY 2005 VL 62 IS 9 BP 3320 EP 3336 DI 10.1175/JAS3542.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 969ZP UT WOS:000232275300018 ER PT J AU Karlsson, I Grivel, JC Chen, SS Karlsson, A Albert, J Fenyo, EM Margolis, LB AF Karlsson, I Grivel, JC Chen, SS Karlsson, A Albert, J Fenyo, EM Margolis, LB TI Differential pathogenesis of primary CCR5-using human immunodeficiency virus type 1 isolates in ex vivo human lymphoid tissue SO JOURNAL OF VIROLOGY LA English DT Article ID CD4(+) T-CELLS; DISEASE PROGRESSION; HIV-INFECTION; IN-VITRO; GASTROINTESTINAL-TRACT; CORECEPTOR USE; MESSENGER-RNA; REPLICATION; LYMPHOCYTES; VARIANTS AB In the course of human immunodeficiency virus (HIV) disease, CCR5-utilizing HIV type 1 (HIV-1) variants (R5), which typically transmit infection and dominate its early stages, persist in approximately half of the infected individuals (nonswitch virus patients), while in the other half (switch virus patients), viruses using CXCR4 (X4 or R5X4) emerge, leading to rapid disease progression. Here, we used a system of ex vivo tonsillar tissue to compare the pathogeneses of sequential primary R5 HIV-1 isolates from patients in these two categories. The absolute replicative capacities of HIV-1 isolates seemed to be controlled by tissue factors. In contrast, the replication level hierarchy among sequential isolates and the levels of CCR5(+) CD4(+) T-cell depletion caused by the R5 isolates seemed to be controlled by viral factors. R5 viruses isolated from nonswitch virus patients depleted more target cells than R5 viruses isolated from switch virus patients. The high depletion of CCR5+ cells by HIV-1 isolates from nonswitch virus patients may explain the steady decline of CD4+ T cells in patients with continuous dominance of R5 HIV-1. The level of R5 pathogenicity, as measured in ex vivo lymphoid tissue, may have a predictive value reflecting whether, in an infected individual, X4 HIV-1 will eventually dominate. C1 Lund Univ, Dept Lab Med, Div Med Microbiol, Virol Unit, S-22362 Lund, Sweden. NICHHD, NIH, Bethesda, MD 20892 USA. NIH, NASA, Ctr Dimens Tissue Culture 3, Bethesda, MD 20892 USA. NICHHD, Lab Cellular & Mol Biophys, Bethesda, MD 20892 USA. Karolinska Univ Hosp, Stockholm, Sweden. Karolinska Inst, Swedish Inst Dis Control, Stockholm, Sweden. Karolinska Inst, Microbiol & Tumorbiol Ctr, Stockholm, Sweden. RP Karlsson, I (reprint author), Lund Univ, Dept Lab Med, Div Med Microbiol, Virol Unit, Solvegatan 23, S-22362 Lund, Sweden. EM Ingrid.Karlsson@mmb.lu.se NR 61 TC 19 Z9 21 U1 0 U2 1 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0022-538X J9 J VIROL JI J. Virol. PD SEP PY 2005 VL 79 IS 17 BP 11151 EP 11160 DI 10.1128/JVI.79.17.11151-11160.2005 PG 10 WC Virology SC Virology GA 956ML UT WOS:000231303900030 PM 16103166 ER PT J AU Greenblatt, RJ Work, TM Dutton, P Sutton, CA Spraker, TR Casey, RN Diez, CE Parker, D St Leger, J Balazs, GH Casey, JW AF Greenblatt, RJ Work, TM Dutton, P Sutton, CA Spraker, TR Casey, RN Diez, CE Parker, D St Leger, J Balazs, GH Casey, JW TI Geographic variation in marine turtle fibropapillomatosis SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Chelonia mydas; fibropapillomatosis; green turtle; herpesvirus ID GREEN TURTLES; CHELONIA-MYDAS AB We document three examples of fibropapillomatosis by histology, quantitative polymerase chain reaction (qPCR), and sequence analysis from three different geographic areas. Tumors compatible in morphology with fibropapillomatosis were seen in green turtles from Puerto Rico and San Diego (California) and in a hybrid loggerhead/ hawksbill turtle from Florida Bay (Florida). Tumors were confirmed as fibropapillomas on histology, although severity of disease varied between cases. Polymerase chain reaction (PCR) analyses revealed infection with the fibropapilloma-associated turtle herpesvirus (FPTHV) in all cases, albeit at highly variable copy numbers per cell. Alignment of a portion of the polymerase gene from each fibropapilloma-associated turtle herpesvirus isolate demonstrated geographic variation in sequence. These cases illustrate geographic variation in both the pathology and the virology of fibropapillomatosis. C1 Cornell Univ, Coll Vet Med, Dept Microbiol & Immunol, Ithaca, NY 14853 USA. US Geol Survey, Natl Wildlife Hlth Ctr, Honolulu Field Stn, Honolulu, HI 96850 USA. SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, La Jolla Lab, La Jolla, CA 92037 USA. Colorado State Univ, Coll Vet Med, Diagnost Lab, Ft Collins, CO 80526 USA. DRNA PR, Programa Especies Protegidas, San Juan, PR 00906 USA. Sea World San Diego, Vet Care Dept, San Diego, CA 92019 USA. Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA. RP Casey, JW (reprint author), Cornell Univ, Coll Vet Med, Dept Microbiol & Immunol, Ithaca, NY 14853 USA. RI Work, Thierry/F-1550-2015 OI Work, Thierry/0000-0002-4426-9090 FU NIEHS NIH HHS [2T32 ES07052-26] NR 11 TC 10 Z9 11 U1 1 U2 16 PU AMER ASSOC ZOO VETERINARIANS PI MEDIA PA 6 NORTH PENNELL ROAD, MEDIA, PA 19063 USA SN 1042-7260 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD SEP PY 2005 VL 36 IS 3 BP 527 EP 530 DI 10.1638/04-051.1 PG 4 WC Veterinary Sciences SC Veterinary Sciences GA 995QG UT WOS:000234118300025 PM 17312778 ER PT J AU Bucur, B Allen, PA Sanders, RE Ruthruff, E Murphy, MD AF Bucur, B Allen, PA Sanders, RE Ruthruff, E Murphy, MD TI Redundancy gain and coactivation in bimodal detection: Evidence for the preservation of coactive processing in older adults SO JOURNALS OF GERONTOLOGY SERIES B-PSYCHOLOGICAL SCIENCES AND SOCIAL SCIENCES LA English DT Article ID COGNITIVE AGING RESEARCH; DIVIDED ATTENTION; AGE-DIFFERENCES; INFORMATION; SELECTION; NOISE AB Previous investigations of adult age differences in the redundant signals effect suggest that both older and younger adults benefit from the presentation of redundant information. However, age deficits in divided attention may cause older adults to process redundant information in a different manner. In the present experiment, we tested between two competing explanations for the redundant signals effect: separate activation and coactivation. To investigate this issue, we used a bimodal detection task in which the auditory signal was a 1000-Hz tone and the visual signal was an asterisk. Both age groups showed significant violations of Miller's race model inequality, providing evidence for coactivation. These results suggest that, despite age-related deficits in divided attention, the ability to coactivate information from bimodal signals is spared with increased age. C1 Univ Akron, Dept Psychol, Akron, OH 44325 USA. NASA Ames Res Ctr, Moffett Field, CA USA. RP Bucur, B (reprint author), Univ Akron, Dept Psychol, Akron, OH 44325 USA. EM bb@geri.duke.edu FU NIA NIH HHS [T32 AG00029] NR 19 TC 13 Z9 13 U1 2 U2 5 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1079-5014 EI 1758-5368 J9 J GERONTOL B-PSYCHOL JI J. Gerontol. Ser. B-Psychol. Sci. Soc. Sci. PD SEP PY 2005 VL 60 IS 5 BP P279 EP P282 PG 4 WC Geriatrics & Gerontology; Gerontology; Psychology; Psychology, Multidisciplinary SC Geriatrics & Gerontology; Psychology GA 959NA UT WOS:000231523500008 PM 16131623 ER PT J AU Chaloupka, M Balazs, G AF Chaloupka, M Balazs, G TI Modelling the effect of fibropapilloma disease on the somatic growth dynamics of Hawaiian green sea turtles SO MARINE BIOLOGY LA English DT Article ID GREAT-BARRIER-REEF; CHELONIA-MYDAS; MARINE TURTLES; FORAGING AREA; HERPESVIRUS; PATHOLOGY; RATES; ISLANDS; SPLINES; FLORIDA AB The effect of the tumour-forming disease, fibropapillomatosis, on the somatic growth dynamics of green turtles resident in the Pala'au foraging grounds (Moloka'i, Hawai'i) was evaluated using a Bayesian generalised additive mixed modelling approach. This regression model enabled us to account for fixed effects (fibropapilloma tumour severity), nonlinear covariate functional form (carapace size, sampling year) as well as random effects due to individual heterogeneity and correlation between repeated growth measurements on some turtles. Somatic growth rates were found to be nonlinear functions of carapace size and sampling year but were not a function of low-to-moderate tumour severity. On the other hand, growth rates were significantly lower for turtles with advanced fibropapillomatosis, which suggests a limited or threshold-specific disease effect. However, tumour severity was an increasing function of carapace size-larger turtles tended to have higher tumour severity scores, presumably due to longer exposure of larger (older) turtles to the factors that cause the disease. Hence turtles with advanced fibropapillomatosis tended to be the larger turtles, which confounds size and tumour severity in this study. But somatic growth rates for the Pala'au population have also declined since the mid-1980s (sampling year effect) while disease prevalence and severity increased from the mid-1980s before levelling off by the mid-1990s. It is unlikely that this decline was related to the increasing tumour severity because growth rates have also declined over the last 10-20 years for other green turtle populations resident in Hawaiian waters that have low or no disease prevalence. The declining somatic growth rate trends evident in the Hawaiian stock are more likely a density-dependent effect caused by a dramatic increase in abundance by this once-seriously-depleted stock since the mid-1980s. So despite increasing fibropapillomatosis risk over the last 20 years, only a limited effect on somatic growth dynamics was apparent and the Hawaiian green turtle stock continues to increase in abundance. C1 Univ Queensland, Ecol Modelling Serv Pty Ltd, St Lucia, Qld 4067, Australia. NOAA, Natl Marine Fisheries Serv, Pcific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA. RP Chaloupka, M (reprint author), Univ Queensland, Ecol Modelling Serv Pty Ltd, POB 6150, St Lucia, Qld 4067, Australia. EM m.chaloupka@uq.edu.au NR 49 TC 26 Z9 29 U1 1 U2 17 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD SEP PY 2005 VL 147 IS 5 BP 1251 EP 1260 DI 10.1007/s00227-005-0026-1 PG 10 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 970SJ UT WOS:000232329600021 ER PT J AU Stamatelatos, M AF Stamatelatos, M TI Venturing to the far reaches SO MECHANICAL ENGINEERING LA English DT Article C1 NASA, Off Safety & Mission Assurance, Safety & Assurance Requirements Div, Washington, DC 20546 USA. RP Stamatelatos, M (reprint author), NASA, Off Safety & Mission Assurance, Safety & Assurance Requirements Div, Washington, DC 20546 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA SN 0025-6501 J9 MECH ENG JI Mech. Eng. PD SEP PY 2005 VL 127 IS 9 BP 38 EP 40 PG 3 WC Engineering, Mechanical SC Engineering GA 961HL UT WOS:000231652400024 ER PT J AU Horz, F Cintala, MJ See, TH Le, L AF Horz, F Cintala, MJ See, TH Le, L TI Shock melting of ordinary chondrite powders and implications for asteroidal regoliths SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID LASER IRRADIATION; LUNAR REGOLITH; SOLAR-SYSTEM; METEORITE; CRATER; IRON; SPECTROSCOPY; METAMORPHISM; CONSTRAINTS; SIMULATION AB A series of 59 impacts in the laboratory reduced a coherent 460 g piece of the L6 ordinary chondrite ALH 85017 to a coarse-grained "regolith." We then subjected the 125-250 mu m fines from this sample to reverberation shock stresses of 14.5-67 GPa in order to delineate the melting behavior of porous, unconsolidated, chondritic asteroid surfaces during meteorite impact. The initial pore space (40-50%) was completely closed at 14.5 GPa and a dense aggregate of interlocking grains resulted. Grain-boundary melting commenced at < 27 GPa and similar to 50% of the total charge was molten at 67 GPa; this stress corresponds to typical asteroid impacts at similar to 5 km/sec. Melting of the entire sample most likely mandates > 80 GPa, which is associated with impact velocities > 8 km/sec. The Fe-Ni and troilite clasts of the original meteorite melted with particular ease, forming immiscible melts that are finely disseminated throughout the silicate glass. These metal droplets are highly variable in size, extending to < 100 nm and most likely to superparamagnetic domains; such opaques are also observed in the natural melt veins of ordinary chondrites. It follows that melting and dissemination of pre-existing, Fe-rich phases may substantially affect the optical properties of asteroidal surfaces. It seems unnecessary to invoke reduction of Fe2+ (or Fe3+) by sputtering or impact-processes-in analogy to the lunar surface-to produce "space weathering" effects on S-type asteroids. We note that HED meteorites contain ample FeO (comparable to that in lunar basalts) for reduction processes to take place, yet their probable parent object(s), Vesta and its collisional fragments, display substantially unweathered surfaces. Howardites, eucrites, and diogenites (HEDs), however, contain little native metal (typically < 0.5%), in contrast to ordinary chondrites (commonly 10-15%) and their S-type parent objects. These considerations suggest that the modal content of native metal and sulfides is more important for space weathering on asteroids than total FeO. C1 SR NASA, Lyndon B Johnson Space Ctr, Astromat Res Off, Houston, TX 77058 USA. NASA, Lockheed Martin Space Operat, Houston, TX 77058 USA. RP Horz, F (reprint author), SR NASA, Lyndon B Johnson Space Ctr, Astromat Res Off, Houston, TX 77058 USA. EM friedrich.p.horz1@jsc.nasa.gov NR 68 TC 30 Z9 30 U1 1 U2 4 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP-OCT PY 2005 VL 40 IS 9-10 BP 1329 EP 1346 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 991LV UT WOS:000233816400006 ER PT J AU Meibom, A Righter, K Chabot, N Dehn, G Antignano, A McCoy, TJ Krot, AN Zolensky, ME Petaev, MI Keil, K AF Meibom, A Righter, K Chabot, N Dehn, G Antignano, A McCoy, TJ Krot, AN Zolensky, ME Petaev, MI Keil, K TI Shock melts in QUE 94411, Hammadah al Hamra 237, and Bencubbin: Remains of the missing matrix? SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID ZONED METAL GRAINS; CARBONACEOUS CHONDRITES; CH CHONDRITES; PRIMITIVE CHONDRITE; METEORITIC BRECCIA; NITROGEN ISOTOPE; SOLAR NEBULA; CONDENSATION; ORIGIN; METAMORPHISM AB We have studied the CB carbonaceous chondrites Queen Alexandra Range (QUE) 94411, Hammadah al Hamra (HH) 237, and Bencubbin with an emphasis on the petrographical and mineralogical effects of the shock processing that these meteorite assemblages have undergone. Iron-nickel metal and chondrule silicates are the main components in these meteorites. These high-temperature components are held together by shock melts consisting of droplets of dendritically intergrown Fe,Ni-metal/sulfide embedded in silicate glass, which is substantially more FeO-rich (3040 wt%) than the chondrule silicates (FeO < 5 wt%). Fine-grained matrix material, which is a major component in most other chondrite classes, is extremely scarce in QUE 94411 and HH 237, and has not been observed in Bencubbin. This material occurs as rare, hydrated matrix lumps with major and minor element abundances roughly similar to the ferrous silicate shock melts (and Cl). We infer that hydrated, fine-grained material, compositionally similar to these matrix lumps, was originally present between the Fe,Ni-metal grains and chondrules, but was preferentially shock melted. Other shock-related features in QUE 94411, HH 237, and Bencubbin include an alignment and occasionally strong plastic deformation of metal and chondrule fragments. The existence of chemically zoned and metastable Fe,Ni-metal condensates in direct contact with shock melts indicates that the shock did not substantially increase the average temperature of the rock. Because porphyritic olivine-pyroxene chondrules are absent in QUE 94411, HH 237, and Bencubbin, it is difficult to determine the precise shock stage of these meteorites, but the shock was probably relatively light (S2-S3), consistent with a bulk temperature increase of the assemblages of less than similar to 300 degrees C. The apparently similar shock processing of Bencubbin, Weatherford, Gujba (CBa) and QUE 94411/HH 237 (CBb) supports the idea of a common asteroidal parent body for these meteorites. C1 Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Sch Ocean & Earth Sci & Technol, Honolulu, HI 96822 USA. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Colorado Coll, Dept Geol, Colorado Springs, CO 80903 USA. Smithsonian Inst, Natl Museum Amer Hist, Dept Mineral Sci, Washington, DC 20560 USA. George Washington Univ, Dept Earth & Environm Sci, Washington, DC 20052 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. RP Meibom, A (reprint author), Museum Hist Nat, Lab Etud Mat Extraterr, USM 0205 LEME, Case Postale 5257 Rue Cuvier, F-75005 Paris, France. EM meibom@mnhn.fr RI Chabot, Nancy/F-5384-2015 OI Chabot, Nancy/0000-0001-8628-3176 NR 61 TC 15 Z9 15 U1 0 U2 2 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP-OCT PY 2005 VL 40 IS 9-10 BP 1377 EP 1391 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 991LV UT WOS:000233816400010 ER PT J AU Arnold, JR Metzger, AE Trombka, JI Reedy, RC AF Arnold, JR Metzger, AE Trombka, JI Reedy, RC TI The global view of lunar geochemistry from the Apollo gamma ray spectrometer SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 Univ Calif San Diego, Dept Chem & Biochem, La Jolla, CA 92093 USA. NASA, Jet Propuls Lab, Pasadena, CA 91109 USA. NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA. Univ New Mexico, Inst Mech, Albuquerque, NM 87131 USA. EM rreedy@unm.edu NR 8 TC 1 Z9 1 U1 1 U2 1 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A17 EP A17 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000015 ER PT J AU Berthet, S Malavergne, V Corgne, A Righter, K Fei, Y AF Berthet, S Malavergne, V Corgne, A Righter, K Fei, Y TI High pressure and temperature experiments on the indarch (EH4) chondrite: Constraints on phase relations and partitioning behavior SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc ID EARTH C1 Lunar & Planetary Inst, Houston, TX 77058 USA. Univ Paris 12, Lab Geomat, F-77454 Champs Sur Marne, France. Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM berthet@lpi.usra.edu NR 4 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A19 EP A19 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000019 ER PT J AU Bogard, DD Garrison, DH AF Bogard, DD Garrison, DH TI Ar-39-Ar-41 ages and trapped Ar in Martian nakhlites and chassignites SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 NASA, Lyndon B Johnson Space Ctr, ARES Code KR, Houston, TX 77058 USA. Barrios Technol, ESCG, Houston, TX 77058 USA. NR 4 TC 2 Z9 2 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A22 EP A22 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000025 ER PT J AU Chabot, NL Campbell, AJ Humayun, M Jones, JH Lauer, HV AF Chabot, NL Campbell, AJ Humayun, M Jones, JH Lauer, HV TI Distinguishing between sulfur and carbon-bearing metallic liquids during meteorite histories SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc ID IRON-METEORITES C1 Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. Florida State Univ, Natl High Magnet Field Lab, Tallahassee, FL 32310 USA. Florida State Univ, Dept Geol Sci, Tallahassee, FL 32310 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Barrios Technol, ESCG, Houston, TX 77258 USA. EM nancy.chabot@jhuapl.edu RI Chabot, Nancy/F-5384-2015 OI Chabot, Nancy/0000-0001-8628-3176 NR 7 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A27 EP A27 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000035 ER PT J AU Clemett, SJ Keller, LP McKay, DS AF Clemett, SJ Keller, LP McKay, DS TI Lunar organic compounds: Search and characterization SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 NASA, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA. EM simon.j.clemett@nasa.gov NR 3 TC 0 Z9 0 U1 0 U2 2 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A31 EP A31 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000042 ER PT J AU Cole, KJ Dod, BD Jerman, GA Pelisson, R Sipiera, PP AF Cole, KJ Dod, BD Jerman, GA Pelisson, R Sipiera, PP TI A review of 62 meteorites recovered from Algeria, Libya, and Western Sahara SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 Harper Coll, Schmitt Meteorite Res Grp, Palatine, IL 60067 USA. NASA, George C Marshall Space Flight Ctr, Met Diagnost Facil, Huntsville, AL 35812 USA. Mercer Univ, Dept Phys & Earth Sci, Macon, GA USA. Sahara Meteorite Prospectin, LaTerrasse, France. EM kcole@atriton.edu NR 6 TC 2 Z9 2 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A32 EP A32 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000045 ER PT J AU Consolmagno, GJ Rothschild, LJ Strait, MM Britt, DT AF Consolmagno, GJ Rothschild, LJ Strait, MM Britt, DT TI Can meteorite porosity provide habitats for interplanetary transport of microbes? SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 Specola Vaticana, V-00120 Vatican City, Vatican. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Alma Coll, Alma, MI 48801 USA. Univ Cent Florida, Orlando, FL 32816 USA. EM gjc@specola.va NR 6 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A33 EP A33 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000046 ER PT J AU Danielson, LR Humayun, M Righter, K AF Danielson, LR Humayun, M Righter, K TI Highly siderophile elements in the Admire, Imilac, and Springwater pallasites SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc ID IRON-METEORITES; PHASES; OS C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Florida State Univ, Dept Geol Sci, Natl High Magnet Field Lab, Tallahassee, FL 32310 USA. EM ldaniels@ems.jsc.nasa.gov NR 8 TC 0 Z9 0 U1 1 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 SEP PY 2005 VL 40 IS 9 SU S BP A35 EP A35 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000050 ER PT J AU Echaurren, JC Ocampo, AC Rocca, MCL AF Echaurren, JC Ocampo, AC Rocca, MCL TI A mathematic model for the Monturaqui impact crater, Chile, South America SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 NASA, Jet Propuls Lab, Pasadena, CA 91109 USA. EM jecha001@codelco.cl; rnaxrocca@hotmail.com NR 3 TC 0 Z9 0 U1 0 U2 5 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A43 EP A43 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000066 ER PT J AU Elsila, JE Bernstein, MP Sandford, SA AF Elsila, JE Bernstein, MP Sandford, SA TI UU irradiation of aromatic nitrogen heterocycles in interstellar ice analogs SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM jelsila@mail.arc.nasa.gov RI Elsila, Jamie/C-9952-2012 NR 4 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A44 EP A44 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000069 ER PT J AU Foley, CN Nittler, LR Brown, MRM McCoy, TJ Lim, L AF Foley, CN Nittler, LR Brown, MRM McCoy, TJ Lim, L TI Cr, Mn, and Ni on 433 Eros: Further evidence of ordinary chondrite composition SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc ID X-RAY SPECTROMETER; ELEMENTAL COMPOSITION C1 Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM foley@dtm.ciw.edu RI Lim, Lucy/C-9557-2012 OI Lim, Lucy/0000-0002-9696-9654 NR 6 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A50 EP A50 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000081 ER PT J AU Gaffey, MJ Abell, PA Hardersen, PS Vilas, F Jarvis, KS Landis, R AF Gaffey, MJ Abell, PA Hardersen, PS Vilas, F Jarvis, KS Landis, R TI Compositions of binary near-Earth objects: Implications for the meteorite flux SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc ID ASTEROIDS C1 Univ N Dakota, Grand Forks, ND 58202 USA. NASA, Lyndon B Johnson Space Ctr, Planetary Astron Grp, Houston, TX 77058 USA. NASA, Lyndon B Johnson Space Ctr, Mission Operat, Houston, TX 77058 USA. EM gaffey@space.edu NR 8 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A53 EP A53 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000086 ER PT J AU Garrison, DH Bogard, DD Herzog, GF Xue, S Klein, J Middleton, R AF Garrison, DH Bogard, DD Herzog, GF Xue, S Klein, J Middleton, R TI Early impact melting and space exposure history of the PAT 91501 L chondrite SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc ID AGES C1 Barrios, ESCG, Houston, TX 77058 USA. NASA, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA. Rutgers State Univ, Piscataway, NJ 08854 USA. Univ Penn, Philadelphia, PA 19104 USA. RI Klein, Jeffrey/E-3295-2013 NR 6 TC 1 Z9 1 U1 0 U2 1 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A54 EP A54 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000088 ER PT J AU Gibson, EK Socki, RA Wentworth, SJ Romanek, CS McKay, DS AF Gibson, EK Socki, RA Wentworth, SJ Romanek, CS McKay, DS TI Record of water in Martian meteorites and the history of Mars SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 NASA, Lyndon B Johnson Space Ctr, ARES, KR, Houston, TX 77058 USA. Savannah River Ecol Lab, Aiken, SC 29802 USA. EM everett.k.gibson@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A55 EP A55 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000091 ER PT J AU Grimberg, A Buhler, F Bochsler, P Heber, VS Tosatti, S Jurewicz, AJG Hays, CC McNamara, K Allton, JH Burnett, DS Baur, H Wieler, R AF Grimberg, A Buhler, F Bochsler, P Heber, VS Tosatti, S Jurewicz, AJG Hays, CC McNamara, K Allton, JH Burnett, DS Baur, H Wieler, R TI Solar wind noble gases - Preliminary results from bulk metallic glass flown on Genesis SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 ETH, Isotope Geol, Zurich, Switzerland. Univ Bern, Inst Phys, Bern, Switzerland. ETH, Surface Sci & Technol, Zurich, Switzerland. NASA, Jet Prop Lab, Pasadena, CA 91109 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. CALTECH, GPS, Pasadena, CA 91125 USA. EM grimberg@erdw.ethz.ch RI Wieler, Rainer/A-1355-2010 OI Wieler, Rainer/0000-0001-5666-7494 NR 4 TC 0 Z9 0 U1 0 U2 3 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A60 EP A60 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000101 ER PT J AU Grossman, JN Zolensky, ME Tonui, EK AF Grossman, JN Zolensky, ME Tonui, EK TI What are the petrologic types of thermally metamorphosed CM chondrites? SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 US Geol Survey, Natl Ctr 954, Reston, VA 20192 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. EM jgrossman@usgs.gov NR 4 TC 3 Z9 3 U1 0 U2 1 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A61 EP A61 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000102 ER PT J AU Herrin, JS Mittlelfehldt, DW Jones, JH AF Herrin, JS Mittlelfehldt, DW Jones, JH TI Early metal records: Metal inclusions in acapulcoite-lodranite silicates SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 NASA, Lyndon B Johnson Space Ctr, KR, Houston, TX 77058 USA. EM jason.s.herrin1@jsc.nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A65 EP A65 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000111 ER PT J AU Johnson, NM Martin, M Dworkin, JP Nuth, JA AF Johnson, NM Martin, M Dworkin, JP Nuth, JA TI Synthesizing organics using amorphous Mg- and Fe-silicate grains SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc ID SOLAR NEBULA; CHEMISTRY C1 NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA. Catholic Univ Amer, Washington, DC 20064 USA. RI Johnson, Natasha/E-3093-2012; Dworkin, Jason/C-9417-2012 OI Dworkin, Jason/0000-0002-3961-8997 NR 4 TC 0 Z9 0 U1 0 U2 1 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A77 EP A77 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000134 ER PT J AU Jones, JH AF Jones, JH TI Calculations of lunar bulk composition SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 NASA, Lyndon B Johnson Space Ctr, KR, Houston, TX 77058 USA. EM jjones2@em.s.jsc.nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A78 EP A78 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000136 ER PT J AU Keller, LP Christoffersen, R AF Keller, LP Christoffersen, R TI Spectrum imaging of space-weathered rims on lunar soil grains SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A79 EP A79 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000138 ER PT J AU Kletetschka, G Wasilewski, PT Zila, V AF Kletetschka, G Wasilewski, PT Zila, V TI Magnetic paleofield estimates for chondrules extracted from Bjurbole (L4) meteorite SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 Catholic Univ, Washington, DC USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. ASCR, Inst Geol, Prague, Czech Republic. Charles Univ, Prague, Czech Republic. EM gunther.kletetschka@gsfc.nasa.gov RI Kletetschka, Gunther/C-9996-2011 OI Kletetschka, Gunther/0000-0002-0645-9037 NR 4 TC 0 Z9 0 U1 0 U2 5 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A83 EP A83 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000146 ER PT J AU Koscheev, AP Gromov, MD Gorokhov, PV Ott, U Huss, GR Daulton, TL AF Koscheev, AP Gromov, MD Gorokhov, PV Ott, U Huss, GR Daulton, TL TI Ion implantation into nanodiamonds and the mechanism of high temperature release of noble gases from meteoritic diamonds SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc ID PRESOLAR DIAMONDS C1 Karpov Inst Phys Chem, Moscow 105064, Russia. Max Planck Inst Chem, D-55128 Mainz, Germany. Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. USN, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA. EM koscheev@cc.nifhi.ac.ru NR 4 TC 4 Z9 4 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A87 EP A87 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000154 ER PT J AU Madden, MEE Bodnar, RJ Cheung, K Zolensky, M AF Madden, MEE Bodnar, RJ Cheung, K Zolensky, M TI Development of a nondestructive technique using Raman spectroscopy to measure the D/H ratio of extraterrestrial water SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc ID MONAHANS 1998; CHONDRITE; HALITE C1 Virginia Tech, Dept Geosci, Blacksburg, VA 24061 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM rjb@vt.edu RI Bodnar, Robert/A-1916-2009; Elwood Madden, Megan/C-3381-2009 NR 3 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A45 EP A45 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000070 ER PT J AU McKay, G Mikouchi, T AF McKay, G Mikouchi, T TI Minor element zoning in nakhlites: What's going on? SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 NASA, Lyndon B Johnson Space Ctr, Astromat Res Off, Houston, TX 77058 USA. Univ Tokyo, Tokyo, Japan. EM Gordon.mckay@jsc.nasa.gov NR 2 TC 1 Z9 1 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A100 EP A100 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000181 ER PT J AU Mikouchi, T Righter, K AF Mikouchi, T Righter, K TI SEM-EBSD analysis on symplectic inclusion in the QUE 93148 olivine SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc ID EXSOLUTION; PALLASITE C1 Univ Tokyo, Dept Earth & Planetary Sci, Tokyo 1130033, Japan. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM mikouchi@eps.s.u-tokyo.ac.jp NR 4 TC 0 Z9 0 U1 1 U2 1 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A103 EP A103 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000186 ER PT J AU Milam, KA Deane, B King, PL Lee, PC Hawkins, M AF Milam, KA Deane, B King, PL Lee, PC Hawkins, M TI Inside of the Flynn creek impact and processes of central uplift forniation: The view from Hawkins impact cave SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. Univ Western Ontario, Dept Earth Sci, London, ON N6A 5B7, Canada. NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. DeKalb Cty High Sch, Smithville, TN 37166 USA. EM kmilam@utk.edu NR 4 TC 0 Z9 0 U1 1 U2 2 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A103 EP A103 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000187 ER PT J AU Mittlefehldt, DW AF Mittlefehldt, DW TI Origin of main-group pallasites SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM david.w.mittlefehldt@nasa.gov NR 4 TC 3 Z9 3 U1 0 U2 1 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A104 EP A104 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000189 ER PT J AU Nakamura, K Messenger, S Keller, LP AF Nakamura, K Messenger, S Keller, LP TI Experimental hydrothermal alteration of anhydrous IDPs SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 NASA, Lyndon B Johnson Space Ctr, Robert M Walker Lab Space Sci, ARES, Houston, TX 77058 USA. EM keiko.nakamural@jsc.nasa.gov NR 7 TC 6 Z9 6 U1 0 U2 1 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A110 EP A110 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000200 ER PT J AU Norman, M Taylor, L Shih, C Reese, Y Nyquist, L Bowen-Thomas, J AF Norman, M Taylor, L Shih, C Reese, Y Nyquist, L Bowen-Thomas, J TI Lifting the veil: A pre-cataclysm lunar impact melt SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 Lunar & Planetary Inst, Houston, TX 77058 USA. Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT, Australia. Univ Tennessee, Planetary Sci Inst, Knoxville, TN 37996 USA. NASA, Johnson Space Ctr, Houston, TX 77058 USA. EM Marc.Norman@anu.edu.au NR 0 TC 1 Z9 1 U1 1 U2 2 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A115 EP A115 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000211 ER PT J AU Nuth, JA Johnson, NM AF Nuth, JA Johnson, NM TI A new paradigm for organic chemistry in nebulae: Protostars as chemical factories SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 NASA, Goddard Space Flight Ctr, Astrochem Lab, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. EM nuth@gsfc.nasa.gov RI Johnson, Natasha/E-3093-2012 NR 0 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A116 EP A116 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000212 ER PT J AU Nyquist, LE Shih, CY AF Nyquist, LE Shih, CY TI The lunar Rb/Sr ratio and implications for lunar history SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc ID MANTLE C1 NASA, Johnson Sp Ctr, Houston, TX 77058 USA. ESCG Jacobs Sverdrup, Houston, TX 77058 USA. EM laurence.e.nyquist@nasa.gov NR 7 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A116 EP A116 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000213 ER PT J AU Ocampo, AC Garrido, AC Rabassa, J Rocca, MCL Echaurren, JC Mazzoni, E AF Ocampo, AC Garrido, AC Rabassa, J Rocca, MCL Echaurren, JC Mazzoni, E TI A possible impact crater in basalt at Meseta de la Barda Negra, Neuquen, Argentina SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 NASA, Jet Propuls Lab, Pasadena, CA 91109 USA. Museo Carmen Funes, RA-8318 Neuquen, Argentina. CADIC, Tierra Del Fuego, Argentina. Univ Nacl Patagonia Austral, Santa Cruz, CA USA. EM adriana.c.ocampo@jpl.nasa.gov NR 5 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A117 EP A117 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000215 ER PT J AU Rankenburg, K Brandon, A Norman, M Righter, K AF Rankenburg, K Brandon, A Norman, M Righter, K TI LAP 02205: An evolved member of the Apollo 12 olivine basalt suite? SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 NASA, Johnson Space Ctr, Houston, TX 77058 USA. Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT 0200, Australia. EM kai.rankenburgl@jsc.nasa.gov NR 11 TC 3 Z9 3 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A125 EP A125 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000231 ER PT J AU Righter, K AF Righter, K TI The contribution of lunar meteorites to our understanding of the Moon SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 NASA, Johnson Space Ctr, Houston, TX 77058 USA. EM kevin.righter-l@nasa.gov NR 9 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A127 EP A127 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000234 ER PT J AU Russell, SS Zolensky, M Righter, K Folco, L Jones, R Connolly, HC Grady, MM Grossman, JN AF Russell, SS Zolensky, M Righter, K Folco, L Jones, R Connolly, HC Grady, MM Grossman, JN TI The Meteoritical Bulletin, No. 89, 2005 September SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID CARBONACEOUS CHONDRITES; METAMORPHISM AB This Bulletin lists 1768 meteorites, bringing the total known meteorites to over 30,000 at 30,907. Of these, 10 10 are from Antarctica, 569 from Africa, 92 from Asia (83 of which are from Oman), 85 from North America, one from South America and I I from Europe. The Bulletin reports seven falls (Benguerir, Bukhara, Kasauli, Maigatari-Danduma, Oum Dreyga, Rahimyar Khan, and San Michele). Noteworthy specimens include 20 lunar meteorites, Four Martian meteorites, two pallasites, three mesosiderites, and two Bencubbin-like meteorites. Additional information can be found at http://meteoriticalsociety.org/bulletin/database.html. C1 Nat Hist Museum, Dept Mineral, London SW7 5BD, England. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Museo Nazl Antartide, I-53100 Siena, Italy. Univ New Mexico, Inst Meteorit, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. CUNY, Kingsborough Coll, Dept Phys Sci, Brooklyn, NY 11235 USA. CUNY, Grad Sch, Brooklyn, NY 11235 USA. Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 11024 USA. Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England. US Geol Survey, Reston, VA 20192 USA. RP Russell, SS (reprint author), Nat Hist Museum, Dept Mineral, Cromwell Rd, London SW7 5BD, England. EM sara.russell@nhm.ac.uk NR 19 TC 52 Z9 53 U1 0 U2 1 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A201 EP A263 PG 63 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000335 ER PT J AU Sipiera, PP Cole, KJ Schwade, JR Jerman, GA Dod, BD AF Sipiera, PP Cole, KJ Schwade, JR Jerman, GA Dod, BD TI Status of the James M. DuPont meteorite collection 1995-2004 SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc ID ESCARPMENT; ANTARCTICA C1 Harper Coll, Schmitt Meteorite Res Grp, Palatine, IL 60067 USA. NASA, Marshall Space Flight Ctr, Met Diagnost Facil, Huntsville, AL 35812 USA. Mercer Univ, Dept Phys & Earth Sci, Macon, GA 31207 USA. EM psipiera@harpercollege.edu NR 5 TC 1 Z9 1 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A142 EP A142 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000265 ER PT J AU Tomioka, N Tomeoka, K Nakamura, K AF Tomioka, N Tomeoka, K Nakamura, K TI Analytical transmission electron microscopy of experimentally shocked murchison CM chondrite SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc ID ATMOSPHERIC ENTRY; MICROMETEORITES C1 Kobe Univ, Dept Earth & Planetary Sci, Kobe, Hyogo 6578501, Japan. NASA, Johnson Space Ctr, Houston, TX 77058 USA. EM nao@kobe-u.ac.jp NR 6 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A156 EP A156 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000292 ER PT J AU Velbel, MA Tonui, EK Zolensky, ME AF Velbel, MA Tonui, EK Zolensky, ME TI Aqueous alteration in QUE 93005 (CM2): Diiferent alteration scales for Antarctic and non-Antarctic CM chondrites? SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc ID CARBONACEOUS CHONDRITES C1 Michigan State Univ, Dept Geol Sci, E Lansing, MI 48824 USA. Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA. NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Off, Houston, TX 77058 USA. EM velbel@msu.edu NR 6 TC 2 Z9 2 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A161 EP A161 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000303 ER PT J AU Zolensky, ME Le, L AF Zolensky, ME Le, L TI Identifying the source of the hydrous chondritic interplanetary dust particles SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc ID METEORITES C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. ESCG Jacobs Sverdrup, Houston, TX 77058 USA. EM michael.e.zolensky@nasa.gov NR 5 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A175 EP A175 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000330 ER PT J AU Battye, RA Weller, J AF Battye, RA Weller, J TI Optimizing the yield of Sunyaev-Zel'dovich cluster surveys SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : clusters; cosmic microwave background ID GALAXY CLUSTERS; COSMOLOGICAL CONSTRAINTS; POWER-SPECTRUM; MATTER; ABUNDANCE; CONSTANT; SKY; PARAMETERS; TELESCOPE; EVOLUTION AB We consider the optimum depth of a cluster survey selected using the Sunyaev-Zel'dovich effect. By using simple models for the evolution of the cluster mass function and detailed modelling for a variety of observational techniques, we show that the optimum survey yield is achieved when the average size of the clusters selected is close to the size of the telescope beam. For a total power measurement, we compute the optimum noise threshold per beam as a function of the beam size and then discuss how our results can be used in more general situations. As a by-product we gain some insight into what is the most advantageous instrumental set-up. In the case of beam switching observations one is not severely limited if one manages to set the noise threshold close to the point which corresponds to the optimum yield. Considering a variety of alternative scenarios, we discuss how robust our conclusions are to modifications in the cluster model and cosmological parameters. The precise optimum is particularly sensitive to the amplitude of fluctuations and the profile of the gas in the cluster. C1 Univ Manchester, Sch Phys & Astron, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. NASA, Fermi Natl Accelerator Lab, Fermilab Astrophys Ctr, Batavia, IL 60510 USA. UCL, Dept Phys & Astron, London WC1E 6BT, England. RP Univ Manchester, Sch Phys & Astron, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. EM rbattye@jb.man.ac.uk; jweller@fnal.gov OI Weller, Jochen/0000-0002-8282-2010 NR 42 TC 6 Z9 6 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 1 PY 2005 VL 362 IS 1 BP 171 EP 183 DI 10.1111/j.1365-2966.2005.09271.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 963KP UT WOS:000231803500014 ER PT J AU Vaughan, S Uttley, P AF Vaughan, S Uttley, P TI Where are the X-ray quasi-periodic oscillations in active galaxies? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : active; galaxies : Seyfert; X-ray : galaxies ID BLACK-HOLE CANDIDATES; ALL-SKY MONITOR; GALACTIC NUCLEI; POWER SPECTRUM; GRO J1655-40; VELOCITY DISPERSION; SEYFERT-1 GALAXIES; RED NOISE; CYG X-1; FREQUENCY AB In this paper, we address the question of whether existing X-ray observations of Seyfert galaxies are sufficiently sensitive to detect quasi-periodic oscillations (QPOs) similar to those observed in the X-ray variations of Galactic black holes (GBHs). We use data from XMM-Newton and simulated data based on the best Rossi X-ray Timing Explorer (RXTE) long-term monitoring light curves to show that if X-ray QPOs are present in Seyfert X-ray light curves - with similar shapes and strengths to those observed in GBHs, but at lower frequencies commensurate with their larger black hole masses - they would be exceedingly difficult to detect. Our results offer a simple explanation for the present lack of QPO detections in Seyferts. We discuss the improvements in telescope size and monitoring patterns needed to make QPO detections feasible. The most efficient type of future observatory for searching for X-ray QPOs in active Galactic nuclei (AGN) is an X-ray All-Sky Monitor (ASM). A sufficiently sensitive ASM would be ideally suited to detect low-frequency QPOs in nearby AGN. The detection of AGN QPOs would strengthen the AGN-GBH connection, and could serve as powerful diagnostics of the black hole mass and the structure of the X-ray emitting region in AGN. C1 Univ Leicester, X Ray & Observat Astron Grp, Leicester LE1 7RH, Leics, England. NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. RP Vaughan, S (reprint author), Univ Leicester, X Ray & Observat Astron Grp, Leicester LE1 7RH, Leics, England. EM sav2@star.le.ac.uk NR 54 TC 25 Z9 25 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 1 PY 2005 VL 362 IS 1 BP 235 EP 244 DI 10.1111/j.1365-2966.2005.09296.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 963KP UT WOS:000231803500019 ER PT J AU Fox-Rabinovitz, MS Berbery, EH Takacs, LL Govindaraju, RC AF Fox-Rabinovitz, MS Berbery, EH Takacs, LL Govindaraju, RC TI A multiyear ensemble simulation of the US climate with a stretched-grid GCM SO MONTHLY WEATHER REVIEW LA English DT Article ID GENERAL-CIRCULATION MODEL; SHALLOW-WATER EQUATIONS; NUMERICAL WEATHER PREDICTION; DYNAMICAL CORE; GLA GCM; SYSTEM; PARAMETERIZATION; CONVECTION; PROJECT; EVENTS AB Multiyear (1987-97) limited ensemble integrations using a stretched-grid GCM, previously developed and experimented with by the authors, are employed for U.S. regional climate simulations. The ensemble members (six in total) are produced at two different regional resolutions: three members with 60-km and the other three members with 10-km regional resolution. The use of these two finer and coarser regional resolution ensemble members allows one to examine the impact of resolution on the overall quality of the simulated regional fields. For the multiyear ensemble simulations, an efficient regional downscaling to realistic mesoscales has been obtained. The ensemble means of the midtroposphere prognostic variables (height and meridional wind) show an overall good resemblance to the global reanalysis, especially for summer. Low-level features like the warm season Great Plains low-level jet are well represented in the simulations. During winter the 100-km simulations develop a southward wind east of the Rockies that is present neither in the reanalyses nor in the 60-km simulations. The analysis of the annual mean precipitation and its variance reveals that the ensemble simulations reproduce many of the observed features of a high-resolution rain gauge dataset analyzed on a 0.5 degrees X 0.5 degrees grid. Signal-to-noise ratios are larger than 1.5 s over a major part of the United States, especially over the Midwest and also over the mountainous regions like the Rockies and the Appalachians, suggesting that the orographic forcing is contributing to a larger signal. The ratios are smaller toward the eastern and western U.S. coastlines. This result could be attributed, at least in part, to limits in the representation of the land-sea contrasts. For comparison purposes, an additional simulation has been performed using a global uniform 2 degrees X 2.5 degrees grid with the same number of global grid points as those of the above stretched grids. The stretched-grid GCM ensemble means show, overall, a better regional depiction of features than those of the uniform-grid GCM. The results of the study show that even using limited ensemble integrations with a state-of-the-art stretched-grid GCM is beneficial for reducing the uncertainty of the multiyear regional climate simulation, especially when using finer 60-km regional resolution. C1 Univ Maryland, ESSIC, College Pk, MD 20742 USA. Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. Sci Applicat Int Corp, Beltsville, MD USA. RP Fox-Rabinovitz, MS (reprint author), Univ Maryland, ESSIC, Room 2207,224 CSS Bldg, College Pk, MD 20742 USA. EM foxrab@essic.umd.edu RI Berbery, Ernesto/F-4560-2010 OI Berbery, Ernesto/0000-0003-2587-3345 NR 43 TC 7 Z9 7 U1 0 U2 2 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0027-0644 J9 MON WEATHER REV JI Mon. Weather Rev. PD SEP PY 2005 VL 133 IS 9 BP 2505 EP 2525 DI 10.1175/MWR2956.1 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 965LP UT WOS:000231952300001 ER PT J AU Ray, RD Poulose, S AF Ray, RD Poulose, S TI Terdiurnal surface-pressure oscillations over the continental United States SO MONTHLY WEATHER REVIEW LA English DT Article ID LOWER THERMOSPHERE; TIDE; MESOSPHERE AB The small terdiurnal pressure oscillation S-3(p) is determined over the conterminous United States by analyzing long time series of hourly barometer data from 180 stations. Spectral analysis of these time series reveals that the terdiurnal band is dominated by three or four spectral peaks, separated in frequency by 1 cpy. The central peak at 3 cpd is invariably smaller than the two immediate side peaks, indicative of extraordinarily strong seasonal variations in the tide. The largest terdiurnal tide occurs over the south-central United States in winter where amplitudes exceed 300 mu bar. Summertime amplitudes are roughly one-half as large. Summer and winter tides are almost completely out of phase, with rapid 180 degrees shifts occurring in the equinox seasons when amplitudes are very small. C1 NASA, Goddard Space Flight Ctr, Terr Phys Lab, Greenbelt, MD 20771 USA. Raytheon ITSS, Lanham, MD USA. RP Ray, RD (reprint author), NASA, Goddard Space Flight Ctr, Terr Phys Lab, Code 926, Greenbelt, MD 20771 USA. EM richard.ray@gsfc.nasa.gov RI Ray, Richard/D-1034-2012 NR 17 TC 3 Z9 3 U1 0 U2 1 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 SEP PY 2005 VL 133 IS 9 BP 2526 EP 2534 DI 10.1175/MWR2988.1 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 965LP UT WOS:000231952300002 ER PT J AU Zhu, P Bretherton, CS Kohler, M Cheng, AN Chlond, A Geng, QZ Austin, P Golaz, JC Lenderink, G Lock, A Stevens, B AF Zhu, P Bretherton, CS Kohler, M Cheng, AN Chlond, A Geng, QZ Austin, P Golaz, JC Lenderink, G Lock, A Stevens, B TI Intercomparison and interpretation of single-column model simulations of a nocturnal stratocumulus-topped marine boundary layer SO MONTHLY WEATHER REVIEW LA English DT Article ID LARGE-SCALE MODELS; MIXING SCHEME; PART I; CLOUD; ENTRAINMENT; PARAMETERIZATION; INSTABILITY; TURBULENCE; CLIMATE; TESTS AB Ten single-column models (SCMs) from eight groups are used to simulate a nocturnal nonprecipitating marine stratocumulus-topped mixed layer as part of an intercomparison organized by the Global Energy and Water Cycle Experiment Cloud System Study, Working Group 1. The case is idealized from observations from the Dynamics and Chemistry of Marine Stratocumulus II, Research Flight 1. SCM simulations with operational resolution are supplemented by high-resolution simulations and compared with observations and large-eddy simulations. All participating SCMs are able to maintain a sharp inversion and a mixed cloud-topped layer, although the moisture profiles show a slight gradient in the mixed layer and produce entrainment rates broadly consistent with observations, but the liquid water paths vary by a factor of 10 after only 1 h of simulation at both high and operational resolution. Sensitivity tests show insensitivity to activation of precipitation and shallow convection schemes in most models, as one would observationally expect for this case. C1 Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England. NASA, Langley Res Ctr, Hampton, VA 23665 USA. Max Planck Inst Meteorol, Hamburg, Germany. Univ British Columbia, Vancouver, BC V5Z 1M9, Canada. USN, Res Lab, Natl Res Council, Monterey, CA USA. Koninklijk Nederlands Meteorol Inst, De Bilt, Netherlands. United Kingdom Meteorol Off, Exeter, Devon, England. Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA. RP Zhu, P (reprint author), Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. EM pzhu@cgd.ucar.edu RI Stevens, Bjorn/A-1757-2013; Golaz, Jean-Christophe/D-5007-2014; OI Stevens, Bjorn/0000-0003-3795-0475; Golaz, Jean-Christophe/0000-0003-1616-5435; lenderink, geert/0000-0002-1572-4867 NR 26 TC 41 Z9 41 U1 0 U2 5 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0027-0644 J9 MON WEATHER REV JI Mon. Weather Rev. PD SEP PY 2005 VL 133 IS 9 BP 2741 EP 2758 DI 10.1175/MWR2997.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 965LP UT WOS:000231952300014 ER PT J AU Lettington, AH Dunn, D Alexander, NE Wabby, A Lyons, BN Doyle, R Walshe, J Attia, MF Blankson, I AF Lettington, AH Dunn, D Alexander, NE Wabby, A Lyons, BN Doyle, R Walshe, J Attia, MF Blankson, I TI Design and development of a high-performance passive millimeter-wave imager for aeronautical applications SO OPTICAL ENGINEERING LA English DT Article DE passive millimeter-wave imaging; opto-mechanical scanning AB We describe a high performance optomechanically scanned millimeter-wave imager intended to monitor the ground movement of aircraft in adverse weather conditions. It employs two counter-rotating mirrors that are tilted about their axes of rotation. They simulate the linear scan of a single high speed, large aperture flapping mirror, When used with a linear receiver array, they can produce a 2-D scan of the scene at TV rates. In the present application, they were used with a single receiver and a large flapping mirror to produce a 2-D scan of the scene +/- 10 deg vertically and 60 deg horizontally. One of the rotating mirrors has a concave surface and acts as the focusing element in the imager. The two mirrors are driven from a single servo motor using timing belts and toothed pulleys. The flapping mirror is slaved to the motion of the rotating disks using an electronic cam, The single channel 94-GHz receiver consisted of an InP LNA followed by a down converter and a detector. The video output passes to an A/D converter and is displayed on a conventional PC. This system has virtually 100% transmission and can be used at any waveband. (c) 2005 Society of Photo-Optical Instrumentation Engineers. C1 Univ Reading, Dept Phys, Reading RG6 6AF, Berks, England. Farran Technol Ltd, Cork, Ireland. Johnson C Smith Univ, Charlotte, NC 28216 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Lettington, AH (reprint author), Univ Reading, Dept Phys, Reading RG6 6AF, Berks, England. EM alan@lettington.org.uk NR 8 TC 9 Z9 9 U1 1 U2 2 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 SEP PY 2005 VL 44 IS 9 AR 093202 DI 10.1117/1.2050447 PG 6 WC Optics SC Optics GA 981NG UT WOS:000233094700009 ER PT J AU Astafieva, MM Rozanov, AY Hoover, R AF Astafieva, MM Rozanov, AY Hoover, R TI Framboids: Their structure and origin SO PALEONTOLOGICAL JOURNAL LA English DT Article DE framboid; pyritohedron; pentagonal dodecahedron; octahedron; pyrite; sulfate-reducing bacteria ID PYRITE FORMATION; MARINE-SEDIMENTS; SULFUR; MECHANISM; SULFIDE AB Framboidal structures are common both in terrestrial rocks and in meteorites (carbonate chondrites). The paper discusses the main origins of these structures. The role of biogenic factors in the formation of framboids is evaluated. Crystallites composing natural framboids are compared with those obtained under laboratory conditions. It is proposed that pyritohedral and icosahedral crystal forms are typical of biogenic framboids. C1 Russian Acad Sci, Inst Paleontol, Moscow 117997, Russia. George C Marshall Space Flight Ctr, Space Sci Lab, Huntsville, AL USA. RP Astafieva, MM (reprint author), Russian Acad Sci, Inst Paleontol, Profsoyuznaya 123, Moscow 117997, Russia. EM astafieva@paleo.ru NR 30 TC 9 Z9 9 U1 5 U2 17 PU INTERPERIODICA PI BIRMINGHAM PA PO BOX 1831, BIRMINGHAM, AL 35201-1831 USA SN 0031-0301 J9 PALEONTOL J+ JI Paleontol. J. PD SEP-OCT PY 2005 VL 39 IS 5 BP 457 EP 464 PG 8 WC Paleontology SC Paleontology GA 971EL UT WOS:000232364200001 ER PT J AU Middleton, EM Kim, MS Krizek, DT Bajwa, RKS AF Middleton, EM Kim, MS Krizek, DT Bajwa, RKS TI Evaluating UV-B effects and EDU protection in soybean leaves using fluorescence SO PHOTOCHEMISTRY AND PHOTOBIOLOGY LA English DT Article ID LASER-INDUCED FLUORESCENCE; IN-FIELD CORN; CHLOROPHYLL-FLUORESCENCE; IMAGING-SYSTEM; PHASEOLUS-VULGARIS; BLUE FLUORESCENCE; PISUM-SATIVUM; PLANT STRESS; GREEN PLANTS; GROWTH AB A growth-chamber experiment was conducted to evaluate whether ethylenenediurea (EDU), a chemical shown to be protective against ozone pollution, could ameliorate foliar damage induced by ultraviolet-B (UV-B) radiation exposure in 'Roanoke' soybean (Glycine max L.), a UV-B-sensitive cultivar, and whether these effects could be discriminated using fluorescence (F) observations. The experiment had four treatment groups: control; biologically effective UV-B (18 kJ m(-2) day(-1)); EDU (500 mu mol mol(-1)); and both UV-B and EDU (UV/EDU). Measurements included photosynthetic pigments, F image system (FIS) images of adaxial surfaces in four spectral regions (blue, green, red and far-red) and F emission spectra of the pigment extracts produced at two excitation wavelengths, 280 nm (280EX) and 380 nm (380EX). Several F ratios from 280EX, 380EX and the FIS images successfully separated the low UV vs high EDU group responses based on means alone, with intermediate values for controls and the combined UV/ EDU groups. A UV-B/blue emission ratio, F315/F420 (280EX), was correlated with chlorophyll content (mu g cm(-2))(R = 0.88, P < 0.001), as was a ratio of emissions at two UV-A wavelengths: F330/F385 (280EX) (R = 0.87). These two 280EX ratios were also linearly correlated with emission ratios produced by 380EX, such as the far-red/green ratio, F730/F525 (380EX) (R = 0.92, P < 0.001), and clearly distinguished the UV-B and EDU groups separately, and which bracketed the similar intermediate responses of the UV/EDU and control groups. The FIS images additionally captured the following anatomical spatial patterns across the leaf surfaces: (1) emissions of UV-B-irradiated leaves were more uniform but lower in intensity than those of other groups; and (2) emissions of EDU-treated leaves exhibited the greatest variation in spatial patterns because veins had elevated blue F and leaf edges had enhanced red and far-red F. This experiment supports the hypothesis that EDU substantially ameliorated UV-B damage to foliage, a result that relied on the combined use of FIS images and emission spectra. C1 NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. USDA ARS, Instrumentat & Sensing Lab, Beltsville, MD USA. USDA ARS, Sustainable Agr Syst Lab, Beltsville, MD USA. Bergen Cty Acad, Dept Biol, Hackensack, NJ USA. RP Middleton, EM (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Code 661, Greenbelt, MD 20771 USA. EM Elizabeth.M.Middleton@nasa.gov NR 52 TC 4 Z9 4 U1 1 U2 10 PU AMER SOC PHOTOBIOLOGY PI AUGUSTA PA BIOTECH PARK, 1021 15TH ST, SUITE 9, AUGUSTA, GA 30901-3158 USA SN 0031-8655 J9 PHOTOCHEM PHOTOBIOL JI Photochem. Photobiol. PD SEP-OCT PY 2005 VL 81 IS 5 BP 1075 EP 1085 DI 10.1562/2005-04-25-RA-498 PG 11 WC Biochemistry & Molecular Biology; Biophysics SC Biochemistry & Molecular Biology; Biophysics GA 975CS UT WOS:000232639200008 PM 16022558 ER PT J AU Florescu, M Lee, H Stimpson, AJ Dowling, J AF Florescu, M Lee, H Stimpson, AJ Dowling, J TI Thermal emission and absorption of radiation in finite inverted-opal photonic crystals SO PHYSICAL REVIEW A LA English DT Article ID BAND-GAP; ATOMS; TRANSMISSION; SYSTEMS; LASER; EDGE AB We study theoretically the optical properties of a finite inverted-opal photonic crystal. The light-matter interaction is strongly affected by the presence of the three-dimensional photonic crystal and the alterations of the light emission and absorption processes can be used to suppress or enhance the thermal emissivity and absorptivity of the dielectric structure. We investigate the influence of the absorption present in the system on the relevant band edge frequencies that control the optical response of the photonic crystal. Our study reveals that the absorption processes cause spectral broadening and shifting of the band edge optical resonances, and determine a strong reduction of the photonic band gap spectral range. Using the angular and spectral dependence of the band edge frequencies for stop bands along different directions, we argue that by matching the blackbody emission spectrum peak with a prescribed maximum of the absorption coefficient, it is possible to achieve an angle-sensitive enhancement of the thermal emission/absorption of radiation. This result opens a way to realize a frequency-sensitive and angle-sensitive photonic crystal absorbers/emitters. C1 CALTECH, Jet Prop Lab, Quantum Comp Technol Grp, Pasadena, CA 91109 USA. Louisiana State Univ, Hearne Inst Theoret Phys, Dept Phys & Astron, Baton Rouge, LA 70803 USA. Texas A&M Univ, Inst Quantum Studies, Dept Phys, College Stn, TX 77843 USA. RP Florescu, M (reprint author), CALTECH, Jet Prop Lab, Quantum Comp Technol Grp, MS 126-347,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM marian.florescu@jpl.nasa.gov RI Florescu, Marian/E-9009-2010; DOWLING, JONATHAN/L-2749-2013 NR 43 TC 25 Z9 25 U1 2 U2 10 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD SEP PY 2005 VL 72 IS 3 AR 033821 DI 10.1103/PhysRevA.72.033821 PG 9 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 969IR UT WOS:000232228300171 ER PT J AU Bachlechner, ME Zhang, J Wang, Y Schiffbauer, J Knudsen, SR Korakakis, D AF Bachlechner, ME Zhang, J Wang, Y Schiffbauer, J Knudsen, SR Korakakis, D TI Molecular dynamics simulations of the mechanical strength of Si/Si3N4 interfaces SO PHYSICAL REVIEW B LA English DT Article ID SILICON-NITRIDE; PARALLEL COMPUTERS; SI(111)/SI3N4(001) INTERFACE; DISLOCATION EMISSION; ELECTRONIC-STRUCTURE; CHARGE-TRANSFER; STRAIN-RATE; THIN-FILMS; FRACTURE; TEMPERATURE AB Molecular dynamics simulations are performed on parallel computers to investigate the crystalline Si(111)/Si3N4(0001) interface that is modeled as an eight-component system. The average total energy per particle and the average kinetic energy per particle of the subsystems are monitored during the preparation of the system. The Young's modulus of the interface is compared with that of the silicon part alone and that of the silicon-nitride film, respectively. The results for one extended simulation feature a crack in the silicon-nitride film and dislocated atoms in silicon below the crack. Simulations at rates of strain ranging from 0.00125 to 0.05 ps(-1) show that for lower strain rates, the systems stretched faster reach their ultimate strength at a higher strain value than those that were stretched more slowly. At the highest strain rates, however, the failure mechanisms change qualitatively indicative of a more ductile behavior. C1 W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. Morgantown High Sch, NASA, Independent Verificat & Validat Facil, Sci & Engn Apprenticeship Program, Morgantown, WV 26501 USA. Inst Sci Res Inc, Fairmont, WV 26555 USA. W Virginia Univ, Lane Dept Comp Sci & Elect Engn, Morgantown, WV 26506 USA. RP Bachlechner, ME (reprint author), W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. EM Martina.Bachlechner@mail.wvu.edu NR 54 TC 10 Z9 10 U1 0 U2 8 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 J9 PHYS REV B JI Phys. Rev. B PD SEP PY 2005 VL 72 IS 9 AR 094115 DI 10.1103/PhysRevB.72.094115 PG 10 WC Physics, Condensed Matter SC Physics GA 969IT UT WOS:000232228500044 ER PT J AU Maslov, AV Ning, CZ AF Maslov, AV Ning, CZ TI Band structure and optical absorption of GaN nanowires grown along the c axis SO PHYSICAL REVIEW B LA English DT Article ID QUANTUM-WELL LASERS; PARAMETERS; WIRES; ALN; SEMICONDUCTORS; GAIN AB We study the optical properties of wurtzite GaN nanowires in which the geometrical axis coincides with the c axis of the crystal. The band mixing is typically very strong for the valence subbands and this results in rather complicated behaviors of the dispersion curves. However, in a very thin nanowire, the top valence subband is found to contain mostly parallel to z > components near the zone center; this is in contrast to bulk GaN where the top state has parallel to x > and parallel to y > components only. A particularly interesting feature of bandmixing is that the nearest-to-band-edge valence state can be either optically dark or bright, depending on the radius of the nanowire. We show that near the band edge, the optical absorption is greater when the optical field is polarized along the wire and this polarization anisotropy becomes stronger as the radius decreases; above the band edge, the transverse component of absorption may dominate. This absorption dependence is again in contrast to that in bulk GaN where the band edge absorption is much greater for the optical polarization perpendicular to the c axis. The absorption properties are also directly relevant for the polarization of luminescence and laser emission in GaN nanowires. C1 NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Maslov, AV (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, Mail Stop 229-1, Moffett Field, CA 94035 USA. RI Maslov, Alexey/E-5158-2011; Ning, C. Z./D-4699-2009 OI Maslov, Alexey/0000-0002-7835-2474; Ning, C. Z./0000-0003-4583-8889 NR 20 TC 23 Z9 23 U1 0 U2 8 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 J9 PHYS REV B JI Phys. Rev. B PD SEP PY 2005 VL 72 IS 12 AR 125319 DI 10.1103/PhysRevB.72.125319 PG 7 WC Physics, Condensed Matter SC Physics GA 969JC UT WOS:000232229400085 ER PT J AU Osipov, VV Bratkovsky, AM AF Osipov, VV Bratkovsky, AM TI Spin accumulation in degenerate semiconductors near modified Schottky contact with ferromagnets: Spin injection and extraction SO PHYSICAL REVIEW B LA English DT Article ID LIGHT-EMITTING DIODE; GIANT MAGNETORESISTANCE; QUANTUM COMPUTATION; ROOM-TEMPERATURE; TRANSPORT; POLARIZATION; SPINTRONICS; JUNCTIONS; BARRIER; METAL AB We study spin transport in forward and reverse biased junctions between a ferromagnetic metal and a degenerate semiconductor with a delta-doped layer near the interface at relatively low temperatures. We show that spin polarization of electrons in the semiconductor, P-n, near the interface increases both with the forward and reverse current and reaches saturation at certain relatively large current while the spin injection coefficient, Gamma, increases with reverse current and decreases with the forward current. We analyze the condition for efficient spin polarization of electrons in degenerate semiconductor near interface with ferromagnet. We compare the accumulation of spin polarized electrons in degenerate semiconductors at low temperatures with that in nondegenerate semiconductors at relatively high, room temperatures. C1 Hewlett Packard Labs, Palo Alto, CA 94304 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Hewlett Packard Labs, 1501 Page Mill Rd,1L, Palo Alto, CA 94304 USA. NR 75 TC 18 Z9 18 U1 1 U2 7 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9950 EI 2469-9969 J9 PHYS REV B JI Phys. Rev. B PD SEP PY 2005 VL 72 IS 11 AR 115322 DI 10.1103/PhysRevB.72.115322 PG 9 WC Physics, Condensed Matter SC Physics GA 969IZ UT WOS:000232229100103 ER PT J AU Osman, MA Srivastava, D AF Osman, MA Srivastava, D TI Molecular dynamics simulation of heat pulse propagation in single-wall carbon nanotubes SO PHYSICAL REVIEW B LA English DT Article ID THERMAL-CONDUCTIVITY; SECOND SOUND; DIAMOND; FILMS; NAF AB The propagation of heat pulses in single-wall carbon nanotubes has been investigated using molecular dynamics simulations. It is found that heat pulses of picosecond duration in (10,0), (7,0), and (5,5) single-wall carbon nanotubes induce several wave packets that propagate at different propagation speeds. The leading wave packets move at the speed of sound corresponding to that of longitudinal acoustic (LA) phonons, followed by wave packets with speeds corresponding to twisted phonon mode (TW), second sound wave, and diffusive components. The waves corresponding to ballistic LA and TW phonon modes in (10,0) and (7,0) zig-zag nanotubes carry more heat energy than in (5,5) armchair nanotubes. The energy carried by wave packets corresponding to the speed of second sound waves is larger than those carried by TW and LA modes. These are used to explain the higher thermal conductivity of zig-zag nanotubes as compared to armchair nanotubes reported recently. C1 Washington State Univ, Sch Elect Engn & Comp Sci, Pullman, WA 99164 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. UARC UCSC, Moffett Field, CA 94035 USA. RP Washington State Univ, Sch Elect Engn & Comp Sci, Pullman, WA 99164 USA. NR 25 TC 29 Z9 32 U1 1 U2 6 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9950 EI 2469-9969 J9 PHYS REV B JI Phys. Rev. B PD SEP PY 2005 VL 72 IS 12 AR 125413 DI 10.1103/PhysRevB.72.125413 PG 7 WC Physics, Condensed Matter SC Physics GA 969JC UT WOS:000232229400130 ER PT J AU Abbott, B Abbott, R Adhikari, R Ageev, A Agresti, J Allen, B Allen, J Amin, R Anderson, SB Anderson, WG Araya, M Armandula, H Ashley, M Asiri, F Aufmuth, P Aulbert, C Babak, S Balasubramanian, R Ballmer, S Barish, BC Barker, C Barker, D Barnes, M Barr, B Barton, MA Bayer, K Beausoleil, R Belczynski, K Bennett, R Berukoff, SJ Betzwieser, J Bhawal, B Bilenko, IA Billingsley, G Black, E Blackburn, K Blackburn, L Bland, B Bochner, B Bogue, L Bork, R Bose, S Brady, PR Braginsky, VB Brau, JE Brown, DA Bullington, A Bunkowski, A Buonanno, A Burgess, R Busby, D Butler, WE Byer, RL Cadonati, L Cagnoli, G Camp, JB Cannizzo, J Cannon, K Cantley, CA Cardenas, L Carter, K Casey, MM Castiglione, J Chandler, A Chapsky, J Charlton, P Chatterji, S Chelkowski, S Chen, Y Chickarmane, V Chin, D Christensen, N Churches, D Cokelaer, T Colacino, C Coldwell, R Coles, M Cook, D Corbitt, T Coyne, D Creighton, JDE Creighton, TD Crooks, DRM Csatorday, P Cusack, BJ Cutler, C Dalrymple, J D'Ambrosio, E Danzmann, K Davies, G Daw, E DeBra, D Delker, T Dergachev, V Desai, S DeSalvo, R Dhurandhar, S Di Credico, A Diaz, M Ding, H Drever, RWP Dupuis, RJ Edlund, JA Ehrens, P Elliffe, EJ Etzel, T Evans, M Evans, T Fairhurst, S Fallnich, C Farnham, D Fejer, MM Findley, T Fine, M Finn, LS Franzen, KY Freise, A Frey, R Fritschel, P Frolov, VV Fyffe, M Ganezer, KS Garofoli, J Giaime, JA Gillespie, A Goda, K Goggin, L Gonzalez, G Gossler, S Grandclement, P Grant, A Gray, C Gretarsson, AM Grimmett, D Grote, H Grunewald, S Guenther, M Gustafson, E Gustafson, R Hamilton, WO Hammond, M Hanson, J Hardham, C Harms, J Harry, G Hartunian, A Heefner, J Hefetz, Y Heinzel, G Heng, IS Hennessy, M Hepler, N Heptonstall, A Heurs, M Hewitson, M Hild, S Hindman, N Hoang, P Hough, J Hrynevych, M Hua, W Ito, M Itoh, Y Ivanov, A Jennrich, O Johnson, B Johnson, WW Johnston, WR Jones, DI Jones, G Jones, L Jungwirth, D Kalogera, V Katsavounidis, E Kawabe, K Kawamura, S Kells, W Kern, J Khan, A Killbourn, S Killow, CJ Kim, C King, C King, P Klimenko, S Koranda, S Kotter, K Kovalik, J Kozak, D Krishnan, B Landry, M Langdale, J Lantz, B Lawrence, R Lazzarini, A Lei, M Leonor, I Libbrecht, K Libson, A Lindquist, P Liu, S Logan, J Lormand, M Lubinski, M Luck, H Luna, M Lyons, TT Machenschalk, B MacInnis, M Mageswaran, M Mailand, K Majid, W Malec, M Mandic, V Mann, F Marin, A Marka, S Maros, E Mason, J Mason, K Matherny, O Matone, L Mavalvala, N McCarthy, R McClelland, DE McHugh, M Melissinos, A Mendell, G Mercer, RA Meshkov, S Messaritaki, E Messenger, C Mikhailov, E Mitra, S Mitrofanov, VP Mitselmakher, G Mittleman, R Miyakawa, O Miyoki, S Mohanty, S Moreno, G Mossavi, K Mueller, G Mukherjee, S Murray, P Myers, E Myers, J Nagano, S Nash, T Nayak, R Newton, G Nocera, F Noel, JS Nutzman, P Olson, T O'Reilly, B Ottaway, DJ Ottewill, A Ouimette, D Overmier, H Owen, BJ Pan, Y Papa, MA Parameshwaraiah, V Ajith, P Parameswariah, C Pedraza, M Penn, S Pitkin, M Plissi, M Prix, R Quetschke, V Raab, F Radkins, H Rahkola, R Rakhmanov, M Rao, SR Rawlins, K Ray-Majumder, S Re, V Redding, D Regehr, MW Regimbau, T Reid, S Reilly, KT Reithmaier, K Reitze, DH Richman, S Riesen, R Riles, K Rivera, B Rizzi, A Robertson, DI Robertson, NA Robinson, C Robison, L Roddy, S Rodriguez, A Rollins, J Romano, JD Romie, J Rong, H Rose, D Rotthoff, E Rowan, S Rudiger, A Ruet, L Russell, P Ryan, K Salzman, I Sandberg, V Sanders, GH Sannibale, V Sarin, P Sathyaprakash, B Saulson, PR Savage, R Sazonov, A Schilling, R Schlaufman, K Schmidt, V Schnabel, R Schofield, R Schutz, BF Schwinberg, P Scott, SM Seader, SE Searle, AC Sears, B Seel, S Seifert, F Sellers, D Sengupta, AS Shapiro, CA Shawhan, P Shoemaker, DH Shu, QZ Sibley, A Siemens, X Sievers, L Sigg, D Sintes, AM Smith, JR Smith, M Smith, MR Sneddon, PH Spero, R Spjeld, O Stapfer, G Steussy, D Strain, KA Strom, D Stuver, A Summerscales, T Sumner, MC Sung, M Sutton, PJ Sylvestre, J Takamori, A Tanner, DB Tariq, H Taylor, I Taylor, R Taylor, R Thorne, KA Thorne, KS Tibbits, M Tilav, S Tinto, M Tokmakov, KV Torres, C Torrie, C Traylor, G Tyler, W Ugolini, D Ungarelli, C Vallisneri, M van Putten, M Vass, S Vecchio, A Veitch, J Vorvick, C Vyachanin, SP Wallace, L Walther, H Ward, H Ward, R Ware, B Watts, K Webber, D Weidner, A Weiland, U Weinstein, A Weiss, R Welling, H Wen, L Wen, S Wette, K Whelan, JT Whitcomb, SE Whiting, BF Wiley, S Wilkinson, C Willems, PA Williams, PR Williams, R Willke, B Wilson, A Winjum, BJ Winkler, W Wise, S Wiseman, AG Woan, G Woods, D Wooley, R Worden, J Wu, W Yakushin, I Yamamoto, H Yoshida, S Zaleski, KD Zanolin, M Zawischa, I Zhang, L Zhu, R Zotov, N Zucker, M Zweizig, J AF Abbott, B Abbott, R Adhikari, R Ageev, A Agresti, J Allen, B Allen, J Amin, R Anderson, SB Anderson, WG Araya, M Armandula, H Ashley, M Asiri, F Aufmuth, P Aulbert, C Babak, S Balasubramanian, R Ballmer, S Barish, BC Barker, C Barker, D Barnes, M Barr, B Barton, MA Bayer, K Beausoleil, R Belczynski, K Bennett, R Berukoff, SJ Betzwieser, J Bhawal, B Bilenko, IA Billingsley, G Black, E Blackburn, K Blackburn, L Bland, B Bochner, B Bogue, L Bork, R Bose, S Brady, PR Braginsky, VB Brau, JE Brown, DA Bullington, A Bunkowski, A Buonanno, A Burgess, R Busby, D Butler, WE Byer, RL Cadonati, L Cagnoli, G Camp, JB Cannizzo, J Cannon, K Cantley, CA Cardenas, L Carter, K Casey, MM Castiglione, J Chandler, A Chapsky, J Charlton, P Chatterji, S Chelkowski, S Chen, Y Chickarmane, V Chin, D Christensen, N Churches, D Cokelaer, T Colacino, C Coldwell, R Coles, M Cook, D Corbitt, T Coyne, D Creighton, JDE Creighton, TD Crooks, DRM Csatorday, P Cusack, BJ Cutler, C Dalrymple, J D'Ambrosio, E Danzmann, K Davies, G Daw, E DeBra, D Delker, T Dergachev, V Desai, S DeSalvo, R Dhurandhar, S Di Credico, A Diaz, M Ding, H Drever, RWP Dupuis, RJ Edlund, JA Ehrens, P Elliffe, EJ Etzel, T Evans, M Evans, T Fairhurst, S Fallnich, C Farnham, D Fejer, MM Findley, T Fine, M Finn, LS Franzen, KY Freise, A Frey, R Fritschel, P Frolov, VV Fyffe, M Ganezer, KS Garofoli, J Giaime, JA Gillespie, A Goda, K Goggin, L Gonzalez, G Gossler, S Grandclement, P Grant, A Gray, C Gretarsson, AM Grimmett, D Grote, H Grunewald, S Guenther, M Gustafson, E Gustafson, R Hamilton, WO Hammond, M Hanson, J Hardham, C Harms, J Harry, G Hartunian, A Heefner, J Hefetz, Y Heinzel, G Heng, IS Hennessy, M Hepler, N Heptonstall, A Heurs, M Hewitson, M Hild, S Hindman, N Hoang, P Hough, J Hrynevych, M Hua, W Ito, M Itoh, Y Ivanov, A Jennrich, O Johnson, B Johnson, WW Johnston, WR Jones, DI Jones, G Jones, L Jungwirth, D Kalogera, V Katsavounidis, E Kawabe, K Kawamura, S Kells, W Kern, J Khan, A Killbourn, S Killow, CJ Kim, C King, C King, P Klimenko, S Koranda, S Kotter, K Kovalik, J Kozak, D Krishnan, B Landry, M Langdale, J Lantz, B Lawrence, R Lazzarini, A Lei, M Leonor, I Libbrecht, K Libson, A Lindquist, P Liu, S Logan, J Lormand, M Lubinski, M Luck, H Luna, M Lyons, TT Machenschalk, B MacInnis, M Mageswaran, M Mailand, K Majid, W Malec, M Mandic, V Mann, F Marin, A Marka, S Maros, E Mason, J Mason, K Matherny, O Matone, L Mavalvala, N McCarthy, R McClelland, DE McHugh, M Melissinos, A Mendell, G Mercer, RA Meshkov, S Messaritaki, E Messenger, C Mikhailov, E Mitra, S Mitrofanov, VP Mitselmakher, G Mittleman, R Miyakawa, O Miyoki, S Mohanty, S Moreno, G Mossavi, K Mueller, G Mukherjee, S Murray, P Myers, E Myers, J Nagano, S Nash, T Nayak, R Newton, G Nocera, F Noel, JS Nutzman, P Olson, T O'Reilly, B Ottaway, DJ Ottewill, A Ouimette, D Overmier, H Owen, BJ Pan, Y Papa, MA Parameshwaraiah, V Ajith, P Parameswariah, C Pedraza, M Penn, S Pitkin, M Plissi, M Prix, R Quetschke, V Raab, F Radkins, H Rahkola, R Rakhmanov, M Rao, SR Rawlins, K Ray-Majumder, S Re, V Redding, D Regehr, MW Regimbau, T Reid, S Reilly, KT Reithmaier, K Reitze, DH Richman, S Riesen, R Riles, K Rivera, B Rizzi, A Robertson, DI Robertson, NA Robinson, C Robison, L Roddy, S Rodriguez, A Rollins, J Romano, JD Romie, J Rong, H Rose, D Rotthoff, E Rowan, S Rudiger, A Ruet, L Russell, P Ryan, K Salzman, I Sandberg, V Sanders, GH Sannibale, V Sarin, P Sathyaprakash, B Saulson, PR Savage, R Sazonov, A Schilling, R Schlaufman, K Schmidt, V Schnabel, R Schofield, R Schutz, BF Schwinberg, P Scott, SM Seader, SE Searle, AC Sears, B Seel, S Seifert, F Sellers, D Sengupta, AS Shapiro, CA Shawhan, P Shoemaker, DH Shu, QZ Sibley, A Siemens, X Sievers, L Sigg, D Sintes, AM Smith, JR Smith, M Smith, MR Sneddon, PH Spero, R Spjeld, O Stapfer, G Steussy, D Strain, KA Strom, D Stuver, A Summerscales, T Sumner, MC Sung, M Sutton, PJ Sylvestre, J Takamori, A Tanner, DB Tariq, H Taylor, I Taylor, R Taylor, R Thorne, KA Thorne, KS Tibbits, M Tilav, S Tinto, M Tokmakov, KV Torres, C Torrie, C Traylor, G Tyler, W Ugolini, D Ungarelli, C Vallisneri, M van Putten, M Vass, S Vecchio, A Veitch, J Vorvick, C Vyachanin, SP Wallace, L Walther, H Ward, H Ward, R Ware, B Watts, K Webber, D Weidner, A Weiland, U Weinstein, A Weiss, R Welling, H Wen, L Wen, S Wette, K Whelan, JT Whitcomb, SE Whiting, BF Wiley, S Wilkinson, C Willems, PA Williams, PR Williams, R Willke, B Wilson, A Winjum, BJ Winkler, W Wise, S Wiseman, AG Woan, G Woods, D Wooley, R Worden, J Wu, W Yakushin, I Yamamoto, H Yoshida, S Zaleski, KD Zanolin, M Zawischa, I Zhang, L Zhu, R Zotov, N Zucker, M Zweizig, J CA LIGO Sci Collaboration TI Upper limits on gravitational wave bursts in LIGO's second science run SO PHYSICAL REVIEW D LA English DT Article ID ROTATIONAL CORE COLLAPSE; DETECTORS; PERFORMANCE; ALGORITHM; SIGNAL AB We perform a search for gravitational wave bursts using data from the second science run of the LIGO detectors, using a method based on a wavelet time-frequency decomposition. This search is sensitive to bursts of duration much less than a second and with frequency content in the 100-1100 Hz range. It features significant improvements in the instrument sensitivity and in the analysis pipeline with respect to the burst search previously reported by LIGO. Improvements in the search method allow exploring weaker signals, relative to the detector noise floor, while maintaining a low false alarm rate, O(0.1) mu Hz. The sensitivity in terms of the root-sum-square (rss) strain amplitude lies in the range of h(rss)similar to 10(-20)-10(-19) Hz(-1/2). No gravitational wave signals were detected in 9.98 days of analyzed data. We interpret the search result in terms of a frequentist upper limit on the rate of detectable gravitational wave bursts at the level of 0.26 events per day at 90% confidence level. We combine this limit with measurements of the detection efficiency for selected waveform morphologies in order to yield rate versus strength exclusion curves as well as to establish order-of-magnitude distance sensitivity to certain modeled astrophysical sources. Both the rate upper limit and its applicability to signal strengths improve our previously reported limits and reflect the most sensitive broad-band search for untriggered and unmodeled gravitational wave bursts to date. C1 CALTECH, LIGO, Pasadena, CA 91125 USA. Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany. Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany. Australian Natl Univ, Canberra, ACT 0200, Australia. Calif State Univ Dominguez Hills, Carson, CA 90747 USA. CALTECH, CaRT, Pasadena, CA 91125 USA. Cardiff Univ, Cardiff CF2 3YB, Wales. Carleton Coll, Northfield, MN 55057 USA. Columbia Univ, New York, NY 10027 USA. Hobart & William Smith Coll, Geneva, NY 14456 USA. Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. MIT, LIGO, Cambridge, MA 02139 USA. LIGO Hanford Observ, Richland, WA 99352 USA. LIGO Livingston Observ, Livingston, LA 70754 USA. Louisiana State Univ, Baton Rouge, LA 70803 USA. Louisiana Tech Univ, Ruston, LA 71272 USA. Loyola Univ, New Orleans, LA 70118 USA. Max Planck Inst Quantum Opt, D-85748 Garching, Germany. Moscow MV Lomonosov State Univ, Moscow 119992, Russia. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Natl Astron Observ Japan, Tokyo 1818588, Japan. Northwestern Univ, Evanston, IL 60208 USA. Salish Kootenai Coll, Pablo, MT 59855 USA. SE Louisiana Univ, Hammond, LA 70402 USA. Stanford Univ, Stanford, CA 94305 USA. Syracuse Univ, Syracuse, NY 13244 USA. Penn State Univ, University Pk, PA 16802 USA. Univ Texas, Brownsville, TX 78520 USA. Texas Southmost Coll, Brownsville, TX 78520 USA. Trinity Univ, San Antonio, TX 78212 USA. Leibniz Univ Hannover, D-30167 Hannover, Germany. Univ Illes Balears, E-07122 Palma de Mallorca, Spain. Univ Birmingham, Birmingham B15 2TT, W Midlands, England. Univ Florida, Gainesville, FL 32611 USA. Univ Glasgow, Glasgow G12 8QQ, Lanark, Scotland. Univ Michigan, Ann Arbor, MI 48109 USA. Univ Oregon, Eugene, OR 97403 USA. Univ Rochester, Rochester, NY 14627 USA. Univ Wisconsin, Milwaukee, WI 53201 USA. Vassar Coll, Poughkeepsie, NY 12604 USA. Washington State Univ, Pullman, WA 99164 USA. HP Labs, Palo Alto, CA USA. CNRS, Inst Astrophys Paris, GReCO, F-75700 Paris, France. Univ Tokyo, Inst Cosm Ray Res, Tokyo, Japan. Univ Coll Dublin, Dublin 2, Ireland. IBM Canada Ltd, Toronto, ON, Canada. Jet Prop Lab, Pasadena, CA USA. RP Abbott, B (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA. RI Harms, Jan/J-4359-2012; Frey, Raymond/E-2830-2016; Pitkin, Matthew/I-3802-2013; Vyatchanin, Sergey/J-2238-2012; Chen, Yanbei/A-2604-2013; Barker, David/A-5671-2013; Liu, Sheng/K-2815-2013; Hild, Stefan/A-3864-2010; Vecchio, Alberto/F-8310-2015; Agresti, Juri/G-8168-2012; Ottaway, David/J-5908-2015; Ottewill, Adrian/A-1838-2016; Messaritaki, Eirini/D-7393-2016; Sigg, Daniel/I-4308-2015; Casey, Morag/C-9703-2010; Raab, Frederick/E-2222-2011; Rowan, Sheila/E-3032-2010; Beausoleil, Raymond/C-5076-2009; McClelland, David/E-6765-2010; Kawabe, Keita/G-9840-2011; Lueck, Harald/F-7100-2011; Strain, Kenneth/D-5236-2011; Bilenko, Igor/D-5172-2012; Freise, Andreas/F-8892-2011; Mitrofanov, Valery/D-8501-2012; Allen, Bruce/K-2327-2012; van Putten, Maurice/F-5237-2011; Schutz, Bernard/B-1504-2010; Sylvestre, Julien/A-8610-2009; Finn, Lee Samuel/A-3452-2009; OI Frey, Raymond/0000-0003-0341-2636; Fairhurst, Stephen/0000-0001-8480-1961; Taylor, Ian/0000-0001-5040-0772; Zweizig, John/0000-0002-1521-3397; Aulbert, Carsten/0000-0002-1481-8319; Tanner, David/0000-0003-1940-4710; Heurs, Michele/0000-0002-5577-2273; Messaritaki, Eirini/0000-0002-9917-4160; Pitkin, Matthew/0000-0003-4548-526X; Vecchio, Alberto/0000-0002-6254-1617; Agresti, Juri/0000-0001-6119-2470; Ottewill, Adrian/0000-0003-3293-8450; Sigg, Daniel/0000-0003-4606-6526; McClelland, David/0000-0001-6210-5842; Lueck, Harald/0000-0001-9350-4846; Strain, Kenneth/0000-0002-2066-5355; Allen, Bruce/0000-0003-4285-6256; Sylvestre, Julien/0000-0001-8136-4348; Finn, Lee Samuel/0000-0002-3937-0688; Freise, Andreas/0000-0001-6586-9901; Mitra, Sanjit/0000-0002-0800-4626; Tokmakov, Kirill/0000-0002-2808-6593; Whiting, Bernard F/0000-0002-8501-8669; Veitch, John/0000-0002-6508-0713; Papa, M.Alessandra/0000-0002-1007-5298 NR 45 TC 105 Z9 105 U1 2 U2 11 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 EI 1550-2368 J9 PHYS REV D JI Phys. Rev. D PD SEP PY 2005 VL 72 IS 6 AR 062001 DI 10.1103/PhysRevD.72.062001 PG 25 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 969JJ UT WOS:000232230100009 ER PT J AU Dubrulle, B Dauchot, O Daviaud, F Longaretti, PY Richard, D Zahn, JP AF Dubrulle, B Dauchot, O Daviaud, F Longaretti, PY Richard, D Zahn, JP TI Stability and turbulent transport in Taylor-Couette flow from analysis of experimental data SO PHYSICS OF FLUIDS LA English DT Article ID ROTATING CYLINDERS; ACCRETION DISKS; SHEAR-FLOW; HYDRODYNAMIC STABILITY; VISCOUS-FLOW; INSTABILITY; TRANSITION; BOUNDARY; FRICTION; GRADIENT AB This paper provides discussion and prescription about stability and transport in the Taylor-Couette experiment, a rotating shear flow with shear perpendicular to the rotation axis. Such geometry frequently occurs in geophysical or astrophysical context. The prescriptions we obtain are the result of a detailed analysis of the experimental data obtained in several studies of the transition to turbulence and turbulent transport in Taylor-Couette flow. We first introduce a new set of control parameters, based on dynamical rather than geometrical considerations, so that they may be relevant to any rotating shear flows in general and not only to Taylor-Couette flow. We then investigate the transition thresholds in the supercritical and the subcritical regime in order to extract their general dependencies on the control parameters. The inspection of the mean profiles provides us with some general hints on the turbulent to laminar shear ratio. Then the examination of the torque data allows us to propose a decomposition of the torque dependence on the control parameters in two terms, one completely determined by measurements in the case where the outer cylinder is at rest, the other one being a universal function deduced here from experimental fits. As a result, we obtain a general expression for the turbulent viscosity and compare it to existing prescriptions in the literature. Finally, throughout the paper we discuss the influence of additional effects such as stratification or magnetic fields. (c) 2005 American Institute of Physics. C1 CEA Saclay, CNRS, URA 2464, GIT,SPEC,DRECAM,DSM, F-91191 Gif Sur Yvette, France. Univ Grenoble 1, CNRS, LAOG, UMR 5571, F-38041 Grenoble, France. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Observ Paris, CNRS, LUTh, UMR 8102, F-92195 Meudon, France. RP Dubrulle, B (reprint author), CEA Saclay, CNRS, URA 2464, GIT,SPEC,DRECAM,DSM, F-91191 Gif Sur Yvette, France. RI Dauchot, Olivier/D-7156-2015 OI Dauchot, Olivier/0000-0002-7039-5787 NR 57 TC 73 Z9 73 U1 0 U2 20 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-6631 J9 PHYS FLUIDS JI Phys. Fluids PD SEP PY 2005 VL 17 IS 9 AR 095103 DI 10.1063/1.2008999 PG 19 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA 968LY UT WOS:000232165200037 ER PT J AU Pettit, DR AF Pettit, DR TI Waves in a large free sphere of water on the International Space Station SO PHYSICS OF FLUIDS LA English DT Article; Proceedings Paper CT 22nd Annual Gallery of Fluid Motion Meeting CY 2004 CL Seattle, WA C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Pettit, DR (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NR 0 TC 1 Z9 1 U1 0 U2 2 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-6631 J9 PHYS FLUIDS JI Phys. Fluids PD SEP PY 2005 VL 17 IS 9 AR 091109 DI 10.1063/1.1942522 PG 1 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA 968LY UT WOS:000232165200009 ER PT J AU Rubinstein, R Clark, TT AF Rubinstein, R Clark, TT TI Self-similar turbulence evolution and the dissipation rate transport equation SO PHYSICS OF FLUIDS LA English DT Article ID ENERGY-DISSIPATION; SHEAR TURBULENCE; MODEL AB The dissipation rate transport equation is analyzed in the setting of time- dependent isotropic turbulence driven by a statistically unsteady force. In the limit of slow spectral variation, the balance between vortex stretching and enstrophy destruction postulated by Tennekes and Lumley [A First Course in Turbulence (MIT Press, Cambridge, MA, 1972)] is verified and spectral closure is used to identify the O(Re-0) difference between them; however, no definite formulation of an epsilon-equation results. The epsilon equation is usually calibrated to predict self- similar unit flows such as decaying turbulence and homogeneous shear flow. The limitations of this approach are shown by constructing classes of self- similar states of forced isotropic turbulence. Any choice of constants in the epsilon equation yields a model that is consistent with some self- similar states, but not with all possible states: two- equation models of the standard form select a class of admissible self- similar states and rule out the others. (c) 2005 American Institute of Physics. C1 NASA, Langley Res Ctr, Computat Modeling & Simulat Branch, Hampton, VA 23681 USA. Northrop Grumman Informat Technol, Adv Technol Dv, Albuquerque, NM 87106 USA. RP Rubinstein, R (reprint author), NASA, Langley Res Ctr, Computat Modeling & Simulat Branch, Hampton, VA 23681 USA. NR 21 TC 10 Z9 10 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-6631 J9 PHYS FLUIDS JI Phys. Fluids PD SEP PY 2005 VL 17 IS 9 AR 095104 DI 10.1063/1.2046707 PG 9 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA 968LY UT WOS:000232165200038 ER PT J AU Sakimoto, PJ Rosendhal, JD AF Sakimoto, PJ Rosendhal, JD TI Obliterating myths about minority institutions SO PHYSICS TODAY LA English DT Article C1 Univ Notre Dame, Fac Phys, Notre Dame, IN 46556 USA. NASA, Heaquarters, Space Sci Educ Initiat, Washington, DC 20546 USA. NASA, Heaquarters, Publ Outreach Initiat, Washington, DC 20546 USA. NASA, Heaquarters, Divers Initiat, Washington, DC 20546 USA. RP Sakimoto, PJ (reprint author), Univ Notre Dame, Fac Phys, Notre Dame, IN 46556 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0031-9228 J9 PHYS TODAY JI Phys. Today PD SEP PY 2005 VL 58 IS 9 BP 49 EP 53 DI 10.1063/1.2117823 PG 5 WC Physics, Multidisciplinary SC Physics GA 962FU UT WOS:000231717200031 ER PT J AU Stolc, V Li, L Wang, XF Li, XY Su, N Tongprasit, W Han, B Xue, YB Li, JY Snyder, M Gerstein, M Wang, J Deng, XW AF Stolc, V Li, L Wang, XF Li, XY Su, N Tongprasit, W Han, B Xue, YB Li, JY Snyder, M Gerstein, M Wang, J Deng, XW TI A pilot study of transcription unit analysis in rice using oligonucleotide tiling-path microarray SO PLANT MOLECULAR BIOLOGY LA English DT Article DE gene model; genome annotation; genomics; maskless array synthesis; rice; tiling-path microarray ID COMPARATIVE GENETICS; DRAFT SEQUENCE; GENOME; EXPRESSION; PREDICTION; EVOLUTION; GENES; CHROMOSOME-1; GRASSES; SORGHUM AB As the international efforts to sequence the rice genome are completed, an immediate challenge and opportunity is to comprehensively and accurately define all transcription units in the rice genome. Here we describe a strategy of using high-density oligonucleotide tiling-path microarrays to map transcription of the japonica rice genome. In a pilot experiment to test this approach, one array representing the reverse strand of the last 11.2 Mb sequence of chromosome 10 was analyzed in detail based on a mathematical model developed in this study. Analysis of the array data detected 77% of the reference gene models in a mixture of four RNA populations. Moreover, significant transcriptional activities were found in many of the previously annotated intergenic regions. These preliminary results demonstrate the utility of genome tiling microarrays in evaluating annotated rice gene models and in identifying novel transcription units that will facilitate rice genome annotation. C1 Yale Univ, Dept Mol Cellular & Dev Biol, New Haven, CT 06520 USA. NASA, Ames Res Ctr, Genome Res Facil, Moffett Field, CA 94035 USA. Natl Inst Biol Sci, Beijing 102206, Peoples R China. Chinese Acad Sci, Beijing Inst Genom, Beijing 101300, Peoples R China. Peking Univ, Coll Life Sci, Peking Yale Joint Res Ctr Plant Mol Genet & Agrob, Beijing 100871, Peoples R China. Natl Ctr Crop Design China Bioway Biotech Grp Co, Beijing 100085, Peoples R China. NASA, Ames Res Ctr, Eloret Corp, Moffett Field, CA 94035 USA. Chinese Acad Sci, Shanghai Inst Biol Sci, Natl Ctr Gene Res, Shanghai 200233, Peoples R China. Chinese Acad Sci, Inst Genet & Dev Biol, Beijing 100101, Peoples R China. Yale Univ, Dept Mol Biophys & Biochem, New Haven, CT 06511 USA. RP Deng, XW (reprint author), Yale Univ, Dept Mol Cellular & Dev Biol, New Haven, CT 06520 USA. EM xingwang.deng@yale.edu RI Wang, Jun/C-8434-2016; Wang, Jun/B-9503-2016 OI Wang, Jun/0000-0002-8540-8931; Wang, Jun/0000-0002-2113-5874 NR 47 TC 12 Z9 14 U1 1 U2 8 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-4412 J9 PLANT MOL BIOL JI Plant Mol.Biol. PD SEP PY 2005 VL 59 IS 1 BP 137 EP 149 DI 10.1007/s11103-005-6164-5 PG 13 WC Biochemistry & Molecular Biology; Plant Sciences SC Biochemistry & Molecular Biology; Plant Sciences GA 973BN UT WOS:000232498000012 PM 16217608 ER PT J AU Grenfell, JL AF Grenfell, JL TI 'My dead' SO POETRY WALES LA English DT Poetry C1 NASA, Climate Change Programme, New York, NY USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SEREN BOOKS/POETRY WALES PI BRIDGEND PA ANDMAR HOUSE, BRIDGEND CF31 4LJ, M GLAM, WALES SN 0032-2202 J9 POETRY WALES JI Poetry Wales PD FAL PY 2005 VL 41 IS 2 BP 18 EP 18 PG 1 WC Poetry SC Literature GA 975QI UT WOS:000232676600022 ER PT J AU Shafter, AW Cannizzo, JK Waagen, EO AF Shafter, AW Cannizzo, JK Waagen, EO TI A recurrence time versus orbital period relation for the Z Camelopardalis stars SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID WEAKLY MAGNETIZED DISKS; LOCAL SHEAR INSTABILITY; LONG-TERM BEHAVIOR; X-RAY BINARIES; DWARF-NOVA; CATACLYSMIC VARIABLES; SS-CYGNI; CN ORIONIS; OUTBURSTS; STANDSTILL AB We examine AAVSO (American Association of Variable Star Observers) light curves of 16 Z Camelopardalis systems with measured orbital periods, with particular focus on intervals away from standstill. During these times, most of the systems display a sawtooth-like outburst behavior, with quiescent intervals comparable to the outburst durations. We report the discovery of a linear relation between the characteristic outburst period and orbital period for these systems, which is given by (P-out(days)) = 62.0(+/- 7.7)P-orb(days) + 2.41(+/- 1.87). C1 Univ Maryland Baltimore Cty, NASA Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA. Amer Assoc Variable Star Observers, Cambridge, MA 02138 USA. RP Cannizzo, JK (reprint author), Univ Maryland Baltimore Cty, NASA Goddard Space Flight Ctr, Explorat Universe Div, Code 661, Greenbelt, MD 20771 USA. EM shafter@proteus.sdsu.edu; cannizzo@milkyway.gsfc.nasa.gov; eowaagen@aavso.org NR 40 TC 4 Z9 4 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD SEP PY 2005 VL 117 IS 835 BP 931 EP 937 DI 10.1086/432784 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958LZ UT WOS:000231451100005 ER PT J AU Kirby, L Davidson, JA Dotson, JL Dowell, CD Hildebrand, RH AF Kirby, L Davidson, JA Dotson, JL Dowell, CD Hildebrand, RH TI Improved data reduction for far-infrared/submillimeter polarimetry SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID SUBMILLIMETER POLARIZATION; INFRARED POLARIMETRY; LINEAR-POLARIZATION; ARRAY POLARIMETRY; HERTZ; NOISE AB Fluctuations in atmospheric emission introduce noise and systematic errors into measurements of polarization at far- infrared and submillimeter wavelengths. We describe a new analysis method that corrects for the bias and reduces the errors caused by the fluctuations. The method exploits repeated observations of a source and is especially effective on faint sources for which the polarized flux is on the same order as the atmospheric fluctuations. C1 Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Chicago, Dept Phys, Chicago, IL 60637 USA. RP Kirby, L (reprint author), Univ Chicago, Enrico Fermi Inst, 5640 S Ellis Ave, Chicago, IL 60637 USA. EM lkirby@oddjob.uchicago.edu; jdavidson@sofia.usra.edu; dotson@mail.arc.nasa.gov; cdd@submm.caltech.edu; roger@oddjob.uchicago.edu NR 16 TC 9 Z9 9 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD SEP PY 2005 VL 117 IS 835 BP 991 EP 995 DI 10.1086/432783 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958LZ UT WOS:000231451100013 ER PT J AU Drouin, BJ Maiwald, FW Pearson, JC AF Drouin, BJ Maiwald, FW Pearson, JC TI Application of cascaded frequency multiplication to molecular spectroscopy SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article ID HIGH-RESOLUTION; SUBMILLIMETER; MILLIMETER; GHZ; SPECTRUM; HOCL; BAND; MULTIPLIERS; REGION; PHASE AB Laboratory molecular spectroscopy provides the basis for interpretation of atmospheric, planetary, and astrophysical data gathered by remote sensing. Laboratory studies of atomic and molecular signatures across the electromagnetic spectrum provide high-precision, quantitative data used to interpret the observed environment from remote measurements. Historically, the region of the spectrum above 500 GHz has been relatively unexplored due to atmospheric absorption and technical difficulties generating and detecting radiation. Laboratory spectroscopy at these frequencies has traditionally involved measurement of one or two absorption features and relied on fitting of models to the limited data. We report a new spectrometer built around a computer-controlled commercial synthesizer and millimeter-wave module driving a series of amplifiers followed by a series of wide-bandwidth frequency doublers and triplers. The spectrometer provides the ability to rapidly measure large pieces of frequency space with higher resolution, accuracy, and sensitivity than with Fourier transform infrared techniques. The approach is simple, modular, and requires no custom-built electronics or high voltage and facilitates the use of infrared data analysis techniques on complex submillimeter spectra. (c) 2005 American Institute of Physics. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Drouin, BJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM brian.j.drouin@jpl.nasa.gov NR 51 TC 92 Z9 92 U1 4 U2 21 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0034-6748 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD SEP PY 2005 VL 76 IS 9 AR 093113 DI 10.1063/1.2042687 PG 10 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 966PZ UT WOS:000232034400014 ER PT J AU Kharuk, VI Dvinskaya, ML Ranson, KJ AF Kharuk, VI Dvinskaya, ML Ranson, KJ TI The spatiotemporal pattern of fires in northern Taiga larch forests of central Siberia SO RUSSIAN JOURNAL OF ECOLOGY LA English DT Article DE larch forests; burned-out areas; fire periodicity; permafrost; climatic trends AB The periodicity of fires in larch forests of Evenkia and their relationship with landscape elements have been studied. Cross-sections with "burns" in them caused by past fires have been analyzed in 72 test plots; the fire chronology encompassed the period from the 15th to the 20th century. The between-fire intervals (BFIs) have been calculated by two methods: (1) on the basis of burns alone and (11) on the basis of burns and the start of growth of the new generation of larch after the earliest fire. The BFI depends on local orographic features; it is 86 +/- 11 (105 +/- 12), 61 +/- 8 (73 +/- 8), 139 +/- 17 (138 +/- 18), and 68 +/- 14 (70 +/- 13) years for northeastern slopes, southwestern slopes, bogs, and flatlands, respectively. The mean BFIs calculated by methods I and II are 82 +/- 7 and 95 +/- 7 years, respectively. The permafrost horizon rises at a mean rate of 0.3 cm per year after a forest fire. It has been shown that the number of fires regularly peaks at periods of 36 and 82 years. There is also a temporal trend in fire frequency: the mean BFI was approximately 100 years in the 19th century and 65 years in the 20th century. C1 Russian Acad Sci, Sukachev Inst Forest, Siberian Div, Krasnoyarsk 660036, Russia. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kharuk, VI (reprint author), Russian Acad Sci, Sukachev Inst Forest, Siberian Div, Krasnoyarsk 660036, Russia. RI Ranson, Kenneth/G-2446-2012 OI Ranson, Kenneth/0000-0003-3806-7270 NR 23 TC 16 Z9 16 U1 1 U2 6 PU MAIK NAUKA/INTERPERIODICA/SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013-1578 USA SN 1067-4136 J9 RUSS J ECOL+ JI Russ. J. Ecol. PD SEP-OCT PY 2005 VL 36 IS 5 BP 302 EP 311 DI 10.1007/s11184-005-0077-z PG 10 WC Ecology SC Environmental Sciences & Ecology GA 967LD UT WOS:000232091800002 ER PT J AU Woo, R AF Woo, R TI Relating white-light coronal images to magnetic fields and plasma flow SO SOLAR PHYSICS LA English DT Article ID SOLAR-WIND; INTERPLANETARY SPACE; EMISSION-LINE; STREAMERS; HOLE; POLARIZATION; EVOLUTION; ECLIPSE; SHEET; SUN AB The solar magnetic field is key to a detailed Understanding of the Sun's atmosphere and its transition to the solar wind. However, the lack of detailed magnetic field measurements everywhere except at the photosphere has made it challenging to determine its topology and to understand how it produces the observed plasma properties of the corona and solar wind. Recent progress based on the synthesis of diversified observations has shown that the corona is highly filamentary, that the coronal magnetic field is predominantly radial, and that the ability of closed fields to trap plasma at the base of the corona is a manifestation of how the solar field controls the solar wind. In this paper, we explain how these results are consistent with the relationship between density Structure of white-light images C and fields and flow. We point out that the 'shape' of the corona observed in white-light images is a Consequence of: the steel) fall-off in density with radial distance, Coupled with the inherent limitation in the sensitivity of the observing instrument. We discuss how the significant variation in radial density fall-off with latitude leads to a coronal shape that is more precisely revealed when a radial gradient filter is used, but Which also gives a false impression of the tracing of highly non-radial fields. Instead, the coronal field is predominantly radial, and the two magnetic features that influence the shape of the corona are the closed fields at the base of the corona, and the polarity reversal forming the heliospheric current sheet in the outer corona. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Woo, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 238-725, Pasadena, CA 91109 USA. NR 44 TC 14 Z9 14 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD SEP-OCT PY 2005 VL 231 IS 1-2 BP 71 EP 85 DI 10.1007/s11207-005-1580-x PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 004IO UT WOS:000234746700006 ER PT J AU Kuligowski, DR Ford, MJ Berejikian, BA AF Kuligowski, DR Ford, MJ Berejikian, BA TI Breeding structure of steelhead inferred from patterns of genetic relatedness among nests SO TRANSACTIONS OF THE AMERICAN FISHERIES SOCIETY LA English DT Article ID SALMON SALMO-SALAR; INDIVIDUAL REPRODUCTIVE SUCCESS; TROUT ONCORHYNCHUS-MYKISS; OTOLITH MICROCHEMISTRY; NATURAL-POPULATIONS; SOCKEYE-SALMON; PACIFIC SALMON; CHINOOK SALMON; MICROSATELLITE; WILD AB Ten polylmorphic microsatellite loci were used to infer kinship among steelhead Oncorhynchus mykiss sampled from nest sites in the Hamma Hamma River, Washington. Fertilized eggs were removed from 8 of 11 redds (i.e., individual nests within redds) surveyed in 1998, tagged with unique identifiers, and reared until adulthood as part of a conservation program. On average, individuals sampled from the same redd were more closely related than individuals sampled from different redds, and a tree generated from the pairwise relatedness estimates shows clear clustering of individuals by redd. Despite this general pattern, there was substantial overlap in the pairwise relatedness estimates within and among most redds. Of the eight redds, seven contained more than four alleles at a minimum of one locus and five contained more than six alleles, indicating that most redds were the result of matings by more than a single pair of parents. In total, the eight redds were created by a minimum of 21 parents, which we inferred to consist of at least 5 females and 16 males based on the location and timing of redd construction. The male-biased sex ratio is probably due to matings by either male resident trout or precocial steelhead part with female steelhead. The results of this study indicate that although multiple matings by both sexes are common in this population, the variance in reproductive success is much higher for males than females. C1 Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Conservat Biol Div, Manchester Res Stn, Manchester, WA 98353 USA. RP Kuligowski, DR (reprint author), Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Conservat Biol Div, Manchester Res Stn, POB 130, Manchester, WA 98353 USA. EM david.kuligowski@noaa.gov NR 46 TC 18 Z9 19 U1 0 U2 3 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 0002-8487 J9 T AM FISH SOC JI Trans. Am. Fish. Soc. PD SEP PY 2005 VL 134 IS 5 BP 1202 EP 1212 DI 10.1577/T04-187.1 PG 11 WC Fisheries SC Fisheries GA 976MJ UT WOS:000232737300011 ER PT J AU Berejikian, B Van Doornik, D LaRae, A Tezak, S Lee, J AF Berejikian, B Van Doornik, D LaRae, A Tezak, S Lee, J TI The effects of exercise on behavior and reproductive success of captively reared steelhead SO TRANSACTIONS OF THE AMERICAN FISHERIES SOCIETY LA English DT Article ID TROUT ONCORHYNCHUS-MYKISS; SALMON SALMO-SALAR; ATLANTIC SALMON; SOCKEYE-SALMON; RAINBOW-TROUT; PACIFIC SALMON; BREEDING SUCCESS; CHINOOK SALMON; COHO SALMON; PINK SALMON AB Steel head Oncorhynchus mykiss collected as eyed eggs from the Hamma Hamma River, Washington, and reared in high (similar to 1 body length/s) or low current velocity (similar to 0.25 body lengths/s) were tested for differences in reproductive behavior in both an experimental spawning channel and their natal river. We conducted continuous (24-h/d) behavioral observations in the spawning channel and applied DNA pedigree analyses to explain the variation in individual reproductive success. Female steelhead reared in high and low current velocities did not exhibit differences in reproductive behavior in the spawning channel, but females reared in low current velocity were snore frequently observed constructing nests in the Hamma Hamma River. Males reared in low-velocity tanks were more frequently observed courting females in the spawning channel and in the river. A pedigree analysis revealed no significant differences in reproductive success between the rearing treatments. Male reproductive success in the spawning channel was significantly correlated (r(2) = 0.602; P < 0.001) and the dominant male was identified by the frequency of spawning in both treatments. There was no apparent effect of male or female body mass on breeding behavior or reproductive success in the spawning channel. All 24 females and 23 out of 24 males produced free-swimming offspring in a 5.5% subsample of the fry population. This study suggests that releasing captively reared steelhead reared under conventional (i.e., low current velocity) culture conditions should be considered (along with other options) as a potentially viable component of captive rearing and breeding programs. C1 Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Resource Enhancement & Utilizat Technol Div, Manchester Res Stn, Manchester, WA 98353 USA. Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Conservat Biol Div, Manchester Res Stn, Manchester, WA 98353 USA. Pacific States Marine Fisheries Commiss, Gladstone, OR 97027 USA. Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Resource Enhancement & Ultilizat Technol Div, Manchester Res Stn, Manchester, WA 98353 USA. Long Live Kings, Seattle, WA 98101 USA. RP Berejikian, B (reprint author), Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Resource Enhancement & Utilizat Technol Div, Manchester Res Stn, POB 130, Manchester, WA 98353 USA. EM barry.berejikian@noaa.gov NR 63 TC 5 Z9 5 U1 1 U2 6 PU AMER FISHERIES SOC PI BETHESDA PA 5410 GROSVENOR LANE SUITE 110, BETHESDA, MD 20814-2199 USA SN 0002-8487 J9 T AM FISH SOC JI Trans. Am. Fish. Soc. PD SEP PY 2005 VL 134 IS 5 BP 1236 EP 1252 DI 10.1057/T04-192.1 PG 17 WC Fisheries SC Fisheries GA 976MJ UT WOS:000232737300014 ER PT J AU Pettorelli, N Vik, JO Mysterud, A Gaillard, JM Tucker, CJ Stenseth, NC AF Pettorelli, N Vik, JO Mysterud, A Gaillard, JM Tucker, CJ Stenseth, NC TI Using the satellite-derived NDVI to assess ecological responses to environmental change SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Review ID DIFFERENCE VEGETATION INDEX; NOAA AVHRR DATA; HIGH-RESOLUTION RADIOMETER; TIME-SERIES; SPECIES RICHNESS; CLIMATE-CHANGE; LAND-COVER; INTERANNUAL VARIABILITY; SPECTRAL REFLECTANCE; MIGRATORY BIRD AB Assessing how environmental changes affect the distribution and dynamics of vegetation and animal populations is becoming increasingly important for terrestrial ecologists to enable better predictions of the effects of global warming, biodiversity reduction or habitat degradation. The ability to predict ecological responses has often been hampered by our rather limited understanding of trophic interactions. Indeed, it has proven difficult to discern direct and indirect effects of environmental change on animal populations owing to limited information about vegetation at large temporal and spatial scales. The rapidly increasing use of the Normalized Difference Vegetation Index (NDVI) in ecological studies has recently changed this situation. Here, we review the use of the NDVI in recent ecological studies and outline its possible key role in future research of environmental change in an ecosystem context. C1 Univ Oslo, Dept Biol, Ctr Ecol & Evolutionary Synth, N-0316 Oslo, Norway. Univ Lyon 1, UMR Biometrie & Biol Evolut 5558, F-69622 Villeurbanne, France. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Stenseth, NC (reprint author), Univ Oslo, Dept Biol, Ctr Ecol & Evolutionary Synth, POB 1066 Blindern, N-0316 Oslo, Norway. EM n.c.stenseth@bio.uio.no RI Vik, Jon Olav/B-9350-2008; Stenseth, Nils Chr./G-5212-2016; OI Vik, Jon Olav/0000-0002-7778-4515; Stenseth, Nils Chr./0000-0002-1591-5399; Mysterud, Atle/0000-0001-8993-7382 NR 79 TC 794 Z9 872 U1 51 U2 422 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD SEP PY 2005 VL 20 IS 9 BP 503 EP 510 DI 10.1016/j.tree.2005.05.011 PG 8 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 967YV UT WOS:000232128300010 PM 16701427 ER PT J AU DellaCorte, C AF DellaCorte, C TI Tribology takes center stage SO TRIBOLOGY & LUBRICATION TECHNOLOGY LA English DT Editorial Material AB From its most humble origins, exemplified by the use of animal fats to lubricate primitive machines, to modern synthetic oils, tribology has played an important role in keeping technology moving forward. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP DellaCorte, C (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM cdellacorte@stle.org NR 0 TC 0 Z9 0 U1 0 U2 1 PU SOC TRIBOLOGISTS & LUBRICATION ENGINEERS PI PARK RIDGE PA 840 BUSSE HIGHWAY, PARK RIDGE, IL 60068 USA SN 0024-7154 J9 TRIBOL LUBR TECHNOL JI Tribol. Lubr. Technol. PD SEP PY 2005 VL 61 IS 9 BP 6 EP 6 PG 1 WC Engineering, Mechanical SC Engineering GA 965SG UT WOS:000231970000002 ER PT J AU Dixon, T AF Dixon, T TI Finding the strength of manual GTA welds SO WELDING JOURNAL LA English DT Letter C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Dixon, T (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER WELDING SOC PI MIAMI PA 550 N W LEJEUNE RD, MIAMI, FL 33126 USA SN 0043-2296 J9 WELD J JI Weld. J. PD SEP PY 2005 VL 84 IS 9 BP 18 EP 18 PG 1 WC Metallurgy & Metallurgical Engineering SC Metallurgy & Metallurgical Engineering GA 961CB UT WOS:000231638400008 ER PT J AU Puchtel, IS Brandon, AD Humayun, M Walker, RJ AF Puchtel, IS Brandon, AD Humayun, M Walker, RJ TI Evidence for the early differentiation of the core from Pt-Re-Os isotope systematics of 2.8-Ga komatiites SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Archaen komatiite; Pt-Re-Os isotope sytematics; highly siderophile elements; core-mantle interaction ID KOSTOMUKSHA GREENSTONE-BELT; NW BALTIC SHIELD; MANTLE INTERACTION; THERMAL EVOLUTION; EARTHS CORE; OS-186-OS-187 SYSTEMATICS; ELEMENT GEOCHEMISTRY; HAWAIIAN PICRITES; VETRENY BELT; INNER-CORE AB Komatiite samples from the 2.8-Ga Kostomuksha greenstone belt in the Baltic Shield define Pt-Os and Re-Os isochrons with ages of 2816 +/- 190 and 2880 +/- 83 Ma, respectively. The mean initial (186)Os/(188)Os and (187)Os/(188)Os ratios calculated at T=2821 Ma are 0.1198341 +/- 7 and 0.11042 +/- 69 (gamma(187)Os =+2.5 +/- 0.6), respectively. This Os isotopic composition characterizes that of the source of the Kostomuksha komatiite and is 53 +/- 6 ppm and 2.5 +/- 0.6% more radiogenic in (186)Os/(188)Os and (187)Os/(188)Os , respectively, than the putative contemporary convecting mantle. The coupled (186)Os-(187)Os enrichment cannot be the result of incorporation of the material of aged recycled oceanic crust into the source of the plume, as five to six times more crustal component is required to create the (186)Os-enrichment than the (187)Os-enrichment observed. Moreover, the radiogenic (186)Os/(188)Os ratio combined with the subchondritic Pt/Os in this source calculated from the HSE abundance data is inconsistent with any model of Os isotopic evolution that involves crustal recycling, as these models require substantially suprachondritic Pt/Os in the hybrid sources. The coupled (186)Os-(187)Os enrichment in the source of the Kostomuksha komatiite is best explained via derivation of most of the Os from the outer core. This is most consistent with the Kostomuksha komatiites originating from a mantle plume that arose from the core-mantle boundary (CMB). If this interpretation is correct, the data provide minimum constraints on the (186)Os/(188)Os and (187)Os/(188)Os ratios of the outer core at 2.8 Ga. The existing models of core crystallization based on experimentally determined solid metal-liquid metal partition coefficients for Pt, Re, and Os can adequately explain the Os isotopic composition of the Kostomuksha mantle source, although require the onset of inner core crystallization several hundred million years prior to formation of the Kostomuksha plume. Based on thermodynamic models, such an early onset of inner core crystallization would require a relatively low heat flux across the CMB of similar to 3 TW and the presence of > 100 ppm K in the core. The results of this study combined with the HSE abundance data for the source of komatiites at Kostomuksha indicate that core-mantle interaction, at least in this instance, could occur in the form of isotopic exchange without significant mass transfer from the core to the mantle. (c) 2005 Elsevier B.V. All rights reserved. C1 Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. Univ Maryland, Dept Geol, Isotope Geochem Lab, College Pk, MD 20742 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Florida State Univ, Natl High Magnet Field Lab, Tallahassee, FL 32310 USA. Florida State Univ, Dept Geol Sci, Tallahassee, FL 32310 USA. RP Puchtel, IS (reprint author), Univ Chicago, Dept Geophys Sci, 5734 S Ellis Ave, Chicago, IL 60637 USA. EM ipuchtel@umd.edu RI Walker, Richard/K-6869-2016; OI Walker, Richard/0000-0003-0348-2407; Humayun, Munir/0000-0001-8516-9435 NR 55 TC 44 Z9 45 U1 2 U2 12 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD AUG 30 PY 2005 VL 237 IS 1-2 BP 118 EP 134 DI 10.1016/j.epsl.2005.04.023 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 966UK UT WOS:000232047400009 ER PT J AU Chepfer, H Noel, V Minnis, P Baumgardner, D Nguyen, L Raga, G McGill, MJ Yang, P AF Chepfer, H Noel, V Minnis, P Baumgardner, D Nguyen, L Raga, G McGill, MJ Yang, P TI Particle habit in tropical ice clouds during CRYSTAL-FACE: Comparison of two remote sensing techniques with in situ observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SINGLE-SCATTERING PROPERTIES; CIRRUS CLOUDS; MICROPHYSICAL PROPERTIES; RADIATIVE PROPERTIES; SATELLITE MEASUREMENTS; LIDAR DEPOLARIZATION; OPTICAL-THICKNESS; LIGHT-SCATTERING; TEMPERATURE; PHASE AB [1] Ice crystal shapes in tropical ice clouds are estimated with two different remote sensing methods and compared with measurements from an in situ cloud aerosol spectrometer ( CAS) during the Cirrus Regional Study of Tropical Anvils and Cirrus Layers - Florida Area Cirrus Experiment (CRYSTAL-FACE) campaign conducted in Florida during July 2002. The remote sensing techniques use dual-satellite reflectances and lidar linear depolarization rates. The ice crystal shape is derived from CAS measurements of forward and backscattered light from individual particles in the size range from 1 to 45 mm. The remote sensing and in situ retrievals are based on ice crystal optical models, which incorporate the scattering phase functions integrated over the collection angles used by the CAS, the view angles from dual-satellites retrievals, and the complete scattering matrix for lidar. Owing to the space and time collocation constraint between in situ and remote sensing techniques, data from only 1 day are used to evaluate the dual-satellite technique ( 11 July) and from 3 days for the lidar ( 23, 26, and 29 July). Data from 23 and 29 July are also used to compare the two remote sensing techniques. In total, 40 shape retrievals were obtained for 20 different cloud areas, allowing paired comparisons of the methods. The results show consistent particle shapes for half of the cloud areas studied. The discrepancies for the other cases can be explained by insufficient spatial-temporal collocations of the data or limitations of the CAS that constrain its range to particles <45 mu m, whereas the remote sensing techniques are influenced by particles outside the size range of the CAS. C1 Ecole Polytech, Meteorol Dynam Lab, Inst Pierre Simon Laplace, F-91128 Palaiseau, France. Analyt Serv & Mat Inc, Hampton, VA 23666 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Univ Nacl Autonoma Mexico, Ctr Ciencias Atmosfera, Mexico City 04510, DF, Mexico. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. RP Chepfer, H (reprint author), Ecole Polytech, Meteorol Dynam Lab, Inst Pierre Simon Laplace, F-91128 Palaiseau, France. EM chepfer@lmd.polytechnique.fr RI Yang, Ping/B-4590-2011; McGill, Matthew/D-8176-2012; Noel, Vincent/C-3702-2013; Raga, Graciela/A-4340-2008; Minnis, Patrick/G-1902-2010 OI Noel, Vincent/0000-0001-9494-0340; Minnis, Patrick/0000-0002-4733-6148 NR 59 TC 7 Z9 7 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 30 PY 2005 VL 110 IS D16 AR D16204 DI 10.1029/2004JD005455 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 962JJ UT WOS:000231727300002 ER PT J AU Boy, JP Chao, BF AF Boy, JP Chao, BF TI Precise evaluation of atmospheric loading effects on Earth's time-variable gravity field SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID GRACE; MASS; DEFORMATION; VARIABILITY; SYSTEM AB New space gravity missions will provide gravity measurements with unprecedented accuracy and high spatial resolution. To reveal the oceanic and hydrologic signals in monthly time-variable gravity field from the Gravity Recovery and Climate Experiment (GRACE) satellite (Tapley et al., 2004) entails the removal of the atmospheric contribution, which in turn requires a precise knowledge of the atmospheric mass redistribution. We reconstruct the three-dimensional (3-D) variations of air-density from vertical profiles of pressure, temperature, and specific humidity provided by the National Centers for Environmental Prediction (NCEP) atmospheric model of a realistic topography. We compare our results with those from the classical thin layer (2-D) approximation and show that the differences between the complete 3-D and the 2-D computations are often nonnegligible in the presence of the expected GRACE sensitivity up to harmonic degrees of 15-20, corresponding to wavelengths of 2000-2500 km. For actual computation, we recommend the use of the sigma level atmospheric data with special attention to the latitude and altitude dependence of the Earth's gravity. We also examine and conclude the importance of the differences with previous study which assumed a constant surface gravity acceleration without a latitudinal dependence. C1 NASA, Space Geodesy Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Boy, JP (reprint author), Inst Phys Globe Strasbourg, EOST, UMR CNRS ULP 7516, 5 Rue Rene Descartes, F-67084 Strasbourg, France. EM jpboy@eost.u-strasbg.fr; benjamin.f.chao@nasa.gov RI Chao, Benjamin Fong/N-6156-2013; Boy, Jean-Paul/E-6677-2017 OI Boy, Jean-Paul/0000-0003-0259-209X NR 21 TC 15 Z9 16 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD AUG 30 PY 2005 VL 110 IS B8 AR B08412 DI 10.1029/2002JB002333 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 962JT UT WOS:000231728400001 ER PT J AU Bauschlicher, CW Xue, YQ AF Bauschlicher, CW Xue, YQ TI Current-voltage curves for molecular junctions: Metal basis set vs. cluster size SO CHEMICAL PHYSICS LA English DT Article ID ELECTRONIC DEVICES; POTENTIALS; FORMALISM; TRANSPORT; EXCHANGE; ENERGY; ATOMS; WIRES AB A 21 Au atom description of the contacts supports previous work that used only six An atoms. Using the LANL1 (3s3p3d)/ [1s1p1d] An basis set in conjunction with the six atom cluster leads to solutions with excess charge on the An atoms. While using the (3s3p3d)/[1s1p1d] An basis set for all atoms in a larger 21 An atom cluster also yields a non-physical solution, it is possible to use the full minimal basis set on the An atoms that are not at the edge of the cluster. (C) 2005 Elsevier B.V. All rights reserved. C1 NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. SUNY Albany, Coll Nanoscale Sci & Engn, Albany, NY 12203 USA. RP Bauschlicher, CW (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, Mail Stop 230-3, Moffett Field, CA 94035 USA. EM Charles.W.Bauschlicher@nasa.gov; yxue@uamail.albany.edu NR 26 TC 4 Z9 4 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0301-0104 J9 CHEM PHYS JI Chem. Phys. PD AUG 29 PY 2005 VL 315 IS 3 BP 293 EP 296 DI 10.1016/j.chemphys.2005.04.039 PG 4 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 959QV UT WOS:000231534100008 ER PT J AU Bagdassarian, CK Thompson, DS Davis, LM Thompson, DW Southward, RE AF Bagdassarian, CK Thompson, DS Davis, LM Thompson, DW Southward, RE TI Single-stage near-surface metallization of fluorinated polyimides yielding reflective nanoparticlate silvered hybrid membranes SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 230th National Meeting of the American-Chemical-Society CY AUG 28-SEP 01, 2005 CL Washington, DC C1 Coll William & Mary, Dept Chem, Williamsburg, VA 23187 USA. NASA, Langley Res Ctr, Adv Mat & Proc Branch, Washington, DC 20546 USA. EM ckbagd@wm.edu; dwthom@wm.edu NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 28 PY 2005 VL 230 MA 94-COLL BP U1082 EP U1083 PG 2 WC Chemistry, Multidisciplinary SC Chemistry GA 032TJ UT WOS:000236797302174 ER PT J AU Boal, AK Binsted, K Brown, MV Gaidos, E AF Boal, AK Binsted, K Brown, MV Gaidos, E TI Variations of the helical components of proteins from mesophilic, thermophilic, and halophilic microorganisms SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 230th National Meeting of the American-Chemical-Society CY AUG 28-SEP 01, 2005 CL Washington, DC C1 Univ Hawaii Manoa, NASA, Astrobiol Inst, Honolulu, HI 96822 USA. EM akboal@ifa.hawaii.edu NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 28 PY 2005 VL 230 MA 239-BIOL BP U615 EP U615 PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA 032TJ UT WOS:000236797301234 ER PT J AU Chaban, GM Huo, WM Wang, DY Dateo, CE AF Chaban, GM Huo, WM Wang, DY Dateo, CE TI Use of NASA's Columbia teraflop supercomputer to study DNA damage by charged particles SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 230th National Meeting of the American-Chemical-Society CY AUG 28-SEP 01, 2005 CL Washington, DC C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Eloret Corp, Sunnyvale, CA 94087 USA. EM chaban@nas.nasa.gov NR 0 TC 2 Z9 2 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 28 PY 2005 VL 230 MA 97-COMP BP U1297 EP U1297 PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA 032TJ UT WOS:000236797302609 ER PT J AU Lee, TJ Schwenke, DW Dateo, CE Chaban, GM AF Lee, TJ Schwenke, DW Dateo, CE Chaban, GM TI Reliable spectroscopic constants for CCH-, NH2-and their isotopomers from an accurate potential energy function SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 230th National Meeting of the American-Chemical-Society CY AUG 28-SEP 01, 2005 CL Washington, DC C1 NASA, Ames Res Ctr, Computat Chem Grp, Moffett Field, CA 94035 USA. EM tjlee@mail.arc.nasa.gov RI schwenke, david/I-3564-2013 NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 28 PY 2005 VL 230 MA 98-PHYS BP U2817 EP U2817 PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA 032TJ UT WOS:000236797305557 ER PT J AU Leventis, N AF Leventis, N TI Polymer crosslinked 3-D assemblies of nanoparticles: Mechanically strong lightweight porous materials (X-aerogels) SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 230th National Meeting of the American-Chemical-Society CY AUG 28-SEP 01, 2005 CL Washington, DC C1 NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA. EM Nicholas.Leventis@nasa.gov NR 0 TC 0 Z9 0 U1 1 U2 4 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 28 PY 2005 VL 230 MA 414-COLL BP U1239 EP U1239 PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA 032TJ UT WOS:000236797302492 ER PT J AU Rutledge, SL Shaw, HC Waters, PF AF Rutledge, SL Shaw, HC Waters, PF TI Synthesis of carbon nanotubes and polymers to increase the performance of co-polymers and polymer blends for space flight applications SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 230th National Meeting of the American-Chemical-Society CY AUG 28-SEP 01, 2005 CL Washington, DC C1 NASA, Goddard Space Flight Ctr, Dept Chem, Greenbelt, MD 20771 USA. American Univ, Dept Chem, Washington, DC 20016 USA. EM Shavesha.L.Rutledge@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 28 PY 2005 VL 230 MA 345-PMSE BP U3668 EP U3668 PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA 032TJ UT WOS:000236797307340 ER PT J AU Wal, RLV AF Wal, RLV TI Nanostructure in carbonaceous materials: Origins and implications SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 230th National Meeting of the American-Chemical-Society CY AUG 28-SEP 01, 2005 CL Washington, DC C1 NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, Cleveland, OH USA. EM randy@rvander.grc.nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 28 PY 2005 VL 230 MA 3-ENVR BP U1501 EP U1501 PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA 032TJ UT WOS:000236797303003 ER PT J AU Xu, JC Hunter, GW Evans, LJ Ward, B Liu, CC Vander Wal, RL Berger, GM Lukco, D AF Xu, JC Hunter, GW Evans, LJ Ward, B Liu, CC Vander Wal, RL Berger, GM Lukco, D TI Nanocrystalline copper doped tin oxide as a carbon dioxide gas sensing material and its comparison to tin oxide nanostructures SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 230th National Meeting of the American-Chemical-Society CY AUG 28-SEP 01, 2005 CL Washington, DC C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. Case Western Reserve Univ, Cleveland, OH 44106 USA. NASA, Glenn Res Ctr, NCMR, Cleveland, OH 44135 USA. NASA, Glenn Res Ctr, QSS, Cleveland, OH 44135 USA. EM Jennifer.C.Xu@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 28 PY 2005 VL 230 MA 283-INOR BP U2148 EP U2149 PG 2 WC Chemistry, Multidisciplinary SC Chemistry GA 032TJ UT WOS:000236797304279 ER PT J AU Tanskanen, EI Slavin, JA Tanskanen, AJ Viljanen, A Pulkkinen, TI Koskinen, HEJ Pulkkinen, A Eastwood, J AF Tanskanen, EI Slavin, JA Tanskanen, AJ Viljanen, A Pulkkinen, TI Koskinen, HEJ Pulkkinen, A Eastwood, J TI Magnetospheric substorms are strongly modulated by interplanetary high-speed streams SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID GEOMAGNETIC-ACTIVITY; SOLAR-WIND; EVOLUTION AB The occurrence of substorms was examined over a complete 11-year solar cycle, identifying over 5000 substorms. It was found that high-speed streams strongly modulate the substorm occurrence rate, peak amplitude and ionospheric dissipation in the form of Joule heating and auroral electron precipitation. Substorms occurring during the years of frequent interplanetary high-speed streams ( 1994 and 2003) are 32% more intense, on average, and transfer twice as much magnetic energy to the auroral ionosphere as the substorms occurring during the years of few or no high-speed streams ( 1993, 1995 - 2002). To characterize and to predict the substorm activity we form a new measure, the substorm activity parameter R-su, which we expect to become a powerful tool in analyzing the near-Earth space climate. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. Johns Hopkins Univ, Ctr Cardiovasc Bioinformat & Modeling, Baltimore, MD 21218 USA. Finnish Meteorol Inst, Space Res Unit, FIN-00101 Helsinki, Finland. Univ Helsinki, Dept Phys Sci, Helsinki, Finland. RP Tanskanen, EI (reprint author), Finnish Meteorol Inst, Space Res Unit, FIN-00101 Helsinki, Finland. EM eija.tanskanen@fmi.fi RI Pulkkinen, Tuija/D-8403-2012; Slavin, James/H-3170-2012; Koskinen, Hannu/B-4971-2017 OI Pulkkinen, Tuija/0000-0002-6317-381X; Slavin, James/0000-0002-9206-724X; Koskinen, Hannu/0000-0003-3839-6461 NR 27 TC 35 Z9 35 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 26 PY 2005 VL 32 IS 16 AR L16104 DI 10.1029/2005GL023318 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 960CX UT WOS:000231568900003 ER PT J AU Mingo, N Broido, DA AF Mingo, N Broido, DA TI Carbon nanotube ballistic thermal conductance and its limits SO PHYSICAL REVIEW LETTERS LA English DT Article ID MOLECULAR-DYNAMICS SIMULATION; HEAT-CONDUCTION; QUANTUM; DEPENDENCE; TRANSPORT; GRAPHITE; FLOW AB Calculations of the quantum-mechanical ballistic thermal conductance of single-walled carbon nanotubes, graphene, and graphite are presented, which explain previous experimental results, and directly disprove earlier theoretical calculations. The ballistic thermal conductances are smaller than had been previously thought, whereas the maximum sample lengths in which phonon transport remains ballistic are orders of magnitude larger than previously suggested. Good agreement with previous experiments is obtained, which shows that measured lower bounds to the thermal conductance of multiwalled carbon nanotubes are very close to the upper theoretical bounds for graphite. The bounds shown here draw a line between what is physical and unphysical in any measurements or calculations of carbon nanotube thermal conductance, and constitute a necessary test to their validity. C1 NASA, Ames Ctr Nanotechnol, Moffett Field, CA 94035 USA. Boston Coll, Dept Phys, Chestnut Hill, MA 02467 USA. RP NASA, Ames Ctr Nanotechnol, 229-1, Moffett Field, CA 94035 USA. NR 32 TC 235 Z9 239 U1 14 U2 80 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD AUG 26 PY 2005 VL 95 IS 9 AR 096105 DI 10.1103/PhysRevLett.95.096105 PG 4 WC Physics, Multidisciplinary SC Physics GA 959FR UT WOS:000231503600045 PM 16197233 ER PT J AU Talapatra, S Ganesan, PG Kim, T Vajtai, R Huang, M Shima, M Ramanath, G Srivastava, D Deevi, SC Ajayan, PM AF Talapatra, S Ganesan, PG Kim, T Vajtai, R Huang, M Shima, M Ramanath, G Srivastava, D Deevi, SC Ajayan, PM TI Irradiation-induced magnetism in carbon nanostructures SO PHYSICAL REVIEW LETTERS LA English DT Article ID SURFACE MODIFICATION; DIAMOND; THRESHOLD AB Nitrogen (N-15) and carbon (C-12) ion implantations with implant energy of 100 keV for different doses were performed on nanosized diamond (ND) particles. Magnetic measurements on the doped ND show ferromagnetic hysteresis behavior at room temperature. The saturation magnetization (M-s) in the case of N-15 implanted samples was found to be higher compared to the C-12 implanted samples for dose sizes greater than 10(14) cm(-2). The role of structural modification or defects along with the carbon-nitrogen (C-N) bonding states for the observed enhanced ferromagnetic ordering in N-15 doped samples is explained on the basis of x-ray photoelectron spectroscopy measurements. C1 Rensselaer Polytech Inst, Dept MS & E, Troy, NY 12180 USA. Rensselaer Polytech Inst, Rensselaer Nanotechnol Ctr, Troy, NY 12180 USA. SUNY Albany, Dept Phys, Albany, NY 12203 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Philip Morris Inc, RD & E Ctr, Richmond, VA 23234 USA. RP Rensselaer Polytech Inst, Dept MS & E, Troy, NY 12180 USA. RI Ramanath, Ganpati/C-1157-2011; Pethuraja, Gopal/D-9976-2015 OI Ramanath, Ganpati/0000-0002-8718-9760; Pethuraja, Gopal/0000-0001-9789-5645 NR 22 TC 157 Z9 159 U1 2 U2 17 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD AUG 26 PY 2005 VL 95 IS 9 AR 097201 DI 10.1103/PhysRevLett.95.097201 PG 4 WC Physics, Multidisciplinary SC Physics GA 959FR UT WOS:000231503600055 PM 16197243 ER PT J AU Panda, J Seasholtz, RG Elam, KA AF Panda, J Seasholtz, RG Elam, KA TI Investigation of noise sources in high-speed jets via correlation measurements SO JOURNAL OF FLUID MECHANICS LA English DT Article ID RAYLEIGH-SCATTERING; SOURCE COHERENCE; VELOCITY; FLOW; FLUCTUATIONS AB To locate noise sources in high-speed jets, the far-field sound pressure fluctuations p' were correlated with each of density rho, axial velocity u, radial velocity v, rho uu and rho vv fluctuations measured from various points in jet plumes. Detailed surveys were conducted in fully expanded, unheated plumes of Mach 0.95, 1.4 and 1.8. The velocity and density fluctuations were measured simultaneously using a recently developed non-intrusive point measurement technique based on molecular Rayleigh scattering. The technique uses a continuous-wave narrow line-width laser, Fabry-Perot interferometer and photon counting electronics. Laser light scattered by air molecules from a 1.06 mm long region on the narrow beam was collected and spectrally resolved by the interferometer. It was observed that the fluctuation spectra for air density inside the plume were in general similar to those of axial velocity spectra, while the radial velocity spectra were somewhat different. For the correlation study, microphone polar angles were varied from 30 degrees to 90 degrees to the jet axis. The sound pressure fluctuations p, at the shallowest 30 degrees angle provided the highest correlation with turbulent fluctuations. The correlations sharply decreased as the polar angle was increased to 60 degrees, beyond which all data mostly fell below the experimental noise floor. Among all turbulent fluctuations correlations showed the highest values. Correlation with the first-order terms , and third-order terms was higher than that from the second-order terms <(rho) over baru'u'; p'> and <(u) over bar rho'u'; p'>. Both < v'; p'> and correlations with the 90 degrees microphone signal fell below the experimental noise floor, while that from the shallow 30 degrees microphone showed weaker values. By moving the laser probe to various locations in the jet, it was found that the strongest noise source lay downstream of the end of the potential core and extended many diameters beyond. Correlation measurements from turbulent fluctuations along the lip shear layer showed a Mach-number dependency: significant values were measured in supersonic jets, while correlations fell below the noise floor for subsonic jets. Various additional analyses showed that fluctuations from large coherent structures mostly contributed to the measured correlation, while that from small-scale structures fell below the noise floor. C1 Ohio Aerosp Inst, Brookpark, OH 44142 USA. NASA, Glenn Res Ctr, Cleveland, OH USA. Akima Corp, Fairview Pk, OH USA. RP Panda, J (reprint author), Ohio Aerosp Inst, Brookpark, OH 44142 USA. NR 38 TC 42 Z9 42 U1 0 U2 5 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4211 USA SN 0022-1120 J9 J FLUID MECH JI J. Fluid Mech. PD AUG 25 PY 2005 VL 537 BP 349 EP 385 DI 10.1017/S0022112005005148 PG 37 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA 965FM UT WOS:000231935700015 ER PT J AU Crider, DH Espley, J Brain, DA Mitchell, DL Connerney, JEP Acuna, MH AF Crider, DH Espley, J Brain, DA Mitchell, DL Connerney, JEP Acuna, MH TI Mars Global Surveyor observations of the Halloween 2003 solar superstorm's encounter with Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID MAGNETIC PILEUP BOUNDARY; WIND INTERACTION; OXYGEN-ATOMS; BOW SHOCK; VENUS; FIELD; PRESSURE AB [1] Like at Earth, disturbances from solar storms affect the space environment as they encounter Mars. The effects of the 28 October 2003 solar superstorm were among the greatest observed by the Mars Global Surveyor spacecraft at Mars to date. The disturbance, defined by an increase in incident solar wind pressure, encountered Mars on 30 October 2003 and persisted for 43 hours. We present the effects of the passage of this high-pressure disturbance and compare the modified Martian space environment to more quiescent times. We find that the horizontal component of magnetic field is increased on the dayside. In addition, the solar wind interaction region is compressed during the disturbance. The solar wind flow has access to lower altitudes than typical, which likely increases mass loss from the Martian atmosphere. Regions of opened magnetic field lines can be closed at 400 km due to the compression of minimagnetospheres, thus altering locations where ionospheric plasma is protected from solar wind scavenging at 400 km altitude. C1 Catholic Univ Amer, Dept Phys, Gibsonville, NC 27249 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Rice Univ, Houston, TX 77005 USA. RP Crider, DH (reprint author), Catholic Univ Amer, Dept Phys, 106 Driftwood Dr, Gibsonville, NC 27249 USA. EM crider@cua.edu RI Espley, Jared/I-5118-2013; connerney, john/I-5127-2013; Hurley, Dana/F-4488-2015 OI Espley, Jared/0000-0002-6371-9683; Hurley, Dana/0000-0003-1052-1494 NR 26 TC 30 Z9 31 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD AUG 25 PY 2005 VL 110 IS A9 AR A09S21 DI 10.1029/2004JA010881 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 960EP UT WOS:000231573300001 ER PT J AU Nose, M Taguchi, S Hosokawa, K Christon, SP McEntire, RW Moore, TE Collier, MR AF Nose, M Taguchi, S Hosokawa, K Christon, SP McEntire, RW Moore, TE Collier, MR TI Overwhelming O+ contribution to the plasma sheet energy density during the October 2003 superstorm: Geotail/EPIC and IMAGE/LENA observations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID NEUTRAL ATOM EMISSIONS; SOLAR-WIND CONDITIONS; ALTITUDE POLAR-CAP; ION OUTFLOW; MAGNETIC STORM; EXPANSION PHASE; AMPTE-CCE; SUBSTORM; IONOSPHERE; ACCELERATION AB [1] We studied dynamics of O+ ions during the superstorm that occurred on 29 - 31 October 2003, using energetic (9 - 210 keV/e) ion flux data obtained by the energetic particle and ion composition (EPIC) instrument on board the Geotail satellite and neutral atom data in the energy range of 10 eV to a few keV acquired by the low-energy neutral atom (LENA) imager on board the Imager for Magnetopause-to-Aurora Global Exploration (IMAGE) satellite. Since the low-energy neutral atoms are created from the outflowing ionospheric ions by the charge exchange process, we could examine variations of ionospheric ion outflow with the IMAGE/LENA data. In the near-Earth plasma sheet of X-GSM similar to - 6 R-E to - 8.5 R-E, we found that the H+ energy density showed no distinctive differences between the superstorm and quiet intervals ( 1 - 10 keV cm(-3)), while the O+ energy density increased from 0.05 - 3 keV cm(-3) during the quiet intervals to similar to 100 keV cm(-3) during the superstorm. The O+/ H+ energy density ratio reached 10 - 20 near the storm maximum, which is the largest ratio in the near-Earth plasma sheet ever observed by Geotail, indicating more than 90% of O+ in the total energy density. We argued that such extreme increase of the O+/ H+ energy density ratio during the October 2003 superstorm was due to mass-dependent acceleration of ions by storm-time substorms as well as an additional supply of O+ ions from the ionosphere to the plasma sheet. We compared the ion composition between the ring current and the near-Earth plasma sheet reported by previous studies and found that they are rather similar. On the basis of the similarity, we estimated that the ring current had the O+/ H+ energy density ratio as large as 10 - 20 for the October 2003 superstorm. C1 Kyoto Univ, Grad Sch Sci, Data Anal Ctr Geomagnetism & Space Magnetism, Sakyo Ku, Kyoto 6068502, Japan. Univ Electrocommun, Dept Informat & Commun Engn, Tokyo 1828585, Japan. Focused Anal & Res, Columbia, MD 21044 USA. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Nose, M (reprint author), Kyoto Univ, Grad Sch Sci, Data Anal Ctr Geomagnetism & Space Magnetism, Sakyo Ku, Kyoto 6068502, Japan. EM nose@kugi.kyoto-u.ac.jp RI Moore, Thomas/D-4675-2012; Collier, Michael/I-4864-2013; Nose, Masahito/B-1900-2015; OI Moore, Thomas/0000-0002-3150-1137; Collier, Michael/0000-0001-9658-6605; Nose, Masahito/0000-0002-2789-3588; Christon, Stephen/0000-0003-1770-2458 NR 41 TC 54 Z9 54 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-SPACE JI J. Geophys. Res-Space Phys. PD AUG 25 PY 2005 VL 110 IS A9 AR A09S24 DI 10.1029/2004JA010930 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 960EP UT WOS:000231573300003 ER PT J AU Pulkkinen, A Lindahl, S Viljanen, A Pirjola, R AF Pulkkinen, A Lindahl, S Viljanen, A Pirjola, R TI Geomagnetic storm of 29-31 October 2003: Geomagnetically induced currents and their relation to problems in the Swedish high-voltage power transmission system SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID NATURAL-GAS PIPELINE; ELECTRIC-FIELDS; IMAGES AB On 30 October 2003, an ongoing geomagnetic superstorm knocked down a part of the high- voltage power transmission system in southern Sweden. The blackout lasted for an hour and left about 50,000 customers without electricity. The incident was probably the most severe geomagnetically induced current ( GIC) failure observed since the well- known March 1989 Quebec blackout. The " three- phase'' storm produced exceptionally large geomagnetic activity at the Fennoscandian auroral region. Although the diversity of the GIC drivers is addressed in the study, the problems in operating the Swedish system during the storm are attributed geophysically to substorms, storm sudden commencement, and enhanced ionospheric convection, all of which created large and complex geoelectric fields capable of driving large GIC. On the basis of the basic twofold nature of the failure- related geoelectric field characteristics, a semideterministic approach for forecasting GIC- related geomagnetic activity in which average overall activity is supplemented with statistical estimations of the amplitudes of GIC fluctuations is suggested. The study revealed that the primary mode of GIC- related failures in the Swedish high- voltage power transmission system were via harmonic distortions produced by GIC combined with too sensitive operation of the protective relays. The outage in Malmo " on 30 October 2003 was caused by a combination of an abnormal switching state of the system and tripping of a low- set residual overcurrent relay that had a high sensitivity for the third harmonic of the fundamental frequency. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. Lund Univ Technol, Dept Ind Elect Engn & Automat, SE-22100 Lund, Sweden. Finnish Meteorol Inst, Space Res Unit, FIN-00101 Helsinki, Finland. RP Pulkkinen, A (reprint author), NASA, Goddard Space Flight Ctr, Code 692, Greenbelt, MD 20770 USA. EM antti.pulkkinen@gsfc.nasa.gov; sture.lindahl@iea.lth.se; ari.viljanen@fmi.fi; risto.pirjola@fmi.fi NR 34 TC 65 Z9 66 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD AUG 25 PY 2005 VL 3 IS 8 AR S08C03 DI 10.1029/2004SW000123 PG 19 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 960VZ UT WOS:000231622600001 ER PT J AU Gladstone, RM Ross, I Valdes, PJ Abe-Ouchi, A Braconnot, P Brewer, S Kageyama, M Kitoh, A Legrande, A Marti, O Ohgaito, R Otto-Bliesner, B Peltier, WR Vettoretti, G AF Gladstone, RM Ross, I Valdes, PJ Abe-Ouchi, A Braconnot, P Brewer, S Kageyama, M Kitoh, A Legrande, A Marti, O Ohgaito, R Otto-Bliesner, B Peltier, WR Vettoretti, G TI Mid-Holocene NAO: A PMIP2 model intercomparison SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID NORTH-ATLANTIC OSCILLATION; TEMPERATURE AB The mid-Holocene ( 6000 years before present) North Atlantic Oscillation (NAO) from nine models in the Paleoclimate Modeling Intercomparison Project Phase 2 is studied, primarily through principal component analysis of winter time North Atlantic sea level pressure (SLP). Modeled mid-Holocene NAO and mean SLP show small changes compared to pre-industrial control runs, with a shift in mean state towards a more positive NAO regime for three of the models. Modeled NAO variability shows little change, with a small increase for some models in the fraction of time spent in the NAO-negative phase during the mid-Holocene. Proxy based reconstructions of the NAO indicate a more positive NAO regime compared to present day during the mid-Holocene. We hypothesise that there was a small NAO+ like shift in mean state during the mid-Holocene. C1 Univ Bristol, Sch Geog Sci, Bristol BS8 1SS, Avon, England. Univ Tokyo, Ctr Climat Syst Res, Tokyo 153, Japan. JAMSTEC, FRCGC, Yokohama, Kanagawa 2360001, Japan. IPSL Lab Sci Climat & Environm, F-91191 Gif Sur Yvette, France. Europole Arbois, CEREGE CNRS 6635, F-13545 Aix En Provence, France. Meteorol Res Inst, Tsukuba, Ibaraki 3050052, Japan. NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Natl Ctr Atmospher Res, Boulder, CO 80307 USA. Univ Toronto, Dept Atmospher Sci, Toronto, ON M5S 1A7, Canada. RP Gladstone, RM (reprint author), Univ Bristol, Sch Geog Sci, Univ Rd, Bristol BS8 1SS, Avon, England. EM r.gladstone@bris.ac.uk RI Marti, Olivier/B-2378-2009; Ross, Ian/C-8766-2011; KAGEYAMA, Masa/F-2389-2010; LeGrande, Allegra/D-8920-2012; Peltier, William/A-1102-2008; Gladstone, Rupert/C-1086-2013; Valdes, Paul/C-4129-2013; Abe-Ouchi, Ayako/M-6359-2013 OI KAGEYAMA, Masa/0000-0003-0822-5880; LeGrande, Allegra/0000-0002-5295-0062; Gladstone, Rupert/0000-0002-1582-3857; Abe-Ouchi, Ayako/0000-0003-1745-5952 NR 19 TC 46 Z9 50 U1 2 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 24 PY 2005 VL 32 IS 16 AR L16707 DI 10.1029/2005GL023596 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 960CT UT WOS:000231568500004 ER PT J AU Petropavlovskikh, I Bhartia, PK DeLuisi, J AF Petropavlovskikh, I Bhartia, PK DeLuisi, J TI New Umkehr ozone profile retrieval algorithm optimized for climatological studies SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID INVERSION AB We present a new Umkehr ozone profile retrieval algorithm (UMK04) that has been optimized for the study of monthly mean anomalies (MMA) to assess climate variability in multi-year time series. Although the Umkehr technique is too noisy to monitor short-term variability in atmospheric ozone, it is capable of monitoring long-term changes in MMA with less then 5% uncertainty in the stratosphere, and with no influence from a priori information. By examining the information content of UMK04 we conclude that Umkehr data contain useful information about long-term ozone trend down to the surface, provided the data are analyzed as column ozone amounts in 8-layers, consisting of two similar to 9.6 km layers in the lower atmosphere ( 253 - 1013, 63 - 253 hPa), five similar to 4.8 km layers ( 32 - 63, 16 - 32, 8 - 16, 4 - 8, 2 - 4 hPa) in the stratosphere, plus a broad top layer spanning from 0 - 4 hPa. C1 NOAA, ARL, REAR 1, Cooperat Inst Res Environm Sci, Boulder, CO 80303 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Petropavlovskikh, I (reprint author), NOAA, ARL, REAR 1, Cooperat Inst Res Environm Sci, 325 Broadway, Boulder, CO 80303 USA. EM irini.petro@noaa.gov RI Bhartia, Pawan/A-4209-2016 OI Bhartia, Pawan/0000-0001-8307-9137 NR 13 TC 27 Z9 28 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 24 PY 2005 VL 32 IS 16 AR L16808 DI 10.1029/2005GL023323 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 960CT UT WOS:000231568500001 ER PT J AU Poggi, MA Lillehei, PT Bottomley, LA AF Poggi, MA Lillehei, PT Bottomley, LA TI Chemical force microscopy on single-walled carbon nanotube paper SO CHEMISTRY OF MATERIALS LA English DT Article ID SELF-ASSEMBLED MONOLAYERS; POLYMER COMPOSITES; STRUCTURAL-CHARACTERIZATION; MECHANICAL-PROPERTIES; ELECTRICAL-PROPERTIES; ORGANIC-SURFACES; THIOL MONOLAYERS; ADHESION FORCES; FILMS; GOLD AB Topographical and adhesive force measurements were acquired simultaneously on single-walled carbon nanotube (SWNT) paper using chemically modified atomic force microscopy probe tips. Gold-coated cantilever probe tips were chemically modified with a series of omega-substituted alkanethiols or para-substituted arylthiols. The observed adhesion forces were highly dependent on the contact area between the tip and paper, the type of thiol (alkane versus aryl), and the identity of the terminal group. The adhesion force per molecule interacting with the sidewall of single-walled carbon nanotubes was elucidated after correcting for variations in tip shape and sample topology. C1 Georgia Inst Technol, Sch Chem & Biochem, Atlanta, GA 30332 USA. NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA. RP Georgia Inst Technol, Sch Chem & Biochem, Atlanta, GA 30332 USA. EM lawrence.bottomley@chemistry.gatech.edu RI Lillehei, Peter/C-9196-2009; OI Lillehei, Peter/0000-0001-8183-9980; Bottomley, Lawrence/0000-0002-2325-9862 NR 54 TC 26 Z9 26 U1 1 U2 3 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0897-4756 EI 1520-5002 J9 CHEM MATER JI Chem. Mat. PD AUG 23 PY 2005 VL 17 IS 17 BP 4289 EP 4295 DI 10.1021/cm04834m PG 7 WC Chemistry, Physical; Materials Science, Multidisciplinary SC Chemistry; Materials Science GA 957OL UT WOS:000231379300005 ER PT J AU Ranade, A Nayak, K Fairbrother, D D'Souza, NA AF Ranade, A Nayak, K Fairbrother, D D'Souza, NA TI Maleated and non-maleated polyethylene-montmorillonite layered silicate blown films: creep, dispersion and crystallinity SO POLYMER LA English DT Article DE Burger model; non-linear creep; PE nanocomposites ID HIGH-DENSITY POLYETHYLENE; NONLINEAR MECHANICAL RESPONSE; NANOCOMPOSITES; BEHAVIOR; HYBRID; POLYPROPYLENE; RECOVERY; CLAY AB Non-linear time dependent creep of polyethylene (PE) montmorillonite layered silicate (MLS) nanocomposites was investigated. PE grafted maleic anhydride (PE-g-MA) was used, as a coupling agent to improve the miscibility between PE and organically modified MLS. The creep and tensile response of maleated and non-maleated PE nanocomposites were determined. Tensile properties of maleated PE nanocomposites were higher than the non-maleated nanocomposites. Non-linearity in the creep response was modeled using the Burger model. A drop in the retardation time was observed for maleated PE nanocomposites. XRD, polarized optical microscopy and a differential scanning calorimeter (DSC) were used to probe crystallinity and clay dispersion in the films. The tensile and creep properties were related to dispersion due to presence of MLS. The deformation response of PE blended with PE-g-MA and each of these separately modified by MLS showed synergistic contributions of the constituents. The response was attributed to dispersion effects with marginal effects of crystallinity. (c) 2005 Elsevier Ltd. All rights reserved. C1 Univ N Texas, Dept Mat Sci & Engn, Denton, TX 76203 USA. Huntsman LLC, Odessa, TX 79760 USA. NASA, Wallops Flight Facil, Wallops Isl, VA 23337 USA. RP Univ N Texas, Dept Mat Sci & Engn, POB 305310, Denton, TX 76203 USA. EM ndsouza@unt.edu OI DSouza, Nandika/0000-0002-8553-0347 NR 31 TC 93 Z9 101 U1 0 U2 14 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0032-3861 EI 1873-2291 J9 POLYMER JI Polymer PD AUG 23 PY 2005 VL 46 IS 18 BP 7323 EP 7333 DI 10.1016/j.polymer.2005.04.085 PG 11 WC Polymer Science SC Polymer Science GA 957TW UT WOS:000231397200059 ER PT J AU Wilson, E Pedretti, E Bregman, J Mah, RW Traub, WA AF Wilson, E Pedretti, E Bregman, J Mah, RW Traub, WA TI Adaptive DFT-based interferometer fringe tracking SO EURASIP JOURNAL ON APPLIED SIGNAL PROCESSING LA English DT Article DE fringe tracking; DFT; interferometry; IOTA; real time ID IOTA INTERFEROMETER; PREDICTION AB An automatic interferometer fringe tracking system has been developed, implemented, and tested at the Infrared Optical Telescope Array (IOTA) Observatory at Mount Hopkins, Arizona. The system can minimize the optical path differences (OPDs) for all three baselines of the Michelson stellar interferometer at IOTA. Based on sliding window discrete Fourier-transform (DFT) calculations that were optimized for computational efficiency and robustness to atmospheric disturbances, the algorithm has also been tested extensively on offline data. Implemented in ANSI C on the 266 MHz PowerPC processor running the VxWorks real-time operating system, the algorithm runs in approximately 2.0 milliseconds per scan (including all three interferograms), using the science camera and piezo scanners to measure and correct the OPDs. The adaptive DFT-based tracking algorithm should be applicable to other systems where there is a need to detect or track a signal with an approximately constant-frequency carrier pulse. One example of such an application might be to the field of thin-film measurement by ellipsometry, using a broadband light source and a Fourier-transform spectrometer to detect the resulting fringe patterns. C1 Intellizat, Redwood Shores, CA 94065 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Wilson, E (reprint author), Intellizat, 454 Barkentine Lane, Redwood Shores, CA 94065 USA. EM ed.wilson@intellization.com; epedrett@umich.edu; jesse.bregman-1@nasa.gov; robert.w.mah@nasa.gov; wtraub@cfa.harvard.edu NR 25 TC 0 Z9 0 U1 0 U2 1 PU HINDAWI PUBLISHING CORPORATION PI NEW YORK PA 410 PARK AVENUE, 15TH FLOOR, #287 PMB, NEW YORK, NY 10022 USA SN 1110-8657 J9 EURASIP J APPL SIG P JI EURASIP J Appl. Signal Process. PD AUG 21 PY 2005 VL 2005 IS 15 BP 2559 EP 2572 DI 10.1155/ASP.2005.2559 PG 14 WC Engineering, Electrical & Electronic SC Engineering GA 007FH UT WOS:000234953500014 ER PT J AU Andersson, N Glampedakis, K Haskell, B Watts, AL AF Andersson, N Glampedakis, K Haskell, B Watts, AL TI Modelling the spin equilibrium of neutron stars in low-mass X-ray binaries without gravitational radiation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; gravitational waves; stars : magnetic fields; stars : neutron; pulsars : general; X-rays : binaries ID QUASI-PERIODIC OSCILLATIONS; ADVECTION-DOMINATED ACCRETION; MILLISECOND PULSAR; DISK ACCRETION; BLACK-HOLES; SPECTRAL PROPERTIES; BURST OSCILLATION; XTE J2123-058; KS 1731-260; 4U 1636-53 AB In this paper we discuss the spin equilibrium of accreting neutron stars in low-mass X-ray binaries (LMXBs). We demonstrate that, when combined with a naive spin-up torque, the observed data lead to inferred magnetic fields which are at variance with those of Galactic millisecond radio pulsars. This indicates the need for either additional spin-down torques (e.g. gravitational radiation) or an improved accretion model. We show that a simple consistent accretion model can be arrived at by accounting for radiation pressure in rapidly accreting systems (above a few per cent of the Eddington accretion rate). In our model the inner disc region is thick and significantly sub-Keplerian and the estimated equilibrium periods are such that the LMXB neutron stars have properties that accord well with the Galactic millisecond radio pulsar sample. The implications for future gravitational-wave observations are also discussed briefly. C1 Univ Southampton, Sch Math, Southampton SO17 1BJ, Hants, England. NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. RP Univ Southampton, Sch Math, Southampton SO17 1BJ, Hants, England. EM haskellb@soton.ac.uk NR 86 TC 29 Z9 30 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 21 PY 2005 VL 361 IS 4 BP 1153 EP 1164 DI 10.1111/j.1365-2966.2005.09167.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958PF UT WOS:000231459500005 ER PT J AU McKernan, B Yaqoob, T Reynolds, CS AF McKernan, B Yaqoob, T Reynolds, CS TI Constraints on hot metals in the vicinity of the Galaxy SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques : spectroscopic; galaxy : halo; galaxies : active; intergalactic medium; galaxies : Seyfert; X-rays : galaxies ID X-RAY FOREST; INTERGALACTIC MEDIUM; CHANDRA DETECTION; ABSORPTION-LINES; ALPHA ABSORPTION; GALACTIC-CENTER; GAS; BARYONS; SPECTROSCOPY; PKS-2155-304 AB We have searched for evidence of soft X-ray absorption by hot metals in the vicinity of the Galaxy in the spectra of a small sample of 15 type I active galactic nuclei (AGN) observed with the high-resolution X-ray gratings on board Chandra. This is an extension of our previous survey of hot O VII and O VIII absorbing gas in the vicinity of the Galaxy. The strongest absorption signatures within a few hundred km s(-1) of their rest-frame energies are most likely to be due to warm absorbing outflows from the nearest AGN, which are back-lighting the local hot gas. We emphasize that absorption signatures in the spectra of some distant AGN that are kinematically consistent with the recessional velocity of the AGN are most likely to be due to hot local gas. Along the sightline towards PG 1211+143, PDS 456 and MCG-6-30-15 there is a very large absorbing Fe column density which is kinematically consistent with absorption by hot, local Fe. The sightlines to these three AGN pass through the limb of the Northern Polar Spur (NPS), a local bubble formed from several supernovae which, if rich in Fe, may account for a large local Fe column. We obtain limits on the column density of local, highly ionized N, Ne, Mg, Si along all of the sightlines in our sample. We correlate the column density limits with those of highly ionized 0 along the same sightlines. Assuming the hot local gas is in collisionally ionized equilibrium, we obtain limits on the temperature and relative abundances of the metals in the hot local gas. Our limits on the ionic column densities in the local hot gas seem to be consistent with those observed in the hot halo gas of edge-on normal spiral galaxies. C1 Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP McKernan, B (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM mckernan@astro.umd.edu NR 42 TC 25 Z9 25 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 21 PY 2005 VL 361 IS 4 BP 1337 EP 1344 DI 10.1111/j.1365-2966.2005.09291.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958PF UT WOS:000231459500021 ER PT J AU Staguhn, JG Stern, D Benford, DJ Bertoldi, F Djorgovski, SG Thompson, D AF Staguhn, JG Stern, D Benford, DJ Bertoldi, F Djorgovski, SG Thompson, D TI Near-infrared photometry of the high-redshift quasar RD J030117+002025: Evidence for a massive starburst at z=5.5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; galaxies : starburst; quasars : individual ( RD J030117+002025) ID DIGITAL SKY SURVEY; MM MAMBO/IRAM-30 M; DUST EMISSION; MOLECULAR GAS; ELEMENTAL ABUNDANCES; INTERSTELLAR DUST; STAR-FORMATION; 250 GHZ; GALAXIES AB With a redshift of z = 5.5 and an optical blue magnitude M(B) similar to-24.2 mag (similar to 4.5 x 10(12) L(circle dot)), RD J030117+ 002025 is the most distant, optically faint (M(B) > -26 mag) quasar known. Max-Planck Millimeter Bolometer (MAMBO) continuum observations at lambda 1: 2 mm (185 mu m rest frame) showed that this quasar has a far-infrared (FIR) luminosity comparable to its optical luminosity. We present near-infrared J- and K-band photometry obtained with the Near-Infrared Camera (NIRC) on the Keck I telescope, tracing the slope of the rest- frame ultraviolet (UV) spectrum of this quasar. The observed spectral index is close to the value of alpha(v) similar to-44 measured in composite spectra of optically bright SDSS quasars. It thus appears that the quasar does not suffer from strong dust extinction, which further implies that its low rest- frame UV luminosity is due to an intrinsically faint active galactic nucleus (AGN). The FIR to optical luminosity ratio is then much larger than that observed for themore luminous quasars, supporting the suggestion that the FIR emission is not powered by the AGN but by a massive starburst. C1 NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. Sci Syst & Applicat Inc, Lanham, MD 20706 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Bonn, Inst Radioastron, D-53121 Bonn, Germany. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. RP Staguhn, JG (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. EM staguhn@stars.gsfc.nasa.gov RI Benford, Dominic/D-4760-2012 OI Benford, Dominic/0000-0002-9884-4206 NR 30 TC 7 Z9 7 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2005 VL 629 IS 2 BP 633 EP 635 DI 10.1086/431665 PN 1 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 954MP UT WOS:000231159500003 ER PT J AU Dey, A Bian, C Soifer, BT Brand, K Brown, MJI Chaffee, FH Le Floc'h, E Hill, G Houck, JR Jannuzi, BT Rieke, M Weedman, D Brodwin, M Eisenhardt, P AF Dey, A Bian, C Soifer, BT Brand, K Brown, MJI Chaffee, FH Le Floc'h, E Hill, G Houck, JR Jannuzi, BT Rieke, M Weedman, D Brodwin, M Eisenhardt, P TI Discovery of a large similar to 200 kpc gaseous nebula at z approximate to 2.7 with the Spitzer Space Telescope SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : formation; galaxies : high-redshift; galaxies : starburst; HII regions ID ACTIVE GALACTIC NUCLEI; LYMAN BREAK GALAXIES; SPECTRAL ENERGY-DISTRIBUTIONS; SUPERMASSIVE BLACK-HOLES; LY-ALPHA EMISSION; ARRAY CAMERA IRAC; HIGH-REDSHIFT; RADIO GALAXIES; STANDARD STARS; SPECTROPHOTOMETRIC STANDARDS AB We report the discovery of a very large, spatially extended Ly alpha-emitting nebula at z=2.656 associated with a luminous mid-infrared source. The bright mid-infrared source (F-24 mu m=0.86 mJy) was first detected in observations made using the Spitzer Space Telescope. Existing broadband imaging data from the NOAO Deep Wide-Field Survey revealed the mid-infrared source to be associated with a diffuse, spatially extended, optical counterpart in the B-W band. Spectroscopy and further imaging of this target reveals that the optical source is an almost purely line-emitting nebula with little, if any, detectable diffuse continuum emission. The Ly alpha nebula has a luminosity of L-Ly alpha approximate to 1.7x10(44) ergs s(-1) and an extent of at least 20" (160 kpc). Its central approximate to 8" shows an ordered, monotonic velocity profile; interpreted as rotation, this region encloses a mass M approximate to 6x10(12) M circle dot. Several sources lie within the nebula. The central region of the nebula shows narrow (approximate to 365 km s(-1)) emission lines of C (IV) and He (II). The mid-infrared source is a compact object lying within the nebula but offset from the center by a projected distance of approximate to 2".5 ( 20 kpc), and likely to be an enshrouded AGN. A young star-forming galaxy lies near the northern end of the nebula. We suggest that the nebula is a site of recent multiple galaxy and AGN formation, with the spatial distribution of galaxies within the nebula perhaps tracking the formation history of the system. C1 Natl Opt Astron Observ, Tucson, AZ 85719 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. WM Keck Observ, Kamuela, HI 96743 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Dey, A (reprint author), Natl Opt Astron Observ, 950 N Cherry AVe, Tucson, AZ 85719 USA. EM dey@noao.edu RI Brown, Michael/B-1181-2015 OI Brown, Michael/0000-0002-1207-9137 NR 62 TC 93 Z9 93 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 AUG 20 PY 2005 VL 629 IS 2 BP 654 EP 666 DI 10.1086/430775 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 954MP UT WOS:000231159500005 ER PT J AU Netzer, H Lemze, D Kaspi, S George, IM Turner, TJ Lutz, D Boller, T Chelouche, D AF Netzer, H Lemze, D Kaspi, S George, IM Turner, TJ Lutz, D Boller, T Chelouche, D TI XMM-Newton spectroscopy of the starburst-dominated ultraluminous infrared galaxy NGC 6240 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : nuclei; galaxies : Seyfert; galaxies : starburst; quasars : emission lines ID GRATING SPECTROMETER OBSERVATIONS; ACTIVE GALACTIC NUCLEI; X-RAY-SPECTRUM; NGC 6240; ADAPTIVE OPTICS; STAR-FORMATION; EMISSION; CHANDRA; CONNECTION; NGC-1068 AB We present a new XMM-Newton observation of the ultraluminous infrared galaxy (ULIRG) NGC 6240. We analyze the reflecting grating spectrometer (RGS) data, as well as data from the other instruments, and find a starburst-dominated 0.5-3 keV spectrum with global properties resembling those observed in M82 but with a much higher luminosity. We show that the starburst region can be divided into an outer zone, beyond a radius of about 2.1 kpc, with a gas temperature of about 10(7) K, and a central region with temperatures in the range ( 2 6); 107 K. The gas in the outer region emits most of the observed O (VIII) Ly alpha line, and the gas in the inner region the emission lines of higher ionization ions, including a strong Fe (XXV) line. We also identify a small inner part, very close to the active nuclei, with typical Seyfert 2 properties, including a large amount of photoionized gas producing a strong Fe K alpha 6.4 keV line. The combined abundance, temperature, and emission measure analysis indicates supersolar Ne/O, Mg/O, Si/O, S/O, and possibly also Fe/O. The analysis suggests densities in the range of (0.07-0.28)epsilon(-1/2) cm(-3) and a total thermal gas mass of similar to 4 x 10(8) epsilon(1/2) M-circle dot, where epsilon is the volume filling factor. We used a simple model to argue that a massive starburst with an age of similar or equal to 2 x 10(7) yr can explain most of the observed properties of the source. NGC 6240 is perhaps the clearest case of an X-ray-bright luminous AGN that is in a merger and whose soft X-ray spectrum is dominated by a powerful starburst. C1 Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Wise Observ, IL-69978 Tel Aviv, Israel. Technion Israel Inst Technol, Dept Phys, IL-3200 Haifa, Israel. Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. NASA, Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. Inst Adv Study, Sch Nat Sci, Princeton, NJ 08540 USA. RP Netzer, H (reprint author), Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. EM netzer@wise.tau.ac.il NR 32 TC 25 Z9 25 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 AUG 20 PY 2005 VL 629 IS 2 BP 739 EP 749 DI 10.1086/431474 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 954MP UT WOS:000231159500012 ER PT J AU Graves, GJM Challis, PM Chevalier, RA Crotts, A Filippenko, AV Fransson, C Garnavich, P Kirshner, RP Li, W Lundqvist, P McCray, R Panagia, N Phillips, MM Pun, CJS Schmidt, BP Sonneborn, G Suntzeff, NB Wang, L Wheeler, JC AF Graves, GJM Challis, PM Chevalier, RA Crotts, A Filippenko, AV Fransson, C Garnavich, P Kirshner, RP Li, W Lundqvist, P McCray, R Panagia, N Phillips, MM Pun, CJS Schmidt, BP Sonneborn, G Suntzeff, NB Wang, L Wheeler, JC TI Limits from the Hubble Space Telescope on a point source in SN 1987A SO ASTROPHYSICAL JOURNAL LA English DT Review DE accretion, accretion disks; stars : neutron; supernovae : individual (SN 1987A) ID LARGE-MAGELLANIC-CLOUD; X-RAY PULSAR; SUPERNOVA REMNANT CTB-109; ROTATING MASSIVE STARS; NEUTRON-STAR; BLACK-HOLE; PRESUPERNOVA EVOLUTION; BEPPOSAX OBSERVATIONS; SPHERICAL ACCRETION; MAGNETIC-FIELDS AB We observed supernova 1987A ( SN 1987A) with the Space Telescope Imaging Spectrograph ( STIS) on the Hubble Space Telescope ( HST) in 1999 September and again with the Advanced Camera for Surveys ( ACS) on the HST in 2003 November. Our spectral observations cover ultraviolet ( UV) and optical wavelengths from 1140 to 10266 8, and our imaging observations cover UV and optical wavelengths from 2900 to 9650 angstrom. No point source is observed in the remnant. We obtain a limiting flux of F-opt <= 1. 6; 10(-14) ergs s(-1) cm(-2) in the wavelength range 2900 - 9650 angstrom for any continuum emitter at the center of the supernova remnant ( SNR). This corresponds to an intrinsic luminosity of L-opt <= 5 x 10(33) ergs s (-1). It is likely that the SNR contains opaque dust that absorbs UV and optical emission, resulting in an attenuation of similar to 35% due to dust absorption in the SNR. Correcting for this level of dust absorption would increase our upper limit on the luminosity of a continuum source by a factor of 1.54. Taking into account dust absorption in the remnant, we find a limit of L-opt 8 x 10(33) ergs s (-1). We compare this upper bound with empirical evidence from point sources in other supernova remnants and with theoretical models for possible compact sources. We show that any survivor of a possible binary systemmust be nomore luminous than an F6 main- sequence star. Bright young pulsars such as Kes 75 or the Crab pulsar are excluded by optical and X- ray limits on SN 1987A. Other nonplerionic X- ray point sources have luminosities similar to the limits on a point source in SN 1987A; RCW103 and Cas A are slightly brighter than the limits on SN 1987A, while Pup A is slightly fainter. Of the young pulsars known to be associated with SNRs, those with ages <= 5000 yr are all too bright in X- rays to be compatible with the limits on SN 1987A. Examining theoretical models for accretion onto a compact object, we find that spherical accretion onto a neutron star is firmly ruled out and that spherical accretion onto a black hole is possible only if there is a larger amount of dust absorption in the remnant than predicted. In the case of thin- disk accretion, our flux limit requires a small disk, no larger than 1010 cm, with an accretion rate no more than 0.3 times the Eddington accretion rate. Possible ways to hide a surviving compact object include the removal of all surrounding material at early times by a photon- driven wind, a small accretion disk, or very high levels of dust absorption in the remnant. It will not be easy to improve substantially on our optical- UV limit for a point source in SN 1987A, although we can hope that a better understanding of the thermal infrared emission will provide a more complete picture of the possible energy sources at the center of SN 1987A. C1 Univ Calif Santa Cruz, Dept Astron, UCO, Lick Observ, Santa Cruz, CA 95064 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Columbia Univ, Astrophys Lab, Inst Strings Cosmol & Astroparticle Phys, New York, NY 10027 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Stockholm Univ, Dept Astron, Stockholm Observ, AlbaNova, SE-10691 Stockholm, Sweden. Univ Notre Dame, Dept Phys & Astron, Notre Dame, IN 46556 USA. Univ Colorado, Joint Inst Lab Astrophys, Boulder, CO 80309 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. NASA, Goddard Space Flight Ctr, Lab Astron & Space Phys, Greenbelt, MD 20771 USA. Mt Stromlo & Siding Spring Observ, Canberra, ACT 2611, Australia. Cerro Tololo Interamer Observ, La Serena, Chile. Univ Calif Berkeley, Lawrence Berkeley Lab, Inst Nucl & Particle Astrophys, Berkeley, CA 94720 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. RP Graves, GJM (reprint author), Univ Calif Santa Cruz, Dept Astron, UCO, Lick Observ, Santa Cruz, CA 95064 USA. EM graves@astro.ucsc.edu OI Schmidt, Brian/0000-0001-6589-1287; Schmidt, Brian/0000-0002-8538-9195 NR 109 TC 41 Z9 41 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2005 VL 629 IS 2 BP 944 EP 959 DI 10.1086/431422 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 954MP UT WOS:000231159500032 ER PT J AU Woods, PM Kouveliotou, C Gavriil, FP Kaspi, VM Roberts, MSE Ibrahim, A Markwardt, CB Swank, JH Finger, MH AF Woods, PM Kouveliotou, C Gavriil, FP Kaspi, VM Roberts, MSE Ibrahim, A Markwardt, CB Swank, JH Finger, MH TI X-ray bursts from the transient magnetar candidate XTE J1810-197 SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars : general; stars : individual (XTE J1810-197); X-rays : bursts ID SOFT GAMMA-REPEATERS; SGR 1900+14; NEUTRON-STARS; STATISTICAL PROPERTIES; PULSAR XTE-J1810-197; RADIATIVE MECHANISM; TIMING EXPLORER; SPIN-DOWN; EMISSION; SGR-1900+14 AB We have discovered four X- ray bursts, recorded with the Rossi X-ray Timing Explorer Proportional Counter Array between 2003 September and 2004 April, that we show to originate from the transient magnetar candidate XTE J1810 - 197. The burst morphologies consist of a short spike or multiple spikes lasting similar to 1 s each, followed by extended tails of emission where the pulsed flux from XTE J1810 - 197 is significantly higher. The burst spikes are likely correlated with the pulse maxima, having a chance probability of a random phase distribution of 0.4%. The burst spectra are best fitted to a blackbody with temperatures 4 - 8 keV, considerably harder than the persistent X- ray emission. During the X-ray tails following these bursts, the temperature rapidly cools as the flux declines, maintaining a constant emitting radius after the initial burst peak. During the brightest X- ray tail, we detect a narrow emission line at 12.6 keV, with an equivalent width of 1.4 keV and a probability of chance occurrence of less than 4 x 10(-6). The temporal and spectral characteristics of these bursts closely resemble the bursts seen from 1E 1048.1 - 5937 and a subset of the bursts detected from 1E 2259+ 586, thus establishing XTE J1810 - 197 as a magnetar candidate. The bursts detected from these three objects are sufficiently similar to one another, yet significantly different from those seen from soft gamma repeaters, that they likely represent a new class of bursts from magnetar candidates exclusive ( thus far) to the anomalous X-ray pulsar- like sources. C1 Univ Space Res Assoc, Columbia, MD 21044 USA. Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. George Washington Univ, Dept Phys, Washington, DC 20052 USA. NASA, Goddard Space Flight Ctr, LHEA, Greenbelt, MD 20771 USA. RP Woods, PM (reprint author), Univ Space Res Assoc, Columbia, MD 21044 USA. EM peter.woods@nsstc.nasa.gov RI Ibrahim, Alaa/A-6250-2008; Swank, Jean/F-2693-2012 OI Ibrahim, Alaa/0000-0002-8791-7270; NR 41 TC 65 Z9 65 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2005 VL 629 IS 2 BP 985 EP 997 DI 10.1086/431476 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 954MP UT WOS:000231159500036 ER PT J AU Verner, E Bruhweiler, F Nielsen, KE Gull, TR Kober, GV Corcoran, M AF Verner, E Bruhweiler, F Nielsen, KE Gull, TR Kober, GV Corcoran, M TI Discovery of CH and OH in the-513 km s(-1) ejecta of eta Carinae SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; ISM : molecules; stars : individual (eta Carinae); ultraviolet : stars ID PHOTODISSOCIATION REGIONS; MOLECULE FORMATION; INFRARED-EMISSION; HOMUNCULUS NEBULA; ABSORPTION; SPECTROSCOPY; ULTRAVIOLET; ABUNDANCES; CLOUDS; GAS AB The very massive star eta Carinae ( eta Car) is enshrouded in an unusual complex of stellar ejecta, which is highly depleted in C and O and enriched in He and N. This circumstellar gas gives rise to distinct absorption components corresponding to at least 20 different velocities along the line of sight. The velocity component at - 513 km s(-1) exhibits very low ionization with predominantly neutral species of iron-peak elements. Our statistical equilibrium/photoionization modeling indicates that the low temperature ( T= 760 K) and high density ( n(H) similar to 10(7) cm(-3)) of the - 513 km s(-1) component is conducive to molecule formation including those with the elements C and O. Examination of echelle spectra obtained with the Space Telescope Imaging Spectrograph (STIS) on board the Hubble Space Telescope ( HST) confirms the model's predictions. The molecules H-2, CH, and most likely OH have been identified in the - 513 km s(-1) absorption spectrum. This paper presents the analysis of the HST STIS spectra with the deduced column densities for CH, OH, and C (I) and an upper limit for CO. It is quite extraordinary to see molecular species in a cool environment at such a high velocity. The sharp molecular and ionic absorptions in this extensively CNO-processed material offer us a unique environment for studying the chemistry, dust formation processes, and nucleosynthesis in the ejected layers of a highly evolved massive star. C1 NASA, Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA. Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. Univ Dist Columbia, Dept Engn Architecture & Aerosp Technol, Washington, DC 20008 USA. Sci Syst & Applicat Inc, Lanham, MD 20706 USA. Univ Space Res Assoc, Seabrook, MD 20706 USA. RP Verner, E (reprint author), NASA, Goddard Space Flight Ctr, Explorat Universe Div, Code 667, Greenbelt, MD 20771 USA. EM kverner@fe2.gsfc.nasa.gov; fredb@iacs.gsfc.nasa.gov; nielsen@stis.gsfc.nasa.gov; theodore.r.gull@nasa.gov; gvieira@stis.gsfc.nasa.gov; corcoran@barnegat.gsfc.nasa.gov RI Gull, Theodore/D-2753-2012 OI Gull, Theodore/0000-0002-6851-5380 NR 37 TC 7 Z9 7 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2005 VL 629 IS 2 BP 1034 EP 1039 DI 10.1086/431917 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 954MP UT WOS:000231159500041 ER PT J AU Mattioda, AL Allamandola, LJ Hudgins, DM AF Mattioda, AL Allamandola, LJ Hudgins, DM TI The ultraviolet to near-infrared optical properties of polycyclic aromatic hydrocarbons: A semiempirical model SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; infrared : ISM; ISM : molecules; methods : laboratory; molecular processes; techniques : spectroscopic ID INTERSTELLAR DUST; EMISSION FEATURES; REFLECTION NEBULAE; SPECTROGRAPH IRS; SPECTROSCOPY; EXCITATION; SPECTRA; BANDS; GALAXIES; CARRIERS AB Interstellar polycyclic aromatic hydrocarbon (PAH) infrared emission features represent an important and unique diagnostic tool of the chemical and physical conditions throughout the universe. However, one challenge facing the widely accepted PAH emission model has been the detection of infrared features in regions of low UV flux. Using recently published laboratory near-infrared (NIR) PAH ion absorption data measured in our laboratory, we build on previous models for PAH ion absorption in the UV-visible to extrapolate a new model that incorporates PAH ion absorption in the NIR. This model provides a basis for comparing the relative energy absorption of PAH ions in the UV-visible and NIR regions for a wide variety of stellar types. This model demonstrates that the radiation from late-type stars can pump the mid-IR PAH features. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. SETI Inst, Mountain View, CA 94043 USA. RP Mattioda, AL (reprint author), NASA, Ames Res Ctr, Mail Stop 245-6, Moffett Field, CA 94035 USA. EM amattioda@mail.arc.nasa.gov NR 29 TC 37 Z9 37 U1 0 U2 7 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2005 VL 629 IS 2 BP 1183 EP 1187 DI 10.1086/431303 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 954MP UT WOS:000231159500054 ER PT J AU Mattioda, AL Hudgins, DM Allamandola, LJ AF Mattioda, AL Hudgins, DM Allamandola, LJ TI Experimental near-infrared spectroscopy of polycyclic aromatic hydrocarbons between 0.7 and 2.5 mu m SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; dust, extinction; ISM : general; ISM : molecules; molecular data ID DIFFUSE INTERSTELLAR BANDS; ELECTRONIC ABSORPTION-SPECTROSCOPY; DI-VALENT IONS; REFLECTION NEBULAE; RADICAL CATIONS; EMISSION BANDS; BENDING MODES; MONO-VALENT; SOLID ARGON; SPECTRA AB The near-infrared (NIR) spectra and absolute band strengths of 27 polycyclic aromatic hydrocarbon (PAH) cations and anions ranging in size from C14H10 to C50H22 are reported. The spectra of all the ionized PAHs we have studied to date have strong, broad absorption bands in the NIR. This work shows that ionized PAHs have significant absorption bands at wavelengths longer than predicted by the current astronomical models that consider PAHs in their treatment of the radiation balance of the interstellar medium. Two implications are (1) that ionized/open-shell interstellar PAHs should add weak, broadband structure to the NIR portion of the interstellar extinction curve and (2) that UV-poor radiation fields can pump the PAH emission bands, provided ionized/open-shell PAHs are present. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. SETI Inst, Mountain View, CA 94043 USA. RP Mattioda, AL (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 62 TC 45 Z9 45 U1 2 U2 8 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2005 VL 629 IS 2 BP 1188 EP 1210 DI 10.1086/430757 PN 1 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 954MP UT WOS:000231159500055 ER PT J AU Corbin, MR Vacca, WD Hibbard, JE Somerville, RS Windhorst, RA AF Corbin, MR Vacca, WD Hibbard, JE Somerville, RS Windhorst, RA TI Hubble Space Telescope imaging of the ultracompact blue dwarf galaxy HS 0822+3542: An assembling galaxy in a local void? SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : dwarf; galaxies : formation; galaxies : individual (HS 0822+3542); galaxies : starburst; galaxies : stellar content ID POPULATION SYNTHESIS; HII GALAXIES; STARBURST; STELLAR; MASS; CLUSTERS AB We present deep U-band, narrow V-band, and I-band images and photometry of the ultracompact blue dwarf HS 0822 + 3542 obtained with the Advanced Camera for Surveys/High Resolution Channel of the Hubble Space Telescope. This object is also extremely metal-poor [12 + log (O/H) = 7.45] and resides in a nearby void. The images resolve it into two physically separate components that were previously described as star clusters in a single galaxy. The primary component is only similar to 100 pc in maximum extent and consists of a starburst region surrounded by a ringlike structure of relatively redder stars. The secondary component is similar to 50 pc in size and lies at a projected distance of similar to 80 pc away from the primary, and is also actively star-forming. We estimate masses of similar to 10(7) and similar to 10(6) M(circle dot) for the two components based on their luminosities, with an associated dynamical timescale for the system of a few megayears. This timescale and the structure of the components suggest that a collision between them triggered their starbursts. The spectral energy distributions of both components can be fitted by the combination of a recent (a few megayears old) starburst and an evolved (several gigayears old) underlying stellar population, similar to larger blue compact dwarf galaxies. This indicates that despite its metal deficiency, the object is not forming its first generation of stars. However, the small sizes and masses of the two components suggest that HS 0822 + 3542 represents a dwarf galaxy in the process of assembling from clumps of stars intermediate in size between globular clusters and objects previously classified as galaxies. Its relatively high ratio of neutral gas mass to stellar mass (similar to 1) and high specific star formation rate, also log (SFR/M(circle dot)) similar or equal to -9.2, suggest that it is still converting much of its gas to stars. C1 Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA. NASA, Ames Res Ctr, Univ Space Res Assoc, Mountain View, CA 94025 USA. Natl Radio Astron Observ, Charlottesville, VA 22903 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Corbin, MR (reprint author), Arizona State Univ, Dept Phys & Astron, POB 871504, Tempe, AZ 85287 USA. EM michael.corbin@asu.edu; wvacca@mail.arc.nasa.gov; jhibbard@nrao.edu; somerville@stsci.edu; rogier.windhorst@asu.edu NR 24 TC 10 Z9 10 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2005 VL 629 IS 2 BP L89 EP L92 DI 10.1086/491581 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 954MT UT WOS:000231159900005 ER PT J AU Woo, R Habbal, SR AF Woo, R Habbal, SR TI Origin and acceleration of the slow solar wind SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; Sun : corona ID ULTRAVIOLET CORONAGRAPH SPECTROMETER; HELIOSPHERIC PLASMA SHEET; STREAMER BELT; INNER CORONA; TEMPERATURES; EVOLUTION; POLARITY; MINIMUM; FLOW AB This Letter uses Doppler dimming measurements by SOHO UVCS to elucidate the origin and acceleration of the slow solar wind. By investigating plasma flow in the corona over an active region during 2000 May 14-16, we confirm what has been suggested by the presence of the imprint of active regions in the solar wind near Earth orbit, that active regions are a source of slow wind. The observed active region does not have an associated streamer in the outer corona. We explain how this implies that any related heliospheric current sheet must be transverse to the line of sight. It is this favorable geometry of a transverse heliospheric current sheet that allows the plasma flow over the active region to be isolated in path-integrated Doppler dimming measurements. The results also show that acceleration of the slow wind associated with active regions toward its terminal speed is faster than that along the heliospheric current sheet. These differences in acceleration explain why the signatures of the heliospheric current sheet are dissimilar in velocity, but not in density, between the corona and solar wind measured near Earth orbit. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Woo, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 238-725, Pasadena, CA 91109 USA. EM richard.woo@jpl.nasa.gov; shadia@ifa.hawaii.edu NR 27 TC 13 Z9 13 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2005 VL 629 IS 2 BP L129 EP L132 DI 10.1086/447767 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 954MT UT WOS:000231159900015 ER PT J AU Rohen, G von Savigny, C Sinnhuber, M Llewellyn, EJ Kaiser, JW Jackman, CH Kallenrode, MB Schroter, J Eichmann, KU Bovensmann, H Burrows, JP AF Rohen, G von Savigny, C Sinnhuber, M Llewellyn, EJ Kaiser, JW Jackman, CH Kallenrode, MB Schroter, J Eichmann, KU Bovensmann, H Burrows, JP TI Ozone depletion during the solar proton events of October/November 2003 as seen by SCIAMACHY SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ULTRAVIOLET SPECTROMETER; MIDDLE ATMOSPHERE; LOWER MESOSPHERE; LIMB-SCATTERING; NITROGEN; MODEL; CLIMATOLOGY; TEMPERATURE; RETRIEVAL; SATELLITE AB [1] We use atmospheric ozone density profiles between 35 and 65 km altitude derived from SCIAMACHY limb measurements to quantify the ozone changes caused by the solar proton events from 26 October to 6 November 2003, known as the "Halloween storm.'' Detailed maps and daily resolved time series up to 5 weeks after the first event are compared with the results from a chemistry, transport, and photolysis model of the middle atmosphere that includes NOx and HOx production due to energetic particle precipitation. The general features of the ozone loss are captured by the model fairly well. A strong ozone depletion of more than 50% even deep into the stratosphere is observed at high geomagnetic latitudes in the Northern Hemisphere, whereas the observed ozone depletion in the more sunlit Southern Hemisphere is much weaker. Reasons for these interhemispheric differences are given. Two regimes can be distinguished, one above about 50 km dominated by HOx ( H, OH, HO2) driven ozone loss, one below about 50 km, dominated by NOx ( NO, NO2) driven ozone loss. The regimes display a different temporal evolution of ozone depletion and recovery. We observe for the first time an establishment of two contemporaneous maxima of ozone depletion at different altitudes, which solely can be explained by these regimes. C1 Univ Bremen, Inst Environm Phys, D-28359 Bremen, Germany. Univ Saskatchewan, Inst Space & Atmospher Studies, Dept Phys & Engn Phys, Saskatoon, SK S7N 5E2, Canada. Univ Zurich, Dept Geog, Remote Sensing Labs, CH-8057 Zurich, Switzerland. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Osnabruck, Dept Phys, D-49076 Osnabruck, Germany. RP Rohen, G (reprint author), Univ Bremen, Inst Environm Phys, Otto Hahn Allee 1, D-28359 Bremen, Germany. EM rohen@iup.physik.uni-bremen.de RI Sinnhuber, Miriam/A-7252-2013; Kaiser, Johannes/A-7057-2012; von Savigny, Christian/B-3910-2014; Jackman, Charles/D-4699-2012; Bovensmann, Heinrich/P-4135-2016; Burrows, John/B-6199-2014 OI Kaiser, Johannes/0000-0003-3696-9123; Bovensmann, Heinrich/0000-0001-8882-4108; Burrows, John/0000-0002-6821-5580 NR 43 TC 53 Z9 53 U1 3 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD AUG 20 PY 2005 VL 110 IS A9 AR A09S39 DI 10.1029/2004JA010984 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 957XO UT WOS:000231406900001 ER PT J AU Fuke, H Maeno, T Abe, K Haino, S Makida, Y Matsuda, S Matsumoto, H Mitchell, JW Moiseev, AA Nishimura, J Nozaki, M Orito, S Ormes, JF Sasaki, M Seo, ES Shikaze, Y Streitmatter, RE Suzuki, J Tanaka, K Tanizaki, K Yamagami, T Yamamoto, A Yamamoto, Y Yamato, K Yoshida, T Yoshimura, K AF Fuke, H Maeno, T Abe, K Haino, S Makida, Y Matsuda, S Matsumoto, H Mitchell, JW Moiseev, AA Nishimura, J Nozaki, M Orito, S Ormes, JF Sasaki, M Seo, ES Shikaze, Y Streitmatter, RE Suzuki, J Tanaka, K Tanizaki, K Yamagami, T Yamamoto, A Yamamoto, Y Yamato, K Yoshida, T Yoshimura, K TI Search for cosmic-ray antideuterons SO PHYSICAL REVIEW LETTERS LA English DT Article ID PRIMORDIAL BLACK-HOLES; CROSS-SECTIONS; PARTICLE ASTROPHYSICS; ANTIPROTON SPECTRUM; ONBOARD BESS; ENERGY; COLLISIONS; MATTER; MULTIPLICITIES; ANTIHELIUM AB We performed a search for cosmic-ray antideuterons using data collected during four BESS balloon flights from 1997 to 2000. No candidate was found. We derived, for the first time, an upper limit of 1.9x10(-4) (m(2)s sr GeV/nucleon)(-1) for the differential flux of cosmic-ray antideuterons, at the 95% confidence level, between 0.17 and 1.15 GeV/nucleon at the top of the atmosphere. C1 JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. Kobe Univ, Kobe, Hyogo 6578501, Japan. KEK, High Energy Accelerator Res Org, Tsukuba, Ibaraki 3050801, Japan. Univ Tokyo, Tokyo 1130033, Japan. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland, College Pk, MD 20742 USA. RP Fuke, H (reprint author), JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. EM fuke@balloon.isas.jaxa.jp OI Seo, Eun-Suk/0000-0001-8682-805X NR 33 TC 56 Z9 57 U1 0 U2 4 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 AUG 19 PY 2005 VL 95 IS 8 AR 081101 DI 10.1103/PhysRevLett.95.081101 PG 4 WC Physics, Multidisciplinary SC Physics GA 956OY UT WOS:000231310900010 PM 16196846 ER PT J AU Kim, TH Lee, GW Sieve, B Gangopadhyay, AK Hyers, RW Rathz, TJ Rogers, JR Robinson, DS Kelton, KF Goldman, AI AF Kim, TH Lee, GW Sieve, B Gangopadhyay, AK Hyers, RW Rathz, TJ Rogers, JR Robinson, DS Kelton, KF Goldman, AI TI In situ high-energy X-ray diffraction study of the local structure of supercooled liquid Si SO PHYSICAL REVIEW LETTERS LA English DT Article ID UNDERCOOLED MOLTEN SILICON; TRANSITIONS; DENSITY; SYSTEMS AB Employing the technique of electrostatic levitation, coupled with high-energy x-ray diffraction and rapid data acquisition methods, we have obtained high quality structural data more deeply into the supercooled regime of liquid silicon than has been possible before. No change in coordination number is observed in this temperature region, calling into question previous experimental claims of structural evidence for the existence of a liquid-liquid phase transition. C1 Washington Univ, Dept Phys, St Louis, MO 63130 USA. Iowa State Univ Sci & Technol, Ames Lab, USDOE, Ames, IA 50011 USA. Iowa State Univ Sci & Technol, Dept Phys & Astron, Ames, IA 50011 USA. Univ Massachusetts, Amherst, MA 01003 USA. Univ Alabama, Huntsville, AL 35899 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Washington Univ, Dept Phys, St Louis, MO 63130 USA. RI Hyers, Robert/G-3755-2010 NR 18 TC 49 Z9 51 U1 3 U2 15 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD AUG 19 PY 2005 VL 95 IS 8 AR 085501 DI 10.1103/PhysRevLett.95.085501 PG 4 WC Physics, Multidisciplinary SC Physics GA 956OY UT WOS:000231310900032 PM 16196868 ER PT J AU Brandon, AD Humayun, M Puchtel, IS Leya, I Zolensky, M AF Brandon, AD Humayun, M Puchtel, IS Leya, I Zolensky, M TI Osmium isotope evidence for an s-process carrier in primitive chondrites SO SCIENCE LA English DT Article ID EARLY SOLAR-SYSTEM; NEUTRON-CAPTURE; METEORITES; ABUNDANCES; NUCLEOSYNTHESIS; NEBULA; DIAMOND; STARS AB Osmium extracted from unequilibrated bulk chondrites has isotope anomalies consistent with an insoluble s-process carrier, termed Os(i) here. Osmium from metamorphosed bulk chondrites does not have isotope anomalies, implying that the Os(i) carrier was destroyed by metamorphism. The isotopic homogeneity of metamorphosed bulk chondrites is consistent with extremely effective mixing of presolar grains from varied sources in the nebula. Osmium in the Os(i) carrier is likely from nucleosynthetic sites with a neutron density about two to four times as high as that of the average solar s-process Os. C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Florida State Univ, Natl High Magnet Field Lab, Tallahassee, FL 32310 USA. Florida State Univ, Dept Geol Sci, Tallahassee, FL 32310 USA. Univ Maryland, Dept Geol, College Pk, MD 20742 USA. Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. RP Brandon, AD (reprint author), NASA, Lyndon B Johnson Space Ctr, Mail Stop KR, Houston, TX 77058 USA. EM alan.d.brandon1@jsc.nasa.gov NR 27 TC 70 Z9 71 U1 1 U2 5 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD AUG 19 PY 2005 VL 309 IS 5738 BP 1233 EP 1236 DI 10.1126/sciance.1115053 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 957TE UT WOS:000231395400043 PM 16109878 ER PT J AU Tagliaferri, G Goad, M Chincarini, G Moretti, A Campana, S Burrows, DN Perri, M Barthelmy, SD Gehrels, N Krimm, H Sakamoto, T Kumar, P Meszaros, PI Kobayashi, S Zhang, B Angelini, L Banat, P Beardmore, AP Capalbi, M Covino, S Cusumano, G Giommi, P Godet, O Hill, JE Kennea, JA Mangano, V Morris, DC Nousek, JA O'Brien, PT Osborne, JP Pagani, C Page, KL Romano, P Stella, L Wells, A AF Tagliaferri, G Goad, M Chincarini, G Moretti, A Campana, S Burrows, DN Perri, M Barthelmy, SD Gehrels, N Krimm, H Sakamoto, T Kumar, P Meszaros, PI Kobayashi, S Zhang, B Angelini, L Banat, P Beardmore, AP Capalbi, M Covino, S Cusumano, G Giommi, P Godet, O Hill, JE Kennea, JA Mangano, V Morris, DC Nousek, JA O'Brien, PT Osborne, JP Pagani, C Page, KL Romano, P Stella, L Wells, A TI An unexpectedly rapid decline in the X-ray afterglow emission of long gamma-ray bursts SO NATURE LA English DT Article ID TELESCOPE; BATSE; MODEL AB 'Long' gamma-ray bursts (GRBs) are commonly accepted to originate in the explosion of particularly massive stars, which give rise to highly relativistic jets. Inhomogeneities in the expanding flow result in internal shock waves that are believed to produce the gamma-rays we see(1,2). As the jet travels further outward into the surrounding circumstellar medium, 'external' shocks create the afterglow emission seen in the X-ray, optical and radio bands(1,2). Here we report observations of the early phases of the X-ray emission of five GRBs. Their X-ray light curves are characterised by a surprisingly rapid fall-off for the first few hundred seconds, followed by a less rapid decline lasting several hours. This steep decline, together with detailed spectral properties of two particular bursts, shows that violent shock interactions take place in the early jet outflows. C1 Osserv Astron Brera, INAF, I-23807 Merate, Italy. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. Univ Milan Bicocca, I-20126 Milan, Italy. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. ASI Sci Data Ctr, I-00044 Frascati, Italy. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Space Res Assoc, Columbia, MD 21044 USA. CNR, Washington, DC 20418 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Ist Astrofis Spaziale & Com, INAF, I-90146 Palermo, Italy. Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. RP Tagliaferri, G (reprint author), Osserv Astron Brera, INAF, Via Bianchi 46, I-23807 Merate, Italy. EM tagliaferri@merate.mi.astro.it RI Gehrels, Neil/D-2971-2012; Barthelmy, Scott/D-2943-2012; OI Campana, Sergio/0000-0001-6278-1576; giommi, paolo/0000-0002-2265-5003; Cusumano, Giancarlo/0000-0002-8151-1990; moretti, alberto/0000-0002-9770-0315; Tagliaferri, Gianpiero/0000-0003-0121-0723 NR 30 TC 199 Z9 203 U1 0 U2 7 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD AUG 18 PY 2005 VL 436 IS 7053 BP 985 EP 988 DI 10.1038/nature03934 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 955XQ UT WOS:000231263900042 PM 16107840 ER PT J AU Lauenstein, JM Barth, JL Sibeck, DG AF Lauenstein, JM Barth, JL Sibeck, DG TI Toward the development of new standard radiation belt and space plasma models for spacecraft engineering SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID ENVIRONMENT; ELECTRONS AB An international meeting on New Standard Radiation Belt and Space Plasma Models for Spacecraft Engineering, sponsored by NASA's Living With a Star Program, was held in 2004 to begin rebuilding the infrastructure required to develop new standard radiation belt and plasma environment models. The goal of one standard model will be accomplished in stages, including the formation of interim regional models, the calibration and incorporation of existing data sets, and the gathering of new data through future science missions. The Committee on Space Research/ Panel for Radiation Belt Environment Modeling will play a central role in standardization and data archiving. Workshop attendees support the standardization of two interim models: a model of geostationary orbit electrons and a model of inner belt protons. Two future missions are planned or are being planned to provide missing measurements and to increase the scientific understanding of the particle dynamics. This information will lead to more robust modeling of the particle environment for the design and operation of spacecraft for space exploration as well as for industry and military applications. C1 Muniz Engn Inc, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lauenstein, JM (reprint author), Muniz Engn Inc, Greenbelt, MD 20771 USA. EM Jean.Marie.Lauenstein@gsfc.nasa.gov RI Sibeck, David/D-4424-2012 NR 13 TC 1 Z9 1 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD AUG 17 PY 2005 VL 3 IS 8 AR S08B03 DI 10.1029/2005SW000160 PG 4 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 960VW UT WOS:000231622300001 ER PT J AU Yang, YL Gupta, MC Dudley, KL Lawrence, RW AF Yang, YL Gupta, MC Dudley, KL Lawrence, RW TI Conductive carbon nanoriber-polymer foam structures SO ADVANCED MATERIALS LA English DT Article ID INTERFERENCE SHIELDING EFFECTIVENESS; ELECTRICAL-PROPERTIES; COMPLEX PERMITTIVITY; COMPOSITES; POLYCARBONATE; POLYETHYLENE; COMPRESSION; FABRICS; FIBERS AB A novel foam structure of carbon nanofiber-polymer composite (see Figure) with improved electrical conductivity and percolation behavior is reported. Ibis foam structure is very promising for use as an effective electromagnetic-interference shielding material owing to its light weight, electrical conduction, and easy processability. C1 Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22904 USA. NASA, Langley Res Ctr, Electromagnet Res Branch, Hampton, VA 23681 USA. RP Gupta, MC (reprint author), Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22904 USA. EM mgupta@virginia.edu NR 31 TC 228 Z9 235 U1 13 U2 145 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0935-9648 J9 ADV MATER JI Adv. Mater. PD AUG 16 PY 2005 VL 17 IS 16 BP 1999 EP + DI 10.1002/adma.200500615 PG 6 WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA 956WO UT WOS:000231331000017 ER PT J AU Chen, JL Wilson, CR Famiglietti, JS Rodell, M AF Chen, JL Wilson, CR Famiglietti, JS Rodell, M TI Spatial sensitivity of the Gravity Recovery and Climate Experiment (GRACE) time-variable gravity observations SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID FIELD; VARIABILITY; ROTATION; SYSTEM AB We analyze the spatial sensitivities of terrestrial water storage and geoid height changes determined from the time- variable gravity observed by the Gravity Recovery and Climate Experiment ( GRACE) twin satellite mission. On the basis of 15 GRACE monthly gravity solutions, covering the period April 2002 to December 2003, we examine the effects of spatial smoothing at radii varying from 400 to 2000 km and conclude that a 800 km Gaussian smoothing radius is effective for GRACE- derived terrestrial water storage and produces the minimum RMS residuals over the land of the differences between GRACE results and estimated water storage change from a global land data assimilation system. For GRACE estimated geoid height change, the effective smoothing radius can go down to 600 km. When the annual ( e. g., the sine and cosine) components are the primary concern, the effective spatial resolution can reach 600 and 400 km for GRACE estimated terrestrial water storage or geoid height change, respectively. C1 Univ Texas, Ctr Space Res, Austin, TX 78759 USA. Univ Texas, Dept Geol Sci, Austin, TX 78712 USA. Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. RP Chen, JL (reprint author), Univ Texas, Ctr Space Res, 3925 W Braker Lane,Suite 200, Austin, TX 78759 USA. EM chen@csr.utexas.edu RI Rodell, Matthew/E-4946-2012 OI Rodell, Matthew/0000-0003-0106-7437 NR 16 TC 55 Z9 65 U1 4 U2 15 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 AUG 16 PY 2005 VL 110 IS B8 AR B08408 DI 10.1029/2004JB003536 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 957XH UT WOS:000231406200006 ER PT J AU Canzian, A Mosca, HO Bozzolo, G AF Canzian, A Mosca, HO Bozzolo, G TI Modeling of Fe growth on Mo(110) SO APPLIED SURFACE SCIENCE LA English DT Article DE thin film growth; computer simulations; iron; molybdenum; semi-empirical methods and model calculations ID EPITAXIAL-GROWTH; SURFACE ALLOYS; FILMS; FE(110); W(110); MONOLAYER; SYSTEMS AB Atomistic modeling of Fe deposition of Mo growth using the BFS method for alloys describes the early stages of the formation of ultrathin Fe films on refractory metal substrates (Mo). Atom-by-atorn analysis and Monte Carlo simulations are used to examine the composition of the islands with increasing Fe coverage. Experimentally known features for submonolayer coverage are successfully reproduced and explained. Beyond 1 ML, simulation results suggest that the stability of the Fe interlayer might be compromised, leading to the formation of islands with mixed composition. (c) 2004 Elsevier B.V. All rights reserved. C1 Ohio Aerosp Inst, Cleveland, OH 44142 USA. Univ Tecnol Nacl, FacReg Gral Pacheo, Pcia De Bs As, Argentina. UAM, Comis Nacl Energia Atom, San Martin, Argentina. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Bozzolo, G (reprint author), Ohio Aerosp Inst, 22800 Cedar Pt Rd, Cleveland, OH 44142 USA. EM guillermo.h.bozzolo@grc.nasa.gov NR 18 TC 2 Z9 2 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0169-4332 J9 APPL SURF SCI JI Appl. Surf. Sci. PD AUG 15 PY 2005 VL 249 IS 1-4 BP 97 EP 109 DI 10.1016/j.apsusc.2004.11.062 PG 13 WC Chemistry, Physical; Materials Science, Coatings & Films; Physics, Applied; Physics, Condensed Matter SC Chemistry; Materials Science; Physics GA 946XY UT WOS:000230607800016 ER PT J AU Ahn, JH Grant, SB Surbeck, CQ Digiacomo, PM Nezlin, NP Jiang, S AF Ahn, JH Grant, SB Surbeck, CQ Digiacomo, PM Nezlin, NP Jiang, S TI Coastal water quality impact of stormwater runoff from an urban watershed in southern California SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID FECAL INDICATOR BACTERIA; SANTA-MONICA BAY; POLYMERASE-CHAIN-REACTION; SURF ZONE; HUNTINGTON-BEACH; FIELD-MEASUREMENTS; ORANGE-COUNTY; POLLUTION; VARIABILITY; TRANSPORT AB Field studies were conducted to assess the coastal water quality impact of stormwater runoff from the Santa Ana River, which drains a large urban watershed located in southern California. Stormwater runoff from the river leads to very poor surf zone water quality, with fecal indicator bacteria concentrations exceeding California ocean bathing water standards by up to 500%. However, cross-shore currents (e.g., rip cells) dilute contaminated surf zone water with cleaner water from offshore, such that surf zone contamination is generally confined to < 5 km around the river outlet. Offshore of the surf zone, stormwater runoff ejected from the mouth of the river spreads out over a very large area, in some cases exceeding 100 km(2) on the basis of satellite observations. Fecal indicator bacteria concentrations in these large stormwater plumes generally do not exceed California ocean bathing water standards, even in cases where offshore samples test positive for human pathogenic viruses (human adenoviruses and enteroviruses) and fecal indicator viruses (F(+) coliphage). Multiple lines of evidence indicate that bacteria and viruses in the offshore stormwater plumes are either associated with relatively small particles (< 53 mu m) or not particle-associated. Collectively, these results demonstrate that stormwater runoff from the Santa Ana River negatively impacts coastal water quality, both in the surf zone and offshore. However, the extent of this impact, and its human health significance, is influenced by numerous factors, including prevailing ocean currents, within-plume processing of particles and pathogens, and the timing, magnitude, and nature of runoff discharged from river outlets over the course of a storm. C1 Univ Calif Irvine, Henry Samueli Sch Engn, Dept Chem Engn & Mat Sci, Irvine, CA 92697 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. So Calif Coastal Water Res Project, Westminster, CA 92683 USA. Univ Calif Irvine, Sch Social Ecol, Dept Environm Hlth Sci & Policy, Irvine, CA 92697 USA. RP Grant, SB (reprint author), Univ Calif Irvine, Henry Samueli Sch Engn, Dept Chem Engn & Mat Sci, Irvine, CA 92697 USA. EM sbgrant@uci.edu RI DiGiacomo, Paul/F-5584-2010; Jiang, Sunny/H-7702-2012; Grant, Stanley/K-8179-2016 OI DiGiacomo, Paul/0000-0003-4550-1899; Jiang, Sunny/0000-0002-4993-8038; Grant, Stanley/0000-0001-6221-7211 NR 43 TC 84 Z9 85 U1 5 U2 50 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD AUG 15 PY 2005 VL 39 IS 16 BP 5940 EP 5953 DI 10.1021/es0501464 PG 14 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 955CR UT WOS:000231203100010 PM 16173550 ER PT J AU Hu, YY Tung, KK Liu, JP AF Hu, YY Tung, KK Liu, JP TI A closer comparison of early and late-winter atmospheric trends in the northern hemisphere SO JOURNAL OF CLIMATE LA English DT Article ID PLANETARY WAVE ACTIVITY; GREENHOUSE GASES; OZONE DEPLETION; ARCTIC OSCILLATION; PROJECTED CHANGES; CLIMATE TRENDS; UNITED-STATES; ANNULAR MODE; CIRCULATION; PRECIPITATION AB Decadal trends are compared in various fields between Northern Hemisphere early winter, November-December (ND), and late-winter, February-March (FM), months using reanalysis data. It is found that in the extratropics and polar region the decadal trends display nearly opposite tendencies between ND and FM during the period from 1979 to 2003. Dynamical trends in late winter (FM) reveal that the polar vortex has become stronger and much colder and wave fluxes from the troposphere to the stratosphere are weaker, consistent with the positive trend of the Arctic Oscillation (AO) as found in earlier studies, while trends in ND appear to resemble a trend toward the low-index polarity of the AO. In the Tropics, the Hadley circulation shows significant intensification in both ND and FM, with stronger intensification in FM. Unlike the Hadley cell, the Ferrel cell shows opposite trends between ND and FM, with weakening in ND and strengthening in FM. Comparison of the observational results with general circulation model simulations is also discussed. C1 Peking Univ, Dept Atmospher Sci, MOE Key Lab Severe Storm & Flood Disasters, Beijing 100871, Peoples R China. Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY USA. Columbia Univ, Ctr Climate Syst Res, New York, NY USA. Univ Washington, Dept Appl Math, Seattle, WA 98195 USA. Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. RP Hu, YY (reprint author), Peking Univ, Dept Atmospher Sci, MOE Key Lab Severe Storm & Flood Disasters, Beijing 100871, Peoples R China. EM yyhu@pku.edu.cn RI Hu, Yongyun /B-6786-2016; LIU, JIPING/N-6696-2016 OI Hu, Yongyun /0000-0002-4003-4630; NR 37 TC 19 Z9 23 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 AUG 15 PY 2005 VL 18 IS 16 BP 3204 EP 3216 DI 10.1175/JCLI3468.1 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 966VT UT WOS:000232051600008 ER PT J AU Bromwich, DH Toracinta, ER Oglesby, RJ Fastook, JL Hughes, TJ AF Bromwich, DH Toracinta, ER Oglesby, RJ Fastook, JL Hughes, TJ TI LGM summer climate on the southern margin of the Laurentide Ice Sheet: Wet or dry? SO JOURNAL OF CLIMATE LA English DT Article ID LAST GLACIAL MAXIMUM; POLAR MM5 SIMULATIONS; MESOSCALE PREDICTION SYSTEM; GENERAL-CIRCULATION MODEL; FINITE-ELEMENT MODEL; NORTH-AMERICA; REGIONAL CLIMATE; BOREAL FOREST; CONVECTIVE PARAMETERIZATION; ATMOSPHERIC CIRCULATION AB Regional climate simulations are conducted using the Polar fifth-generation Pennsylvania State University (PSU)-NCAR Mesoscale Model (MM5) with a 60-km horizontal resolution domain over North America to explore the summer climate of the Last Glacial Maximum (LGM: 21 000 calendar years ago), when much of the continent was covered by the Laurentide Ice Sheet (LIS). Output from a tailored NCAR Community Climate Model version 3 (CCM3) simulation of the LGM climate is used to provide the initial and lateral boundary conditions for Polar MM5. LGM boundary conditions include continental ice sheets, appropriate orbital forcing, reduced CO2 concentration, paleovegetation, modified sea surface temperatures, and lowered sea level. The simulated LGM summer climate is characterized by a pronounced low-level thermal gradient along the southern margin of the LIS resulting from the juxtaposition of the cold ice sheet and adjacent warm ice-free land surface. This sharp thermal gradient anchors the midtropospheric jet stream and facilitates the development of synoptic cyclones that track over the ice sheet, some of which produce copious liquid precipitation along and south of the LIS terminus. Precipitation on the southern margin is orographically enhanced as moist southerly low-level flow (resembling a contemporary, Great Plains low-level jet configuration) in advance of the cyclone is drawn up the ice sheet slope. Composites of wet and dry periods on the LIS southern margin illustrate two distinctly different atmospheric flow regimes. Given the episodic nature of the summer rain events, it may be possible to reconcile the model depiction of wet conditions on the LIS southern margin during the LGM summer with the widely accepted interpretation of aridity across the Great Plains based on geological proxy evidence. C1 Ohio State Univ, Byrd Polar Res Ctr, Polar Meteorol Grp, Columbus, OH 43210 USA. Ohio State Univ, Atmospher Sci Program, Dept Geog, Columbus, OH 43210 USA. NASA, George C Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Huntsville, AL 35812 USA. Univ Maine, Inst Quaternary & Climate Studies, Bangor, ME USA. RP Bromwich, DH (reprint author), Ohio State Univ, Byrd Polar Res Ctr, Polar Meteorol Grp, 1090 Carmack Rd, Columbus, OH 43210 USA. EM bromwich@polarmet1.mps.ohio-state.edu RI Bromwich, David/C-9225-2016 NR 63 TC 35 Z9 35 U1 0 U2 11 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 J9 J CLIMATE JI J. Clim. PD AUG 15 PY 2005 VL 18 IS 16 BP 3317 EP 3338 DI 10.1175/JCLI3480.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 966VT UT WOS:000232051600015 ER PT J AU Wright, R Carn, SA Flynn, LP AF Wright, R Carn, SA Flynn, LP TI A satellite chronology of the May-June 2003 eruption of Anatahan volcano SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH LA English DT Article; Proceedings Paper CT Fall Meeting of the American-Geophysical-Union CY DEC 08-12, 2003 CL San Francisco, CA SP Amer Geophys Union DE Anatahan; remote sensing; MODIS; TOMS; ash; SO2 ID MODIS AB The first recorded eruption of Anatahan began at approximately 17:00 local time on May 10, 2003. Here, we present observations made by a suite of Earth-orbiting satellites of the heat, ash and gas emitted from the volcano before, during and after the eruption. No thermal or sulphur dioxide emissions are apparent in MODIS (Moderate Resolution Imaging Spectroradiometer), AIRS (Atmospheric Infrared Sounder), EP TOMS (Earth Probe Total Ozone Mapping Spectrometer) and ASTER (Advanced Spaceborne Thermal Emission and Reflection Radiometer) satellite images acquired prior to the eruption. However, within 24 h of eruption onset, the University of Hawaii's near-real-time satellite thermal monitoring system 'MODVOLC' detected the eruption and confirmed Anatahan's eastern caldera as the center of the activity. Although the eruption was initially phreatic, it quickly transitioned into a magmatic phase that culminated in the emplacement of a dacitic lava dome. The onset of the magmatic phase is recorded by MODVOLC as an order of magnitude increase in the heat flux from the volcano after May 16, indicative of fresh lava at the surface, relative to low values (50-90 MW) observed during the initial phreatic phase. MODVOLC detected thermal emission from the volcano on a further 22 occasions during the next 2 weeks, allowing us to quantitatively document temporal variations in thermal output during the eruption. We use MODIS, EP TOMS and AIRS data to document ash and sulphur dioxide emissions from Anatahan covering the period May 10-June 13, 2003. Using daily satellite observations in conjunction with ground-based estimates, we arrive at a total SO2 discharge of similar to 0.51 Mt for the similar to 1 month of activity, of which similar to 0.11 Mt was emitted during activity on May 10-12. Decreases in measured SO2 flux prior to the observation of a lava dome on June 4 indicate that the emerging dome may have blocked the upper conduit and inhibited degassing during this period. A new episode of dome growth was detected by MODVOLC on April 12, 2004. So far, the level of thermal emission during the recent period of activity is substantially lower than that observed during the May-June 2003 eruption. (c) 2005 Elsevier B.V All rights reserved. C1 Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. Univ Maryland Baltimore Cty, NASA, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. RP Wright, R (reprint author), Univ Hawaii, Hawaii Inst Geophys & Planetol, 1680 E West Rd, Honolulu, HI 96822 USA. EM wright@higp.hawaii.edu NR 30 TC 27 Z9 27 U1 0 U2 6 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0377-0273 EI 1872-6097 J9 J VOLCANOL GEOTH RES JI J. Volcanol. Geotherm. Res. PD AUG 15 PY 2005 VL 146 IS 1-3 BP 102 EP 116 DI 10.1016/j.jvolgeores.2004.10.021 PG 15 WC Geosciences, Multidisciplinary SC Geology GA 962NC UT WOS:000231738500007 ER PT J AU Ziemke, JR Chandra, S Bhartia, PK AF Ziemke, JR Chandra, S Bhartia, PK TI A 25-year data record of atmospheric ozone in the Pacific from Total Ozone Mapping Spectrometer (TOMS) cloud slicing: Implications for ozone trends in the stratosphere and troposphere SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID COLUMN OZONE; SATELLITE MEASUREMENTS; NIMBUS-7 SBUV; DATA SETS; EL-NINO; RECOVERY; VARIABILITIES; CLIMATOLOGY; OSCILLATION; AEROSOL AB [1] The newly reprocessed solar backscatter ultraviolet (SBUV) and Total Ozone Mapping Spectrometer ( TOMS) version 8 data from 1979 to 2003 are used to estimate the seasonal cycle, latitude dependence, and long-term trends in ozone averaged over the Pacific region (120 degrees W to 120 degrees E) in three broad layers of the atmosphere: upper stratosphere ( 32 hPa and above), lower stratosphere ( 32 hPa to tropopause), and the troposphere. The ozone amount in these layers is derived by first determining stratospheric column ozone in the Pacific from TOMS using deep convective clouds, which are numerous in the region. Tropospheric column ozone (TCO) for the Pacific is then determined by taking the difference between total column ozone and stratospheric column ozone. This "cloud-slicing'' technique is extensively tested from the tropics extending to +/-60 degrees latitude using stratospheric ozone data from the Stratospheric Aerosol and Gas Experiment II instrument. The validity of the cloud-slicing technique in obtaining TCO is also tested using data from ozonesondes over a wide range of latitude. SBUV ozone profiles are used to measure upper stratospheric column ozone for the Pacific region. Lower stratospheric column ozone is then derived from the difference between stratospheric column ozone and upper stratospheric column ozone. This process yields a unique 25-year record of Pacific mean ozone in three atmospheric layers covering all latitudes and seasons. The analysis of the data shows that the seasonal cycles, latitude dependence, and trends in these layers are substantially different. Over the 25-year record most ozone depletion has occurred in the lower stratosphere below similar to 25 km altitude. In middle and high latitudes, ozone losses are 3 - 4 times larger in the lower stratosphere compared with the upper stratosphere, even though the ozone amounts in the two regions are about the same. For the troposphere, TCO shows a statistically significant upward trend in the midlatitudes of both hemispheres but not in the tropics. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Goddard Earth Sci & Technol Ctr, Baltimore, MD USA. RP NASA, Goddard Space Flight Ctr, Code 916, Greenbelt, MD 20771 USA. EM ziemke@jwocky.gsfc.nasa.gov RI Bhartia, Pawan/A-4209-2016 OI Bhartia, Pawan/0000-0001-8307-9137 NR 49 TC 39 Z9 42 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 13 PY 2005 VL 110 IS D15 AR D15105 DI 10.1029/2004JD005687 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 957PD UT WOS:000231381700003 ER PT J AU Keller, KA Fok, MC Narock, A Hesse, M Rastaetter, L Kuznetsova, MM Gombosi, TI DeZeeuw, DL AF Keller, KA Fok, MC Narock, A Hesse, M Rastaetter, L Kuznetsova, MM Gombosi, TI DeZeeuw, DL TI Effect of multiple substorms on the buildup of the ring current SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID INNER PLASMA SHEET; MAGNETIC STORM; PHASE; MODEL; SIMULATION; ORBIT AB [1] The effect of magnetospheric substorms on the ring current is not completely understood. Using a combination of the University of Michigan's BAT-S-RUS Model and Fok Ring Current Model, we modeled the effects of multiple substorms on the ring current by modeling multiple dipolarizations in the tail. Increasing the number of substorms corresponds to increases in the number of injections into the ring current. The ionospheric potential increases during periods of southward IMF. Energy increases are more dependent on the duration of large ionospheric potential than the number of substorm dipolarizations. C1 NASA, Goddard Space Flight Ctr, SP Syst Inc, Greenbelt, MD 20771 USA. Univ Michigan, Space Phys Res Lab, Ann Arbor, MI 48109 USA. RP Keller, KA (reprint author), 13815H Braddock Springs Rd, Centreville, VA 20121 USA. EM mei-ching.h.fok@nasa.gov RI De Zeeuw, Darren/F-3667-2011; Hesse, Michael/D-2031-2012; Rastaetter, Lutz/D-4715-2012; Kuznetsova, Maria/F-6840-2012; Fok, Mei-Ching/D-1626-2012; Gombosi, Tamas/G-4238-2011 OI Rastaetter, Lutz/0000-0002-7343-4147; Gombosi, Tamas/0000-0001-9360-4951 NR 22 TC 5 Z9 6 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD AUG 13 PY 2005 VL 110 IS A8 AR A08202 DI 10.1029/2004JA010747 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 957PR UT WOS:000231383400001 ER PT J AU Patra, PK Behera, SK Herman, JR Maksyutov, S Akimoto, H Yamagata, T AF Patra, PK Behera, SK Herman, JR Maksyutov, S Akimoto, H Yamagata, T TI The Indian summer monsoon rainfall: interplay of coupled dynamics, radiation and cloud microphysics SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID DIPOLE; OCEAN AB The Indian summer monsoon rainfall (ISMR), which has a strong connection to agricultural food production, has been less predictable by conventional models in recent times. Two distinct years 2002 and 2003 with lower and higher July rainfall, respectively, are selected to help understand the natural and anthropogenic influences on ISMR. We show that heating gradients along the meridional monsoon circulation are reduced due to aerosol radiative forcing and the Indian Ocean Dipole in 2002. An increase in the dust and biomass-burning component of the aerosols through the zonal monsoon circulation resulted in reduction of cloud droplet growth in July 2002. These conditions were opposite to those in July 2003 which led to an above average ISMR. In this study, we have utilized NCEP/NCAR reanalyses for meteorological data ( e. g. sea-surface temperature, horizontal winds, and precipitable water), NOAA interpolated outgoing long-wave radiation, IITM constructed all-India rainfall amounts, aerosol parameters as observed from the TOMS and MODIS satellites, and ATSR fire count maps. Based on this analysis, we suggest that monsoon rainfall prediction models should include synoptic as well as interannual variability in both atmospheric dynamics and chemical composition. C1 Frontier Res Ctr Global Change JAMSTEC, Yokohama, Kanagawa 2360001, Japan. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Tokyo, Dept Earth & Planetary Sci, Tokyo 1130033, Japan. RP Patra, PK (reprint author), Frontier Res Ctr Global Change JAMSTEC, Yokohama, Kanagawa 2360001, Japan. EM prabir@jamstec.go.jp RI Yamagata, Toshio/A-1807-2009; Behera, Swadhin/B-7839-2009; Maksyutov, Shamil/G-6494-2011; Patra, Prabir/B-5206-2009; OI Behera, Swadhin/0000-0001-8692-2388; Maksyutov, Shamil/0000-0002-1200-9577; Patra, Prabir/0000-0001-5700-9389; Herman, Jay/0000-0002-9146-1632 NR 26 TC 31 Z9 31 U1 1 U2 9 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PD AUG 12 PY 2005 VL 5 BP 2181 EP 2188 PG 8 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 954LS UT WOS:000231157200002 ER PT J AU Anbar, AD Arnold, GL Lyons, TW Barling, J AF Anbar, AD Arnold, GL Lyons, TW Barling, J TI Response to comment on "Molybdenum isotope evidence for widespread anoxia in mid-proterozoic oceans" SO SCIENCE LA English DT Editorial Material ID FRACTIONATION C1 Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. Arizona State Univ, Dept Chem & Biochem, Tempe, AZ 85287 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. Univ Calif Riverside, Dept Earth Sci, Riverside, CA 92521 USA. Univ British Columbia, Dept Earth & Ocean Sci, Vancouver, BC V5Z 1M9, Canada. RP Anbar, AD (reprint author), Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. EM anbar@asu.edu RI Arnold, Gail/A-5572-2010; Barling, Jane/F-9443-2015 NR 8 TC 0 Z9 0 U1 1 U2 14 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD AUG 12 PY 2005 VL 309 IS 5737 DI 10.1126/science.1105521 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 955MN UT WOS:000231230100020 ER PT J AU Stordal, F Myhre, G Stordal, EJG Rossow, WB Lee, DS Arlander, DW Svendby, T AF Stordal, F Myhre, G Stordal, EJG Rossow, WB Lee, DS Arlander, DW Svendby, T TI Is there a trend in cirrus cloud cover due to aircraft traffic? SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID HIGH-LEVEL CLOUDS; ISCCP; CONTRAILS; CLIMATE; IMPACT AB Trends in cirrus cloud cover have been estimated based on 16 years of data from ISCCP ( International Satellite Cloud Climatology Project). The results have been spatially correlated with aircraft density data to determine the changes in cirrus cloud cover due to aircraft traffic. The correlations are only moderate, as many other factors have also contributed to changes in cirrus. Still we regard the results to be indicative of an impact of aircraft on cirrus amount. The main emphasis of our study is on the area covered by the METEOSAT satellite to avoid trends in the ISCCP data resulting from changing satellite viewing geometry. In Europe, which is within the METEOSAT region, we find indications of a trend of about 1 - 2% cloud cover per decade due to aircraft, in reasonable agreement with previous studies. The positive trend in cirrus in areas of high aircraft traffic contrasts with a general negative trend in cirrus. Extrapolation in time to cover the entire period of aircraft operations and in space to cover the global scale yields a mean estimate of 0.03 Wm(-2) ( lower limit 0.01, upper limit 0.08 Wm(-2) ) for the radiative forcing due to aircraft induced cirrus. The mean is close to the value given by IPCC ( 1999) as an upper limit. C1 Univ Oslo, Dept Geosci, N-0316 Oslo, Norway. Norwegian Inst Air Res, Kjeller, Norway. NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Manchester Metropolitan Univ, Dept Geog & Environm Sci, Manchester M15 6BH, Lancs, England. RP Stordal, F (reprint author), Univ Oslo, Dept Geosci, N-0316 Oslo, Norway. EM frode.stordal@geo.uio.no RI Myhre, Gunnar/A-3598-2008; Rossow, William/F-3138-2015; OI Myhre, Gunnar/0000-0002-4309-476X; Stordal, Frode/0000-0002-5190-6473 NR 28 TC 44 Z9 45 U1 0 U2 0 PU EUROPEAN GEOSCIENCES UNION PI KATLENBURG-LINDAU PA MAX-PLANCK-STR 13, 37191 KATLENBURG-LINDAU, GERMANY SN 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PD AUG 11 PY 2005 VL 5 BP 2155 EP 2162 PG 8 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 954LP UT WOS:000231156900004 ER PT J AU Huba, JD Warren, HP Joyce, G Pi, X Iijima, B Coker, C AF Huba, JD Warren, HP Joyce, G Pi, X Iijima, B Coker, C TI Global response of the low-latitude to midlatitude ionosphere due to the Bastille Day flare SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SOLAR-FLARE; MODEL; REGION; SAMI2 AB The first global simulation study and comparison to data of the ionospheric effects associated with the enhanced EUV irradiance of the Bastille Day flare are presented. This is done by incorporating a time-dependent EUV spectrum, based on data and hydrodynamic modeling, into the NRL ionosphere model SAMI3. The simulation results indicate that the total electron content (TEC) increases to over 7 TEC units in the daytime, low-latitude ionosphere. In addition, it is predicted that the maximum density in the F-layer (NmF2) increases by 20% and that the height of the maximum electron density (HmF2) decreases by 20%. These results are explained by the increased ionization at altitudes < 400 km which increases TEC and NmF2 while decreasing HmF2. The results are in reasonably good agreement with data obtained from GPS satellites and the TOPEX satellite. C1 USN, Div Plasma Phys, Res Lab, Washington, DC 20375 USA. USN, Div Space Sci, Res Lab, Washington, DC 20375 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Praxis Inc, Alexandria, VA 22303 USA. RP Huba, JD (reprint author), USN, Div Plasma Phys, Res Lab, Code 6790, Washington, DC 20375 USA. EM huba@ppdu.nrl.navy.mil NR 15 TC 18 Z9 18 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 11 PY 2005 VL 32 IS 15 AR L15103 DI 10.1029/2005GL023291 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 957OQ UT WOS:000231380200005 ER PT J AU Glaze, LS Anderson, SW Stofan, ER Baloga, S Smrekar, SE AF Glaze, LS Anderson, SW Stofan, ER Baloga, S Smrekar, SE TI Statistical distribution of tumuli on pahoehoe flow surfaces: Analysis of examples in Hawaii and Iceland and potential applications to lava flows on Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID KILAUEA VOLCANO; MOUNT-ETNA; MAUNA-ULU; INFLATION; EMPLACEMENT; ERUPTION; ORIGIN; TUBES; FIELD AB [1] Spatial distributions of tumuli on lava flow surfaces can be quantitatively linked to subsurface inflation processes. Three distinct styles of flow emplacement are studied: ( 1) lava flows undergo inflation that changes as a function of space and time resulting in random spatial distributions of tumuli, ( 2) lava flows with preferred pathways result in systematic clustering of inflation features, and ( 3) established tubes or narrow pahoehoe flows produce chains of tumuli. Statistical analyses are required to distinguish between styles one and two. Comparison of the spatial distribution of tumuli on a portion of a lava flow at Mauna Ulu with the Poisson distribution indicates that tumuli are randomly distributed on the flow surface, typical of style one emplacement where small-scale topographic variability and low slope influence development of preferred pathways that evolve over time. At Thrainsskjoldur, direct statistical comparisons to the Poisson spatial distribution are inconclusive but nearest- neighbor analysis indicates significant clustering. An initially random spatial distribution is inferred that developed preferred pathways and systematic clustering of inflation features, as with style two. At Elysium Planitia on Mars, the flow margin is significantly deficient in inflation features, while away from the margin, the flow exhibits a random spatial distribution of tumuli typical of style one emplacement. The flow is interpreted as multiple units or a single flow that migrated in space during emplacement. At the 1843 flow on Mauna Loa, tumuli occur on a linear trend, consistent with style three emplacement. C1 Proxemy Res, Bowie, MD 20715 USA. Black Hills State Univ, Spearfish, SD 57799 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Proxemy Res, 14300 Gallant Fox Lane,Suite 225, Bowie, MD 20715 USA. EM lori@proxemy.com; steveanderson@bhsu.edu; ellen@proxemy.com; steve@proxemy.com; ssmrekar@mail1.jpl.nasa.gov RI Glaze, Lori/D-1314-2012 NR 16 TC 32 Z9 33 U1 0 U2 1 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 AUG 11 PY 2005 VL 110 IS B8 AR B08202 DI 10.1029/2004JB003564 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 957PJ UT WOS:000231382400001 ER PT J AU Ebihara, Y Fok, MC Sazykin, S Thomsen, MF Hairston, MR Evans, DS Rich, FJ Ejiri, M AF Ebihara, Y Fok, MC Sazykin, S Thomsen, MF Hairston, MR Evans, DS Rich, FJ Ejiri, M TI Ring current and the magnetosphere-ionosphere coupling during the superstorm of 20 November 2003 SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID FIELD-ALIGNED CURRENTS; TRANSPOLAR POTENTIAL SATURATION; ION-CYCLOTRON WAVES; ELECTRIC-FIELD; MAGNETIC STORM; GEOMAGNETIC STORMS; CURRENT DYNAMICS; MILLSTONE HILL; PLASMA SHEET; SOLAR-CYCLE AB [1] We investigated the impact on the terrestrial ring current of a coronal mass ejection (CME) and the associated magnetic cloud that severely disturbed the Earth's magnetosphere on 20 November 2003. This CME decreased the Dst index to - 472 nT, which makes it the second largest storm, based on the minimum Dst index values, observed between 1957 and 2004. Data from the DMSP, NOAA, and LANL satellites showed the unique characteristics of this storm; a polar cap potential that increased to at least 200 kV, a polar cap boundary that moved as low as about 60 degrees MLAT, a plasma sheet density that increased to 5 cm(-3) at L = 6.6 when the Dst index was near its minimum, and the inner edge of the plasma sheet ion population that penetrated into a region for which L <= 1.5. In order to study the dynamics of the ring current and the associated magnetosphere-ionosphere coupling, we performed a ring current simulation that computed the evolution of the phase space density of the ring current ions and the closure of the electric current between the magnetosphere and the ionosphere. Major results were as follows: ( 1) The ring current, in terms of the Dst index and the inner edge of the plasma sheet, can result from the enhancement of the convection electric field, given the polar cap potentials used in the model; ( 2) The solar wind particles probably penetrated quickly into the geosynchronous altitude on the nightside with a lag of about 80 min, resulting in further enhancement of the ring current; ( 3) Dense geocoronal neutral hydrogen or a large coefficient of pitch angle diffusion (> 10(-4) s(-1)) is probably needed to account for the rapid motion of the inner edge of the plasma sheet ( or the ring current) population to a higher L value; ( 4) Both the simulated and observed field-aligned current (FAC) distributions show multiple current sheets, rather than the normally expected two current sheets. Fluctuations in the polar cap potential and the plasma sheet density are believed to cause the multiple sheets of field-aligned currents; ( 5) The equatorward edge of the Region 2 type field-aligned currents was observed to expand as low as 40 degrees MLAT, which is consistent with the simulation; and ( 6) The convection pattern can be much more complicated than an average one due to a strong Region 2 FAC. A noticeable feature was the reversal of the zonal ionospheric plasma flow that emerged on the dawnside. In particular, a westward flow was observed in the equatorial region of the eastward plasma flow at dawn. Its speed had a local maximum of about 5 degrees equatorward of the flow reversal. The flow reversal is thought to have resulted from the relatively strong shielding electric field. C1 Natl Inst Polar Res, Itabashi Ku, Tokyo 1738515, Japan. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Univ Texas, Ctr Space Sci, Richardson, TX 75083 USA. NOAA, Space Environm Lab, Boulder, CO 80303 USA. USAF, Res Lab, Hanscom AFB, MA 01731 USA. RP Natl Inst Polar Res, Itabashi Ku, 1-9-10 Kaga, Tokyo 1738515, Japan. EM ebihara@nipr.ac.jp; mei-ching.h.fok@nasa.gov; sazykin@rice.edu; mthomsen@lanl.gov; hairston@utdallas.edu; david.s.evans@noaa.gov; frederick.rich@hanscom.af.mil; ejiri@nipr.ac.jp RI Fok, Mei-Ching/D-1626-2012; Sazykin, Stanislav/C-3775-2008; Ebihara, Yusuke/D-1638-2013; Moore, Thomas/D-4675-2012 OI Sazykin, Stanislav/0000-0002-9401-4248; Ebihara, Yusuke/0000-0002-2293-1557; Moore, Thomas/0000-0002-3150-1137 NR 73 TC 68 Z9 69 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD AUG 11 PY 2005 VL 110 IS A9 AR A09S22 DI 10.1029/2004JA010924 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 957PT UT WOS:000231383700001 ER PT J AU Espley, JR Cloutier, PA Crider, DH Brain, DA Acuna, MH AF Espley, JR Cloutier, PA Crider, DH Brain, DA Acuna, MH TI Low-frequency plasma oscillations at Mars during the October 2003 solar storm SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID GLOBAL SURVEYOR; MAGNETIC-FIELD; WIND; BOUNDARY AB [1] The powerful x-class flare which occurred on the Sun on 28 October 2003 had important effects on plasma environments throughout the solar system. We present here observations of the effects at Mars from the Mars Global Surveyor (MGS) Magnetometer/ Electron Reflectometer experiment. In particular we focus on the changes in the nature of the magnetic oscillations observed at an altitude of 400 km (MGS's current orbital altitude) during the passage of the solar storm. We find that strong, regular oscillations are observed in both the B-parallel to and B-perpendicular to components of the magnetic field at all solar zenith angles. We emphasize in particular the powerful, coherent oscillations observed in the normally quiet nightside region. These oscillations carry power at the proton gyrofrequency and at and below the oxygen gyrofrequency. This implies that ions of planetary origin are interacting with the solar wind plasma and raises the possibility that significant atmospheric loss may occur during the passage of large solar storms at Mars. C1 Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA. Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20701 USA. RP Espley, JR (reprint author), Rice Univ, Dept Phys & Astron, MS-108, Houston, TX 77005 USA. EM espley@rice.edu; pac@spacibm.rice.edu; dcrider@lepvax.gsfc.nasa.gov; brain@ssl.berkeley.edu; mario.acuna@gsfc.nasa.gov RI Espley, Jared/I-5118-2013; Hurley, Dana/F-4488-2015 OI Espley, Jared/0000-0002-6371-9683; Hurley, Dana/0000-0003-1052-1494 NR 18 TC 16 Z9 16 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 AUG 11 PY 2005 VL 110 IS A9 AR A09S33 DI 10.1029/2004JA010935 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 957PT UT WOS:000231383700002 ER PT J AU Hickson, KM Keyser, LF AF Hickson, KM Keyser, LF TI A kinetic and product study of the Cl+HO2 reaction SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID PLUS CLO REACTION; REACTION CL&HO2; RATE-CONSTANT; HO2; TEMPERATURES; DEPENDENCE; CHLORINE; PRESSURE; RADICALS; ATOMS AB Absolute rate data and product branching ratios for the reactions Cl + HO2 -> HCl + O-2 (k(1a)) and Cl + HO2 -> OH + CIO (k(1b)) have been measured from 226 to 336 K at a total pressure of I Torr of helium using the discharge flow resonance fluorescence technique coupled with infrared diode laser spectroscopy. For kinetic measurements, pseudo-first-order conditions were used with both reagents in excess in separate experiments. HO2 was produced by two methods: through the termolecular reaction of H atoms with 02 and also by the reaction of F atoms with H2O2. Cl atoms were produced by a microwave discharge of Cl-2 in He. HO2 radicals were converted to OH radicals prior to detection by resonance fluorescence at 308 nm. Cl atoms were detected directly at 138 nm also by resonance fluorescence. Measurement of the consumption of HO2 in excess Cl yielded k1a and measurement of the consumption of Cl in excess HO2 yielded the total rate coefficient, k(1). Values of k(1a) and k(1) derived from kinetic experiments expressed in Arrhenius form are (1.6 +/- 0.2) x 10(-11) exp[(249 +/- 34)/T] and (2.8 +/- 0.1) x 10(-11) exp[(123 +/- 15)T] cm(3) molecule(-1) s(-1), respectively. As the expression for k(1) is only weakly temperature dependent, we report a temperature-independent value of k(1) = (4.5 +/- 0.4) x 10(-11) cm(3) molecule' s(-1). Additionally, an Arrhenius expression for k(1b) can also be derived: k(1b) = (7.7 +/- 0.8) x 10(-11) exp[-(708 +/- 29)/T] cm(3) molecule(-1) s(-1). These expressions for k(1a) and k1b are valid for 226 K :: T :! 336 and 256 K T : 296 K, respectively. The cited errors are at the level of a single standard deviation. For the product measurements, an excess of Cl was added to known concentrations of HO2 and the reaction was allowed to reach completion. HCI product concentrations were determined by IR absorption yielding the ratio k(1a)/k(1) over the temperature range 236 K <= T <= 296 K. OH product concentrations were determined by resonance fluorescence giving rise to the ratio k1blk, over the temperature range 226 K <= T <= 336 K. Both of these ratios were subsequently converted to absolute numbers. Values of k(1a) and k(1b) from the product experiments expressed in Arrhenius form are (1.5 +/- 0.1) x 10(-11) exp[(222 +/- 17)/T] and (10.6 +/- 1.5) x 10(-11) exp[-(733 +/- 41)/T] cm(3) molecule(-1) s(-1), respectively. These expressions for k(1a) and k(1b) are valid for 256 K <= T <= 296 and 226 K <= T <= 336 K, respectively. A combination of the kinetic and product data results in the following Arrhenius expressions for k(1a) and k(1b) of (1.4 +/- 0.3) x 10(-11) exp[(269 +/- 58)/T] and (12.7 +/- 4.1) x 10(-11) exp[-(801 +/- 94)/T] cm(3) molecule(-1) s(-1), respectively. Numerical simulations were used to check for interferences from secondary chemistry in both the kinetic and product experiments and also to quantify the losses incurred during the conversion process HO2 - OH for detection purposes. C1 CALTECH, Jet Prop Lab, Div Earth & Space Sci, Pasadena, CA 91109 USA. RP Hickson, KM (reprint author), CALTECH, Jet Prop Lab, Div Earth & Space Sci, Pasadena, CA 91109 USA. EM kevin.hickson@jpl.nasa.gov RI Hickson, Kevin/A-2443-2012 OI Hickson, Kevin/0000-0001-8317-2606 NR 26 TC 5 Z9 5 U1 0 U2 3 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 J9 J PHYS CHEM A JI J. Phys. Chem. A PD AUG 11 PY 2005 VL 109 IS 31 BP 6887 EP 6900 DI 10.1021/jp051176w PG 14 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 952YN UT WOS:000231042500014 PM 16834046 ER PT J AU Goldstein, ML AF Goldstein, ML TI Magnetospheric physics - Turbulence on a small scale SO NATURE LA English DT Editorial Material C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Goldstein, ML (reprint author), NASA, Goddard Space Flight Ctr, Code 612-2, Greenbelt, MD 20771 USA. EM melvyn.l.goldstein@nasa.gov RI Goldstein, Melvyn/B-1724-2008 NR 5 TC 6 Z9 6 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 AUG 11 PY 2005 VL 436 IS 7052 BP 782 EP 783 DI 10.1038/436782a PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 953XG UT WOS:000231116500026 PM 16094351 ER PT J AU Bonamente, M Lieu, R Mittaz, JPD Kaastra, JS Nevalainen, J AF Bonamente, M Lieu, R Mittaz, JPD Kaastra, JS Nevalainen, J TI Thermal and nonthermal nature of the soft excess emission from Sersic 159-03 observed with XMM-Newton SO ASTROPHYSICAL JOURNAL LA English DT Article DE large-scale structure of universe; X-rays : galaxies : clusters; X-rays : individual (Sersic 159-03) ID X-RAY EXCESS; HOT INTERGALACTIC MEDIUM; GALAXY CLUSTERS; SHOCK FRONTS; PKS 2155-304; BL LACERTAE; COSMIC-RAYS; BEPPOSAX; ACCELERATION; CONSTRAINTS AB Several nearby clusters exhibit an excess of soft X-ray radiation that cannot be attributed to the hot virialized intra-cluster medium. There is no consensus to date on the origin of the excess emission: it could be either of thermal origin or due to an inverse Compton scattering of the cosmic microwave background. Using high-resolution XMM-Newton data of Sersic 159-03 we first show that strong soft excess emission is detected out to a radial distance of 0.9 Mpc. The data are interpreted using the two viable models available, i.e., by invoking either a warm reservoir of thermal gas or relativistic electrons that are part of a cosmic-ray population. The thermal interpretation of the excess emission, slightly favored by the goodness-of-fit analysis, indicates that the warm gas responsible for the emission is high in mass and low in metallicity. C1 NASA, George C Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. SRON, Natl Inst Space Res, NL-3584 CA Utrecht, Netherlands. Univ Helsinki, Observatory, Tahtitornimaki 00014, Finland. RP Bonamente, M (reprint author), NASA, George C Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, 320 Sparkman Dr, Huntsville, AL 35805 USA. NR 42 TC 13 Z9 13 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 AUG 10 PY 2005 VL 629 IS 1 BP 192 EP 203 DI 10.1086/430776 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 952JK UT WOS:000230999600018 ER PT J AU Sakamoto, T Lamb, DQ Kawai, N Yoshida, A Graziani, C Fenimore, EE Donaghy, TQ Matsuoka, M Suzuki, M Ricker, G Atteia, JL Shirasaki, Y Tamagawa, T Torii, K Galassi, M Doty, J Vanderspek, R Crew, GB Villasenor, J Butler, N Prigozhin, G Jernigan, JG Barraud, C Boer, M Dezalay, JP Olive, JF Hurley, K Levine, A Monnelly, G Martel, F Morgan, E Woosley, SE Cline, T Braga, J Manchanda, R Pizzichini, G Takagishi, K Yamauchi, M AF Sakamoto, T Lamb, DQ Kawai, N Yoshida, A Graziani, C Fenimore, EE Donaghy, TQ Matsuoka, M Suzuki, M Ricker, G Atteia, JL Shirasaki, Y Tamagawa, T Torii, K Galassi, M Doty, J Vanderspek, R Crew, GB Villasenor, J Butler, N Prigozhin, G Jernigan, JG Barraud, C Boer, M Dezalay, JP Olive, JF Hurley, K Levine, A Monnelly, G Martel, F Morgan, E Woosley, SE Cline, T Braga, J Manchanda, R Pizzichini, G Takagishi, K Yamauchi, M TI Global characteristics of X-ray flashes and X-ray-rich gamma-ray bursts observed by HETE-2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts ID JET MODEL; ENERGY; BATSE; PERFORMANCE; UNIVERSAL; DISTRIBUTIONS; XRF-020903; AFTERGLOW; SPECTRA; CATALOG AB We describe and discuss the global properties of 45 gamma-ray bursts (GRBs) observed by HETE-2 during the first 3 years of its mission, focusing on the properties of X- ray flashes (XRFs) and X- ray - rich GRBs (XRRs). We find that the numbers of XRFs, XRRs, and GRBs are comparable, and that the durations and the sky distributions of XRFs and XRRs are similar to those of GRBs. We also find that the spectral properties of XRFs and XRRs are similar to those of GRBs, except that the values of the peak energy E(peak)(obs) of the burst spectrum in nu F(nu), the peak energy flux F(peak), and the energy fluence S(E) of XRFs are much smaller ( and those of XRRs are smaller) than those of GRBs. Finally, we find that the distributions of all three kinds of bursts form a continuum in the [S(E)(2 - 30 keV), S(E)(30 - 400) keV] plane, the [S(E)( 2 - 400 keV), E(peak)] plane, and the [F(peak)(50 - 300 keV), E(peak)] plane. These results provide strong evidence that all three kinds of bursts arise from the same phenomenon. C1 Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528551, Japan. RIKEN, Inst Phys & Chem Res, Wako, Saitama 3510198, Japan. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. Aoyama Gakuin Univ, Dept Phys, Setagaya Ku, Tokyo 1578572, Japan. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Natl Space Dev Agcy Japan, Tsukuba Space Ctr, Tsukuba, Ibaraki 3058505, Japan. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Observ Midi Pyrenees, Astrophys Lab, F-31400 Toulouse, France. Natl Astron Observ, Tokyo 1818588, Japan. Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Osaka 5600043, Japan. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. UPS, CNRS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France. Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, Brazil. Tata Inst Fundamental Res, Dept Astron & Astrophys, Bombay 400005, Maharashtra, India. INAF IASF, Sez Bologna, I-40129 Bologna, Italy. Miyazaki Univ, Fac Engn, Miyazaki 8892192, Japan. RP Sakamoto, T (reprint author), Tokyo Inst Technol, Dept Phys, Meguro Ku, 2-12-1 Ookayama, Tokyo 1528551, Japan. OI Boer, Michel/0000-0001-9157-4349 NR 32 TC 170 Z9 170 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2005 VL 629 IS 1 BP 311 EP 327 DI 10.1086/431235 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 952JK UT WOS:000230999600030 ER PT J AU Berger, E Fox, DB Kulkarni, SR Krzeminski, W Soderberg, AM Frail, DA Burrows, DN Cenko, SB Murphy, EJ Price, PA Gal-Yam, A Moon, DS Gehrels, N Freedman, WL Persson, SE Barthelmy, S Hill, JE Nousek, JA Moretti, A AF Berger, E Fox, DB Kulkarni, SR Krzeminski, W Soderberg, AM Frail, DA Burrows, DN Cenko, SB Murphy, EJ Price, PA Gal-Yam, A Moon, DS Gehrels, N Freedman, WL Persson, SE Barthelmy, S Hill, JE Nousek, JA Moretti, A TI The discovery of the optical and near-IR afterglows of the first swift gamma-ray bursts SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts ID EMISSION AB We present optical and near-infrared searches for afterglow emission from the first four Swift bursts with accurate positions from the X-Ray Telescope (XRT). Using telescopes at Las Campanas, Keck, and Palomar observatories, we rapidly identified and followed up afterglows for three of the four bursts and subsequently identified the redshift of GRB 050126 (z = 1.290). In three cases the burst positions were also observed with the Very Large Array, but no radio afterglow emission was detected. The optical/near-IR afterglows are fainter than about 70% of all afterglows detected to date, with GRB 050126 being the faintest, and were identified thanks to accurate and rapid positions from the XRT and rapid response with greater than or similar to 1 m telescopes. This suggests that the fraction of dust-obscured bursts is small, less than or similar to 20% when combined with afterglows localized by the HETE-2 Soft X-ray Camera. The X-ray fluxes are typical of the known population, with the exception of GRB 050126, which has the faintest X-ray afterglow to date ( normalized to Delta t = 10 hr) and was detected thanks to a response time of only 130 s after the burst. Finally, we find that all three optical/near-IR afterglows are located less than or similar to 2 '' away from the nominal XRT positions, suggesting that the XRT is capable of delivering highly accurate positions, which will revolutionize afterglow studies. C1 Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. Princeton Univ Observ, Princeton, NJ 08544 USA. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. Carnegie Observ, Campanas Observ, La Serena, Chile. Natl Radio Astron Observ, Socorro, NM 87801 USA. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Yale Univ, Dept Astron, New Haven, CT 06520 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Osserv Astron Brera, INAF, I-23807 Merate, Italy. RP Berger, E (reprint author), Observ Carnegie Inst Washington, 813 Santa Barbara St, Pasadena, CA 91101 USA. RI Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; OI moretti, alberto/0000-0002-9770-0315 NR 36 TC 21 Z9 21 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 AUG 10 PY 2005 VL 629 IS 1 BP 328 EP 333 DI 10.1086/431579 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 952JK UT WOS:000230999600031 ER PT J AU Pollock, AMT Corcoran, MF Stevens, IR Williams, PM AF Pollock, AMT Corcoran, MF Stevens, IR Williams, PM TI Bulk velocities, chemical composition, and ionization structure of the X-ray shocks in WR 140 near periastron as revealed by the Chandra gratings SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; shock waves; stars : abundances; stars : individual (WR 140); stars : winds, outflows; stars : Wolf-Rayet; X-rays : stars ID WIND BINARY WR-140; HELIUM-LIKE IONS; EARLY-TYPE STARS; SUPERNOVA-REMNANTS; LINE RATIOS; WC STARS; MULTIFREQUENCY VARIATIONS; RADIO OBSERVATIONS; EMISSION; SPECTRUM AB The Wolf-Rayet WC7+O4-5 binary WR 140 went through the periastron passage of its 8 yr eccentric binary orbit in early 2001 as the two stars made their closest approach. Both stars have powerful supersonic stellar winds that crash into each other between the stars to produce X-rays. Chandra grating observations were made when the X-rays were at their peak, making WR 140 the brightest hot-star X-ray source in the sky and giving the opportunity to study the velocity profiles of lines, all of which were resolved and blueshifted before periastron. In the general context of shock physics, the measurements constrain the flow of hot gas and where different ions were made. The brightness of lines relative to the strong continuum in conjunction with plasma models gives interim abundance estimates for eight different elements in WC-type material including an Ne/S ratio in good agreement with earlier long-wavelength measurements. The lower velocity widths of cool ions imply a plasma that was not in equilibrium, probably due to the collisionless nature of the shock transitions and the slow character of both the postshock energy exchange between ions and electrons and subsequent ionization. Electron heat conduction into fast-moving preshock gas was absent, probably suppressed by the magnetic field involved in WR 140's synchrotron emission. After periastron, the spectrum was weaker due mainly to absorption by cool Wolf-Rayet star material. C1 Univ Space Res Assoc, Seabrook, MD 20706 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. Comp & Sci Co Ltd, Sheffield S10 3GS, S Yorkshire, England. RP Pollock, AMT (reprint author), European Space Agcy, XMM Newton Sci Operat Ctr, European Space Astron Ctr, Apartado 50727, Madrid 28080, Spain. EM andy.pollock@esa.int NR 54 TC 71 Z9 71 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2005 VL 629 IS 1 BP 482 EP 498 DI 10.1086/431193 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 952JK UT WOS:000230999600045 ER PT J AU Uzpen, B Kobulnicky, HA Olsen, KAG Clemens, DP Laurance, TL Meade, MR Babler, BL Indebetouw, R Whitney, BA Watson, C Wolfire, MG Wolff, MJ Benjamin, RA Bania, TM Cohen, M Devine, KE Dickey, JM Heitsch, F Jackson, JM Marston, AP Mathis, JS Mercer, EP Stauffer, JR Stolovy, SR Backman, DE Churchwell, E AF Uzpen, B Kobulnicky, HA Olsen, KAG Clemens, DP Laurance, TL Meade, MR Babler, BL Indebetouw, R Whitney, BA Watson, C Wolfire, MG Wolff, MJ Benjamin, RA Bania, TM Cohen, M Devine, KE Dickey, JM Heitsch, F Jackson, JM Marston, AP Mathis, JS Mercer, EP Stauffer, JR Stolovy, SR Backman, DE Churchwell, E TI Identification of main-sequence stars with mid-infrared excesses using GLIMPSE: beta Pictoris analogs? SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; open clusters and associations : individual (Westerlund 2); planetary systems : formation ID SPITZER-SPACE-TELESCOPE; INFRARED ARRAY CAMERA; WOLF-RAYET STARS; OPEN CLUSTERS; SEARCH; WESTERLUND-2; DISCOVERY; RCW-49; DISK AB Spitzer IRAC 3.6-8 mu m photometry obtained as part of the GLIMPSE survey has revealed mid-infrared excesses for 33 field stars with known spectral types in a 1.2 deg(2) field centered on the southern Galactic H II region RCW49. These stars comprise a subset of 184 stars with known spectral classification, most of which were preselected to have unusually red IR colors. We propose that the mid-IR excesses are caused by circumstellar dust disks that are either very late remnants of stellar formation or debris disks generated by planet formation. Of these 33 stars, 29 appear to be main-sequence stars on the basis of optical spectral classifications. Five of the 29 main-sequence stars are O or B stars with excesses that can be plausibly explained by thermal bremsstrahlung emission, and four are post-main-sequence stars. The lone O star is an O4V((f)) at a spectrophotometric distance of 3233(-535)(+540) pc and may be the earliest member of the Westerlund 2 cluster. Of the remaining 24 main-sequence stars, 18 have spectral energy distributions that are consistent with hot dusty debris disks, a possible signature of planet formation. Modeling the excesses as blackbodies demonstrates that the blackbody components have fractional bolometric disk-to-star luminosity ratios, L-IR/L-*, ranging from 10(-3) to 10(-2) with temperatures ranging from 220 to 820 K. The inferred temperatures are more consistent with asteroid belts than with the cooler temperatures expected for Kuiper belts. Mid-IR excesses are found in all spectral types from late B to early K. C1 Univ Wyoming, Dept Phys & Astron, Dept 3905, Laramie, WY 82071 USA. Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. Space Sci Inst, Boulder, CO 80301 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Univ Wisconsin, Dept Phys, Whitewater, WI 53190 USA. Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. Univ Munich, Inst Astron & Astrophys, D-81679 Munich, Germany. European Space Agcy, Estec, SCI SA, NL-2200 AG Noordwijk, Netherlands. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. NASA, Ames Res Ctr, SOFIA, Moffett Field, CA 94035 USA. RP Uzpen, B (reprint author), Univ Wyoming, Dept Phys & Astron, Dept 3905, Laramie, WY 82071 USA. RI Dickey, John/C-6156-2013; Bania, Thomas/H-2318-2014; OI Dickey, John/0000-0002-6300-7459 NR 36 TC 23 Z9 23 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2005 VL 629 IS 1 BP 512 EP 525 DI 10.1086/431479 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 952JK UT WOS:000230999600048 ER PT J AU Yamauchi, Y Wang, H Jiang, Y Schwadron, N Moore, RL AF Yamauchi, Y Wang, H Jiang, Y Schwadron, N Moore, RL TI Study of H alpha macrospicules in coronal holes: Magnetic structure and evolution in relation to photospheric magnetic setting SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : chromosphere; Sun : corona; Sun : magnetic fields ID QUIET SUN; SOLAR SPICULES; ACTIVE REGIONS; MASS EJECTIONS; FLUX; CANCELLATION; NETWORK; FLARES; JETS AB Small-scale solar dynamic events such as spicules, macrospicules, and microflares may play an important role in the coronal heating and solar wind acceleration in coronal holes. In these regions, the network fields concentrated along edges of supergranules are probably the source of the fine-scale activity that may drive the heating and acceleration. Recent H alpha limb observations from Big Bear Solar Observatory (BBSO) have shown that most macrospicules have two different forms of magnetic structure - a spiked jet or an erupting loop, suggesting two different formation mechanisms. In this paper, we analyze BBSO H alpha images and magnetograms of a coronal hole region near the disk center to study the evolution of the two types of macrospicule in relation to the magnetic arrangement at their base. We identified 78 macrospicules from the best day of 3 days of observations. Of these, 65 events were in the form of a spiked jet and were rooted in compact bipolar fields at the edges of the magnetic network. This supports the idea that spiky macrospicules are driven by reconnection between the network bipole and open magnetic fields. We also found five macrospicules that were in the form of an erupting loop oriented along a neutral line between the positive and negative network flux. They appear to be minifilament eruptions. Our results verify the magnetic structure inferred from our previous limb observations and support scenarios of coronal heating and solar wind generation through fine-scale explosive reconnection events seated in the magnetic network. C1 New Jersey Inst Technol, Ctr Solar Terr Res, Newark, NJ 07102 USA. NAOC, Yunnan Observ, Kunming 650011, Peoples R China. SW Res Inst, San Antonio, TX 78238 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Yamauchi, Y (reprint author), New Jersey Inst Technol, Ctr Solar Terr Res, Univ Hts, Newark, NJ 07102 USA. EM yohei.yamauchi@njit.edu NR 35 TC 16 Z9 16 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2005 VL 629 IS 1 BP 572 EP 581 DI 10.1086/431664 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 952JK UT WOS:000230999600054 ER PT J AU Boselli, A Cortese, L Deharveng, JM Gavazzi, G Yi, KS de Paz, AG Seibert, M Boissier, S Donas, J Lee, YW Madore, BF Martin, DC Rich, RM Sohn, YJ AF Boselli, A Cortese, L Deharveng, JM Gavazzi, G Yi, KS de Paz, AG Seibert, M Boissier, S Donas, J Lee, YW Madore, BF Martin, DC Rich, RM Sohn, YJ TI UV properties of early-type galaxies in the Virgo Cluster SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : individual (Virgo); galaxies : elliptical and lenticular, cD; galaxies : evolution; ultraviolet : galaxies ID BAND SURFACE PHOTOMETRY; DWARF ELLIPTIC GALAXIES; TULLY-FISHER RELATION; STAR-FORMATION; S0 GALAXIES; STELLAR POPULATIONS; EVOLUTION-EXPLORER; SAMPLE; HISTORIES; CATALOG AB We study the UV properties of a volume-limited sample of early-type galaxies in the Virgo Cluster combining new GALEX far-ultraviolet (1530 angstrom) and near-ultraviolet (2310 angstrom) data with spectrophotometric data available at other wavelengths. The sample includes 264 elliptical, lenticular, and dwarf galaxies spanning a large range in luminosity (M-B greater than or equal to - 15). While the NUV to optical or near-IR color-magnitude relations (CMRs) are similar to those observed at optical wavelengths, with a monotonic reddening of the color index with increasing luminosity, the (FUV - V) and (FUV - H) CMRs show a discontinuity between massive and dwarf objects. An even more pronounced dichotomy is observed in the (FUV - NUV) CMR. For elliptical galaxies, the (FUV - NUV) color becomes bluer with increasing luminosity and with increasing reddening of the optical or near-IR color indices. For the dwarfs, the opposite trend is observed. These observational evidences are consistent with the idea that the UV emission is dominated by hot, evolved stars in giant systems, while in dwarf ellipticals residual star formation activity is more common. C1 Lab Astrophys Marseille, F-13376 Marseille, France. Univ Milan Bicocca, I-20126 Milan, Italy. Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. CALTECH, NASA IPAC Extragalact Database, Pasadena, CA 91125 USA. Yonsei Univ, Ctr Space Astrophys, Seoul 120749, South Korea. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. RP Boselli, A (reprint author), Lab Astrophys Marseille, BP8,Traverse Siphon, F-13376 Marseille, France. OI Cortese, Luca/0000-0002-7422-9823 NR 38 TC 58 Z9 58 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2005 VL 629 IS 1 BP L29 EP L32 DI 10.1086/444534 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 952JN UT WOS:000230999900008 ER PT J AU Jaffe, TR Banday, AJ Eriksen, HK Gorski, KM Hansen, FK AF Jaffe, TR Banday, AJ Eriksen, HK Gorski, KM Hansen, FK TI Evidence of vorticity and shear at large angular scales in the WMAP data: A violation of cosmological isotropy? SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmology : observations; methods : numerical ID MICROWAVE-ANISOTROPY-PROBE; POWER SPECTRUM ANALYSIS; SKY MAPS; ROTATION; SPHERE AB Motivated by the large-scale asymmetry observed in the cosmic microwave background sky, we consider a specific class of anisotropic cosmological models - Bianchi type VIIh - and compare them to the WMAP first-year data on large angular scales. Remarkably, we find evidence of a correlation that is ruled out as a chance alignment at the 3 sigma level. The best-fit Bianchi model corresponds to x = 0.55, Omega(o) = 0.5, a rotation axis in the direction ( l, b) = (222 degrees, -62 degrees), shear (sigma/H)(o) = 2.4 x 10(-10), and a right-handed vorticity (omega/H)(o) = 4.3 x 10(-10). Correcting for this component greatly reduces the significance of the large-scale power asymmetry, resolves several anomalies detected on large angular scales (i.e., the low quadrupole amplitude and quadrupole/octopole planarity and alignment), and can account for a non-Gaussian "cold spot" on the sky. Despite the apparent inconsistency with the best-fit parameters required in inflationary models to account for the acoustic peaks, we consider the results sufficiently provocative to merit further consideration. C1 Max Planck Inst Astrophys, D-85741 Garching, Germany. Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Jaffe, TR (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1,Postfach 1317, D-85741 Garching, Germany. EM tjaffe@mpa-garching.mpg.de; banday@mpa-garching.mpg.de; h.k.k.eriksen@astro.uio.no; krzysztof.m.gorski@jpl.nasa.gov; f.k.hansen@astro.uio.no NR 24 TC 166 Z9 169 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 AUG 10 PY 2005 VL 629 IS 1 BP L1 EP L4 DI 10.1086/444454 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 952JN UT WOS:000230999900001 ER PT J AU Yoo, BY Huang, CK Lim, JR Herman, J Ryan, MA Fleurial, JP Myung, NV AF Yoo, BY Huang, CK Lim, JR Herman, J Ryan, MA Fleurial, JP Myung, NV TI Electrochemically deposited thermoelectric n-type Bi2Te3 thin films SO ELECTROCHIMICA ACTA LA English DT Article DE bismuth; tellurium; electrodeposition; thermoelectric; microstructure ID TE ALLOY-FILMS; BISMUTH TELLURIDE; NANOWIRE ARRAYS; P-TYPE; ELECTRODEPOSITION; COEVAPORATION; SB2TE3 AB Electrochemically deposited n-type BiTe alloy thin films were grown from nitric acid baths on sputtered BixTey/SiO/Si substrates. The film compositions, which varied from 57 to 63 at.% Te were strongly dependent on the deposition conditions. Surface morphologies varied from needle-like to granular structures depending on deposited Te content. Electrical and thermoelectric properties of these electrodeposited BixTey thin films were measured before and after annealing and compared to those of bulk Bi2Te3. Annealing at 250 degrees C in reducing H-2 atmosphere enhanced thermoelectric properties by reducing film defects. In-plane electrical resistivity was highly dependent on composition and microstructure. In-plane Hall mobility decreased with increasing carrier concentration, while the magnitude of the Seebeck coefficient increased with increasing electrical conductivity to a maximum of -188.5 mu V/K. Overall, the thermoelectric properties of electrodeposited n-type BiTe thin films after annealing were comparable to those of bulk BiTe films. (c) 2005 Elsevier Ltd. All rights reserved. C1 Univ Calif Riverside, Dept Environm Chem & Engn, Riverside, CA 92521 USA. CALTECH, Jet Prop Lab, Mat & Device Technol Grp, Pasadena, CA 91109 USA. RP Myung, NV (reprint author), Univ Calif Riverside, Dept Environm Chem & Engn, Riverside, CA 92521 USA. EM myung@engr.ucr.edu NR 32 TC 139 Z9 141 U1 11 U2 138 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0013-4686 J9 ELECTROCHIM ACTA JI Electrochim. Acta PD AUG 10 PY 2005 VL 50 IS 22 BP 4371 EP 4377 DI 10.1016/j.electacta.2005.02.016 PG 7 WC Electrochemistry SC Electrochemistry GA 957EZ UT WOS:000231353800006 ER PT J AU Cohen, CMS Stone, EC Mewaldt, RA Leske, RA Cummings, AC Mason, GM Desai, MI von Rosenvinge, TT Wiedenbeck, ME AF Cohen, CMS Stone, EC Mewaldt, RA Leske, RA Cummings, AC Mason, GM Desai, MI von Rosenvinge, TT Wiedenbeck, ME TI Heavy ion abundances and spectra from the large solar energetic particle events of October-November 2003 SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ADVANCED COMPOSITION EXPLORER; CHARGE STATES; ISOTOPE SPECTROMETER; ACCELERATION; SHOCKS; ENERGIES; FLARES; WIND; ACE AB [1] Observations from the Solar Isotope Spectrometer and the Ultra Low Energy Isotope Spectrometer on the ACE spacecraft during the extremely large events of October and November 2003 are combined to create heavy ion spectra over more than 3 decades in energy. The resulting spectra differed substantially in shape from event to event, as well as from element to element within a given event, resulting in energy-dependent abundance ratios. Although the effects of strong local shock acceleration are apparent in the intensities of the 28 and 29 October events, these do not explain the order of magnitude differences between the event-integrated abundances obtained at 0.64 - 0.91 MeV/nucleon and those at 12 - 60 MeV/nucleon. The higher- energy abundances relative to the lower-energy ones show trends with nuclear charge or charge-to-mass ratio that are similar for all the events and suggest that heavier ions are less efficiently accelerated to high energies. The position of the breaks in the energy spectra of O, Ne, Mg, Si, S, Ca, and Fe can be understood in terms of leakage from the shock region, if the mean free path is assumed to be a power law in rigidity. The resulting rigidity dependence is consistent with a source of wave turbulence in the vicinity of the shock when the ions are accelerated. C1 CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. Univ Maryland, Dept Phys, College Pk, MD 20742 USA. Univ Maryland, Inst Phys Sci & Technol, College Pk, MD 20742 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Cohen, CMS (reprint author), CALTECH, Space Radiat Lab, MC 220-47, Pasadena, CA 91125 USA. EM cohen@srl.caltech.edu; ecs@srl.caltech.edu; rmewaldt@srl.caltech.edu; ral@srl.caltech.edu; ace@srl.caltech.edu; glenn.mason@umail.um.edu; desai@uleis.umd.edu; tycho@milkyway.gsfc.nasa.gov; mark.e.wiedenbeck@jpl.nasa.gov NR 34 TC 43 Z9 43 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 AUG 10 PY 2005 VL 110 IS A9 AR A09S16 DI 10.1029/2005JA011004 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 957PS UT WOS:000231383600002 ER PT J AU Zhou, DK Smith, WL Liu, X Larar, AM Huang, HLA Li, J McGill, MJ Mango, SA AF Zhou, DK Smith, WL Liu, X Larar, AM Huang, HLA Li, J McGill, MJ Mango, SA TI Thermodynamic and cloud parameter retrieval using infrared spectral data SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID CIRRUS AB High-resolution infrared radiance spectra obtained from near nadir observations provide atmospheric, surface, and cloud property information. A fast radiative transfer model, including cloud effects, is used for atmospheric profile and cloud parameter retrieval. The retrieval algorithm is presented along with its application to recent field experiment data from the NPOESS Airborne Sounder Testbed - Interferometer (NAST-I). The retrieval accuracy dependence on cloud properties is discussed. It is shown that relatively accurate temperature and moisture retrievals can be achieved below optically thin clouds. For optically thick clouds, accurate temperature and moisture profiles down to cloud top level are obtained. For both optically thin and thick cloud situations, the cloud top height can be retrieved with an accuracy of approximately 1.0 km. Preliminary NAST-I retrieval results from the recent Atlantic-THORPEX Regional Campaign (ATReC) are presented and compared with coincident observations obtained from dropsondes and the nadir-pointing Cloud Physics Lidar (CPL). C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. Natl Polar Orbiting Operat Environm Satellite Sys, Integrated Program Off, Silver Spring, MD 20910 USA. NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. Hampton Univ, Ctr Atmospher Studies, Hampton, VA 23681 USA. Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI 53706 USA. RP Zhou, DK (reprint author), NASA, Langley Res Ctr, 21 Langley Blvd, Hampton, VA 23681 USA. EM daniel.k.zhou@nasa.gov RI McGill, Matthew/D-8176-2012; Li, Jun/H-3579-2015 OI Li, Jun/0000-0001-5504-9627 NR 14 TC 21 Z9 21 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 9 PY 2005 VL 32 IS 15 AR L15805 DI 10.1029/2005GL023211 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 957ON UT WOS:000231379900003 ER PT J AU Kaufman, YJ Koren, I Remer, LA Rosenfeld, D Rudich, Y AF Kaufman, YJ Koren, I Remer, LA Rosenfeld, D Rudich, Y TI The effect of smoke, dust, and pollution aerosol on shallow cloud development over the Atlantic Ocean SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE cloud cover; cloud height; indirect effect; radiative forcing; air quality ID OPTICAL-PROPERTIES; STRATIFORM CLOUDS; SOLAR-RADIATION; AIR-POLLUTION; SAFARI 2000; CLIMATE; MODIS; IMPACT; SATELLITE; HAZE AB Clouds developing in a polluted environment tend to have more numerous but smaller droplets. This property may lead to suppression of precipitation and longer cloud lifetime. Absorption of incoming solar radiation by aerosols, however, can reduce the cloud cover. The net aerosol effect on clouds is currently the largest uncertainty in evaluating climate forcing. Using large statistics of 1-km resolution MODIS (Moderate Resolution Imaging Spectro-radiometer) satellite data, we study the aerosol effect on shallow water clouds, separately in four regions of the Atlantic Ocean, for June through August 2002: marine aerosol (30 degrees S-20 degrees S), smoke (20 degrees S-5 degrees N), mineral dust (5 degrees N-25 degrees N), and pollution aerosols (30 degrees N160 degrees N). All four aerosol types affect the cloud droplet size. We also find that the coverage of shallow clouds increases in all of the cases by 0.2-0.4 from clean to polluted, smoky, or dusty conditions. Covariability analysis with meteorological parameters associates most of this change to aerosol, for each of the four regions and 3 months studied. In our opinion, there is low probability that the net aerosol effect can be explained by coincidental, unresolved, changes in meteorological conditions that also accumulate aerosol, or errors in the data, although further in situ measurements and model developments are needed to fully understand the processes. The radiative effect at the top of the atmosphere incurred by the aerosol effect on the shallow clouds and solar radiation is -11 +/- 3 W/m(2) for the 3 months studied; 2/3 of it is due to the aerosol-induced cloud changes, and 1/3 is due to aerosol direct radiative effect. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland, Joint Ctr Earth Syst Technol, Catonsville, MD 21228 USA. Hebrew Univ Jerusalem, Inst Earth Sci, IL-91904 Jerusalem, Israel. Weizmann Inst Sci, Dept Environm Sci, IL-76100 Rehovot, Israel. RP Kaufman, YJ (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. EM kaufman@climate.gsfc.nasa.gov RI Rudich, Yinon/K-1498-2012; Koren, Ilan/K-1417-2012; Xiongfei, Zhao/G-7690-2015; Rosenfeld, Daniel/F-6077-2016; OI Koren, Ilan/0000-0001-6759-6265; Rosenfeld, Daniel/0000-0002-0784-7656; Rudich, Yinon/0000-0003-3149-0201 NR 49 TC 306 Z9 315 U1 6 U2 65 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD AUG 9 PY 2005 VL 102 IS 32 BP 11207 EP 11212 DI 10.1073/pnas.0505191102 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 955UP UT WOS:000231253400017 PM 16076949 ER PT J AU Popovic, S Exton, RJ Herring, GC AF Popovic, S Exton, RJ Herring, GC TI Transition from diffuse to filamentary domain in a 9.5 GHz microwave-induced surface discharge SO APPLIED PHYSICS LETTERS LA English DT Article AB The transition from the low-pressure diffuse to the high-pressure filamentary domain of a 9.5 GHz microwave-induced surface discharge in air is recorded. The discharge employs several half-wavelength initiators that locally enhance the electric field to achieve breakdown in the higher-pressure subcritical region. Visible light imaging illustrates the qualitative changes in discharge morphology over the pressure range 4.5 to 760 Torr (0.6 to 100 kPa). (c) 2005 American Institute of Physics. C1 NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, Res & Technol Directorate, Hampton, VA 23681 USA. Old Dominion Univ, Dept Phys, Norfolk, VA 23529 USA. RP NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, Res & Technol Directorate, Hampton, VA 23681 USA. EM r.j.exton@larc.nasa.gov NR 7 TC 11 Z9 11 U1 2 U2 4 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 AUG 8 PY 2005 VL 87 IS 6 AR 061502 DI 10.1063/1.2009068 PG 3 WC Physics, Applied SC Physics GA 952PB UT WOS:000231016900014 ER PT J AU Livingston, JM Schmid, B Russell, PB Eilers, JA Kolyer, RW Redemann, J Ramirez, SA Yee, JH Swartz, WH Trepte, CR Thomason, LW Pitts, MC Avery, MA Randall, CE Lumpe, JD Bevilacqua, RM Bittner, M Erbertseder, T McPeters, RD Shetter, RE Browell, EV Kerr, JB Lamb, K AF Livingston, JM Schmid, B Russell, PB Eilers, JA Kolyer, RW Redemann, J Ramirez, SA Yee, JH Swartz, WH Trepte, CR Thomason, LW Pitts, MC Avery, MA Randall, CE Lumpe, JD Bevilacqua, RM Bittner, M Erbertseder, T McPeters, RD Shetter, RE Browell, EV Kerr, JB Lamb, K TI Retrieval of ozone column content from airborne Sun photometer measurements during SOLVE II: comparison with coincident satellite and aircraft measurements SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID OPTICAL-DEPTH SPECTRA; INFERRING TOTAL OZONE; WATER-VAPOR; SOLAR RADIOMETER; POAM-III; DISTRIBUTIONS; PINATUBO; AIR AB During the 2003 SAGE ( Stratospheric Aerosol and Gas Experiment) III Ozone Loss and Validation Experiment (SOLVE) II, the fourteen- channel NASA Ames Airborne Tracking Sunphotometer (AATS-14) was mounted on the NASA DC-8 aircraft and measured spectra of total and aerosol optical depth (TOD and AOD) during the sunlit portions of eight science flights. Values of ozone column content above the aircraft have been derived from the AATS-14 measurements by using a linear least squares method that exploits the differential ozone absorption in the seven AATS-14 channels located within the Chappuis band. We compare AATS-14 columnar ozone retrievals with temporally and spatially near-coincident measurements acquired by the SAGE III and the Polar Ozone and Aerosol Measurement (POAM) III satellite sensors during four solar occultation events observed by each satellite. RMS differences are 19 DU (7% of the AATS value) for AATS-SAGE and 10 DU (3% of the AATS value) for AATS-POAM. In these checks of consistency between AATS-14 and SAGE III or POAM III ozone results, the AATS-14 analyses use airmass factors derived from the relative vertical profiles of ozone and aerosol extinction obtained by SAGE III or POAM III. We also compare AATS-14 ozone retrievals for measurements obtained during three DC-8 flights that included extended horizontal transects with total column ozone data acquired by the Total Ozone Mapping Spectrometer ( TOMS) and the Global Ozone Monitoring Experiment (GOME) satellite sensors. To enable these comparisons, the amount of ozone in the column below the aircraft is estimated either by assuming a climatological model or by combining SAGE and/or POAM data with high resolution in-situ ozone measurements acquired by the NASA Langley Research Center chemiluminescent ozone sensor, FASTOZ, during the aircraft vertical profile at the start or end of each flight. Resultant total column ozone values agree with corresponding TOMS and GOME measurements to within 10 - 15DU ( similar to 3%) for AATS data acquired during two flights - a longitudinal transect from Sweden to Greenland on 21 January, and a latitudinal transect from 47 degrees N to 35 degrees N on 6 February. For the round trip DC-8 latitudinal transect between 34 degrees N and 22 degrees N on 19 - 20 December 2002, resultant AATS-14 ozone retrievals plus below-aircraft ozone estimates yield a latitudinal gradient that is similar in shape to that observed by TOMS and GOME, but resultant AATS values exceed the corresponding satellite values by up to 30 DU at certain latitudes. These differences are unexplained, but they are attributed to spatial and temporal variability that was associated with the dynamics near the subtropical jet but was unresolved by the satellite sensors. For selected cases, we also compare AATS-14 ozone retrievals with values derived from coincident measurements by the other two DC-8 based solar occultation instruments: the National Center for Atmospheric Research Direct beam Irradiance Airborne Spectrometer (DIAS) and the NASA Langley Research Center Gas and Aerosol Monitoring System ( GAMS). AATS and DIAS retrievals agree to within RMS differences of 1% of the AATS values for the 21 January and 19 - 20 December flights, and 2.3% for the 6 February flight. Corresponding AATS-GAMS RMS differences are similar to 1.5% for the 21 January flight; GAMS data were not compared for the 6 February flight and were not available for the 19 - 20 December flight. Line of sight ozone retrievals from coincident measurements obtained by the three DC-8 solar occultation instruments during the SAGE III solar occultation event on 24 January yield RMS differences of 2.1% for AATS-DIAS and 0.5% for AATS-GAMS. C1 SRI Int, Menlo Pk, CA 94025 USA. Bay Area Environm Res Inst, Sonoma, CA USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. NASA, Langley Res Ctr, Hampton, VA 23665 USA. Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. Computat Phys Inc, Springfield, VA USA. USN, Res Lab, Washington, DC 20375 USA. DLR, Oberpfaffenhofen, Wessling, Germany. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Natl Ctr Atmospher Res, Boulder, CO 80307 USA. Environm Canada, Cobble Hill, BC, Canada. Int Ozone Serv Inc, Toronto, ON, Canada. RP Livingston, JM (reprint author), SRI Int, 333 Ravenswood Ave, Menlo Pk, CA 94025 USA. EM jlivingston@mail.arc.nasa.gov RI Swartz, William/A-1965-2010; McPeters, Richard/G-4955-2013; Randall, Cora/L-8760-2014; OI Swartz, William/0000-0002-9172-7189; McPeters, Richard/0000-0002-8926-8462; Randall, Cora/0000-0002-4313-4397; Thomason, Larry/0000-0002-1902-0840 NR 39 TC 10 Z9 10 U1 0 U2 1 PU EUROPEAN GEOSCIENCES UNION PI KATLENBURG-LINDAU PA MAX-PLANCK-STR 13, 37191 KATLENBURG-LINDAU, GERMANY SN 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PD AUG 8 PY 2005 VL 5 BP 2035 EP 2054 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 954LJ UT WOS:000231156300001 ER PT J AU Galletto, P Lin, W Mishchenko, MI Borkovec, M AF Galletto, P Lin, W Mishchenko, MI Borkovec, M TI Light-scattering form factors of asymmetric particle dimers from heteroaggregation experiments SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID RANDOMLY ORIENTED BISPHERES; ELECTROMAGNETIC SCATTERING; RATE CONSTANTS; AGGREGATION; COLLOIDS; SPHERES AB Measurements of form factors of asymmetric particle dimers composed of oppositely charged polystyrene latex particles are presented. These measurements are based on time-resolved static and dynamic light scattering on dilute aggregating aqueous suspensions. The experimental form factors are compared with independent calculations based on the superposition T-matrix method and Rayleigh-Debye-Gans (RDG) approximation. While the RDG approximation is found to be reliable only up to particle diameters of about 250 nm, the superposition T-matrix method is very accurate for all types of dimers investigated. The present results show clearly the appropriateness of the superposition T-matrix method to estimate the optical properties of colloidal particles in the micrometer range reliably. (C) 2005 American Institute of Physics. C1 Univ Geneva, Dept Inorgan Analyt & Appl Chem, CH-1211 Geneva, Switzerland. NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Borkovec, M (reprint author), Univ Geneva, Dept Inorgan Analyt & Appl Chem, CH-1211 Geneva, Switzerland. EM michal.borkovec@unige.ch RI Borkovec, Michal/C-6022-2014; Mishchenko, Michael/D-4426-2012 OI Borkovec, Michal/0000-0002-1114-4865; NR 22 TC 15 Z9 15 U1 0 U2 5 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD AUG 8 PY 2005 VL 123 IS 6 AR 064709 DI 10.1063/1.1996570 PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 956OU UT WOS:000231310500053 PM 16122337 ER PT J AU Zhang, JL Reid, JS Holben, BN AF Zhang, JL Reid, JS Holben, BN TI An analysis of potential cloud artifacts in MODIS over ocean aerosol optical thickness products SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID AERONET; NETWORK AB Using spatially and temporally collocated MODerate Resolution Imaging Spectroradiometer ( MODIS) products and data from seven AErosol RObotic NETwork (AERONET) sun-photometer sites, we explored the relationship between MODIS aerosol optical depth and cloud fraction over remote oceans that have been recently reported in the literature. We show that artifacts such as cloud contamination or adjacency effect contribute to the majority of the relationship in clean marine conditions. This cloud fraction effect could result in a 10 - 20% overestimation in monthly mean aerosol optical depth or aerosol direct forcing values that are derived using MODIS aerosol products over cloud free oceans. It may also explain some of the high optical depth values derived in the mid-latitude southern oceans. We also suggest that covariances of meteorological phenomenon such as wind or humidity in cloudy regions while logical might only account for a minor portion of the ensemble relationship. C1 USN, Marine Meteorol Div, Res Lab, Monterey, CA 93940 USA. NASA, Terr Phys Lab, Goddard Space Flight Ctr, Ctr Data, Greenbelt, MD 20771 USA. RP Zhang, JL (reprint author), USN, Marine Meteorol Div, Res Lab, 542 Sloat Ave 2, Monterey, CA 93940 USA. EM zhang@nrlmry.navy.mil RI Reid, Jeffrey/B-7633-2014 OI Reid, Jeffrey/0000-0002-5147-7955 NR 13 TC 106 Z9 106 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 5 PY 2005 VL 32 IS 15 AR L15803 DI 10.1029/2005GL023254 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 954GH UT WOS:000231141600001 ER PT J AU Norton, G Novarini, J AF Norton, G Novarini, J TI Time domain modeling of pulse propagation in non-isotropic dispersive media SO MATHEMATICS AND COMPUTERS IN SIMULATION LA English DT Article; Proceedings Paper CT 3rd International Conference on Nonlinear Evolution Equations and Wave Phenomena CY APR 07-10, 2003 CL Athens, GA SP IMACS DE time domain; dispersion; finite difference ID ABSORBING BOUNDARY-CONDITIONS; FREQUENCY POWER-LAW; WAVE-PROPAGATION; COMPLEMENTARY OPERATORS; EQUATIONS AB Acoustic pulse propagation requires the inclusion of attenuation and its causal companion, dispersion when propagation is through a non-ideal fluid medium. For acoustic propagation in a linear medium, Szabo [T.L. Szabo, J. Acoust. Soc. Am., 96 (1994) 491-500] introduced the concept of a convolutional propagation operator that plays the role of a casual propagation factor in the time domain. The resulting modified wave equation is solved via the method of finite differences. One aspect of the acoustic field that is of interest to researchers is the monostatic-backscattered field. This field which by definition is small compared to the forward-propagated field is challenging to isolate. Since the numerical grid is of finite size, the received signal has the possibility of being contaminated with spurious reflections coming from the walls of the computational grid even if absorbing boundary conditions (ABCs) are imposed. Therefore, a robust highly accurate absorbing boundary condition is developed. In addition, the finite difference description of the modified wave equation is developed having fourth-order accuracy in both time and space. (c) 2005 IMACS. Published by Elsevier B.V. All rights reserved. C1 Stennis Space Ctr Detachment, Naval Res Lab, SSC, Stennis Space Ctr, MS 39529 USA. Planning Syst Inc, Long Beach, MS 39560 USA. RP Stennis Space Ctr Detachment, Naval Res Lab, SSC, Stennis Space Ctr, MS 39529 USA. EM guy.norton@nrlssc.navy.mil NR 21 TC 5 Z9 6 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-4754 EI 1872-7166 J9 MATH COMPUT SIMULAT JI Math. Comput. Simul. PD AUG 5 PY 2005 VL 69 IS 5-6 BP 467 EP 476 DI 10.1016/j.matcom.2005.03.011 PG 10 WC Computer Science, Interdisciplinary Applications; Computer Science, Software Engineering; Mathematics, Applied SC Computer Science; Mathematics GA 959GN UT WOS:000231506300006 ER PT J AU Chaston, CC Phan, TD Bonnell, JW Mozer, FS Acuna, M Goldstein, ML Balogh, A Andre, M Reme, H Fazakerley, A AF Chaston, CC Phan, TD Bonnell, JW Mozer, FS Acuna, M Goldstein, ML Balogh, A Andre, M Reme, H Fazakerley, A TI Drift-kinetic Alfven waves observed near a reconnection X line in the Earth's magnetopause SO PHYSICAL REVIEW LETTERS LA English DT Article ID SOLAR-WIND; CLUSTER; AURORA; CORONA AB We identify drift-kinetic Alfven waves in the vicinity of a reconnection X line on the Earth's magnetopause. The dispersive properties of these waves have been determined using wavelet interferometric techniques applied to multipoint observations from the Cluster spacecraft. Comparison of the observed wave dispersion with that expected for drift-kinetic Alfven waves shows close agreement. The waves propagate outwards from the X line suggesting that reconnection is a kinetic Alfven wave source. Energetic O+ ions observed in these waves indicate that reconnection is a driver of auroral ion outflow. C1 Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ London Imperial Coll Sci & Technol, London, England. Swedish Inst Space Phys, Uppsala, Sweden. CESR, Toulouse, France. Mullard Space Sci Lab, Dorking, Surrey, England. RP Chaston, CC (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RI Goldstein, Melvyn/B-1724-2008 NR 18 TC 55 Z9 55 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 AUG 5 PY 2005 VL 95 IS 6 AR 065002 DI 10.1103/PhysRevLett.95.065002 PG 4 WC Physics, Multidisciplinary SC Physics GA 952PJ UT WOS:000231017700035 PM 16090960 ER PT J AU Schmidt, GA Shindell, DT Harder, S AF Schmidt, GA Shindell, DT Harder, S TI Reply to comment by W.F. Ruddiman on "A note on the relationship between ice core methane concentrations and insolation'' SO GEOPHYSICAL RESEARCH LETTERS LA English DT Editorial Material ID CLIMATE; ANTARCTICA C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA. Washington State Univ, Environm Sci Program, Vancouver, WA 98686 USA. RP Schmidt, GA (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM gschmidt@giss.nasa.gov; harders@vancouver.wsu.edu RI Schmidt, Gavin/D-4427-2012 OI Schmidt, Gavin/0000-0002-2258-0486 NR 9 TC 0 Z9 0 U1 4 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 4 PY 2005 VL 32 IS 15 AR L15704 DI 10.1029/2005GL022982 PG 2 WC Geosciences, Multidisciplinary SC Geology GA 954GG UT WOS:000231141500004 ER PT J AU Li, Z Adamec, D Takahashi, T Sutherland, SC AF Li, Z Adamec, D Takahashi, T Sutherland, SC TI Global autocorrelation scales of the partial pressure of oceanic CO2 SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID EQUATORIAL PACIFIC-OCEAN; SEA; PCO(2); TEMPERATURE; VARIABILITY; FLUX AB A global database of approximately 1.7 million observations of the partial pressure of carbon dioxide in surface ocean waters (pCO(2)) collected between 1970 and 2003 is used to estimate its spatial autocorrelation structure. The patterns of the lag distance where the autocorrelation exceeds 0.8 is similar to patterns in the spatial distribution of the first baroclinic Rossby radius of deformation indicating that ocean circulation processes play a significant role in determining the spatial variability of pCO(2). Separate calculations for times when the Sun is north and south of the equator revealed no obvious seasonal dependence of the spatial autocorrelation scales. The pCO(2) measurements at Ocean Weather Station (OWS) "P'' in the eastern subarctic Pacific (50 degrees N, 145 degrees W) is the only fixed location where an uninterrupted time series of sufficient length exists to calculate a meaningful temporal autocorrelation function for lags greater than a few days. The estimated temporal autocorrelation function at OWS "P'' is highly variable. A spectral analysis of the longest four pCO(2) time series indicates a high level of variability occurring over periods from the atmospheric synoptic to the maximum length of the time series, in this case 42 days. It is likely that a relative peak in variability with a period of 3-6 days is related to atmospheric synoptic period variability and ocean mixing events due to wind stirring. However, the short length of available time series makes identifying temporal relationships between pCO(2) and atmospheric or ocean processes problematic. C1 Gen Sci Corp, Sci Applicat Int Corp, Beltsville, MD USA. NASA, Goddard Space Flight Ctr, Oceans Sci Branch, Greenbelt, MD 20771 USA. Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. RP Li, Z (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610-1,Bldg 33,Room 214A, Greenbelt, MD 20771 USA. EM zhen.li@gsfc.nasa.gov NR 12 TC 9 Z9 9 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD AUG 4 PY 2005 VL 110 IS C8 AR C08002 DI 10.1029/2004GC002723 PG 12 WC Oceanography SC Oceanography GA 954GQ UT WOS:000231142500001 ER PT J AU West, RA Brown, ME Salinas, SV Bouchez, AH Roe, HG AF West, RA Brown, ME Salinas, SV Bouchez, AH Roe, HG TI No oceans on Titan from the absence of a near-infrared specular reflection SO NATURE LA English DT Article ID OPTICAL-CONSTANTS; ATMOSPHERE; LIQUID; MODEL AB With its substantial atmosphere of nitrogen, hydrocarbons and nitriles, Saturn's moon Titan is a unique planetary satellite. Photochemical processing of the gaseous constituents produces an extended haze that obscures the surface. Soon after the Voyager fly-bys in 1980 and 1981 photochemical models(1-3) led to the conclusion that there should be enough liquid methane/ethane/ nitrogen to cover the surface to a depth of several hundred metres. Recent Earth-based radar echoes imply that surface liquid may be present at a significant fraction of the locations sampled(4). Here we present ground-based observations ( at near-infrared wavelengths) and calculations showing that there is no evidence thus far for surface liquid(5). Combined with the specular signatures from radar observations, we infer mechanisms that produce very flat solid surfaces, involving a substance that was liquid in the past but is not in liquid form at the locations we studied. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. Natl Univ Singapore, Ctr Remote Imaging Sensing & Proc, Singapore 119260, Singapore. WM Keck Observ, Kamuela, HI 96743 USA. RP West, RA (reprint author), CALTECH, Jet Prop Lab, MS 169-237,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Robert.A.West@jpl.nasa.gov NR 17 TC 49 Z9 50 U1 0 U2 6 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD AUG 4 PY 2005 VL 436 IS 7051 BP 670 EP 672 DI 10.1038/nature03824 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 951XA UT WOS:000230964500036 PM 16079839 ER PT J AU Angert, A Biraud, S Bonfils, C Henning, CC Buermann, W Pinzon, J Tucker, CJ Fung, I AF Angert, A Biraud, S Bonfils, C Henning, CC Buermann, W Pinzon, J Tucker, CJ Fung, I TI Drier summers cancel out the CO2 uptake enhancement induced by warmer springs SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE atmospheric CO2 seasonal cycle; global climate change; net primary production; summer drought; water stress ID ATMOSPHERIC CARBON-DIOXIDE; NORTHERN-HEMISPHERE; VEGETATION INDEX; SEASONAL CYCLE; SURFACE; 20TH-CENTURY; LATITUDES; INCREASES; FORESTS; FLUXES AB An increase in photosynthetic activity of the northern hemisphere terrestrial vegetation, as derived from satellite observations, has been reported in previous studies. The amplitude of the seasonal cycle of the annually detrended atmospheric CO2 in the northern hemisphere (an indicator of biospheric activity) also increased during that period. We found, by analyzing the annually detrended CO2 record by season, that early summer (June) CO2 concentrations indeed decreased from 1985 to 1991, and they have continued to decrease from 1994 up to 2002. This decrease indicates accelerating springtime net CO2 uptake. However, the CO2 minimum concentration in late summer (an indicator of net growing-season uptake) showed no positive trend since 1994, indicating that lower net CO2 uptake during summer cancelled out the enhanced uptake during spring. Using a recent satellite normalized difference vegetation index data set and climate data, we show that this lower summer uptake is probably the result of hotter and drier summers in both mid and high latitudes, demonstrating that a warming climate does not necessarily lead to higher CO2 growing-season uptake, even in high-latitude ecosystems that are considered to be temperature limited. C1 Univ Calif Berkeley, Berkeley Atmospher Sci Ctr, Berkeley, CA 94720 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Angert, A (reprint author), Univ Calif Berkeley, Berkeley Atmospher Sci Ctr, Berkeley, CA 94720 USA. EM angert@gmail.com RI Biraud, Sebastien/M-5267-2013; Bonfils, Celine/H-2356-2012 OI Biraud, Sebastien/0000-0001-7697-933X; Bonfils, Celine/0000-0002-4674-5708 NR 30 TC 230 Z9 237 U1 10 U2 69 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD AUG 2 PY 2005 VL 102 IS 31 BP 10823 EP 10827 DI 10.1073/pnas.0501647102 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 953TC UT WOS:000231102400017 PM 16043702 ER PT J AU Herndon, SC Onasch, TB Frank, BP Marr, LC Jayne, JT Canagaratna, MR Grygas, J Lanni, T Anderson, BE Worsnop, D Miake-Lye, RC AF Herndon, SC Onasch, TB Frank, BP Marr, LC Jayne, JT Canagaratna, MR Grygas, J Lanni, T Anderson, BE Worsnop, D Miake-Lye, RC TI Particulate emissions from in-use commercial aircraft SO AEROSOL SCIENCE AND TECHNOLOGY LA English DT Article ID AROMATIC HYDROCARBON CONCENTRATION; AERODYNAMIC DIAMETER MEASUREMENTS; ULTRAFINE AEROSOL-PARTICLES; LOW-PRESSURE IMPACTOR; DENSITY CHARACTERIZATION; AIRBORNE OBSERVATIONS; COMBUSTION AEROSOLS; SIZE DISTRIBUTIONS; COMBINED MOBILITY; TURBINE-ENGINES AB Particulate emission indices ( per kg fuel) have been determined by sampling the advected plumes of in-use commercial aircraft at two different airports using a novel approach. Differences are observed in the number, magnitude, and composition of the particle emissions between idle and take-off. At the first airport, Electrical Low Pressure Impactor (ELPI) data indicate that number based emission indices (EIn) vary by an order of magnitude for take-off plumes from different aircraft. Additionally, EIn values for idle plumes are greater than take-off. At the second airport, EIn values derived from condensation particle counter (CPC) measurements span similar to an order of magnitude (3.50 x 10(15) particles per kg fuel). The median values of the idle and take-off plumes were 1.8 x 10(16) and 7.6 x 10(15) particles per kg fuel, respectively. For take-off plumes, the magnitude of the particulate emission index is not correlated with NOx at either airport. The surface properties of the particulate emissions in take-off and idle plumes differ significantly as measured by diffusion charging (DC) and photoelectric aerosol sensor (PAS) instruments. Results indicate that takeoff plumes are characterized by particles with photoelectric-active surfaces, presumably elemental carbon, whereas idle plumes are composed of non-photoelectric-active constituents and coated soot particles. Measurements of the particulate size distribution (ELPI) show evidence for two modes, one at similar to 90 nm aerodynamic diameter and a second mode at or below the instrument cutoff (< 30 nm). C1 Aerodyne Res Inc, Billerica, MA 01821 USA. New York State Dept Environm Conservat, Albany, NY USA. Virginia Tech, Blacksburg, VA 24061 USA. NASA, Langley Res Ctr, Div Atmospher Sci, Hampton, VA 23665 USA. RP Aerodyne Res Inc, 45 Manning Rd, Billerica, MA 01821 USA. EM herndon@aerodyne.com RI Worsnop, Douglas/D-2817-2009; Marr, Linsey/C-9698-2010; Lucas, Elizabeth/E-2733-2010 OI Worsnop, Douglas/0000-0002-8928-8017; Marr, Linsey/0000-0003-3628-6891; NR 50 TC 55 Z9 55 U1 3 U2 8 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0278-6826 EI 1521-7388 J9 AEROSOL SCI TECH JI Aerosol Sci. Technol. PD AUG PY 2005 VL 39 IS 8 BP 799 EP 809 DI 10.1080/02786820500247363 PG 11 WC Engineering, Chemical; Engineering, Mechanical; Environmental Sciences; Meteorology & Atmospheric Sciences SC Engineering; Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 958UY UT WOS:000231474900012 ER PT J AU Arbocz, J Hilburger, MW AF Arbocz, J Hilburger, MW TI Toward a probabilistic preliminary design criterion for buckling critical composite shells 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, VA SP AIAA, ASME, ASCE, AHS, ASC AB A probability-based analysis method for predicting buckling loads of 6ompression-loaded laminated composite shells is presented, and its potential as a basis for anew shell-stability-design criterion is demonstrated and discussed. In particular, a database containing information about specimen geometry, material properties; and measured initial geometric imperfections for a selected-group of laminated-composite cylindrical shells is used to calculate new buckling-load "knockdown factors: These knockdown factors ire, shown to be substantially-improved and hence much less conservative than the corresponding deterministic knockdown factors that are presently used by industry. The probability integral associated with the analysis is evaluated by using two methods; that is, by using the exact Monte Carlo method and by using an approximate first-order second-moment method. A comparison. of the results from these two methods indicates that the first-order second-moment method yields results that are conservative for the shells considered. Furthermore the results show that the improved; reliability-based knockdown factor presented always yields a safe estimate of the buckling load for the shells examined. C1 Delft Univ Technol, NL-2629 HS Delft, Netherlands. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Arbocz, J (reprint author), Delft Univ Technol, NL-2629 HS Delft, Netherlands. NR 12 TC 19 Z9 19 U1 0 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 AUG PY 2005 VL 43 IS 8 BP 1823 EP 1827 DI 10.2514/1.11368 PG 5 WC Engineering, Aerospace SC Engineering GA 950OR UT WOS:000230867300020 ER PT J AU Odegard, GM Frankland, SJV Gates, TS AF Odegard, GM Frankland, SJV Gates, TS TI Effect of nanotube functionalization on the elastic properties of polyethylene nanotube composites 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, VA SP AIAA, ASME, ASCE, AHS, ASC ID WALLED CARBON NANOTUBES; POLYMER COMPOSITES; SIDEWALL FUNCTIONALIZATION; ORGANIC FUNCTIONALIZATION; OPTICAL-PROPERTIES; SIMULATION; PROTEINS; FIELD AB The, effects of,the chemical functionalization of a single-wall carbon nanotube in nianotube/polyethylene composites on the bulk elastic properties are presented. Constitutive equations are established for composites containing both functionalized and nonfunctionalizeid nanotubes using an equivalent-continuum modeling technique. The elastic properties of both composite systems are predicted- for amorphous and crystalline polyethylene matrices with carious nanotube lengths, volume fractions, and orientations. The results indicate that for the specific composite. materials considered. in this study most of the elastic stiffness constants of the composite with functionalized nanotubes are either less than or equal to those of the composite without functionalized nanotubes. C1 Michigan Technol Univ, Dept Mech Engn Engn Mech, Houghton, MI 49931 USA. Natl Inst Aerosp, Hampton, VA 23666 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Odegard, GM (reprint author), Michigan Technol Univ, Dept Mech Engn Engn Mech, Houghton, MI 49931 USA. OI Odegard, Gregory/0000-0001-7577-6565 NR 40 TC 42 Z9 43 U1 0 U2 8 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD AUG PY 2005 VL 43 IS 8 BP 1828 EP 1835 DI 10.2514/1.9468 PG 8 WC Engineering, Aerospace SC Engineering GA 950OR UT WOS:000230867300021 ER PT J AU Summers, RL Johnston, SL Marshburn, TH Williams, DR AF Summers, RL Johnston, SL Marshburn, TH Williams, DR TI Emergencies in space SO ANNALS OF EMERGENCY MEDICINE LA English DT Article ID LONG-DURATION SPACEFLIGHT; MEDICAL-CARE; ASTRONAUTS; MICROGRAVITY; STATION; TRAUMA; RESUSCITATION; MANAGEMENT; MISSIONS; SUPPORT AB Manned spaceflight is inherently risky and results in unique problems from a trauma and medical perspective. Emergency care under these special physiologic and environmental conditions calls for novel techniques for diagnosis and therapy. C1 Univ Mississippi, Med Ctr, Dept Emergency Med, Jackson, MS 39216 USA. NASA, Lyndon B Johnson Space Ctr, Off Space Med, Houston, TX 77058 USA. RP Summers, RL (reprint author), Univ Mississippi, Med Ctr, Dept Emergency Med, 2500 N State St, Jackson, MS 39216 USA. EM rsummers@pol.net NR 43 TC 14 Z9 15 U1 0 U2 0 PU MOSBY, INC PI ST LOUIS PA 11830 WESTLINE INDUSTRIAL DR, ST LOUIS, MO 63146-3318 USA SN 0196-0644 J9 ANN EMERG MED JI Ann. Emerg. Med. PD AUG PY 2005 VL 46 IS 2 BP 177 EP 184 DI 10.1016/j.annemergmed.2005.02.010 PG 8 WC Emergency Medicine SC Emergency Medicine GA 950KD UT WOS:000230855100015 PM 16046951 ER PT J AU Lies, DP Hernandez, ME Kappler, A Mielke, RE Gralnick, JA Newman, DK AF Lies, DP Hernandez, ME Kappler, A Mielke, RE Gralnick, JA Newman, DK TI Shewanella oneidensis MR-1 uses overlapping pathways for iron reduction at a distance and by direct contact under conditions relevant for biofilms SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID FE(III) OXIDE REDUCTION; PSEUDOMONAS-CHLORORAPHIS PCL1391; EXTRACELLULAR ELECTRON-TRANSFER; PUTREFACIENS MR-1; OUTER-MEMBRANE; DISSIMILATORY FE(III); MN(IV) REDUCTION; FERRIC-IRON; SEDIMENTARY ENVIRONMENTS; GEOBACTER-SULFURREDUCENS AB We developed a new method to measure iron reduction at a distance based on depositing Fe(III) (hydr)oxide within nanoporous glass beads. In this "Fe-bead" system, Shewanella oneidensis reduces at least 86.5% of the iron in the absence of direct contact. Biofilm formation accompanies Fe-bead reduction and is observable both macro- and microscopically. Fe-bead reduction is catalyzed by live cells adapted to anaerobic conditions, and maximal reduction rates require sustained protein synthesis. The amount of reactive ferric iron in the Fe-bead system is available in excess such that the rate of Fe-bead reduction is directly proportional to cell density; i.e., it is diffusion limited. Addition of either lysates prepared from anaerobic cells or exogenous electron shuttles stimulates Fe-bead reduction by S. oneidensis, but iron chelators or additional Fe(II) do not. Neither dissolved Fe(III) nor electron shuttling activity was detected in culture supernatants, implying that the mediator is retained within the biofilm matrix. Strains with mutations in omcB or mtrB show about 50% of the wild-type levels of reduction, while a cymA mutant shows less than 20% of the wild-type levels of reduction and a menF mutant shows insignificant reduction. The Fe-bead reduction defect of the menF mutant can be restored by addition of menaquinone, but menaquinone itself cannot stimulate Fe-bead reduction. Because the menF gene encodes the first committed step of menaquinone biosynthesis, no intermediates of the menaquinone biosynthetic pathway are used as diffusible mediators by this organism to promote iron reduction at a distance. CymA and menaquinone are required for both direct and indirect mineral reduction, whereas MtrB and OmcB contribute to but are not absolutely required for iron reduction at a distance. C1 CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA. CALTECH, Dept Environm Sci & Engn, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Newman, DK (reprint author), CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA. EM dkn@gps.caltech.edu RI Kappler, Andreas/G-7221-2016 NR 70 TC 161 Z9 167 U1 3 U2 53 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0099-2240 J9 APPL ENVIRON MICROB JI Appl. Environ. Microbiol. PD AUG PY 2005 VL 71 IS 8 BP 4414 EP 4426 DI 10.1128/AEM.71.8.4414-4426.2005 PG 13 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA 954OX UT WOS:000231165500035 PM 16085832 ER PT J AU Pelletier, CC Lambert, JL Borchert, M AF Pelletier, CC Lambert, JL Borchert, M TI Determination of glucose in human aqueous humor using Raman spectroscopy and designed-solution calibration SO APPLIED SPECTROSCOPY LA English DT Article DE Raman; partial least squares; PLS; multivariate; calibration; multiplicative signal correction; MSC; quantitative; glucose; aqueous humor ID BIOLOGICAL-FLUIDS; EYE AB Glucose concentrations of in vitro human aqueous humor (HAH) samples from cataract patients were determined using 785 urn Raman spectra and partial least squares (PLS) calibration. PLS models were created from spectra of prepared calibration solutions rather than aqueous humor samples. Spectra were obtained with an excitation energy (100 mW for 150 s), which was higher than can be applied in vivo, to decrease the models' contribution to prediction uncertainty. The solutions contained experimentally designed levels of glucose, bicarbonate, lactate, urea, and ascorbate. Multiplicative signal correction of spectra helped compensate for the +/- 20% drift in laser power observed at the sample over six noncontiguous days of data collection. Seventeen HAH samples containing 38-775 mg/dL of glucose exhibited a root-mean-square error (RMSEP) of 22 mg/dL, coefficient of determination (r(2)) of 0.989, and bias of 6 mg/dL when predicted from lower energy (30 s) spectra collected contemporaneously with fifty calibration spectra. Similar results were obtained even when spectral data were gathered separately for human aqueous humor samples and calibration samples: 10 HAH samples, calibrated on 25 solutions measured 3.6 weeks earlier, exhibited an RMSEP of 23 mg/dL, r(2) of 0.992, and bias of 9 mg/dL. The results demonstrate progress toward the determination of glucose levels in patient-derived aqueous humor using laboratory-derived "artificial aqueous humor" calibration solutions. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ So Calif, Keck Sch Med, Dept Ophthalmol, Los Angeles, CA 90027 USA. Univ So Calif, Childrens Hosp Los Angeles, Div Ophthalmol, Los Angeles, CA 90027 USA. RP Lambert, JL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM James.L.Lambert@jpl.nasa.gov NR 27 TC 15 Z9 15 U1 1 U2 9 PU SOC APPLIED SPECTROSCOPY PI FREDERICK PA 201B BROADWAY ST, FREDERICK, MD 21701 USA SN 0003-7028 J9 APPL SPECTROSC JI Appl. Spectrosc. PD AUG PY 2005 VL 59 IS 8 BP 1024 EP 1031 DI 10.1366/0003702054615133 PG 8 WC Instruments & Instrumentation; Spectroscopy SC Instruments & Instrumentation; Spectroscopy GA 954DM UT WOS:000231134300009 PM 16105211 ER PT J AU Tinetti, G Meadows, VS Crisp, D Fong, W Velusamy, T Snively, H AF Tinetti, G Meadows, VS Crisp, D Fong, W Velusamy, T Snively, H TI Disk-averaged synthetic spectra of Mars SO ASTROBIOLOGY LA English DT Article DE radiative transfer; remote sensing; spectroscopy; extrasolar terrestrial planets; planetary science; Mars ID MU-M; SCATTERING; PLANETS; SURFACE AB The principal goal of the NASA Terrestrial Planet Finder (TPF) and European Space Agency's Darwin mission concepts is to directly detect and characterize extrasolar terrestrial (Earthsized) planets. This first generation of instruments is expected to provide disk-averaged spectra with modest spectral resolution and signal-to-noise. Here we use a spatially and spectrally resolved model of a Mars-like planet to study the detectability of a planet's surface and atmospheric properties from disk-averaged spectra. We explore the detectability as a function of spectral resolution and wavelength range, for both the proposed visible coronograph (TPFC) and mid-infrared interferometer (TPF-I/Darwin) architectures. At the core of our model is a spectrum-resolving (line-by-line) atmospheric/surface radiative transfer model. This model uses observational data as input to generate a database of spatially resolved synthetic spectra for a range of illumination conditions and viewing geometries. The model was validated against spectra recorded by the Mars Global Surveyor-Thermal Emission Spectrometer and the Mariner 9-Infrared Interferometer Spectrometer. Results presented here include disk-averaged synthetic spectra, light curves, and the spectral variability at visible and mid-infrared wavelengths for Mars as a function of viewing angle, illumination, and season. We also considered the differences in the spectral appearance of an increasingly ice-covered Mars, as a function of spectral resolution, signal-to-noise and integration time for both TPF-C and TPFI/Darwin. C1 CALTECH, IPAC, SSC, NASA,Astrobiol Inst, Pasadena, CA 91125 USA. CALTECH, Natl Res Council, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. RP Tinetti, G (reprint author), CALTECH, IPAC, SSC, NASA,Astrobiol Inst, MS 220-66,1200 E Calif, Pasadena, CA 91125 USA. EM tinetti@ipac.caltech.edu OI Tinetti, Giovanna/0000-0001-6058-6654 NR 27 TC 22 Z9 22 U1 0 U2 5 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD AUG PY 2005 VL 5 IS 4 BP 461 EP 482 DI 10.1089/ast.2005.5.461 PG 22 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 954TP UT WOS:000231178100002 PM 16078866 ER PT J AU Schuerger, AC Richards, JT Hintze, PE Kern, RG AF Schuerger, AC Richards, JT Hintze, PE Kern, RG TI Surface characteristics of spacecraft components affect the aggregation of microorganisms and may lead to different survival rates of bacteria on Mars landers SO ASTROBIOLOGY LA English DT Article DE Mars; astrobiology; planetary protection; spacecraft materials ID SIMULATED MARTIAN ENVIRONMENT; BACILLUS-SUBTILIS; TERRESTRIAL MICROORGANISMS; MICROBIOLOGICAL PROFILES; SOLAR-RADIATION; CONTAMINATION AB Layers of dormant endospores of Bacillus subtilis HA101 were applied to eight different spacecraft materials and exposed to martian conditions of low pressure (8.5 mbar), low temperature (-10 degrees C), and high CO2 gas composition and irradiated with a Mars-normal ultraviolet (UV-visible-near-infrared spectrum. Bacterial layers were exposed to either 1 min or 1 h of Mars-normal UV irradiation, which simulated clear-sky conditions on equatorial Mars (0.1 tau). When exposed to 1 min of Mars UV irradiation, the numbers of viable endospores of B. subtilis were reduced three to four orders of magnitude for two brands of aluminum (Al), stainless steel, chemfilm-treated Al, clear-anodized Al, and black-anodized Al coupons. In contrast, bacterial survival was reduced only one to two orders of magnitude for endospores on the non-metal materials astroquartz and graphite composite when bacterial endospores were exposed to 1 min of Mars UV irradiation. When bacterial monolayers were exposed to 1 h of Mars UV irradiation, no viable bacteria were recovered from the six metal coupons listed above. In contrast, bacterial survival was reduced only two to three orders of magnitude for spore layers on astroquartz and graphite composite exposed to 1 h of Mars UV irradiation. Scanning electron microscopy images of the bacterial monolayers on all eight spacecraft materials revealed that endospores of B. subtilis formed large aggregates of multilayered spores on astroquartz and graphite composite, but not on the other six spacecraft materials. It is likely that the foinmation of multilayered aggregates of endospores on astroquartz and graphite composite is responsible for the enhanced survival of bacterial cells on these materials. C1 Univ Florida, Space Life Sci Lab, Kennedy Space Ctr, FL 32899 USA. Gen Dynam Corp, Kennedy Space Ctr, FL USA. Corros Technol Testbed, Kennedy Space Ctr, FL USA. Mars Explorat Directorate, Jet Prop Lab, Pasadena, CA USA. RP Schuerger, AC (reprint author), Univ Florida, Space Life Sci Lab, Bldg M6-1025, Kennedy Space Ctr, FL 32899 USA. EM acschuerger@ifas.ufl.edu OI Hintze, Paul/0000-0002-9962-2955 NR 33 TC 21 Z9 22 U1 2 U2 6 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD AUG PY 2005 VL 5 IS 4 BP 545 EP 559 DI 10.1089/ast.2005.5.545 PG 15 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 954TP UT WOS:000231178100007 PM 16078871 ER PT J AU Evans, NR Carpenter, KG Robinson, R Kienzle, F Dekas, AE AF Evans, NR Carpenter, KG Robinson, R Kienzle, F Dekas, AE TI High-mass triple systems: The classical Cepheid Y Carinae SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : close; Cepheids; stars : evolution; stars : fundamental parameters ID FF-AQL; ORBIT; COMPANION; CYGNI; LUMINOSITY; TELESCOPE; OPACITIES; STARS AB We have obtained a Hubble Space Telescope STIS ultraviolet high-dispersion echelle-mode spectrum of the binary companion of the double-mode classical Cepheid Y Car. The velocity measured for the hot companion from this spectrum is very different from reasonable predictions for binary motion, implying that the companion is itself a short-period binary. The measured velocity changed by 7 km s(-1) during the 4 days between two segments of the observation, confirming this interpretation. We summarize "binary'' Cepheids that are in fact members of a triple system and find that at least 44% are triples. The summary of information on Cepheids with orbits makes it likely that the fraction is underestimated. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Johns Hopkins Univ, Baltimore, MD 21218 USA. Observ Geneva, CH-1290 Sauverny, Switzerland. Harvard Univ, Cambridge, MA 02138 USA. RP Evans, NR (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM nevans@cfa.harvard.edu; kgc@stargate.gsfc.nasa.gov; robinson@pha.jhu.edu; francesco.kienzle@obs.unige.ch RI Carpenter, Kenneth/D-4740-2012 NR 26 TC 15 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 AUG PY 2005 VL 130 IS 2 BP 789 EP 793 DI 10.1086/430458 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 948NC UT WOS:000230721600034 ER PT J AU Shkolnik, E Walker, GAH Rucinski, SM Bohlender, DA Davidge, TJ AF Shkolnik, E Walker, GAH Rucinski, SM Bohlender, DA Davidge, TJ TI Investigating CaII emission in the RS Canum venaticorum binary er vulpeculae using the broadening function formalism SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : eclipsing; binaries : spectroscopic; stars : activity; stars : individual (ER Vulpeculae) ID CHROMOSPHERIC ACTIVITY; DIFFERENTIAL ROTATION; PHYSICAL PARAMETERS; CLOSE BINARIES; LIGHT CURVES; II H; STARS; VUL; VELOCITIES; SYSTEMS AB The synchronously rotating G stars in the detached, short-period (0.7 days), partially eclipsing binary ER Vul are the most chromospherically active solar-type stars known. We have monitored activity in the Ca II H and K reversals for almost an entire orbit. Rucinski's broadening function formalism allows the photospheric contribution to be objectively subtracted from the highly blended spectra. The power of the broadening function technique is also demonstrated by the good agreement of radial velocities with those measured by others from less crowded spectral regions. In addition to strong Ca II emission from the primary and secondary, there appears to be a high-velocity stream flowing onto the secondary, where it stimulates a large active region on the surface 30 degrees - 40 degrees in advance of the subbinary longitude. A model light curve with a spot centered on the same longitude also gives the best fit to the observed light curve. A flare with similar to 13% more power than at other phases was detected in one spectrum. We suggest that ER Vul may offer a magnified view of the more subtle chromospheric effects synchronized to planetary revolution seen in certain 51 Peg - type systems. C1 Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA. Univ Toronto, David Dunlap Observ, Richmond Hill, ON L4C 4Y6, Canada. Herzberg Inst Astrophys, Natl Res Council Canada, Victoria, BC V9E 2E7, Canada. RP Shkolnik, E (reprint author), Univ Hawaii Manoa, NASA Astrobiol Inst, 2565 McCarthy Mall,Room 213, Honolulu, HI 96822 USA. EM shkolnik@hawaii.edu; gordonwa@uvic.ca; rucinski@astro.utoronto.ca; david.bohlender@nrc.ca; tim.davidge@nrc.ca NR 32 TC 9 Z9 9 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 2005 VL 130 IS 2 BP 799 EP 808 DI 10.1086/431364 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 948NC UT WOS:000230721600036 ER PT J AU Welsh, BY Wheatley, JM Heafield, K Seibert, M Browne, SE Salim, S Rich, RM Barlow, TA Bianchi, L Byun, YI Donas, J Forster, K Friedman, PG Heckman, TM Jelinsky, PN Lee, YW Madore, BF Malina, RF Martin, DC Milliard, B Morrissey, P Neff, SG Schiminovich, D Siegmund, OHW Small, T Szalay, AS Wyder, TK AF Welsh, BY Wheatley, JM Heafield, K Seibert, M Browne, SE Salim, S Rich, RM Barlow, TA Bianchi, L Byun, YI Donas, J Forster, K Friedman, PG Heckman, TM Jelinsky, PN Lee, YW Madore, BF Malina, RF Martin, DC Milliard, B Morrissey, P Neff, SG Schiminovich, D Siegmund, OHW Small, T Szalay, AS Wyder, TK TI The GALEX ultraviolet variability catalog SO ASTRONOMICAL JOURNAL LA English DT Article DE stars : flare; stars : variables : other; ultraviolet : stars ID GALAXY-EVOLUTION-EXPLORER; RR LYRAE STARS; PERFORMANCE AB We present version 1.0 of the NASA Galaxy Evolution Explorer (GALEX) ultraviolet variability (GUVV) catalog, which contains information on 84 time-variable and transient sources gained with simultaneous near-ultraviolet ( NUV) and far-ultraviolet (FUV) photometric observations. These time-variable sources were serendipitously revealed in the various 1.degrees 2 diameter star fields currently being surveyed by the GALEX satellite in two ultraviolet bands (NUV 1750 - 2750 angstrom, FUV 1350 - 1750 8) with limiting AB magnitudes of 23 - 25. The largest amplitude variable objects currently detected by GALEX are M dwarf flare stars, which can brighten by 5 - 10 mag in both the NUV and FUV bands during short-duration (< 500 s) outbursts. Other types of large-amplitude ultraviolet variable objects include ab-type RR Lyrae stars, which can vary periodically by 2 - 5 mag in the GALEX FUV band. This first GUVV catalog lists galactic positions and possible source identifications in order to provide the astronomical community with a list of time-variable objects that can now be repeatedly observed at other wavelengths. We expect the total number of time-variable source detections to increase as the GALEX mission progresses, such that later version numbers of the GUVV catalog will contain substantially more variable sources. C1 Univ Calif Berkeley, Space Sci Lab, Expt Astrophys Grp, Berkeley, CA 94720 USA. CALTECH, Pasadena, CA 91125 USA. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA. Yonsei Univ, Ctr Space Astrophys, Seoul 120749, South Korea. Lab Astrophys Marseille, F-13376 Marseille, France. Carnegie Inst Washington Observ, Pasadena, CA 91101 USA. NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. RP Welsh, BY (reprint author), Univ Calif Berkeley, Space Sci Lab, Expt Astrophys Grp, 7 Gauss Way, Berkeley, CA 94720 USA. EM bwelsh@ssl.berkeley.edu; wheat@ssl.berkeley.edu OI malina, roger/0000-0003-3399-3865; Salim, Samir/0000-0003-2342-7501 NR 10 TC 18 Z9 18 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 2005 VL 130 IS 2 BP 825 EP 831 DI 10.1086/431222 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 948NC UT WOS:000230721600039 ER PT J AU Parker, TL Norton, AJ Mukai, K AF Parker, TL Norton, AJ Mukai, K TI X-ray orbital modulations in intermediate polars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : novae; cataclysmic variables; X-rays : stars; stars : magnetic fields; stars : binaries : close ID CATACLYSMIC VARIABLES; YY DRACONIS; V1223 SGR; RAPID OSCILLATIONS; WHITE-DWARF; TV-COLUMBAE; AE AQUARII; LS-PEGASI; ROSAT OBSERVATIONS; 1WGA J1958.2+3232 AB We present an analysis of 30 archival ASCA and RXTE X-ray observations of 16 intermediate polars to investigate the nature of their orbital modulation. We show that X-ray orbital modulation is widespread amongst these systems, but not ubiquitous as indicated by previous studies that included fewer objects. Only seven of the sixteen systems show a clearly statistically significant modulation depth whose amplitude decreases with increasing X-ray energy. Interpreting this as due to photoelectric absorption in material at the edge of an accretion disc would imply that such modulations are visible for all system inclination angles in excess of 60 degrees. However, it is also apparent that the presence of an X-ray orbital modulation can appear and disappear on a timescale of similar to years or months in an individual system. This may be evidence for the presence of a precessing, tilted accretion disc, as inferred in some low mass X-ray binaries. C1 Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Parker, TL (reprint author), Open Univ, Dept Phys & Astron, Walton Hall, Milton Keynes MK7 6AA, Bucks, England. EM t.l.parker@open.ac.uk; a.j.norton@open.ac.uk; mukai@milkyway.gsfc.nasa.gov OI Norton, Andrew/0000-0001-7619-8269 NR 78 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 AUG PY 2005 VL 439 IS 1 BP 213 EP U110 DI 10.1051/0004-6361:20052887 PG 41 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 948LY UT WOS:000230718500019 ER PT J AU Wilhelm, K Schuhle, U Curdt, W Hilchenbach, M Marsch, E Lemaire, P Bertaux, JL Jordan, SD Feldman, U AF Wilhelm, K Schuhle, U Curdt, W Hilchenbach, M Marsch, E Lemaire, P Bertaux, JL Jordan, SD Feldman, U TI On the nature of the unidentified solar emission near 117 nm SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun : UV radiation; atomic processes; radiation mechanisms : non-thermal ID EXTREME-ULTRAVIOLET SUN; TRANSITION REGION; HELIUM LINES; PARAMETRIC FREQUENCY; CONTINUUM EMISSION; EMITTED RADIATION; NEUTRAL HELIUM; 2-PHOTON DECAY; PHOTON PAIRS; QUIET SUN AB Spectral observations of the Sun in the vacuum-ultraviolet wavelength range by SUMER on SOHO led to the discovery of unusual emission features - called humps here - at 116.70 nm and 117.05 nm on either side of the He. 58.43 nm line. This resonance line is seen in the second order of diffraction, whereas the humps are recorded in the first order with the SUMER spectrometer. In its spectra both orders are superimposed. Two less pronounced humps can be detected at 117.27 nm and near 117.85 nm. After rejecting various possibilities of an instrumental cause of the humps, they are studied in different solar regions. Most of the measurements, in particular those related to the limb-brightening characteristics, indicate that the humps are not part of the background continuum. An assembly of spectrally-unresolved atomic or ionic emission lines might be contributing to the hump at 117.05 nm, but no such lines are known near 116.7 nm. It is concluded that we detect genuine radiation, the generation of which is not understood. A two-photon emission process, parametric frequency down conversion, and molecular emissions are briefly considered as causes of the humps, but a final conclusion could not be reached. C1 Max Planck Inst Sonnensystemforsch, D-37191 Lindau, Germany. Univ Paris 11, CNRS, Unite Mixte, Inst Astrophys Spatiale, F-91405 Orsay, France. CNRS, Serv Aeron, F-91371 Verrieres Le Buisson, France. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Artep Inc, Ellicott City, MD 21042 USA. USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA. RP Wilhelm, K (reprint author), Max Planck Inst Sonnensystemforsch, D-37191 Lindau, Germany. EM wilhelm@mps.mpg.de NR 59 TC 7 Z9 7 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2005 VL 439 IS 2 BP 701 EP 711 DI 10.1051/0004-6361:20042580 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 950UP UT WOS:000230883900037 ER PT J AU Barucci, MA Cruikshank, DP Dotto, E Merlin, F Poulet, F Ore, CD Fornasier, S de Bergh, C AF Barucci, MA Cruikshank, DP Dotto, E Merlin, F Poulet, F Ore, CD Fornasier, S de Bergh, C TI Is Sedna another Triton? SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE TNOs; visible; infrared; spectroscopy; photometry ID WATER ICE; SURFACE; CENTAURS; OBJECTS; ORBITS; ORIGIN AB 90377 Sedna is, so far, the largest and most distant trans-neptunian object. It was observed at visible and near-infrared wavelengths using simultaneously two 8.2 m telescopes at the Very Large Telescope of the European Southern Observatory. The spectrum of Sedna suggests the presence on its surface of different ices ( total abundance > 50%). Its surface composition is different from that determined for other trans-neptunian objects, and apparently resembles that of Triton, particularly in terms of the possible presence of nitrogen and methane ices. C1 Observ Paris, LESIA, F-92195 Meudon, France. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. Univ Paris 11, IAS, F-91405 Orsay, France. SETI Inst, Mountain View, CA USA. Dipartimento Astron, I-35122 Padua, Italy. RP Barucci, MA (reprint author), Observ Paris, LESIA, F-92195 Meudon, France. EM antonella.barucci@obspm.fr; Dale.P.Cruikshank@nasa.gov; dotto@mporzio.astro.it; frederic.merlin@obspm.fr; francois.poulet@ias.u-psud.fr; cdalleore@mail.arc.nasa.gov; fornasier@pd.astro.it; catherine.debergh@obspm.fr OI Dotto, Elisabetta/0000-0002-9335-1656 NR 23 TC 49 Z9 49 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2005 VL 439 IS 2 BP L1 EP L4 DI 10.1051/0004-6361:200500144 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 950UP UT WOS:000230883900001 ER PT J AU Filliatre, P D'Avanzo, P Covino, S Malesani, D Tagliaferri, G McGlynn, S Moran, L Goldoni, P Campana, S Chincarini, G Stella, L Della Valle, M Gehrels, N McBreen, S Hanlon, L McBreen, B Nousek, JA Perna, R AF Filliatre, P D'Avanzo, P Covino, S Malesani, D Tagliaferri, G McGlynn, S Moran, L Goldoni, P Campana, S Chincarini, G Stella, L Della Valle, M Gehrels, N McBreen, S Hanlon, L McBreen, B Nousek, JA Perna, R TI Out of the darkness: the infrared afterglow of the INTEGRAL burst GRB040422 observed with the VLT SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma rays : bursts ID GAMMA-RAY BURST; OPTICAL AFTERGLOW; HOST GALAXY; STANDARD STARS; LOW-REDSHIFT; SPECTROMETER; EXTINCTION; EMISSION; SYSTEM; FAINT AB GRB 040422 was detected by the INTEGRAL satellite at an angle of only 3 degrees from the Galactic plane. Analysis of the prompt emission observed with the SPI and IBIS instruments on INTEGRAL are presented. The IBIS spectrum is well fit by the Band model with a break energy of E-0 = 56 +/- 2 keV and E-peak = 41 +/- 3 keV. The peak flux is 1.8 x 10(-7) erg cm(-2) s(-1) and fluence 3.4 x 10(-7) erg cm(-2) in the range 20-200 keV. We then present the observations of the afterglow of GRB 040422, obtained with the ISAAC and FORS 2 instruments at the VLT less than 2 h after the burst. We report the discovery of its near-infrared afterglow, for which we give the astrometry and photometry. No detection could have been obtained in the R and I bands, partly due to the large extinction in the Milky Way. We imaged the position of the afterglow again two months later in the K-s band, and detected a likely bright host galaxy. We compare the magnitude of the afterglow with those of a compilation of promptly observed counterparts of previous GRBs, and show that the afterglow of GRB 040422 lies at the very faint end of the distribution, brighter only than that of GRB 021211, singled out later and in the optical bands, and GRB 040924 after accounting for Milky Way extinction. This observation suggests that the proportion of dark GRBs can be lowered significantly by a more systematic use of 8-m class telescopes in the infrared in the very early hours after the burst. C1 UMR 7164, Lab Astroparticule & Cosmol, F-75231 Paris, France. CEA Saclay, Serv Astrophys, DSM, DAPNIA,SAp, F-91191 Gif Sur Yvette, France. Univ Insubria, Dipartimento Matemat & Fis, I-22100 Como, Italy. Univ Milan, Dipartimento Fis, I-20126 Milan, Italy. INAF, Osservatorio Astrofis Brera, I-23807 Merate, LC, Italy. SISSA, ISAS, I-34014 Trieste, Italy. Univ Coll Dublin, Dept Expt Phys, Dublin 4, Ireland. Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. ESTEC, Astrophys Miss Div, Res Sci Support Dept ESA, Noordwijk, Netherlands. Penn State Univ, Dept Astron & Astrophys, Davey Lab, University Pk, PA 16802 USA. Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. RP Filliatre, P (reprint author), UMR 7164, Lab Astroparticule & Cosmol, 11 Pl Marcelin Berthelot, F-75231 Paris, France. EM filliatr@cea.fr RI Gehrels, Neil/D-2971-2012; OI Campana, Sergio/0000-0001-6278-1576; Covino, Stefano/0000-0001-9078-5507; Tagliaferri, Gianpiero/0000-0003-0121-0723 NR 93 TC 14 Z9 14 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 AUG PY 2005 VL 438 IS 3 BP 793 EP 801 DI 10.1051/0004-6361:20042609 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 946ZK UT WOS:000230611600006 ER PT J AU Masetti, N Palazzi, E Pian, E Hunt, L Fynbo, JPU Gorosabel, J Klose, S Benetti, S Falomo, R Zeh, A Amati, L Andersen, MI Castro-Tirado, AJ Ceron, JMC Danziger, J Frontera, F Fruchter, AS Greiner, J Hjorth, J Jensen, BL Kaper, L Kouveliotou, C Levan, A Magazzu, A Wijers, RAMJ van den Heuvel, EPJ AF Masetti, N Palazzi, E Pian, E Hunt, L Fynbo, JPU Gorosabel, J Klose, S Benetti, S Falomo, R Zeh, A Amati, L Andersen, MI Castro-Tirado, AJ Ceron, JMC Danziger, J Frontera, F Fruchter, AS Greiner, J Hjorth, J Jensen, BL Kaper, L Kouveliotou, C Levan, A Magazzu, A Wijers, RAMJ van den Heuvel, EPJ TI Late-epoch optical and near-infrared observations of the GRB 000911 afterglow and its host galaxy SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma rays : bursts; supernovae : general; radiation mechanisms : non-thermal; cosmology : observations galaxies : high-redshift; galaxy : fundamental parameters ID GAMMA-RAY BURSTS; SOUTHERN SPECTROPHOTOMETRIC STANDARDS; SPECTRAL ENERGY-DISTRIBUTIONS; HUBBLE-SPACE-TELESCOPE; STAR-FORMATION; FOLLOW-UP; INTERSTELLAR EXTINCTION; LUMINOSITY FUNCTION; MAGELLANIC CLOUD; GRB AFTERGLOWS AB We present the results of an optical and near-infrared (NIR) monitoring campaign of the counterpart of Gamma-Ray Burst (GRB) 000911, located at redshift z = 1.06, from 5 days to more than 13 months after explosion. Our extensive dataset is a factor of 2 larger and spans a time interval similar to 4 times longer than the ones considered previously for this GRB afterglow; this allows a more thorough analysis of its light curve and of the GRB host galaxy properties. The afterglow light curves show a single power-law temporal decline, modified at late times by light from a host galaxy with moderate intrinsic extinction, and possibly by an emerging supernova (SN). The afterglow evolution is interpreted within the classical "fireball" scenario as a weakly collimated adiabatic shock propagating in the interstellar medium. The presence of a SN light curve superimposed on the non-thermal afterglow emission is investigated: while in the optical bands no significant contribution to the total light is found from a SN, the NIR J-band data show an excess which is consistent with a SN as bright as the known hypernova SN1998bw. If the SN interpretation is true, this would be the farthest GRB-associated SN, as well as the farthest core-collapse SN, discovered to date. However, other possible explanations of this NIR excess are also investigated. Finally, we studied the photometric properties of the host, and found that it is likely to be a slightly reddened, subluminous, extreme starburst compact galaxy, with luminosity similar to 0.1 L-star, an age of similar to 0.5 Gyr and a specific Star Formation Rate (SFR) of approximate to 30 M-circle dot yr(-1) (L/L-star)(-1). This is the highest specific SFR value for a GRB host inferred from optical/NIR data. C1 INAF, Ist Astrofis Spaziale & Fis Cosm, Sez Bologna, I-40129 Bologna, Italy. CNR, IASF, I-40126 Bologna, Italy. Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. Ist Radioastron, INAF, Sez Firenze, I-50125 Florence, Italy. Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. CSIC, IAA, Granada, Spain. Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. Osserv Astron Padova, INAF, I-35122 Padua, Italy. Astrophys Inst Potsdam, D-14482 Potsdam, Germany. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Ferrara, Dipartimento Fis, I-44100 Ferrara, Italy. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. INAF, Telescopio Nazl Galileo, Roque Los Muchachos Astron Observ, Santa Cruz de La Palma 38700, Spain. European So Observ, D-85748 Garching, Germany. INAF, Ist AStrofis Spacial & Fis Cosm, Sez Palermo, I-90146 Palermo, Italy. Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. European So Observ, Santiago 19, Chile. RP Masetti, N (reprint author), INAF, Ist Astrofis Spaziale & Fis Cosm, Sez Bologna, Via Gobetti 101, I-40129 Bologna, Italy. EM masetti@bo.iasf.cnr.it RI Fynbo, Johan/L-8496-2014; Hjorth, Jens/M-5787-2014; Jensen, Brian Lindgren/E-1275-2015; Palazzi, Eliana/N-4746-2015; Amati, Lorenzo/N-5586-2015; OI Castro-Tirado, A. J./0000-0003-2999-3563; Falomo, Renato/0000-0003-4137-6541; Hunt, Leslie/0000-0001-9162-2371; Masetti, Nicola/0000-0001-9487-7740; Pian, Elena/0000-0001-8646-4858; Fynbo, Johan/0000-0002-8149-8298; Hjorth, Jens/0000-0002-4571-2306; Palazzi, Eliana/0000-0002-8691-7666; Jensen, Brian Lindgren/0000-0002-0906-9771; Amati, Lorenzo/0000-0001-5355-7388; Magazzu, Antonio/0000-0003-1259-4371; Benetti, Stefano/0000-0002-3256-0016; Wijers, Ralph/0000-0002-3101-1808 NR 95 TC 17 Z9 17 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2005 VL 438 IS 3 BP 841 EP 853 DI 10.1051/0004-6361:20052763 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 946ZK UT WOS:000230611600010 ER PT J AU Feissel-Vernier, M Ma, C Gontier, AM Barache, C AF Feissel-Vernier, M Ma, C Gontier, AM Barache, C TI Sidereal orientation of the Earth and stability of the VLBI celestial reference frame SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE reference systems; Earth ID RADIO-SOURCES AB The consideration of time stability of extragalactic radio sources observed by VLBI is shown to allow the realisation of more consistent celestial reference frames. The impact on the estimation of precession and nutation components is investigated over the time span 1984 - 2002. The precession correction to the IAU 2000 value that is obtained when excluding the unstable sources reaches 49 +/- 5 mu as/year, to be compared to 12 +/- 5 mu as/year using the current conventional celestial frame. The determination of the obliquity rate is unaffected and remains at the level of 27 +/- 2 mu as/year. The observed correction to the 18.6-year nutation amplitude using the current conventional celestial frame ie sizeably corrupted by the unstable sources. After accounting for this effect, the estimations relative to both sets of reference radio sources confirm a discrepancy with the IAU 2000 nutation model with a total amplitude of 320 +/- 100 mu as for the observed nutation in longitude, to be compared to the 80 mu as discrepancy found by Mathews et al. ( 2002, JGRB, 107, 1029). The discrepancy in obliquity amounts to 50 +/- 16 mu as. The effect of source instability is shown to have an impact on the determination of universal time at the one microsecond level. The high and medium frequency nutation terms ( up to periods of a few years) are impacted only in the early years of the program. Chapter 7 concerning the observation of the core and inner core free nutations is paralleled by a twin paper ( Dehant et al. 2005, A&A, 438, 1149) that proposes a theoretical development for their atmospheric and oceanic excitation. C1 Observ Paris, SYRTE, CNRS, UMR 8630, F-75014 Paris, France. Inst Geog Natl, LAREG, F-77455 Marne La Vallee, France. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Feissel-Vernier, M (reprint author), Observ Paris, SYRTE, CNRS, UMR 8630, 61 Av Observ, F-75014 Paris, France. EM feissel@ensg.ign.fr; chopa.ma@nasa.gov; anne-marie.gontier@obspm.fr; christophe.barache@obspm.fr RI Ma, Chopo/D-4751-2012 NR 12 TC 8 Z9 8 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2005 VL 438 IS 3 BP 1141 EP 1148 DI 10.1051/0004-6361:20042209 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 946ZK UT WOS:000230611600037 ER PT J AU Swartz, DA Drake, JJ Elsner, RF Ghosh, KK Grady, CA Wassell, E Woodgate, BE Kimble, RA AF Swartz, DA Drake, JJ Elsner, RF Ghosh, KK Grady, CA Wassell, E Woodgate, BE Kimble, RA TI The Herbig Ae star HD 163296 in X-rays SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : emission-line, Be; stars : individual (HD 163296); stars : pre-main-sequence; X-rays : stars ID T-TAURI STARS; INTERMEDIATE-MASS STARS; LINE-PROFILE-VARIABILITY; MAIN-SEQUENCE EVOLUTION; ACCRETION SHOCK-WAVE; AE/BE STARS; HIGH-RESOLUTION; MAGNETIC-FIELD; AU MICROSCOPII; DISK ACCRETION AB Chandra X-ray imaging spectroscopy of the nearby Herbig Ae star HD 163296 at 100 AU angular resolution is reported. A pointlike, soft (kT similar to 0.5 keV), emission-line source is detected at the location of the star with an X-ray luminosity of 4 x 10(29) ergs s(-1) (log L-X/L-bol = -5.48). In addition, faint emission along the direction of a previously detected Ly alpha-emitting jet and Herbig-Haro outflow may be present. The relatively low luminosity, lack of a hard spectral component, and absence of strong X-ray variability in HD 163296 can be explained as originating from optically thin shock-heated gas accreting onto the stellar surface along magnetic field lines. This would require a ( dipole) magnetic field strength at the surface of HD 163296 of at least similar to 100 G and perhaps as high as several kG. HD 163296 joins the T Tauri star TW Hya in being the only examples known to date of pre-main-sequence stars whose quiescent X-ray emission appears to be completely dominated by accretion. C1 NASA, Univ Space Res Assoc, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NASA, Dept Space Sci, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Eureka Sci, Greenbelt, MD 20771 USA. NASA, Astron & Solar Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Thomas Aquinas Coll, Santa Paula, CA USA. Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. RP Swartz, DA (reprint author), NASA, Univ Space Res Assoc, George C Marshall Space Flight Ctr, SD50, Huntsville, AL 35812 USA. RI Woodgate, Bruce/D-2970-2012 NR 60 TC 45 Z9 45 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 AUG 1 PY 2005 VL 628 IS 2 BP 811 EP 816 DI 10.1086/429984 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 949VX UT WOS:000230817300023 ER PT J AU Hartmann, L Calvet, N Watson, DM D'Alessio, P Furlan, E Sargent, B Forrest, WJ Uchida, KI Green, JD Sloan, GC Chen, CH Najita, J Kemper, F Herter, TL Morris, P Barry, DJ Hall, P AF Hartmann, L Calvet, N Watson, DM D'Alessio, P Furlan, E Sargent, B Forrest, WJ Uchida, KI Green, JD Sloan, GC Chen, CH Najita, J Kemper, F Herter, TL Morris, P Barry, DJ Hall, P TI The accretion disk of the lithium-depleted young binary ST 34 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; infrared : stars; stars : formation; stars : pre-main-sequence ID T-TAURI-STARS; SPITZER-SPACE-TELESCOPE; AURIGA MOLECULAR CLOUD; ALPHA EMISSION STARS; INFRARED SPECTROGRAPH; HYDRAE ASSOCIATION; MODELS; DUST; OBJECTS; EXTINCTION AB We present the infrared spectrum of the young binary system St 34 obtained with the Infrared Spectrograph (IRS) on the Spitzer Space Telescope. The IRS spectrum clearly shows excess dust emission, consistent with the suggestion of White & Hillenbrand that St 34 is accreting from a circumbinary disk. The disk emission of St 34 is low in comparison with the levels observed in typical T Tauri stars; silicate features at similar to 10 and 20 mu m are much weaker than typically seen in T Tauri stars; and excess emission is nearly absent at the shortest wavelengths observed (similar to 5 mu m). These features of the infrared spectrum suggest substantial grain growth ( to eliminate silicate features) and possible settling of dust to the disk midplane ( to reduce the continuum excess emission levels), along with a relatively evacuated inner disk, as expected due to gravitational perturbations by the binary system. Although the position of St 34 in the H-R diagram suggests an age of 8 +/- 3 Myr, assuming that it lies at the distance of the Taurus-Auriga molecular clouds, White & Hillenbrand could not detect any Li I absorption, which would indicate a Li depletion age of roughly 25 Myr or more. We suggest that St 34 is closer than the Taurus clouds by similar to 30 - 40 pc and has an age roughly consistent with Li depletion models. Such an advanced age would make St 34 the oldest known low-mass pre-main-sequence object with a dusty accretion disk. The persistence of optically thick dust emission well outside the binary orbit may indicate a failure to make giant planets that could effectively remove dust particles. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. CALTECH, NASA Herschel Sci Ctr, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. RP Hartmann, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hartmann@cfa.harvard.edu RI Kemper, Francisca/D-8688-2011; OI Kemper, Francisca/0000-0003-2743-8240; Furlan, Elise/0000-0001-9800-6248 NR 51 TC 18 Z9 18 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2005 VL 628 IS 2 BP L147 EP L150 DI 10.1086/432756 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 949VY UT WOS:000230817400016 ER PT J AU Markwick-Kemper, F Green, JD Peeters, E AF Markwick-Kemper, F Green, JD Peeters, E TI Spitzer detections of new dust components in the outflow of the red rectangle SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; dust, extinction; ISM : lines and bands; stars : AGB and post-AGB; stars : individual (HD 44179) ID SPACE-TELESCOPE; MU-M; INFRARED SPECTROGRAPH; MOLECULAR-EMISSION; OPTICAL-PROPERTIES; BENDING MODES; HD-44179; FEATURES; SPECTRA; GRAINS AB We present Spitzer high spectral resolution IRS spectroscopy of three positions in the carbon-rich outflow of post - asymptotic giant branch star HD 44179, better known as the Red Rectangle. Surprisingly, the spectra show some strong unknown mid-infrared resonances, in the 13 - 20 mm range. The shape and position of these resonances vary with position in the nebula, and they are not correlated with the polycyclic aromatic hydrocarbon features. We conclude that these features are due to oxygen-rich minerals, located in a region that is believed to be predominantly carbon-rich. We provide possible explanations for the presence of oxygen-rich dust in the carbon-rich outflows. Simple Mg-Fe oxides (Mg1-xFexO) are suggested as carriers of these unidentified features. C1 Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Markwick-Kemper, F (reprint author), Univ Virginia, Dept Astron, POB 3818, Charlottesville, VA 22903 USA. EM ciska@virginia.edu RI Kemper, Francisca/D-8688-2011 OI Kemper, Francisca/0000-0003-2743-8240 NR 27 TC 6 Z9 6 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2005 VL 628 IS 2 BP L119 EP L122 DI 10.1086/432833 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 949VY UT WOS:000230817400009 ER PT J AU Hudson, RL Khanna, RK Moore, MH AF Hudson, RL Khanna, RK Moore, MH TI Laboratory evidence for solid-phase protonation of HNCO in interstellar ices SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE astrochemistry; infrared : ISM; ISM : clouds; ISM : molecules; methods : laboratory; molecular processes ID ION-MOLECULE REACTIONS; ISOCYANIC ACID; INFRARED-SPECTRUM; FTIR SPECTROSCOPY; LOW-TEMPERATURE; GAS-PHASE; REACTIVITY; FORMAMIDE; CHLORIDE; ANALOGS AB A recent study reported production of amino formate, HC(O)ONH2 on warming a solid-phase HNCO + HCl + H2O mixture. Here we reinterpret those results and suggest that the synthesis of amino formate is unlikely and that what was actually observed was the production of ClC(O) NH2 by a low-temperature, solid-phase acid-base reaction. The published infrared spectra are reexamined and are in full agreement with ClC(O) NH2. This new interpretation also agrees with chemical expectations, previous laboratory work, and new density-functional calculations. A number of acid-base pairs are already known in the interstellar medium, and our new interpretation of HNCO + HCl + H2O chemistry suggests that the H2NCO+ cation is probably interstellar as well. C1 Eckerd Coll, Dept Chem, St Petersburg, FL 33711 USA. Univ Maryland, Dept Chem & Biochem, College Pk, MD 20742 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Eckerd Coll, Dept Chem, St Petersburg, FL 33711 USA. EM hudsonrl@eckerd.edu RI Hudson, Reggie/E-2335-2012 NR 33 TC 10 Z9 10 U1 2 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD AUG PY 2005 VL 159 IS 2 BP 277 EP 281 DI 10.1086/430703 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 949VV UT WOS:000230817100004 ER PT J AU Ajello, J Palle, PV Abgrall, H Roueff, E Bhardwaj, A Gustin, J AF Ajello, J Palle, PV Abgrall, H Roueff, E Bhardwaj, A Gustin, J TI The electron excited ultraviolet spectrum of HD: Cross sections and transition probabilities SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE molecular data ID MOLECULAR-HYDROGEN; DISSOCIATIVE EXCITATION; EXTREME-ULTRAVIOLET; VACUUM-ULTRAVIOLET; EMISSION-SPECTRUM; IMPACT EXCITATION; UPPER-ATMOSPHERE; BETA EMISSION; BAND SYSTEMS; SOLAR EUV AB We have analyzed the high-resolution ultraviolet (UV) emission spectrum of molecular deuterium hydride (HD) excited by electron impact at 100 eV under optically thin, single-scattering experimental conditions. The high-resolution spectrum (FWHM = 160 m angstrom) spans the wavelength range from 900 to 1650 angstrom and contains the two Rydberg series of HD: (1)Sigma(u)(+) 1s sigma, np sigma(B, B', B '', n = 2, 3, 4) --> X (1)Sigma(g)(+) and (1)Pi(u)(+)1s sigma, np pi(C, D', D '', D '', n = 2, 3, 4, 5) --> X (1)Sigma(g)(+). A model spectrum of HD, based on newly calculated transition probabilities and line positions including rovibrational coupling for the strongest band systems, B 1 Sigma(u)(+)- X (1)Sigma(+)(g), B' (1)Sigma(u)(+)- X (1)Sigma(g)(+), C (1)Pi(u) - X (1)Sigma(g)(+), and D (1)Pi(u) X (1)Sigma(g)(+), is in excellent agreement with observed intensities. The cross sections for direct excitation at 100 eV of the B (1)Sigma(u)(+), B' (1)Sigma(u)(+), C (1)Pi(u), and D (1)Pi(u) states were derived from a model analysis of the experimental fluorescence spectrum to the ground state. The absolute cross section values for excitation to the B (1)Sigma(u)(+), B' (1)Sigma(u)(+), C (1)Pi(u), and D (1)Pi(u) states were found to be (2.57 +/- 0.26) x 10(-17), (0.22 +/- 0.06) x 10(-17), (2.54 +/- 0,25) x 10(-17), and (0.17 +/- 0.04) x 10(-17) cm(2), respectively. We have also determined the dissociative excitation cross sections at 100 eV for the emission of Ly alpha at 1216 angstrom and Ly beta at 1025 angstrom lines, which are (7.98 +/- 1.12) x 10(-18) and (0.40 +/- 0.10) x 10(-18) cm(2), respectively. The summed excitation function of the closely spaced pair of lines, H Ly alpha and D Ly alpha, resulting from dissociative excitation of HD, has been measured from the threshold to 800 eV and is analytically modeled with a semiempirical relation. The model cross sections are in good agreement with the corrected Ly alpha cross sections of Mohlmann et al. up to 2 keV. Based on measurements of H, D (2s) production cross section values by Mohlmann et al., the H, D (n = 2) cross section is estimated to be 1.6 x 10(-17) cm(2) at 100 eV. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Observ Paris, LUTH, F-92195 Meudon, France. Observ Paris, CNRS, UMR 8102, F-92195 Meudon, France. NASA, George C Marshall Space Flight Ctr, Space Sci Branch, Huntsville, AL 35805 USA. Univ Liege, Liege, Belgium. RP Ajello, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. OI Bhardwaj, Anil/0000-0003-1693-453X NR 64 TC 7 Z9 7 U1 0 U2 4 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 AUG PY 2005 VL 159 IS 2 BP 314 EP 330 DI 10.1086/431309 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 949VV UT WOS:000230817100007 ER PT J AU Serrador, JM Wood, SJ AF Serrador, JM Wood, SJ TI Vasopressin: Neurohumoral link between nausea and motion sickness - Response SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Letter ID MIDDLE CEREBRAL-ARTERIES; FAILURE C1 Harvard Univ, Sch Med, Boston, MA 02115 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Serrador, JM (reprint author), Harvard Univ, Sch Med, Boston, MA 02115 USA. RI Serrador, Jorge/A-9172-2009 NR 10 TC 0 Z9 0 U1 0 U2 0 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD AUG PY 2005 VL 76 IS 8 BP 805 EP 806 PG 2 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 950MM UT WOS:000230861400017 ER PT J AU Eyring, V Harris, NRP Rex, M Shepherd, TG Fahey, DW Amanatidis, GT Austin, J Chipperfield, MP Dameris, M Forster, PMF Gettelman, A Graf, HF Nagashima, T Newman, PA Pawson, S Prather, MJ Pyle, JA Salawitch, RJ Santer, BD Waugh, DW AF Eyring, V Harris, NRP Rex, M Shepherd, TG Fahey, DW Amanatidis, GT Austin, J Chipperfield, MP Dameris, M Forster, PMF Gettelman, A Graf, HF Nagashima, T Newman, PA Pawson, S Prather, MJ Pyle, JA Salawitch, RJ Santer, BD Waugh, DW TI A strategy for process-oriented validation of coupled chemistry-climate models SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID MIDDLE ATMOSPHERE MODEL; QUASI-BIENNIAL OSCILLATION; STRATOSPHERIC WATER-VAPOR; GENERAL-CIRCULATION MODEL; ARCTIC OZONE LOSS; INTERACTIVE CHEMISTRY; POLAR VORTEX; INTERANNUAL VARIABILITY; POTENTIAL VORTICITY; 3-DIMENSIONAL MODEL AB Evaluating CCMs with the presented framework will increase our confidence in predictions of stratospheric ozone change. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Calif Irvine, Earth Syst Sci Dept, Irvine, CA USA. Univ Cambridge, Dept Chem, Ctr Atmospher Sci, Cambridge CB2 1EW, England. CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. Lawrence Livermore Natl Lab, Program Climate Model Diag & Intercompar, Livermore, CA USA. Johns Hopkins Univ, Baltimore, MD USA. RP DLR, Inst Atmospher Phys, Oberpfaffenhofen, Germany. EM Veronika.Eyring@dlr.de RI Newman, Paul/D-6208-2012; Chipperfield, Martyn/H-6359-2013; Forster, Piers/F-9829-2010; Fahey, David/G-4499-2013; Pawson, Steven/I-1865-2014; Waugh, Darryn/K-3688-2016; Eyring, Veronika/O-9999-2016; Rex, Markus/A-6054-2009; Salawitch, Ross/B-4605-2009; Santer, Benjamin/F-9781-2011 OI Harris, Neil/0000-0003-1256-3006; Newman, Paul/0000-0003-1139-2508; Chipperfield, Martyn/0000-0002-6803-4149; Forster, Piers/0000-0002-6078-0171; Fahey, David/0000-0003-1720-0634; Pawson, Steven/0000-0003-0200-717X; Waugh, Darryn/0000-0001-7692-2798; Eyring, Veronika/0000-0002-6887-4885; Rex, Markus/0000-0001-7847-8221; Salawitch, Ross/0000-0001-8597-5832; NR 87 TC 87 Z9 90 U1 2 U2 10 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 EI 1520-0477 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD AUG PY 2005 VL 86 IS 8 BP 1117 EP 1133 DI 10.1175/BAMS-86-8-1117 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 954YV UT WOS:000231192300014 ER PT J AU Rumsey, CL Rivers, SM Morrison, JH AF Rumsey, CL Rivers, SM Morrison, JH TI Study of CFD variation on transport configurations from the second drag-prediction workshop SO COMPUTERS & FLUIDS LA English DT Article ID TURBULENCE MODEL; FLOWS AB This paper describes and analyzes a series of nearly 90 CFD test cases performed as a contribution to the second Drag Prediction Workshop, held in Orlando, Florida in June 2003. Two configurations are included: DLR-F6 wing-body and wing-body-nacelle-pylon. The ability of CFD to predict the drag, lift, and pitching moment from experiment-including the "delta" arising from the addition of the nacelle and pylon-is assessed. In general, at a fixed angle of attack CFD overpredicts lift, but predicts the Delta C-L reasonably well. At low lift levels (C-L < 0.3), Delta C-D is 20-30 drag counts (30-45%) high. At the target lift coefficient of C-L = 0.5, Delta C-D is overpredicted by between 1 and 16 counts. However, the primary contribution of this paper is note so much the assessment of CFD against experiment, but rather a detailed assessment and analysis of CFD variation. The series of test cases are designed to determine the sensitivity/variability of CFD to a variety of factors, including grid, turbulence model, transition, code, and viscous model. Using medium-level grids (6-11 million points) at the target lift coefficient, the maximum variation in drag due to different grids is 5-11 drag counts, due to code is 5-10 counts, due to turbulence model is 715 counts, due to transition is 10-11 counts, and due to viscous model is 4-5 counts. Other specific variations are described in the paper. (c) 2004 Elsevier Ltd. All rights reserved. C1 NASA, Langley Res Ctr, Computat Modeling & Simulat Branch, Hampton, VA 23681 USA. Configurat Aerodynam Branch, Hampton, VA 23681 USA. RP Rumsey, CL (reprint author), NASA, Langley Res Ctr, Computat Modeling & Simulat Branch, Mail Stop 128, Hampton, VA 23681 USA. EM c.l.rumsey@larc.nasa.gov NR 22 TC 5 Z9 8 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0045-7930 J9 COMPUT FLUIDS JI Comput. Fluids PD AUG PY 2005 VL 34 IS 7 BP 785 EP 816 DI 10.1016/j.compfluid.2004.07.003 PG 32 WC Computer Science, Interdisciplinary Applications; Mechanics SC Computer Science; Mechanics GA 936RR UT WOS:000229873600002 ER PT J AU Sobczak, N Singh, M Asthana, R AF Sobczak, Natalia Singh, Mrityunjay (Jay) Asthana, Rajiv TI High-temperature capillarity and interfacial phenomena SO CURRENT OPINION IN SOLID STATE & MATERIALS SCIENCE LA English DT Editorial Material C1 Foundry Res Inst, Krakow, Poland. NASA, Glenn Res Ctr, Ohio Aerosp Inst, Cleveland, OH USA. Univ Wisconsin Stout, Menomonie, WI USA. RP Sobczak, N (reprint author), Foundry Res Inst, Krakow, Poland. EM natalie@iod.krakow.pl NR 0 TC 3 Z9 3 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1359-0286 J9 CURR OPIN SOLID ST M JI Curr. Opin. Solid State Mat. Sci. PD AUG-OCT PY 2005 VL 9 IS 4-5 BP 149 EP 151 DI 10.1016/j.cossms.2006.07.006 PG 3 WC Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Materials Science; Physics GA 114EE UT WOS:000242648700001 ER PT J AU Sobczak, N Singh, M Asthana, R AF Sobczak, Natalia Singh, Mrityunjay Asthana, Rajiv TI High-temperature wettability measurements in metal/ceramic systems - Some methodological issues SO CURRENT OPINION IN SOLID STATE & MATERIALS SCIENCE LA English DT Review DE metal/ceramic systems; contact angle; high-temperature wettability; sessile drop test ID CONTACT-ANGLE; ALUMINUM; ROUGHNESS; SAPPHIRE; SURFACES; ALLOYS AB Methodological differences and inconsistencies in characterizing the wettability in molten metal/solid ceramic systems between different laboratories and research groups are a major source of discrepancy in the measurements of contact angle, theta, surface tension, sigma(lv) and work of adhesion, W-ad reported in the literature. The extreme sensitivity of these parameters to test conditions leads to considerable disagreement between test outcomes for a particular. system from different investigators. In this paper, we focus on some methodological considerations that influence the wettability test outcomes in high-temperature systems. In particular, we highlight the role of substrate surface and atmosphere on the contact angle values in ceramic/metal systems. We also identify practical problems in executing the sessile drop wettability test that influence the test outcomes, and argue in favor of increased uniformity and consistency in conducting the tests and greater transparency in reporting the test conditions and test outcomes. in order to minimize the current discrepancies in measurements. (c) 2006 Elsevier Ltd. All rights reserved. C1 Ctr High Temp Studies Met & Alloys, Foundry Res Inst, Krakow, Poland. NASA, Glenn Res Ctr, Ohio Aerosp Inst, Cleveland, OH 44135 USA. Univ Wisconsin Stout, Menomonie, WI 54751 USA. RP Sobczak, N (reprint author), Ctr High Temp Studies Met & Alloys, Foundry Res Inst, 73 Zakopianska St, Krakow, Poland. EM natalie@iod.krakow.pl; Mrityunjay.Singh@grc.nasa.gov; asthanar@uwstout.edu NR 50 TC 49 Z9 52 U1 1 U2 14 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1359-0286 J9 CURR OPIN SOLID ST M JI Curr. Opin. Solid State Mat. Sci. PD AUG-OCT PY 2005 VL 9 IS 4-5 BP 241 EP 253 DI 10.1016/j.cossms.2006.07.007 PG 13 WC Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Materials Science; Physics GA 114EE UT WOS:000242648700013 ER PT J AU Clement, G Reschke, M Wood, ST AF Clement, G Reschke, M Wood, ST TI Neurovestibular and sensorimotor studies in space and earth benefits SO CURRENT PHARMACEUTICAL BIOTECHNOLOGY LA English DT Review DE sensory-motor function; gravity; microgravity; adaptation; posture; movement; spatial orientation; neurosciences ID VERTICAL AXIS ROTATION; OPTOKINETIC AFTER-NYSTAGMUS; OTOLITH-OCULAR REFLEXES; LINEAR ACCELERATION; EYE-MOVEMENTS; POSTURAL CONTROL; PROLONGED WEIGHTLESSNESS; VESTIBULAR EXPERIMENTS; REBOUND NYSTAGMUS; MOTION PERCEPTION AB This review summarizes what has been learned from studies of human neurovestibillar system in weightless conditions, including balance and locomotion, gaze control, vestibular-autonomic function and spatial orientation, and gives some examples of the potential Earth benefits of this research. Results show that when astronauts and cosmonauts return from space flight both the peripheral and central neural processes are physiologically and functionally altered. There are clear distinctions between the virtually immediate adaptive compensations to weightlessness and those that require longer periods of time to adapt. However, little is known to date about the adaptation of sensory-motor functions to long-duration space missions in weightlessness and to the transitions between various reduced gravitational levels, such as on the Moon and Mars. Results from neurovestibular research in space have substantially enhanced our understanding of the mechanisms and characteristics of postural, gaze, and spatial orientation deficits, analogous to clinical cases of labyrinthine-defective function. Also, space neurosciences research has participated in the development and application of significant new technologies, Such as video recording and processing of three-dimensional eye movements and posture, hardware for the unencumbered measurement of head and body movement, and procedures for investigating otolith function on Earth. In particular, devices such as centrifugation or off-vertical axis rotation could enhance clinical neurological testing because it provides linear acceleration which specifically stimulates the otolith organs in a frequency range close to natural head and body movement. C1 Univ Toulouse 3, CNRS, UMR 5549, Ctr Rech Cerveau & Cognit, F-31062 Toulouse, France. NASA, Lyndon B Johnson Space Ctr, Neurosci Lab, Houston, TX 77058 USA. RP Clement, G (reprint author), Univ Toulouse 3, CNRS, UMR 5549, Ctr Rech Cerveau & Cognit, 113 Route Narbonne, F-31062 Toulouse, France. EM gilles.clement@cerco.tips-tlse.fr NR 80 TC 12 Z9 13 U1 1 U2 8 PU BENTHAM SCIENCE PUBL LTD PI SHARJAH PA EXECUTIVE STE Y26, PO BOX 7917, SAIF ZONE, 1200 BR SHARJAH, U ARAB EMIRATES SN 1389-2010 J9 CURR PHARM BIOTECHNO JI Curr. Pharm. Biotechnol. PD AUG PY 2005 VL 6 IS 4 BP 267 EP 283 DI 10.2174/1389201054553716 PG 17 WC Biochemistry & Molecular Biology; Pharmacology & Pharmacy SC Biochemistry & Molecular Biology; Pharmacology & Pharmacy GA 951FA UT WOS:000230913300003 PM 16101466 ER PT J AU Macias, BR Groppo, ER Eastlack, RK Watenpaugh, DE Lee, SMC Schneider, SM Boda, WL Smith, SM Cutuk, A Pedowitz, RA Meyer, RS Hargens, AR AF Macias, BR Groppo, ER Eastlack, RK Watenpaugh, DE Lee, SMC Schneider, SM Boda, WL Smith, SM Cutuk, A Pedowitz, RA Meyer, RS Hargens, AR TI Space exercise and Earth benefits SO CURRENT PHARMACEUTICAL BIOTECHNOLOGY LA English DT Review DE exercise; space flight; microgravity; countermeasure; bed rest; LBNP; LBPP; rehabilitation ID BODY NEGATIVE-PRESSURE; CELLS IN-VITRO; BED-REST; SIMULATED MICROGRAVITY; UPRIGHT EXERCISE; BIOCHEMICAL-CHANGES; CALCIUM-METABOLISM; MUSCLE ACTIVATION; SKELETAL-MUSCLE; FLUID SHEAR AB The detrimental impact of long duration space flight on physiological systems necessitates the development of exercise countermeasures to protect work capabilities in gravity fields of Earth, Moon and Mars. The respective rates of physiological deconditioning for different organ systems during space flight has been described as a result of data collected during and after missions on the Space Shuttle, International Space Station, Mir, and bed rest Studies on Earth. An integrated countermeasure that simulates the body's hydrostatic pressure gradient, provides mechanical stress to the bones and muscles, and stimulates the neurovestibular system may be critical for maintaining health and well being of crew during long-duration space travel, such as a mission to Mars. Here we review the results of our studies to date of an integrated exercise countermeasure for space flight, lower body negative pressure (LBNP) treadmill exercise, and potential benefits of its application to athletic training on Earth. Additionally, we review the benefits of Lower Body Positive Pressure (LBPP) exercise for rehabilitation of postoperative patients. Presented first are preliminary data from a 30-day bed rest study evaluating the efficacy of LBNP exercise as an integrated exercise countermeasure for the deconditioning effects of microgravity. Next, we review upright LBNP exercise as a training modality for athletes by evaluating effects on the cardiovascular system and gait mechanics. Finally, LBPP exercise as a rehabilitation device is examined with reference to gait mechanics and safety in two groups of postoperative patients. C1 Univ Calif San Diego, Dept Orthopaed Surg, San Diego, CA 92103 USA. Wyle Labs, Houston, TX 77058 USA. Univ New Mexico, Albuquerque, NM 87131 USA. Sonoma State Univ, Rohnert Pk, CA 94928 USA. NASA, Lyndon B Johnson Space Ctr, Human Adaptat & Countermeasures Off, Houston, TX 77058 USA. RP Hargens, AR (reprint author), Univ Calif San Diego, Dept Orthopaed Surg, 350 Dickinson St,Suite 121, San Diego, CA 92103 USA. EM ahargens@ucsd.edu NR 62 TC 10 Z9 11 U1 0 U2 8 PU BENTHAM SCIENCE PUBL LTD PI SHARJAH PA EXECUTIVE STE Y26, PO BOX 7917, SAIF ZONE, 1200 BR SHARJAH, U ARAB EMIRATES SN 1389-2010 J9 CURR PHARM BIOTECHNO JI Curr. Pharm. Biotechnol. PD AUG PY 2005 VL 6 IS 4 BP 305 EP 317 DI 10.2174/1389201054553653 PG 13 WC Biochemistry & Molecular Biology; Pharmacology & Pharmacy SC Biochemistry & Molecular Biology; Pharmacology & Pharmacy GA 951FA UT WOS:000230913300006 PM 16101469 ER PT J AU Pope, K Masuoka, P Rejmankova, E Grieco, J Johnson, S Roberts, D AF Pope, K Masuoka, P Rejmankova, E Grieco, J Johnson, S Roberts, D TI Mosquito habitats, land use, and malaria risk in Belize from satellite imagery SO ECOLOGICAL APPLICATIONS LA English DT Article DE Belize; land use; malaria; marsh; mosquito; remote sensing; satellite imagery; Typha domingensis ID ANOPHELES-ALBIMANUS WIEDEMANN; CULICIDAE LARVAL HABITATS; CENTRAL-AMERICA; YUCATAN PENINSULA; FLIGHT RANGE; EL-SALVADOR; EVERGLADES; DIPTERA; VEGETATION; RADAR AB Satellite imagery of northern Belize is used to examine the relationship between land use and habitats of the malaria vector, the Anopheles mosquito. A land cover classification based on multispectral Systeme Probatoire d'Observation de la Terra (SPOT) and multitemporal Radarsat images identified I I land cover classes, including agricultural, forest, and marsh types. Two of the land cover types, Typha domingensis marsh and flooded forest, are habitats of immature Anopheles vestitipennis, and one, Eleocharis spp. marsh, is the habitat for immature Anopheles albimanus. Geographic information systems (GIS) analyses of land cover demonstrate that the amount of Typha domingensis in a marsh is positively correlated with the amount of agricultural land in the adjacent upland and negatively correlated with the amount of adjacent forest. This finding, coupled with field studies documenting higher soil phosphorus in wetlands adjacent to agricultural fields, supports the hypothesis that nutrient runoff is the cause of higher densities of Typha domingensis in marshes adjacent to fields in northern Belize. Thus, agricultural activities can potentially increase Anopheles vestitipennis habitat and thereby increase malaria risk across a broad region where Anopheles vestitipennis is a malaria vector. C1 Geo Eco Arc Res, Aquasco, MD 20608 USA. NASA, Goddard Space Flight Ctr, Uniformed Serv Univ Hlth Sci, Greenbelt, MD 20771 USA. Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA. Uniformed Serv Univ Hlth Sci, Dept Prevent Med & Biometr, Bethesda, MD 20814 USA. RP Masuoka, P (reprint author), Geo Eco Arc Res, 16305 St Marys Church Rd, Aquasco, MD 20608 USA. EM penny@ltpmail.gsfc.nasa.gov NR 41 TC 36 Z9 38 U1 2 U2 21 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1707 H ST NW, STE 400, WASHINGTON, DC 20006-3915 USA SN 1051-0761 J9 ECOL APPL JI Ecol. Appl. PD AUG PY 2005 VL 15 IS 4 BP 1223 EP 1232 DI 10.1890/04-0934 PG 10 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 950SE UT WOS:000230876900012 ER PT J AU DeGayner, EJ Kramer, MG Doerr, JG Robertsen, MJ AF DeGayner, EJ Kramer, MG Doerr, JG Robertsen, MJ TI Windstorm disturbance effects on forest structure and black bear dens in southeast Alaska SO ECOLOGICAL APPLICATIONS LA English DT Article DE black bear denning ecology; disturbance; forest dynamics; forest succession; spatially explicit models; telemetry; windthrow; winter den site selection ID TEMPERATE RAIN-FORESTS; DYNAMICS; AMERICA; NORTH AB We examined the relationships among forest susceptibility to windstorm damage, forest structure, and black bear winter den site selection in the coastal temperate rain forests of southeastern Alaska, USA. Forest susceptibility to maritime windstorms was determined by applying a wind-disturbance model (WINDSTORM) to two study areas where bear dens had been identified by radio telemetry. We evaluated model predictions for forest structure against field data for one study area. As predicted, forests in wind-protected landscapes contained features indicative of later stages of forest development where larger and older trees are more abundant. By contrast, forests located in storm-susceptible locations contained higher tree densities, less variation in tree diameters, smaller trees, and less evidence of large, old trees with heart rot. Analysis of habitat use relative to its availability on the landscape indicates that bears selected wind-protected landscapes over storm-prone landscapes in both study areas for winter dens. The majority (58%) of den sites were located in forests most protected from catastrophic storm effects. By contrast, only 6% were located in forests most exposed to storm damage. Results suggest that forests most protected from catastrophic windstorm disturbance contain more suitable overwinter habitat for black bears as evidenced by den site selection. C1 US Forest Serv, USDA, Alaska Reg, Petersburg, AK 99833 USA. NASA, Ames Res Ctr, Ecosyst Sci & Technol Branch, Moffett Field, CA 94035 USA. US Forest Serv, USDA, Wrangell Ranger Dist, Wrangell, AK 99929 USA. RP DeGayner, EJ (reprint author), US Forest Serv, USDA, Eastern Reg, 626 E Wisconsin Ave, Milwaukee, WI 53201 USA. EM edegayner@fs.fed.us NR 38 TC 7 Z9 7 U1 1 U2 9 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1707 H ST NW, STE 400, WASHINGTON, DC 20006-3915 USA SN 1051-0761 J9 ECOL APPL JI Ecol. Appl. PD AUG PY 2005 VL 15 IS 4 BP 1306 EP 1316 DI 10.1890/03-5385 PG 11 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 950SE UT WOS:000230876900019 ER PT J AU Spencer, ML Stoner, AW Ryer, CH Munk, JE AF Spencer, ML Stoner, AW Ryer, CH Munk, JE TI A towed camera sled for estimating abundance of juvenile flatfishes and habitat characteristics: Comparison with beam trawls and divers SO ESTUARINE COASTAL AND SHELF SCIENCE LA English DT Article DE survey technique; video; fish; habitat ID CORAL-REEF FISHES; CANCER-MAGISTER; ENGLISH SOLE; CONTINENTAL-SHELF; DUNGENESS CRABS; VISUAL CENSUS; EFFICIENCY; SELECTION; TRANSECT; VETULUS AB An inexpensive towed video camera sled was developed to provide abundance estimates for juvenile flatfishes and other benthic taxa, and to characterize habitat features. The camera sled was compared with beam trawls and diver survey methods in Yaquina Bay, Oregon, and in bays of Kodiak Island, Alaska. In Yaquina Bay the camera sled with a tickler chain (to induce flatfish movement) yielded density estimates for juvenile flatfish (English sole, Pleuronectes vetulus) that were equivalent to those of the divers, but greater than with a I in beam trawl or the camera sled without a tickler chain. Crab (Cancer magister) density estimates were similar between the divers and the camera sled (with or without the tickler chain), but were underestimated with the beam trawl. In Kodiak, densities of juvenile flatfish (northern rock sole, Lepidopsetta polyxystra) were similar between the camera sled with a tickler chain, divers, and a 2 in beam trawl. Density estimates from the camera sled were obtainable for flatfish as small as 20 mm. Habitat features, such as empty bivalve shells, were underestimated with the beam trawl compared with the divers and the camera sled. These results demonstrate the effectiveness of an inexpensive, simple to operate, towed camera sled in surveying abundance and habitat associations of juvenile flatfishes, crabs, and other taxa. Published by Elsevier Ltd. C1 NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Newport, OR 97365 USA. Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Kodiak, AK 99615 USA. RP Spencer, ML (reprint author), NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, 2030 S Marine Sci Dr, Newport, OR 97365 USA. EM mara.spencer@noaa.gov NR 34 TC 30 Z9 31 U1 5 U2 18 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0272-7714 EI 1096-0015 J9 ESTUAR COAST SHELF S JI Estuar. Coast. Shelf Sci. PD AUG PY 2005 VL 64 IS 2-3 BP 497 EP 503 DI 10.1016/j.ecss.2005.03.012 PG 7 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 950QV UT WOS:000230873200034 ER PT J AU Mielke, AF Seasholtz, RG Elam, KA Panda, J AF Mielke, AF Seasholtz, RG Elam, KA Panda, J TI Time-average measurement of velocity, density, temperature, and turbulence velocity fluctuations using Rayleigh and Mie scattering SO EXPERIMENTS IN FLUIDS LA English DT Article ID BRILLOUIN-SCATTERING; LASER VELOCIMETER; KINETIC-MODEL; GAS AB Measurement of time-averaged velocity, density, temperature, and turbulence velocity fluctuations in sparsely seeded gas flows using a non-intrusive, point-wise technique based on Rayleigh and Mie scattering is discussed. A Fabry-Perot interferometer (FPI) is used to spectrally resolve laser light scattered by molecules and particulates in gas flows. The spectral content of the scattered light provides information about velocity, density, and temperature of the gas. A CCD camera is used to record images of the fringes formed by scattered light passing through the interferometer. Models of the spectral components are used in a least squares fitting routine to estimate the parameters from fringe images. Flow measurements are presented for subsonic and supersonic jet flows. The application range for this technique is mostly for high velocity situations (> 25 m/s). Velocity, density, temperature, and turbulence velocity fluctuations were determined with accuracies within 5 m/s, 4%, 2%, and 5 m/s, respectively. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. Akima Corp, Fairview Pk, OH 44126 USA. OAI, Brookpark, OH 44142 USA. RP Mielke, AF (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,MS 77-1, Cleveland, OH 44135 USA. EM amy.f.mielke@nasa.gov NR 25 TC 12 Z9 13 U1 0 U2 4 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0723-4864 J9 EXP FLUIDS JI Exp. Fluids PD AUG PY 2005 VL 39 IS 2 BP 441 EP 454 DI 10.1007/s00348-005-0990-8 PG 14 WC Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA 959EX UT WOS:000231501300026 ER PT J AU Cai, JN Leung, PS Pan, ML Pooley, S AF Cai, JN Leung, PS Pan, ML Pooley, S TI Economic linkage impacts of Hawaii's longline fishing regulations SO FISHERIES RESEARCH LA English DT Article DE Hawaii longline fisheries; economic impacts; input-output modeling; backward linkages; forward linkage ID INPUT-OUTPUT MODEL; PLAUSIBILITY AB Fisheries regulations driven by environmental concerns would not only directly affect fisheries sectors but also tend to indirectly influence other sectors through intersectoral input-output linkages. This paper examines both backward and forward linkages of Hawaii's fisheries sectors to the rest of the economy, and based on this evaluates the potential economic impacts of longline fishing regulations in Hawaii. We find that Hawaii's fisheries sectors have strong linkages it) the rest of the economy, regulations on them will thus have profound economic impacts. (C) 2005 Elsevier B.V. All rights reserved. C1 Univ Hawaii Manoa, Coll Trop Agr & Human Resources, Honolulu, HI 96822 USA. Univ Hawaii Manoa, Dept Econ, Honolulu, HI 96822 USA. Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA. RP Leung, PS (reprint author), Univ Hawaii Manoa, Coll Trop Agr & Human Resources, 3050 Maile Way,Gilmore 111, Honolulu, HI 96822 USA. EM psleung@hawaii.edu NR 16 TC 15 Z9 15 U1 1 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0165-7836 J9 FISH RES JI Fish Res. PD AUG PY 2005 VL 74 IS 1-3 BP 232 EP 242 DI 10.1016/j.fishres.2005.02.006 PG 11 WC Fisheries SC Fisheries GA 941XY UT WOS:000230248700020 ER PT J AU Hansen, CJ Shemansky, DE Hendrix, AR AF Hansen, CJ Shemansky, DE Hendrix, AR TI Cassini UVIS observations of Europa's oxygen atmosphere and torus SO ICARUS LA English DT Article DE Europa; satellites, atmospheres ID OUTER SOLAR-SYSTEM; JOVIAN MAGNETOSPHERE; WATER ICE; GAS TORUS; SURFACES; GANYMEDE; JUPITER AB Observations of the Europa environment using the Cassim UltraViolet Imaging Spectrograph (UVIS) show the presence of an extended atomic oxygen atmosphere in addition to the bound molecular oxygen atmosphere first detected by Hubble Space Telescope in 1994 [D.T. Hall, D.F.. Strobel, P.D. Feldman, M.A. McGrath, H.A. Weaver, 1995, Detection of an oxygen atmosphere on Jupiter's moon Europa, Nature 373, 677-679]. The atomic oxygen measurement provides a direct constraint on the sputtering and loss of Europa's water ice surface and the interaction of Europa's atmosphere with Jupiter's magnetosphere. We derive a loss rate for O-2 based on the emission rate of the OI 1356 angstrom multiplet. UVIS detected substantial variability in the oxygen emission from Europa's oxygen atmosphere that we attribute to the viewing geometry. B.H. Mauk, D.G. Mitchell, S.M. Krimigis, E.C. Roelof, C.P. Paranicas [2003, Energetic neutral atoms from a trans-Europa gas torus at Jupiter, Nature 421, 920-922] inferred the presence of a torus of neutral gas at Europa's orbit based on Cassini's energetic neutral atom (ENA) image of the Jupiter system acquired with the Magnetospheric Imaging Instrument (MIMI), with the most likely torus constituents being hydrogen and oxygen species sputtered from Europa. Cassini UVIS data rule out O and O-2 as the possible torus species reported by Mauk et al. however, unless the torus density is so low that it is undetectable by UVIS (less than 8 atoms/cm(3)). The UVIS observations indicate the presence of atomic hydrogen and possibly other species, but a full analysis is deferred to a following paper. The hydrogen in the present observations shows a local-time asymmetry and complex spatial distribution. Published by Elsevier Inc. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ So Calif, Dept Aerosp Engn, Los Angeles, CA 90089 USA. RP Hansen, CJ (reprint author), CALTECH, Jet Prop Lab, Mail Stop 169-237,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM candice.j.hansen@jpl.nasa.gov; dons@hippolyta.usc.edu; amanda.r.hendrix@jpl.nasa.gov NR 22 TC 30 Z9 30 U1 0 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD AUG PY 2005 VL 176 IS 2 BP 305 EP 315 DI 10.1016/j.icarus.2005.02.007 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 946AA UT WOS:000230543000004 ER PT J AU Mayo, LA Samuelson, RE AF Mayo, LA Samuelson, RE TI Condensate clouds in Titan's north polar stratosphere SO ICARUS LA English DT Article DE titan; condensates; stratosphere; clouds ID VOYAGER INFRARED OBSERVATIONS; VERTICAL-DISTRIBUTION; OPTICAL-CONSTANTS; LOWER ATMOSPHERE; MODEL; SPECTRA; METHANE; TEMPERATURE; TROPOSPHERE; NITRILES AB Analysis of the 250-560 cm(-1) spectral continuum of Titan's north polar hood just after spring equinox reveals, in addition to the ubiquitous aerosol, a tenuous but relatively uniform cloud of small particles permeating the lower stratosphere at altitudes between 58 and 90 km. Voyager 1 IRIS data suggest the particles are highly scattering, almost certainly condensed organics, with radii between 1 and 5 mu m. Mote fractions for the condensed material range between 4 x 10(-8) and 4 x 10(-6), depending upon particle si/e, Vapor pressure arguments imply condensed nitriles near 90 km, the most likely being HCN, with condensed hydrocarbons such as C2II6 restricted to regions considerably nearer the tropopause. No direct chemical identification is possible. Negligible methane superaturation in the troposphere at 67.4 degrees N latitude, when compared with degrees of supersaturation at other latitudes, hints at precipitation fluxes of north polar stratospheric condensates during the previous northern winter that were perhaps three orders of magnitude greater than those at low latitudes during that time, A scale height of 1.5 times the density scale height above 160 kin is reaffirmed for the photochemical acrosol of the north polar hood, There appears to be a depletion of aerosol somewhere below 160 km. An aerosol mole fraction similar to 8 x 10(-8) at 160 km is inferred, about 33% greater than the value derived in a previous study. The Cassini CIRS instrument, with its expanded spectral range and higher spectral resolution, should be able to provide highly complementary information for the time period covering most of the northern winter season. (c) 2005 Elsevier Inc. All rights reserved. C1 Raytheon Corp, Greenbelt, MD 20771 USA. Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Mayo, LA (reprint author), Raytheon Corp, Greenbelt, MD 20771 USA. EM mayo@mail630.gsfc.nasa.gov NR 44 TC 24 Z9 24 U1 0 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD AUG PY 2005 VL 176 IS 2 BP 316 EP 330 DI 10.1016/j.icarus.2005.01.020 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 946AA UT WOS:000230543000005 ER PT J AU McEwen, AS Preblich, BS Turtle, EP Artemieva, NA Golombek, MP Hurst, M Kirk, RL Burr, DM Christensen, PR AF McEwen, AS Preblich, BS Turtle, EP Artemieva, NA Golombek, MP Hurst, M Kirk, RL Burr, DM Christensen, PR TI The rayed crater Zunil and interpretations of small impact craters on Mars SO ICARUS LA English DT Review DE Mars; cratering; regoliths; Moon; impact processes ID PATHFINDER LANDING SITE; NEAR-EARTH ASTEROIDS; GLOBAL SURVEYOR; MARTIAN METEORITES; MERIDIANI-PLANUM; CERBERUS FOSSAE; ORBITER CAMERA; CLIMATE-CHANGE; SOLAR-SYSTEM; FLOOD LAVAS AB A 10-km diameter crater named Zunil in the Cerberus Plains of Mars created similar to 10(7) secondary craters 10 to 200 m in diameter. Many of these secondary craters are concentrated in radial streaks that extend up to 1600 kin front the primary crater, identical to lunar rays. Most of the larger Zunil secondaries are distinctive in both visible and thermal infrared imaging. MOC images of the secondary craters show sharp rims and bright ejecta and rays, but the craters are shallow and often noncircular, as expected for relatively low-velocity impacts. About 80% of the impact craters superimposed over the youngest surfaces in the Cerberus Plains, such as Athabasca Valles, have the distinctive characteristics of Zunil secondaries. We have not identified any other large (>= 10 km diameter) impact crater on Mars with such distinctive rays of young secondary craters, so the age of the crater may be less than a few Ma. Zunil formed in the apparently youngest (least cratered) large-scale lava plains on Mars, and may be an excellent example of how spallation of a competent surface layer can produce high-velocity ejecta. (Melosh, 1984, Impact ejection, spallation. and the origin of meteorites, Icarus 59, 234-260). It could be the source crater for some of the basaltic shergottites, consistent with their crystallization and ejection ages, composition, and the fact that Zunil produced abundant high-velocity ejecta fragments. A 3D hydrodynamic simulation of the impact event produced 10(10) rock fragments >= 10 cm diameter, leading to up to 109 secondary craters >= 10 m diameter. Nearly all of the simulated secondary craters larger than 50 m are within 800 km of the impact site but the more abundant smaller (10-50 m) craters extend out to 3500 kin. If Zunil is representative of large impact events on Mars, then secondaries should be more abundant than primaries at diameters a factor of similar to 1000 smaller than that of the largest primary crater that contributed secondaries. As a result, most small craters on Mars could be secondaries. Depth/diameter ratios of 1300 small craters (10-500 m diameter) in Isidis Planitia and Gusev crater have a mean value of 0.08; the freshest of these craters give a ratio of 0.11, identical to that of fresh secondary craters on the Moon (Pike and Wilhelms, 1978, Secondary-impact craters on the Moon: topographic form and geologic process, Lunar Planet. Sci. IX, 907-909) and significantly less than the value of similar to 0.2 or more expected for fresh primary craters of this size range. Several observations suggest that the production functions of Hartmann and Neukum (2001, Cratering chronology and the evolution of Mars, Space Sci. Rev. 96, 165-194) predict too many primary craters smaller than a few hundred meters in diameter. Fewer small, high-velocity impacts may explain why there appears to be little impact regolith over Amazonian terrains. Martian terrains dated by small craters could be older than reported in recent publications. (c) 2005 Elsevier Inc. All rights reserved. C1 Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Russian Acad Sci, Inst Dynam Geospheres, Moscow, Russia. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Brigham Young Univ, Dept Geol, Provo, UT 84602 USA. US Geol Survey, Astrogeol Team, Flagstaff, AZ 86001 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. RP McEwen, AS (reprint author), Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab, Tucson, AZ 85721 USA. EM mcewen@pirl.lpl.arizona.edu RI Turtle, Elizabeth/K-8673-2012 OI Turtle, Elizabeth/0000-0003-1423-5751 NR 136 TC 198 Z9 199 U1 0 U2 15 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD AUG PY 2005 VL 176 IS 2 BP 351 EP 381 DI 10.1016/j.icarus.2005.02.009 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 946AA UT WOS:000230543000007 ER PT J AU Lowry, SC Weissman, PR Hicks, MD Whiteley, RJ Larson, S AF Lowry, SC Weissman, PR Hicks, MD Whiteley, RJ Larson, S TI Physical properties of Asteroid (25143) Itokawa - Target of the Hayabusa sample return mission SO ICARUS LA English DT Article DE near-Earth Asteroids; photometry; spcctroscopy; Hayabusa ID NEAR-EARTH ASTEROIDS; 1998 SF36; SPECTRAL PROPERTIES; CCD PHOTOMETRY; OBJECTS AB We present results of a ground-based observational study of the Hayabusa Mission target near-Earth Asteroid (25143) Itokawa. Our data consist of BVRI-filter CCD photometry and low resolution CCD spectroscopy, from which the asteroid's rotation period, axial ratio, broadband colors, and taxonomic classification are derived. Analysis of the R-filter lightcurve data shows a synodic rotation period of 12.12 +/- 0.02 h, consistent with results front other observers. We observed a maximum peak-to-peak amplitude Of 1.05 magnitudes. which.-depending on the taxonornic class assumed when correcting for phase angle effects-implies a minimum axial ratio of 2.14 The shape of the rotation lightcurves varies considerably between data sets due to the changing viewing geometry, The lightcurve data from this study has been included in the shape model analysis of Kausalainen et al. (2003 Astron. Astrophys. 40.5, 1,29-1,32) and the Hapke analysis of Lederer et al. (2005 Icarus 173,153-165). Color variations were also observed. with the interpolated color indices at lightcurve midpoint being: (B-V) = 0.94 +/- 0.05. (V-R) = 0.40 +/- 0.06, and (V-I) = 0.74 +/- 0.07. Our low resolution Palomar spectra from March 2001 covered a wavelength range of 0.3-1.0 mu m. We measured a spectral slope of 9.3 +/- 0.3%/100 nm between 0.55-0.70 mu m and a deep 1 mu m absorption (equivalent ECAS color: v-x = -0.111 +/- 0.003, v-x = 0.031 +/- 0.003). Comparison of our spectra with Published ECAS data from Zellner et al. (1985 Icarus 61, 355-416) indicates that this object is most likely of Q- or S-type. similar to ordinary chondrite meteorites, Our data are more consistent with a Q-type body when both the spectroscopic data and the available BVRI photometry are taken into account. (c) 2005 Elsevier Inc. All rights reserved. C1 Queens Univ Belfast, APS Div, Dept Phys & Astron, Belfast BT7 1NN, Antrim, North Ireland. Jet Prop Lab, Pasadena, CA 91109 USA. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. RP Lowry, SC (reprint author), Queens Univ Belfast, APS Div, Dept Phys & Astron, Belfast BT7 1NN, Antrim, North Ireland. EM s.c.lowry@qub.ac.uk NR 22 TC 10 Z9 11 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 AUG PY 2005 VL 176 IS 2 BP 408 EP 417 DI 10.1016/j.icarus.2005.02.002 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 946AA UT WOS:000230543000010 ER PT J AU Hicks, MD Simonelli, DP Buratti, BJ AF Hicks, MD Simonelli, DP Buratti, BJ TI Photometric behavior of 20000 Varuna at very small solar phase angles SO ICARUS LA English DT Article DE Kuiper Belt Objects; photometry ID KUIPER-BELT OBJECTS; SIERRA-NEVADA; VARIABILITY; COMETS; SYSTEM AB Six nights of R-band CCD observations of the classical Kuiper Belt Object (KBO) 20000 Varuna (2000 WR 106) were obtained at the Palomar Mountain 60- and 200-in telescopes. The observations were scheduled to take advantage of a particularly favorable apparition which allowed us to sample down to extremely small solar phase angle (alpha = 0.036 degrees), After rotational lightcurve subtraction, we found that the KBO exhibited a strong opposition surge of similar to 0.1 mag at phase angles alpha < 0.1 degrees, We modeled our composite solar phase curve of Varuna using both H-G parameterization and Hapke theory and concluded that similar opposition surges may he wide spread among KBOs and that the regolith of Varuna may be significantly more porous than a typical main-belt C-type asteroid, Wide-spread opposition surges lead to higher albedos than derived assuming linear phase behavior: on the whole KBOs may be brighter than previously assumed, (c) 2005 Elsevier Inc. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Hicks, MD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 183-501, Pasadena, CA 91109 USA. EM michael.d.hicks@jpl.nasa.gov NR 29 TC 6 Z9 6 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 AUG PY 2005 VL 176 IS 2 BP 492 EP 498 DI 10.1016/j.icarus.2005.01.013 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 946AA UT WOS:000230543000016 ER PT J AU Bratkovsky, AM Osipov, VV AF Bratkovsky, AM Osipov, VV TI Ultrafast low-power spin-injection devices based on modified ferromagnetic-semiconductor junctions SO IEE PROCEEDINGS-CIRCUITS DEVICES AND SYSTEMS LA English DT Article ID LIGHT-EMITTING DIODE; GIANT MAGNETORESISTANCE; ROOM-TEMPERATURE; SCHOTTKY-BARRIER; TRANSPORT; POLARIZATION; SPINTRONICS; METAL; CO; HETEROSTRUCTURE AB The authors describe recent theoretical and experimental advances in achieving large accumulated spin polarisation in semiconductors and suggest new classes of low-power ultrafast devices. Tunnelling of electrons between nonmagnetic semiconductors (S) and ferromagnets (FM) through a Schottky barrier modified by a delta-doped layer at the interface is described. It is shown that, in such reverse (forward) biased FM-S junctions, electrons with a certain spin projection can be efficiently injected in (extracted from) S, while electrons with the opposite spin can efficiently accumulate in S near the interface. This occurs due to spin filtering of electrons in the tunnelling process, and the authors found conditions for most efficient accumulation of spin polarisation. Extraction of spin can proceed in degenerate semiconductors at low temperatures. Novel spin-valve ultrafast devices with small dissipated power are described: a magnetic sensor, a spin transistor, an amplifier, a frequency multiplier, a square-law detector and a source of polarised radiation. C1 Hewlett Packard Labs, Palo Alto, CA 94304 USA. NASA, Ames Res Ctr, Stanford, CA 94305 USA. RP Hewlett Packard Labs, 1501 Page Mill Rd,1L, Palo Alto, CA 94304 USA. EM alex.bratkovski@hp.com NR 71 TC 0 Z9 0 U1 0 U2 1 PU INST ENGINEERING TECHNOLOGY-IET PI HERTFORD PA MICHAEL FARADAY HOUSE SIX HILLS WAY STEVENAGE, HERTFORD SG1 2AY, ENGLAND SN 1350-2409 J9 IEE P-CIRC DEV SYST JI IEE Proc.-Circuit Device Syst. PD AUG PY 2005 VL 152 IS 4 BP 323 EP 333 DI 10.1049/ip-cds:20050017 PG 11 WC Engineering, Electrical & Electronic SC Engineering GA 973QI UT WOS:000232537300006 ER PT J AU Gawronski, W Souccar, K AF Gawronski, W Souccar, K TI Control systems of the large millimeter telescope SO IEEE ANTENNAS AND PROPAGATION MAGAZINE LA English DT Article DE antennas; antenna mechanical factors; antenna transient analysis; control systems; control engineering; reflector antenna mechanical factors ID RADIO-TELESCOPES; ANTENNAS; LQG AB This paper presents the analysis results (in terms of settling time, bandwidth, and servo error in wind disturbances) of four control systems designed for the Large Millimeter Telescope (LMT). The first system, called PIP, consists of the proportional and integral (PI) controllers in the rate and position loops, and is widely used in the antenna and radio telescope industry. The analysis shows that the PP control system's performance is remarkably good when compared to similar control systems applied to typical antennas. This performance is achieved because the LMT structure is exceptionally rigid; however, it does not meet the stringent LMT pointing requirements. The second system, called PL, consists of the PI controller in the rate loop, and the linear-quadratic-Gaussian (LQG) controller in the position loop. This type of controller is implemented in the NASA Deep Space Network antennas, where pointing accuracy is twice that of the PP control system. The third system, called LP, consists of the LQG controller in the rate loop, and the proportional-integral-derivative (PID) controller in the position loop. This type of loop has not been yet implemented at known antennas or radio telescopes, but the analysis shows that its pointing accuracy is the ten times better than the PP control system. The fourth system, called LL, consists of the LQG controller in both the rate loop and the position loop. It is the best of the four, with accuracy 250 times better than the PP system. It is thus worth further investigation to identify implementation challenges for telescopes with high pointing requirements. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Massachusetts, Dept Astron, LMT Project, Amherst, MA 01003 USA. RP Gawronski, W (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 238-528, Pasadena, CA 91109 USA. EM Wodek.K.Gawronski@jpl.nasa.gov; souccar@astro.umass.edu NR 9 TC 5 Z9 6 U1 1 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1045-9243 EI 1558-4143 J9 IEEE ANTENN PROPAG M JI IEEE Antennas Propag. Mag. PD AUG PY 2005 VL 47 IS 4 BP 41 EP 49 DI 10.1109/MAP.2005.1589873 PG 9 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 004QT UT WOS:000234768000004 ER PT J AU Huang, J AF Huang, J TI Paper-thin membrane aperture-coupled L-band antennas SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION LA English DT Article DE antenna; aperture-coupled; microstrip patch; slot; thin membrane AB A microstrip line on very thin membrane substrate (0.05 mm) is slot-coupled through a thick air substrate (12.7 mm) to excite an L-band radiating patch element. A breadboard unit achieved a relatively wide bandwidth of 100 MHz (8%). Very narrow coupling slot is used with aspect ratio of 160 (conventional slot aspect ratio is between 10 to 30). This new feed design makes the thin-membrane or inflatable array antenna technology more practical. It reduces the number of thin-membrane layers required for a dual-pol wide-band inflatable array from three layers in a previous design to two layers. In addition, this technology allows the thin-membrane array antenna elements to be readily integrated with thin-membrane-mounted transmit/receive (T/R) modules. Calculation shows that, without the patch, the microstrip line and slot combination can also radiate as a paper-thin (0.05 mm) radiator at the L-band frequencies. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Huang, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM John.huang@jpl.nasa.gov NR 8 TC 2 Z9 2 U1 0 U2 0 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-926X J9 IEEE T ANTENN PROPAG JI IEEE Trans. Antennas Propag. PD AUG PY 2005 VL 53 IS 8 BP 2499 EP 2502 DI 10.1109/TAP.2005.852277 PN 1 PG 4 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 954LH UT WOS:000231156100017 ER PT J AU Rahmat-Samii, Y Huang, J Lopez, B Lou, M Im, E Durden, SL Bahadori, K AF Rahmat-Samii, Y Huang, J Lopez, B Lou, M Im, E Durden, SL Bahadori, K TI Advanced precipitation radar antenna: Array-fed offset membrane cylindrical reflector antenna SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION LA English DT Article DE cylindrical reflector antenna; linear array feed; membrane reflector; precipitation radar antenna AB As part of the overall NASA earth science technology research effort, a half-size prototype model of light-weight, dual-frequency and wide-swath scanning antenna-for the next generation of spaceborne precipitation radar has recently been developed. It operates radar channels at both 13.6 and 35 GHz for improved rainfall retrieval accuracy. The antenna for proposed spaceborne precipitation radar is an offset parabolic cylindrical reflector fed by two linear arrays. This design is adopted, instead of a double-curved offset reflector, because it provides the required wide scan angle in the cross-track plane at both the Ku and Ka band operating frequencies. To demonstrate the technological readiness of the concept, the focus is on a half-scale model of 2.65 to operating at Ku and Ka band. In this paper, the technology development status on this Advanced Precipitation Radar Antenna will be presented. Design and characterization of the 2.65 m antenna is detailed by presenting the features of various components of the antenna, including simulation of the performance, 2 x 166 Ku and 4 x 166 Ka element feed array designs and evaluation and the design concept of the membrane reflector. Measurement results of the entire antenna system using a compact range facility will also be summarized. C1 Univ Calif Los Angeles, Los Angeles, CA 90095 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Univ Calif Los Angeles, Los Angeles, CA 90095 USA. EM rahmat@ee.ucla.edu; keyvan@ee.ucla.edu NR 17 TC 25 Z9 25 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-926X EI 1558-2221 J9 IEEE T ANTENN PROPAG JI IEEE Trans. Antennas Propag. PD AUG PY 2005 VL 53 IS 8 BP 2503 EP 2515 DI 10.1109/TAP.2005.852599 PN 1 PG 13 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 954LH UT WOS:000231156100018 ER PT J AU McCown, R Gross, FB Calle, CI AF McCown, R Gross, FB Calle, CI TI Comparison of two particle charging experiments for testing the JSC Mars-1 Martian regolith simulant against man-made materials SO IEEE TRANSACTIONS ON DIELECTRICS AND ELECTRICAL INSULATION LA English DT Article DE triboelectric charging; charge transfer; electrostatics; saltation; Mars AB NASA has great interest in testing the electrostatic charging of various materials due to the saltation process near the surface of Mars. As wind blows over the Martian regolith, particles are picked up, travel over a distance, and then fall back to the surface. These moving particles collide with each other and with any other materials present giving rise to a triboelectric charge transfer. Variables involved in this charge transfer include the number of particles, the frequency of collisions, and the particle velocities. It is necessary to know the extent of charging of man-made materials in this process in order to better plan future Mars missions. Two different methods for creating frictional charging between the regolith simulant and the materials in question are described. The first method utilizes a deflection board apparatus. The second uses a shaker box apparatus. The benefits and drawbacks of each experimental approach are listed. Some experimental data obtained through each method is provided but further study is required to fully characterize these charging processes. C1 Florida A&M Univ, Coll Engn, Dept Elect & Comp Engn, Tallahassee, FL 32310 USA. NASA, Electrostat & Surface Phys Lab, Kennedy Space Ctr, Kennedy Space Ctr, FL 32899 USA. RP McCown, R (reprint author), Florida A&M Univ, Coll Engn, Dept Elect & Comp Engn, Tallahassee, FL 32310 USA. NR 8 TC 1 Z9 3 U1 3 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1070-9878 J9 IEEE T DIELECT EL IN JI IEEE Trns. Dielectr. Electr. Insul. PD AUG PY 2005 VL 12 IS 4 BP 821 EP 826 DI 10.1109/TDEI.2005.1511108 PG 6 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 963UJ UT WOS:000231831300021 ER PT J AU Walsh, EJ Banner, ML Churnside, JH Shaw, JA Vandemark, DC Wright, CW Jensen, JB Lee, S AF Walsh, EJ Banner, ML Churnside, JH Shaw, JA Vandemark, DC Wright, CW Jensen, JB Lee, S TI Visual demonstration of three-scale sea-surface roughness under light wind conditions SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE light wind; mean square slope (MSS); microwave; optical; sea surface ID MEAN-SQUARE SLOPE; SPECTRUM SPATIAL VARIATION; OCEAN WAVES EXPERIMENT; GENERATED WAVES; RADAR ALTIMETER; AIRBORNE LIDAR; MODEL; SCATTERING; SCATTEROMETRY; BACKSCATTER AB During the Southern Ocean Waves Experiment (SOWEX) an aircraft carried a down-looking video camera to help document the sea surface. Reflected images of the aircraft were intermittently observed in the video recorded at 15-30-m height under light and variable wind conditions. A numerical simulation was developed to relate image contrast to the gravity-capillary wave contribution to sea-surface mean square slope (mss). "Carnival fun-house" mirror-type distortions of the image in the absence of the gravity-capillary waves relate to intermediate-scale wave persistence when wind forcing stops. Video image estimates of mss correlated better with 36-GHz scanning radar altimeter estimates than with the wind speed measured at 30-m height. When the gravity-capillary waves disappeared in the absence of wind forcing, about one-third of the 0.0015 residual mss was contributed by the dominant waves, and about two-thirds was contributed by the 1-10-m wavelength region. Near the shores of a lake in Alaska, reflected aircraft images were also observed, indicating that the gravity-capillary wave contribution to mss was only about 0.000001, even though the wind speed at the 160-m aircraft height was 10 m/s. C1 NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA. Univ New S Wales, Dept Math, Sydney, NSW 2052, Australia. NOAA, Environm Technol Lab, Boulder, CO 80305 USA. CSIRO Atmospher Res, Aspendale, Vic 3195, Australia. RP Walsh, EJ (reprint author), NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA. EM Edward.Walsh@nasa.gov RI Churnside, James/H-4873-2013; OI Banner, Michael/0000-0002-0799-5341 NR 39 TC 3 Z9 3 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 AUG PY 2005 VL 43 IS 8 BP 1751 EP 1762 DI 10.1109/TGRS.2005.851633 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 949BX UT WOS:000230761000006 ER PT J AU Sun, JQ Xiong, XXJ Barnes, WL AF Sun, JQ Xiong, XXJ Barnes, WL TI MODIS solar diffuser stability monitor sun view modeling SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE modeling; Moderate Resolution Imaging Spectroradiometer (MODIS); screen; solar diffuser (SD); Solar Diffuser Stability Monitor (SDSM); simulation ID PERFORMANCE; BANDS AB The Moderate Resolution Imaging Spectroradiometer (MODIS) reflective solar bands (RSBs) are calibrated on-orbit using an onboard solar diffuser (SD) panel, made of Spectralon. An onboard Solar Diffuser Stability Monitor (SDSM) tracks the SDs degradation. The SDSM views the sun through a 1.44% attenuation screen during SD calibration. The observed SDSM sun view response has shown serious unexpected ripples that are as large as 10% of the averaged response and consequently disable the originally designed SD degradation tracking algorithms. In this report, a model based on geometric factors and design parameters is developed to simulate the SDSM sun view response. It is shown that the ripples are induced by erroneous design parameters and incorrect installation of the involved optical elements. The model could be used to improve the MODIS SD calibration and to provide helpful information for the design of future remote sensing systems. C1 Sci Syst & Applicat Inc, Lanham, MD 20706 USA. NASA, Goddard Space Flight Ctr, Terr Phys Lab, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, JCET, Baltimore, MD 21250 USA. RP Sun, JQ (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA. EM junqiang_sun@ssaihq.com NR 12 TC 13 Z9 13 U1 1 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 AUG PY 2005 VL 43 IS 8 BP 1845 EP 1854 DI 10.1109/TGRS.2005.852710 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 949BX UT WOS:000230761000015 ER PT J AU Schmalzel, J Figueroa, F Morris, J Mandayam, S Polikar, R AF Schmalzel, J Figueroa, F Morris, J Mandayam, S Polikar, R TI An architecture for intelligent systems based on smart sensors SO IEEE TRANSACTIONS ON INSTRUMENTATION AND MEASUREMENT LA English DT Article; Proceedings Paper CT IEEE Instrumentation and Measurement Technology Conference CY MAY 18-20, 2004 CL Como, ITALY SP IEEE Instrumentat & Measurement Soc DE health management; IEEE 1451; integrated system health management (ISHM); integrated vehicle health monitoring (IVHM); rocket testing; sensor fusion; smart sensors AB Based on requirements for a next-generation rocket test facility, elements of a prototype intelligent rocket test facility (IRTF) have been implemented. The preliminary results provide the basis for future advanced development and validation using rocket test stand facilities at Stennis Space Center (SSC). Key components include distributed smart sensor elements integrated using a knowledge-driven environment. One of the specific goals is to imbue sensors with the intelligence needed to perform self-diagnosis of health and to participate in a hierarchy of health determination at sensor, process, and system levels. We have identified issues important to further development of health-enabled networks, which should be of interest to others working with smart sensors and intelligent health management systems. C1 Rowan Univ, Dept Elect & Comp Engn, Glassboro, NJ 08028 USA. Stennis Space Ctr, Program Dev Directorate, Technol Dev & Transfer Off, Stennis Space Ctr, MS 39529 USA. RP Schmalzel, J (reprint author), Rowan Univ, Dept Elect & Comp Engn, Glassboro, NJ 08028 USA. EM j.schmalzel@ieee.org RI Polikar, Robi/N-4742-2015 OI Polikar, Robi/0000-0002-2739-4228 NR 10 TC 40 Z9 41 U1 1 U2 8 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9456 J9 IEEE T INSTRUM MEAS JI IEEE Trans. Instrum. Meas. PD AUG PY 2005 VL 54 IS 4 SI SI BP 1612 EP 1616 DI 10.1109/TIM.2005.851477 PG 5 WC Engineering, Electrical & Electronic; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 947FK UT WOS:000230628600042 ER PT J AU Suzuki, M Tashiro, M Sato, G Watanabe, S Nakazawa, K Takahashi, T Okada, Y Takahashi, H Parsons, A Barthelmy, S Cummings, J Gehrels, N Hullinger, D Krimm, H Tueller, J AF Suzuki, M Tashiro, M Sato, G Watanabe, S Nakazawa, K Takahashi, T Okada, Y Takahashi, H Parsons, A Barthelmy, S Cummings, J Gehrels, N Hullinger, D Krimm, H Tueller, J TI Hard x-ray response of CdZnTe detectors in the swift burst alert telescope SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article DE BAT; CdZnTe; energy calibration; gamma-ray detector; mobility-lifetime products; spectral modeling; Swift ID BAT; ARRAY AB The Burst Alert Telescope (BAT) onboard the Swift gamma-ray burst explorer has a coded aperture mask and a detector array of 32 K CdZnTe semiconductor devices. Due to the small mobility and short lifetime of carriers, the electron-hole pairs generated by gamma-ray irradiation cannot be fully collected. Hence the shape of the measured spectra has a broad low-energy tail. We have developed a method to model the spectral response by taking into account the charge transport properties which depend on the depth of the photon interaction [1]. The mobility-lifetime products for detectors derived from our method vary by more than one order of magnitude among detectors. In this paper, we focus on the nonuniformity of the mobility at the millimeter scale by employing a scanning experiment for a single detector. We reveal almost an order of magnitude variance in the mobility-lifetime product of holes within a single detector, while those of electrons, remains fairly uniform. C1 Saitama Univ, Dept Phys, Saitama 3388570, Japan. Inst Space & Astronaut Sci, JAXA, Kanagawa 2298510, Japan. Univ Tokyo, Dept Phys, Tokyo 1130033, Japan. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Suzuki, M (reprint author), Saitama Univ, Dept Phys, Saitama 3388570, Japan. RI Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; Tueller, Jack/D-5334-2012; Parsons, Ann/I-6604-2012; Tashiro, Makoto/J-4562-2012 NR 9 TC 4 Z9 4 U1 1 U2 7 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD AUG PY 2005 VL 52 IS 4 BP 1033 EP 1035 DI 10.1106/TNS.2005.0852968 PG 3 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 958IA UT WOS:000231436700033 ER PT J AU Goebel, DM Schneider, AC AF Goebel, DM Schneider, AC TI High-voltage breakdown and conditioning of carbon and molybdenum electrodes SO IEEE TRANSACTIONS ON PLASMA SCIENCE LA English DT Article; Proceedings Paper CT 26th International Power Modulator Symposium/High Voltage Workshop CY MAY 23-26, 2004 CL San Francisco, CA SP IEEE Dielect & Elect Insulat Soc, IEEE Electron Devices Soc DE accelerators; electrical breakdown; ion sources; traveling wave tubes ID VACUUM ARCS; GRAPHITE CATHODES; FIELD-EMISSION; EROSION AB Carbon and molybdenum electrodes employed in high-voltage devices such as ion sources and traveling wave tubes can be easily damaged by electrical breakdown and arcing events. Modification of the electrode surfaces due to these events can impact the voltage hold-off capability of the surfaces, which could lead to additional arcing, further damage, and the potential for device failure. Power supplies driving these devices are usually rated for their damage potential by the amount of stored energy. However, many systems that use arc discharges characterize the lifetime of the device for voltage hold-off and the amount of material removed from the surfaces by the amount of current that passes through the arc, or the "Coulomb-transfer rating:" The results of a series of tests that were performed on the voltage hold-off capability and damage to several different carbon and molybdenum surfaces due to induced arcing are presented. Damage to the surfaces was characterized by the field emission threshold after arcing events, by the amount of Coulomb-transfer in the arc, and by scanning electron microscope photographs of the subsequent surfaces. Both conditioning and damage to the surfaces were observed, and are related to the characteristics of the materials and the electrical breakdowns. C1 Jet Propuls Lab, Pasadena, CA 91109 USA. RP Goebel, DM (reprint author), Jet Propuls Lab, Pasadena, CA 91109 USA. EM dan.m.goebel@jpl.nasa.gov; analyn.c.schneider@jpl.nasa.gov NR 32 TC 4 Z9 4 U1 1 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0093-3813 EI 1939-9375 J9 IEEE T PLASMA SCI JI IEEE Trans. Plasma Sci. PD AUG PY 2005 VL 33 IS 4 BP 1136 EP 1148 DI 10.1109/TPS.2005.852410 PN 1 PG 13 WC Physics, Fluids & Plasmas SC Physics GA 956RC UT WOS:000231316500002 ER PT J AU Howe, DA Beard, RL Greenhall, CA Vernotte, F Riley, WJ Peppler, TK AF Howe, DA Beard, RL Greenhall, CA Vernotte, F Riley, WJ Peppler, TK TI Enhancements to GPS operations and clock evaluations using a "total" Hadamard deviation SO IEEE TRANSACTIONS ON ULTRASONICS FERROELECTRICS AND FREQUENCY CONTROL LA English DT Article ID FREQUENCY STABILITY; ALLAN VARIANCE; ESTIMATORS AB We describe a method based on the total deviation approach whereby we improve the confidence of the estimation of the Hadamard deviation that is used primarily in global positioning system (GPS) operations. The Hadamard-total deviation described in this paper provides a significant improvement in confidence indicated by an increase of 1.3 to 3.4 times the one degree of freedom of the plain Hadamard deviation at the longest averaging time. The new Hadamard-total deviation is slightly negatively biased with respect to the usual Hadamard deviation, and tau values are restricted to less than or equal to T/3, to be consistent with the usual Hadamard's definition. We give a method of automatically removing bias by a power-law detection scheme. We review the relationship between Kalman filter parameters and the Hadamard and Allan variances, illustrate the operational problems associated with estimating these parameters, and discuss how the Hadamard-total variance can improve management of present and future GPS satellite clocks. C1 Natl Inst Stand & Technol, Div Time & Frequency, Boulder, CO 80305 USA. USN, Res Lab, Washington, DC 20375 USA. Jet Propuls Lab, Pasadena, CA 91109 USA. Observ Besancon, Besancon, France. Hamilton Tech Serv, Beaufort, SC 29907 USA. RP Howe, DA (reprint author), Natl Inst Stand & Technol, Div Time & Frequency, Boulder, CO 80305 USA. EM dhowe@boulder.nist.gov NR 18 TC 8 Z9 13 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0885-3010 J9 IEEE T ULTRASON FERR JI IEEE Trans. Ultrason. Ferroelectr. Freq. Control PD AUG PY 2005 VL 52 IS 8 BP 1253 EP 1261 DI 10.1109/TUFFC.2005.1509784 PG 9 WC Acoustics; Engineering, Electrical & Electronic SC Acoustics; Engineering GA 961BK UT WOS:000231636700007 PM 16245595 ER PT J AU Tang, XD Tao, G Joshi, SM AF Tang, XD Tao, G Joshi, SM TI Adaptive output feedback actuator failure compensation for a class of non-linear systems SO INTERNATIONAL JOURNAL OF ADAPTIVE CONTROL AND SIGNAL PROCESSING LA English DT Article DE adaptive control; actuator failure; output feedback AB An adaptive compensation control scheme using output feedback is designed and analysed for a class of non-linear systems with state-dependent non-linearities in the presence of unknown actuator failures. For a linearly parameterized model of actuator failures with unknown failure values, time instants and pattern, a robust backstepping-based adaptive non-linear controller is employed to handle the system failure, parameter and dynamics uncertainties. Robust adaptive parameter update laws are derived to ensure closed-loop signal boundedness and small tracking errors, in general, and asymptotic regulation, in particular. An application to controlling the angle of attack of a non-linear hypersonic aircraft dynamic model in the presence of elevator segment failures is studied and simulation results show that the developed adaptive control scheme has desired actuator failure compensation performance. Copyright (c) 2004 John Wiley & Sons, Ltd. C1 Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22903 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22903 USA. EM xt3f@virginia.edu; gt9s@virginia.edu; s.m.oshi@larc.nasa.gov NR 14 TC 40 Z9 41 U1 1 U2 8 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0890-6327 EI 1099-1115 J9 INT J ADAPT CONTROL JI Int. J. Adapt. Control Signal Process. PD AUG PY 2005 VL 19 IS 6 BP 419 EP 444 DI 10.1002/acs.843 PG 26 WC Automation & Control Systems; Engineering, Electrical & Electronic SC Automation & Control Systems; Engineering GA 958HZ UT WOS:000231436600001 ER PT J AU Hatamleh, O Beek, J Forman, R Shivakumar, V Lyons, J AF Hatamleh, O Beek, J Forman, R Shivakumar, V Lyons, J TI Strip yield model numerical application to different geometries and loading conditions SO INTERNATIONAL JOURNAL OF FRACTURE LA English DT Article DE Crack Tip Opening Displacement; (CTOD); Dugdale model; strip yield model ID CRACKS AB A new numerical method based on the strip yield analysis approach was developed for calculating the Crack Tip Opening Displacement (CTOD). This approach can be applied to any crack geometry, of either infinite or finite extent, with arbitrary applied loading conditions. The technique is an adaptation of the dislocation-density based boundary element method to obtain crack-face opening displacements at any point on a crack, and Succeeds in obtaining the requisite values as a series of definite integrals, the functional parts of each of which are evaluated exactly in closed form. The power of the technique is demonstrated by obtaining solutions to several crack configurations of practical interest. C1 NASA, Johnson Space Ctr, Struct & Dynam Branch, Houston, TX 77058 USA. NASA, Johnson Space Ctr, Mat & Proc Branch, Houston, TX 77058 USA. Jacobs Sverdup ESC Grp, Houston, TX 77058 USA. Univ S Carolina, Dept Mech Engn, Columbia, SC 29208 USA. RP Hatamleh, O (reprint author), NASA, Johnson Space Ctr, Struct & Dynam Branch, Houston, TX 77058 USA. EM omar.hatamleh-1@nasa.gov NR 14 TC 6 Z9 6 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0376-9429 J9 INT J FRACTURE JI Int. J. Fract. PD AUG PY 2005 VL 134 IS 3-4 BP 251 EP 265 DI 10.1007/s10704-005-0746-8 PG 15 WC Materials Science, Multidisciplinary; Mechanics SC Materials Science; Mechanics GA 995ZA UT WOS:000234143000004 ER PT J AU Jarzembski, MA Tankosic, DV AF Jarzembski, MA Tankosic, DV TI Discharge of negatively charged micrometer size particles in an electrodynamic balance due to radioactivity SO JOURNAL OF AEROSOL SCIENCE LA English DT Article DE micrometer size particle; electrodynamic balance; cosmic rays; terrestrial radioactivity; gamma radioactivity AB The radiation dose rate of the combined natural sources of both cosmic rays and terrestrial radioactivity was measured from the discharge of a negatively charged 10.2 mu m diameter polystyrene particle levitated in an electrodynamic balance, giving good agreement with the predicted natural dose. This measurement was based upon a series of discharge experiments of these particles due to the influence of a cesium 137 gamma ray radioactive source for various cases of amplitude V-ac (800-2000 V) and frequency f (200-700 Hz) of the alternating potential applied to the balance's ring electrode, covering a full range of possible operating V-ac and f values for the balance. These set of measurements revealed an interesting complex behavior of discharge rates. Effects of the initial amount of charge on the particle and the density of gamma rays were also studied as well. A least squares logarithmic second order equation was fitted to these measured discharge data, which easily offered a method of measuring the activity of the natural sources at V-ac=800 V and f=700 Hz. (C) 2004 Elsevier Ltd. All rights reserved. C1 NASA, George C Marshall Space Flight Ctr, Global Hydrol & Climate Ctr, Huntsville, AL 35805 USA. Univ Alabama, Huntsville, AL 35805 USA. RP Jarzembski, MA (reprint author), NASA, George C Marshall Space Flight Ctr, Global Hydrol & Climate Ctr, 320 Sparkman Dr, Huntsville, AL 35805 USA. EM maurice.a.jarzembski@nasa.gov; tankosd@email.uah.edu NR 13 TC 1 Z9 1 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0021-8502 J9 J AEROSOL SCI JI J. Aerosol. Sci. PD AUG PY 2005 VL 36 IS 8 BP 1023 EP 1035 DI 10.1016/j.jaerosci.2004.10.016 PG 13 WC Engineering, Chemical; Engineering, Mechanical; Environmental Sciences; Meteorology & Atmospheric Sciences SC Engineering; Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 955FF UT WOS:000231210100006 ER PT J AU Bakunov, MI Maslov, AV Bodrov, SB AF Bakunov, MI Maslov, AV Bodrov, SB TI Phase-matched generation of a terahertz surface wave by a subluminous optical strip SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID FEMTOSECOND ELECTROMAGNETIC PULSES; TIME-DOMAIN SPECTROSCOPY; ULTRASHORT LASER-PULSES; POLED LITHIUM-NIOBATE; SEMICONDUCTOR SURFACES; NARROW-BAND; CHERENKOV RADIATION; TRANSMISSION-LINES; SHOCK-WAVES; THZ AB We show that a weakly focused ultrashort laser pulse with tilted intensity front can efficiently excite a terahertz surface wave via phase-matched optical rectification at the surface of a semiconductor. The surface wave is excited by a strip of nonlinear polarization moving along the semiconductor surface with subluminous velocity. The amplitude and power of the radiated surface wave are calculated. For a 90-fs optical pulse with a peak intensity of 2 GW/cm(2), we estimate the energy conversion coefficient to be 10(-7) at the surface of GaAs. The direct excitation of surface waves at terahertz frequencies can be particularly attractive for terahertz spectroscopy of semiconductor surfaces. (c) 2005 American Institute of Physics. C1 Univ Nizhny Novgorod, Dept Radiophys, Nizhnii Novgorod 603950, Russia. Russian Acad Sci, Inst Appl Phys, Nizhnii Novgorod 603950, Russia. NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Bakunov, MI (reprint author), Univ Nizhny Novgorod, Dept Radiophys, Nizhnii Novgorod 603950, Russia. EM bakunov@rf.unn.ru RI Maslov, Alexey/E-5158-2011; Bodrov, Sergey/D-1962-2012; Bakunov, Michael/E-2875-2017 OI Maslov, Alexey/0000-0002-7835-2474; Bakunov, Michael/0000-0002-4209-1372 NR 30 TC 7 Z9 7 U1 0 U2 3 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-8979 J9 J APPL PHYS JI J. Appl. Phys. PD AUG 1 PY 2005 VL 98 IS 3 AR 033101 DI 10.1063/1.1999828 PG 7 WC Physics, Applied SC Physics GA 955RV UT WOS:000231246100001 ER PT J AU Kyparos, A Feeback, DL Layne, CS Martinez, DA Clarke, MSF AF Kyparos, A Feeback, DL Layne, CS Martinez, DA Clarke, MSF TI Mechanical stimulation of the plantar foot surface attenuates soleus muscle atrophy induced by hindlimb unloading in rats SO JOURNAL OF APPLIED PHYSIOLOGY LA English DT Article DE mechanical foot stimulation; plantar stimulation; sensory receptors; proprioception; skeletal muscle atrophy; soleus; mechanical unloading; rat ID SKELETAL-MUSCLE; NEUROMUSCULAR ACTIVATION; IN-FLIGHT; SUSPENSION; CONTRACTILE; ADAPTATIONS; ADULT; YOUNG; HYPOKINESIA; SPACEFLIGHT AB Unloading-induced muscle atrophy occurs in the aging population, bedridden patients, and astronauts. This study was designed to determine whether dynamic foot stimulation (DFS) applied to the plantar surface of the rat foot can serve as a countermeasure to soleus muscle atrophy normally observed in hindlimb unloaded (HU) rats. Forty-four mature (6 mo old), male Wistar rats were randomly assigned to ambulatory control, HU alone, HU with active DFS (i.e., plantar contact with active inflation), HU with passive DFS (i.e., plantar contact without active inflation), and HU while wearing a DFS boot with no plantar contact groups. Application of active DFS during HU significantly counteracted the atrophic response by preventing similar to 85% of the reduction in type I myofiber cross-sectional area (CSA) in the soleus while preventing similar to 57% of the reduction in type I myofiber CSA and 43% of the reduction in type IIA myofiber CSA of the medial gastrocnemius muscle. Wearing of a DFS boot without active inflation prevented myofiber atrophy in the soleus of HU animals in a fashion similar to that observed in HU animals that wore an actively inflated DFS boot. However, when a DFS boot without plantar surface contact was worn during HU, no significant protection from HU-induced myofiber atrophy was observed. These results illustrate that the application of mechanical foot stimulation to the plantar surface of the rat foot is an effective countermeasure to muscle atrophy induced by HU. C1 Univ Houston, Dept Hlth & Human Performance, Lab Integrated Physiol, Houston, TX 77204 USA. Univ Houston, Inst Space Syst Operat, Houston, TX 77204 USA. Univ Houston, Connect Tissue Physiol Lab, Dept Biol & Biochem, Houston, TX 77204 USA. NASA, Lyndon B Johnson Space Ctr, Space Life Sci Directorate, Muscle Res Lab, Houston, TX 77058 USA. RP Clarke, MSF (reprint author), Univ Houston, Dept Hlth & Human Performance, Lab Integrated Physiol, 3855 Holman St,Garrison Rm 104D, Houston, TX 77204 USA. EM mclarke@mail.uh.edu RI Martinez, Daniel/A-5825-2008 NR 32 TC 19 Z9 22 U1 0 U2 1 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 AUG PY 2005 VL 99 IS 2 BP 739 EP 746 DI 10.1152/japplphysiol.00771.2004 PG 8 WC Physiology; Sport Sciences SC Physiology; Sport Sciences GA 945EU UT WOS:000230486200046 PM 15817719 ER PT J AU Pearson, C Manning, SW Coleman, M Jarvis, K AF Pearson, C Manning, SW Coleman, M Jarvis, K TI Can tree-ring chemistry reveal absolute dates for past volcanic eruptions? SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE dendrochronology; dendrochemistry; tree-rings; dating volcanic eruptions; LA-ICP-MS ID PLASMA-MASS-SPECTROMETRY; GREENLAND ICE CORE; BALSAMEA L MILL; TRACE-ELEMENTS; SPRUCE WOOD; DENDROCHEMICAL ANALYSIS; SPATIAL-DISTRIBUTION; ENVIRONMENTAL-CHANGE; SUMMER-TEMPERATURE; HISTORICAL CHANGES AB Discussion of the significance of volcanically induced impacts on human history, the natural environment, and climate through the Holocene, has frequently stalled because of controversy concerning certain key volcanic eruptions and their precise relationships with the archaeological/environmental record. A major stumbling block in such debates is a failure to obtain precise and accurate dates for many of these key volcanic events. Most existing dates currently float against archaeological, historical, environmental, and climate data. A potential means to resolution lies with tree rings: these can be dated precisely by dendrochronology, are available from a wide range of loci around the world, and can record global climatic influences. It has been suggested that certain growth anomalies in dendrochronological sequences could offer "proxy" absolutely dated records of major, climatically effective, volcanic eruptions. However, this assertion has been widely disputed given the lack of a direct, positive, causal connection. The hypothesis that the required connection may be chemically encoded in individual annual growth rings from dated sequences is explored here both via review of existing literature on dendrochemical techniques, and by LA-ICP-MS chemical analysis of two tree ring sequences. It is concluded that dendrochemistry provides a promising means by which absolute dates may one day be attributed to key volcanic eruptions of pre-modern times. (c) 2005 Elsevier Ltd. All rights reserved. C1 Univ Reading, Sch Human & Environm Sci, Reading RG6 6AB, Berks, England. CALTECH, Jet Prop Lab, NASA, Ctr Life Detect, Pasadena, CA 91109 USA. Kingston Univ, Sch Earth Sci & Geog, NERC, ICP MS Facil, Kingston upon Thames KT1 2EE, Surrey, England. RP Pearson, C (reprint author), Univ Reading, Sch Human & Environm Sci, POB 227, Reading RG6 6AB, Berks, England. EM c.l.pearson@rdg.ac.uk RI Coleman, Max/A-1303-2007 OI Coleman, Max/0000-0002-5514-1826 NR 98 TC 32 Z9 33 U1 4 U2 32 PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0305-4403 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD AUG PY 2005 VL 32 IS 8 BP 1265 EP 1274 DI 10.1016/j.jas.2005.03.007 PG 10 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 942ZR UT WOS:000230321900011 ER PT J AU Freed, AD Doehring, TC AF Freed, AD Doehring, TC TI Elastic model for crimped collagen fibrils SO JOURNAL OF BIOMECHANICAL ENGINEERING-TRANSACTIONS OF THE ASME LA English DT Article ID CONNECTIVE TISSUES; MAMMALIAN TENDON; PATELLAR TENDON; LIGAMENT; ULTRASTRUCTURE; ELONGATION; MORPHOLOGY AB A physiologic constitutive expression is presented in algorithmic format for the nonlinear elastic response of wavy collagen fibrils found in soft connective tissues. The model is based on the observation that crimped fibrils in a fascicle have a three-dimensional structure at the micron scale that we approximate as a helical spring. The symmetry of this wave form allows the force/displacement relationship derived from Castigliano's theorem to be solved in closed form: all integrals become analytic. Model predictions are in good agreement with experimental observations for mitral-valve chord ae tendine ae. C1 NASA, John H Glenn Res Ctr Lewis Field, Bio Sci & Technol Branch, Cleveland, OH 44135 USA. Cleveland Clin Fdn, Lerner Res Inst, Dept Biomed Engn, Cleveland, OH 44195 USA. RP Freed, AD (reprint author), NASA, John H Glenn Res Ctr Lewis Field, Bio Sci & Technol Branch, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM alan.d.freed@nasa.gov; doehrint@ccf.org RI Guo, Zaoyang/A-5279-2008; OI Guo, Zaoyang/0000-0002-7609-3472; Freed, Alan/0000-0002-3492-0628 FU NHLBI NIH HHS [HL 72598] NR 34 TC 60 Z9 60 U1 1 U2 13 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA SN 0148-0731 J9 J BIOMECH ENG-T ASME JI J. Biomech. Eng.-Trans. ASME PD AUG PY 2005 VL 127 IS 4 BP 587 EP 593 DI 10.1115/1.1934145 PG 7 WC Biophysics; Engineering, Biomedical SC Biophysics; Engineering GA 952VS UT WOS:000231034400005 PM 16121528 ER PT J AU Martinez, DM Ferguson, FT Heist, RH Nuth, JA AF Martinez, DM Ferguson, FT Heist, RH Nuth, JA TI Experimental studies of the vapor phase nucleation of refractory compounds. VI. The condensation of sodium SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID ULTRAFINE METAL PARTICLES; HOMOGENEOUS NUCLEATION; SUPERSATURATED VAPOR; CLOUD CHAMBER; LIQUID; SIO AB In this paper we discuss the condensation of sodium vapor and the formation of a sodium aerosol as it occurs in a gas evaporation condensation chamber. A one-dimensional model describing the vapor transport to the vapor/aerosol interface was employed to determine the onset supersaturation, in which we assume the observed location of the interface is coincident with a nucleation rate maximum. We then present and discuss the resulting nucleation onset supersaturation data within the context of nucleation theory based on the liquid droplet model. Nucleation results appear to be consistent with a cesium vapor-to-liquid nucleation study performed in a thermal diffusion cloud chamber. (C) 2005 American Institute of Physics. C1 Univ Rochester, Dept Chem Engn, Rochester, NY 14627 USA. Catholic Univ Amer, Dept Chem, Washington, DC 20064 USA. Manhattan Coll, Dept Chem Engn, Riverdale, NY 10471 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Martinez, DM (reprint author), Univ Rochester, Dept Chem Engn, Rochester, NY 14627 USA. EM daniel.m.martinez@nasa.gov RI Ferguson, Frank/C-9493-2012; Nuth, Joseph/E-7085-2012 NR 34 TC 3 Z9 3 U1 0 U2 6 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD AUG 1 PY 2005 VL 123 IS 5 AR 054323 DI 10.1063/1.1998834 PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 954QD UT WOS:000231168700039 PM 16108655 ER PT J AU Friend, AD Kiang, NY AF Friend, AD Kiang, NY TI Land surface model development for the GISS GCM: Effects of improved canopy physiology on simulated climate SO JOURNAL OF CLIMATE LA English DT Article ID AMAZONIAN RAIN-FOREST; STOMATAL CONDUCTANCE; CARBON-DIOXIDE; WATER-VAPOR; PHOTOSYNTHETIC CAPACITY; SEASONAL-VARIATION; MECHANISTIC MODEL; BIOCHEMICAL-MODEL; GLOBAL RADIATION; DIRECT COMPONENT AB A new physiology-based model of canopy stomatal conductance and photosynthesis is described and included in the latest version of the Goddard Institute for Space Studies (GISS) GCM, ModelE1. The submodel includes responses to atmospheric humidity and CO2 concentration, responses missing from previous GISS GCM land surface schemes. Measurements of moisture, energy, and CO2 fluxes over four vegetation types are used to test and calibrate the submodel. Photosynthetic leaf N is calibrated for each vegetation type from the flux measurements. The new submodel results in surface cooling over many regions previously too warm. Some warm biases of over 2 degrees C are cooled by more than 0.5 degrees C, including over central Eurasia, South America, the western United States, and Australia. In addition, some regions that were previously too cool are warmed, such as northern Eurasia and the Tibetan Plateau. A number of precipitation biases are also reduced, particularly over South America (by up to 1 mm day(-1)) and the oceanic ITCZs (by over +/- 1 mm day(-1)); coastal west Africa becomes significantly wetter. Cloud cover increases over many land areas previously too clear. Higher absolute canopy conductances, and positive feedbacks with atmospheric humidity, are largely responsible for the simulated vegetation influence on the atmosphere. High-latitude climate changes through remote effects of increased tropical latent beating, resulting directly from improved characterization of tropical forest canopy conductance. Realistic representation of the stomatal control on land evaporation is critical for accurate simulation of atmospheric dynamics in the GISS GCM. C1 Lab Sci Climat & Environm Orme, F-91191 Gif Sur Yvette, France. Columbia Univ, NASA, Goddard Inst Space Studies, Earth Inst,Ctr Climate Syst Res, New York, NY USA. RP Lab Sci Climat & Environm Orme, Bat 712, F-91191 Gif Sur Yvette, France. EM friend@lsce.saclay.cea.fr RI Garcia Bustamante, Elena/H-4188-2012 OI Garcia Bustamante, Elena/0000-0002-2677-0252 NR 76 TC 57 Z9 59 U1 0 U2 8 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD AUG 1 PY 2005 VL 18 IS 15 BP 2883 EP 2902 DI 10.1175/JCLI3425.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 962NA UT WOS:000231738300006 ER PT J AU Su, CH AF Su, CH TI Composition-temperature-partial pressures data for Cd0.8Zn0.2Te by optical absorption measurements SO JOURNAL OF CRYSTAL GROWTH LA English DT Article DE phase diagrams; solubility; semiconducting II-VI materials ID TERNARY-SYSTEM; CRYSTAL-GROWTH; CDTE; ZN AB Known weights of Cd, Zn and Te were reacted in silica optical cells of known volume, and the partial pressures of Te, and Cd between 485 and 1160 degrees C were determined by measuring the optical density of the vapor in the ultra-violet to visible range. The composition of the condensed phase or phases was calculated from the original weights and the amount of material in the vapor phase. The corresponding composition-temperature-partial pressures, x(Te) -T-P-Tc2,data, including five Te-rich solidus points, were established. The solubility range for the Te-rich Cd0.8Zn0.2Te(s) is similar to that of CdTe(s) with X-Te = 0.50005 at 809 degrees C and an estimated maximum solubility of X-Te = 0.50012 at about 1000 degrees C. The partial pressures of Cd and Te, measured over the Cd0.8Zn0.2Te melt at 1140 degrees C were about 1.55 and 0.02 atm, respectively, and the corresponding Zn partial pressure was estimated to be 0.05 atm. It was recommended that a Cd reservoir maintained at 800-820 degrees C should be used during directional solidification of Cd0.8Zn0.2Te to prevent the preferential loss of Cd to the vapor phase. (c) 2005 Elsevier B.V. All rights reserved. C1 NASA, George C Marshall Space Flight Ctr, Sci & Technol Directorate, Explorat Sci & Technol Div XD42, Huntsville, AL 35812 USA. RP Su, CH (reprint author), NASA, George C Marshall Space Flight Ctr, Sci & Technol Directorate, Explorat Sci & Technol Div XD42, Huntsville, AL 35812 USA. EM ching.hua.su@msfc.nasa.gov NR 14 TC 2 Z9 2 U1 0 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0248 J9 J CRYST GROWTH JI J. Cryst. Growth PD AUG 1 PY 2005 VL 281 IS 2-4 BP 577 EP 586 DI 10.1016/j.jcrysgro.2005.04.099 PG 10 WC Crystallography; Materials Science, Multidisciplinary; Physics, Applied SC Crystallography; Materials Science; Physics GA 952NR UT WOS:000231011600054 ER PT J AU Padmini, P Tompkins, F Shojah-Ardalan, S Kale, P Wilkins, R Pandey, RK AF Padmini, P Tompkins, F Shojah-Ardalan, S Kale, P Wilkins, R Pandey, RK TI Influence of proton radiation on the nonlinear current-voltage characteristics of pulsed laser deposited ilmenite-hematite thin films SO JOURNAL OF ELECTRONIC MATERIALS LA English DT Article DE ilmenite-hematite (IH); varistor; protons; radiation ID SOLID SOLUTION SERIES; SPACE; IRRADIATION; ENVIRONMENT; CERAMICS; DEVICES AB Ilmenite-hematite (IH) [(1-x)FeTio(3)center dot xFe(2)O(3)] solid solutions are unique classes of materials showing both magnetic and semiconducting properties, which make them potential candidates for novel applications in microelectronics and spintronics. This paper focuses on their varistor behavior before and after exposure to 40 MeV and 10 MeV proton radiations up to a fluence of 5 X 10(10) p/cm(2). The IH films are tolerant to these irradiations with little significant change to the nonlinear current-voltage characteristics. The switching voltage of the devices is in the regime of practical applications, and the radiation tolerance makes these materials suitable for aerospace applications. C1 Univ Alabama, Dept Elect & Comp Engn, Tuscaloosa, AL 35487 USA. Prairie View A&M Univ, Dept Elect Engn, Prairie View, TX 77446 USA. NASA, Ctr Appl Radiat Res, Prairie View, TX 77446 USA. RP Padmini, P (reprint author), Univ Alabama, Dept Elect & Comp Engn, Tuscaloosa, AL 35487 USA. EM padmini@bama.ua.edu NR 20 TC 9 Z9 9 U1 1 U2 5 PU MINERALS METALS MATERIALS SOC PI WARRENDALE PA 184 THORN HILL RD, WARRENDALE, PA 15086 USA SN 0361-5235 J9 J ELECTRON MATER JI J. Electron. Mater. PD AUG PY 2005 VL 34 IS 8 BP 1095 EP 1098 DI 10.1007/s11664-005-0235-x PG 4 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Materials Science; Physics GA 953CE UT WOS:000231052800001 ER PT J AU Rivera, G Savitzky, AH Hinkley, JA AF Rivera, G Savitzky, AH Hinkley, JA TI Mechanical properties of the integument of the common gartersnake, Thamnophis sirtalis (Serpentes : Colubridae) SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE integument; skin; biomechanics; feeding; snake; Thamnophis sirtalis ID VANCOUVER-ISLAND; SKIN MECHANICS; FISH SKIN; SNAKES; MORPHOLOGY; HABITS; GEKKONIDAE; EVOLUTION; AMPHIBIA; REPTILIA AB The evolution of the ophidian feeding mechanism has involved substantial morphological restructuring associated with the ability to ingest relatively large prey. Previous studies examining the morphological consequences of macrophagy have concentrated on modifications of the skull and cephalic musculature. Although it is evident that macrophagy requires highly compliant skin, the mechanical properties of the ophidian integument have received limited attention, particularly in the context of feeding. We examined mechanical properties of skin along the body axis in Thamnophis sirtalis (Colubridae). Data were collected from tensile tests and were analyzed using a multivariate analysis of variance (MANOVA) and post-hoc multiple comparison tests. Significant differences in mechanical properties were detected among regions of the body. In general, prepyloric skin is more compliant than postpyloric skin, consistent with the demands of macrophagy. C1 Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA. RP Rivera, G (reprint author), Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA. EM grivera@clemson.edu NR 47 TC 7 Z9 7 U1 4 U2 11 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL, CAMBS, ENGLAND SN 0022-0949 J9 J EXP BIOL JI J. Exp. Biol. PD AUG PY 2005 VL 208 IS 15 BP 2913 EP 2922 DI 10.1242/jeb.01715 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 960FO UT WOS:000231575800020 PM 16043596 ER PT J AU Willis, P Ries, JC AF Willis, P Ries, JC TI Defining a DORIS core network for Jason-1 precise orbit determination based on ITRF2000: methods and realization SO JOURNAL OF GEODESY LA English DT Article DE terrestrial reference frame; precise orbit determination; DORIS; satellite tracking networks ID TERRESTRIAL REFERENCE FRAME; VERTICAL CRUSTAL MOTIONS; SEA-LEVEL; PLATE MOTIONS; TIME-SERIES; SYSTEM; CONSTRAINTS; GPS AB In view of the future adoption of the new precise orbit determination (POD) standards for the TOPEX/Poseidon and Jason-1 satellites, we propose a method to evaluate terrestrial reference frames for POD. We applied this method to the ITRF2000 realization of the DORIS network using local geodetic ties, plate motion models, the recent DORIS IGN04D02 cumulative solution and DORIS weekly time-series of coordinates. We propose to adopt a selection of the ITRF2000 realization based on specific criteria that we define here, and to extend it with ground stations for which we propose new coordinates and velocities. Only 13 out of 131 stations were considered to be inappropriate for POD activities. The result is a robust and well-distributed DORIS core network of 118 stations (DPOD2000) suitable for POD during the 1993-2008 period considered here. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Inst Geog Natl, Direct Tech, St Mande, France. Univ Texas, Ctr Space Res, Austin, TX 78712 USA. RP Willis, P (reprint author), CALTECH, Jet Prop Lab, MS 238-600,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM pascal.r.willis@jpl.nasa.gov RI Willis, Pascal/A-8046-2008 OI Willis, Pascal/0000-0002-3257-0679 NR 38 TC 29 Z9 31 U1 0 U2 1 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0949-7714 EI 1432-1394 J9 J GEODESY JI J. Geodesy PD AUG PY 2005 VL 79 IS 6-7 BP 370 EP 378 DI 10.1007/s00190-005-0475-9 PG 9 WC Geochemistry & Geophysics; Remote Sensing SC Geochemistry & Geophysics; Remote Sensing GA 966JM UT WOS:000232016000007 ER PT J AU Leftwich, TE von Frese, RRB Potts, LV Kim, HR Roman, DR Taylor, PT Barton, M AF Leftwich, TE von Frese, RRB Potts, LV Kim, HR Roman, DR Taylor, PT Barton, M TI Crustal modeling of the North Atlantic from spectrally correlated free-air and terrain gravity SO JOURNAL OF GEODYNAMICS LA English DT Article DE North Atlantic; Iceland; Greenland-Scotland Ridge; gravity; crust; moho ID ICELAND RIDGE EXPERIMENT; BANK CONTINENTAL-MARGIN; HEAT-FLOW; PARTIAL MELT; UPPER-MANTLE; RIFT-ZONE; SKAERGAARD INTRUSION; SATELLITE ALTIMETRY; THERMAL STRUCTURE; BENEATH ICELAND AB We investigate the use of the correlations between free-air and terrain gravity for extending critical, but spatially restricted seismic constraints on the crust of the North Atlantic region. In this tectonically complicated area, we spectrally correlate spherical coordinate free-air gravity anomalies against computed gravity effects of the terrain at 20 km altitude for regional crustal thickness variations. However, at the Mid-Atlantic Ridge, thermal plume, and rift zones of Iceland, our gravity Moho estimates are deeper than the seismic estimates to suggest local reductions of upper mantle density. Invoking thermal expansion, partial melting, and related mantle depletion effectively accounts for the reductions that range up to a few percent of mantle density. The resultant North Atlantic crustal model conforms well to regional seismic constraints. Crustal thickness estimates for Iceland ranging from 25 to 35 km are consistent with seismic predictions of a thickened crust. However, about the plume and rift zones, temperatures approaching the basalt solidus may reach depths up to about 20 km. Continental crust extending from the Jan Mayen Platform to the eastern Iceland Plateau appears to have rifted off eastern Greenland by magnetic chron 7 (ca. 2628 Ma). A now obscure transform boundary on the Iceland Plateau that may include a rift or fault separating the southeastern Iceland Plateau from the rest of the plateau transformed Reykjanes Ridge spreading from the extinct Aegir Ridge. Thickened crust extends up to 500 km across the Greenland-Scotland Ridge. Prominent necking of our crustal thickness estimates for the Greenland-Iceland Ridge immediately west and east of the Iceland Plateau may reflect the reduction in the strength of the Icelandic Plume at ca. 26-28 Ma. However, our results also map the broad, thickened crust of the Iceland Plateau and prominent Reykjanes Ridge that developed with the resurgence of the Icelandic Plume at ca. 25 Ma. (c) 2005 Elsevier Ltd. All rights reserved. C1 Ohio State Univ, Dept Geol Sci, Columbus, OH 43210 USA. Ohio State Univ, Dept Civil & Environm Engn & Geodet Sci, Columbus, OH 43210 USA. NASA, Goddard Space Flight Ctr, Geodynam Branch, Greenbelt, MD 20771 USA. NOAA, Natl Geodet Survey, Silver Spring, MD 20910 USA. RP Leftwich, TE (reprint author), Ohio State Univ, Dept Geol Sci, Columbus, OH 43210 USA. EM leftwich.12@osu.edu; vonfrese@osu.edu; potts.3@osu.edu; kimhr@cored.gsfc.nasa.gov; droman@ngs.noaa.gov; Patrick.Taylor@nasa.gov; barton.2@osu.edu RI Taylor, Patrick/D-4707-2012 OI Taylor, Patrick/0000-0002-1212-9384 NR 86 TC 11 Z9 12 U1 1 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0264-3707 J9 J GEODYN JI J. Geodyn. PD AUG PY 2005 VL 40 IS 1 BP 23 EP 50 DI 10.1016/j.jog.2005.05.001 PG 28 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 988UJ UT WOS:000233626200002 ER PT J AU Xue, YK Sun, SF Lau, KM Ji, JJ Poccard, I Zhang, RH Kang, HS Wu, GX Schaake, JC Zhang, JY Jiao, YJ AF Xue, YK Sun, SF Lau, KM Ji, JJ Poccard, I Zhang, RH Kang, HS Wu, GX Schaake, JC Zhang, JY Jiao, YJ TI Multiscale variability of the river runoff system in China and its long-term link to precipitation and sea surface temperature SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID SINGULAR-VALUE DECOMPOSITION; ASIAN SUMMER MONSOON; EMPIRICAL ORTHOGONAL FUNCTIONS; NINO SOUTHERN OSCILLATION; TROPICAL WESTERN PACIFIC; EL-NINO; UNITED-STATES; RAINFALL VARIABILITY; CLIMATE; TRENDS AB This is an exploratory study to investigate the spatial and temporal characteristics of east China's (EC) river runoff and their relationship with precipitation and sea surface temperature (SST) at the continental scale. Monthly mean data from 72 runoff stations and 160 precipitation stations in EC, covering a period between 1951 and 1983, are used for this study. The station river runoff data have been spatially interpolated onto 1 degrees grid boxes as runoff depth based on an extracted drainage network. Comparing runoff depth with precipitation shows that seasonal variation in runoff is consistent with the development of the summer monsoon, including the delayed response of runoff in several subregions. The dominant spatial scales and temporal patterns of summer runoff and precipitation are studied with empirical orthogonal function.(EOF) analysis and wavelet analyses. The analyses show interannual, biennial, and longer-term variations in the EOF modes. South-north dipole anomaly patterns for the first two runoff EOF's spatial distributions have been identified. The first/second runoff principal components (PCs) are highly correlated with the second/ first precipitation PCs, respectively. The summer runoff's EOF PCs also show significant correlations with the multivariate El Nino-Southern Oscillation index (MEI) of the summer and winter months, while the summer precipitation PCs do not. Statistic analysis shows that EOF1 of runoff and EOF2 of precipitation are related to El Nino, while EOF2 of runoff and EOF1 of precipitation are related to a dipole SST anomaly over the northwestern Pacific. The interdecadal relationship between summer runoff, precipitation, and SST variability is further studied by singular value decomposition (SVD) analysis. Pronounced warming (SST) and drying (runoff) trends in first SVD PCs have been identified. These SVDs are used to reconstruct a decadal anomaly pattern, which produces flooding in part of the Chang Jiang River basin and dryness in the northern EC, consistent with observations. C1 Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90095 USA. Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA. LASG, Inst Atmospher Phys, Beijing, Peoples R China. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Chinese Acad Meteorol Sci, Beijing, Peoples R China. NOAA, Natl Weather Serv, Silver Spring, MD 20910 USA. Minist Hydraul Engn & Water Resources, Beijing, Peoples R China. Univ Quebec, Montreal, PQ H3C 3P8, Canada. RP Xue, YK (reprint author), Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90095 USA. EM yxue@geog.ucla.edu RI Lau, William /E-1510-2012 OI Lau, William /0000-0002-3587-3691 NR 45 TC 11 Z9 11 U1 1 U2 13 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X J9 J HYDROMETEOROL JI J. Hydrometeorol. PD AUG PY 2005 VL 6 IS 4 BP 550 EP 570 DI 10.1175/JHM439.1 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 970JR UT WOS:000232304500013 ER PT J AU Schneider, JA Nunes, AC Chen, PS Steele, G AF Schneider, JA Nunes, AC Chen, PS Steele, G TI TEM study of the FSW nugget in AA2195-T81 SO JOURNAL OF MATERIALS SCIENCE LA English DT Article ID FRICTION STIR WELD; DYNAMIC RECRYSTALLIZATION; ALUMINUM-ALLOYS; PRECIPITATION; MICROSTRUCTURE; PROPERTY AB During friction stir welding (FSW) the material being joined is subjected to a thermal-mechanical process in which the temperature, strain and strain rates are not completely understood. To produce a defect free weld, process parameters for the weld and tool pin design must be chosen carefully. The ability to select the weld parameters based on the thermal processing requirements of the material, would. allow optimization of mechanical properties in the weld region. In this study, an attempt is made to correlate the microstructure with the variation in thermal history the material experiences during the FSW process. (c) 2005 Springer Science + Business Media, Inc. C1 Mississippi State Univ, Dept Mech Engn, Mississippi State, MS 39762 USA. NASA, George C Marshall Space Flight Ctr, Mat Proc & Mfg Met Mat, Huntsville, AL 35812 USA. Morgan Res Corp, Huntsville, AL USA. RP Schneider, JA (reprint author), Mississippi State Univ, Dept Mech Engn, Mississippi State, MS 39762 USA. EM schneider@me.msstate.edu NR 23 TC 26 Z9 29 U1 3 U2 11 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0022-2461 J9 J MATER SCI JI J. Mater. Sci. PD AUG PY 2005 VL 40 IS 16 BP 4341 EP 4345 DI 10.1007/s10853-005-2808-8 PG 5 WC Materials Science, Multidisciplinary SC Materials Science GA 958AO UT WOS:000231417300024 ER PT J AU King, TT Kletetschka, G Jah, MA Beamesderfer, MA Li, MJ Wang, LL Moseley, SH Sparr, LM Jhabvala, MD Kutyrev, AS Silverberg, RF Rapchun, D Zheng, Y Schwinger, DS Voellmer, GM AF King, TT Kletetschka, G Jah, MA Beamesderfer, MA Li, MJ Wang, LL Moseley, SH Sparr, LM Jhabvala, MD Kutyrev, AS Silverberg, RF Rapchun, D Zheng, Y Schwinger, DS Voellmer, GM TI Cryogenic characterization and testing of magnetically-actuated microshutter arrays for the James Webb Space Telescope SO JOURNAL OF MICROMECHANICS AND MICROENGINEERING LA English DT Article AB Two-dimensional MEMS microshutter arrays (MSA) have been fabricated at the NASA Goddard Space Flight Center (GSFC) for the James Webb Space Telescope (JWST) to enable cryogenic (similar to 35 K) spectrographic astronomy measurements at near-infrared wavelengths. Functioning as a focal plane object selection device, the MSA is a 2D programmable aperture mask with fine resolution, high efficiency and high contrast. The MSA are close-packed silicon nitride shutters (cell size of 100 mu m x 200 mu m) patterned with a torsion flexure to allow their opening to 90 degrees. A layer of magnetic material is deposited onto each shutter to permit magnetic actuation. Two electrodes are deposited, one onto each shutter and another onto the support structure side-wall, permitting electrostatic latching and 2D addressing. New techniques were developed to test MSA under mission-similar conditions (8 K <= T < 300 K). The 'magnetic rotisserie' has proven to be an excellent tool for rapid characterization of MSA. Tests conducted with the magnetic rotisserie method include accelerated cryogenic lifetesting of unpackaged 128 x 64 MSA and parallel measurement of the magneto-mechanical stiffness of shutters in `pathfinder' test samples containing multiple MSA designs. Lifetest results indicate a logarithmic failure rate out to similar to 10(6) shutter actuations. These results have increased our understanding of failure mechanisms and provide a means to predict the overall reliability of MSA devices. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Catholic Univ Amer, Washington, DC 20064 USA. Swales Aerosp Co, Beltsville, MD 20705 USA. Sci Syst & Applicat Inc, Lanham, MD 20706 USA. Global Sci & Technol, Greenbelt, MD 20770 USA. QSS Grp Inc, Lanham, MD 20770 USA. RP NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Kletetschka, Gunther/C-9996-2011; Moseley, Harvey/D-5069-2012 OI Kletetschka, Gunther/0000-0002-0645-9037; NR 10 TC 3 Z9 3 U1 3 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0960-1317 EI 1361-6439 J9 J MICROMECH MICROENG JI J. Micromech. Microeng. PD AUG PY 2005 VL 15 IS 8 BP 1594 EP 1600 DI 10.1088/0960-1317/15/8/031 PG 7 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology; Instruments & Instrumentation; Physics, Applied SC Engineering; Science & Technology - Other Topics; Instruments & Instrumentation; Physics GA 959IX UT WOS:000231512500031 ER PT J AU Predoi-Cross, A Brown, LR Devi, VM Brawley-Tremblay, M Benner, DC AF Predoi-Cross, A Brown, LR Devi, VM Brawley-Tremblay, M Benner, DC TI Multispectrum analysis of (CH4)-C-12 from 4100 to 4635 cm(-1): 1. Self-broadening coefficients (widths and shifts) SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE methane; octad; self-broadening; multispectrum; widths; pressure shifts ID MOLECULAR SPECTROSCOPIC DATABASE; Q-BRANCH; LASER SPECTROSCOPY; FITTING TECHNIQUE; LINE PARAMETERS; HALF-WIDTHS; MU-M; METHANE; BAND; INTENSITIES AB The Lorentz self-broadening (halfwidths) and self-induced pressure-shift coefficients were measured for the first time in the octad region of methane. All spectra were recorded at 0.011 cm(-1) resolution using the McMath-Pierce Fourier transform spectrometer located at the National Solar Observatory on Kitt Peak, Arizona. C-12-enriched CH4 gas samples at room temperature were used, and high signal-to-noise ratios of 2000:1 were achieved. The multispectrum nonlinear least squares fitting technique enabled us to fit simultaneously a total of 10 high-resolution laboratory absorption spectra consisting of six self-broadened and four air-broadened spectra. In this paper, we report the self-broadened widths and self-induced pressure shift coefficients for 1423 transitions belonging to five bands with a maximum J of 16. The numbers of measurements by bands are: 71 for nu(2) + 2 nu(4), 202 for nu(1) + nu(4), 824 for nu(3) + nu(4), 58 for 2 nu(2) + nu(4), and 268 for nu(2) + nu(3). The observed widths varied from 0.045 to about 0.090 cm(-1) atm(-1) at 296 K. The measured pressure-shift coefficients had values extending from about -0.020 to -0.005 cm(-1) atm(-1) at 298.3 +/- 1.2 K. The results obtained for the broadening coefficients in the various bands were compared with each other and with measurements reported in the literature for other methane bands. (c) 2005 Elsevier Inc. All rights reserved. C1 Univ Lethbridge, Dept Phys, Lethbridge, AB T1K 3M4, Canada. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA. RP Predoi-Cross, A (reprint author), Univ Lethbridge, Dept Phys, 4401 Univ Dr, Lethbridge, AB T1K 3M4, Canada. EM adriana.predoicross@uleth.ca NR 29 TC 25 Z9 26 U1 0 U2 2 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD AUG PY 2005 VL 232 IS 2 BP 231 EP 246 DI 10.1016/j.jms.2005.04.007 PG 16 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA 949EW UT WOS:000230768700011 ER PT J AU Ueno, T Macias, BR Yost, WT Hargens, AR AF Ueno, T Macias, BR Yost, WT Hargens, AR TI Noninvasive assessment of intracranial pressure waveforms by using pulsed phase lock loop technology - Technical note SO JOURNAL OF NEUROSURGERY LA English DT Article DE intracranial pressure; pulsed phase lock loop; Fourier transform; coherence; distortion ratio ID SEVERE HEAD-INJURY; CEREBRAL AUTOREGULATION; ULTRASOUND; EXPERIENCE; MANAGEMENT; MONITOR; SYSTEM AB Elevated intracranial pressure (ICP) is a major factor associated with incidences of morbidity and mortality in patients with neurological disorders. The use of conventional methods for ICP monitoring is currently limited to patients with severe neurological conditions because of the methods' invasive nature. The authors have developed an ultrasonic device capable of monitoring ICP waveforms noninvasively by using a pulsed phase lock loop (PPLL) technique. The PPLL device records skull movement (several meters) associated with ICP pulsations. The purpose of this study was to correlate PPLL waveforms with invasively measured ICP waveforms in patients at the University of California San Diego Medical Center (13 patients). A linear regression analysis revealed a high correlation between PPLL waveforms and invasively measured ICP waveforms during the same time domain (r(2) = 0.88). A coherence function analysis, which provides the fractional portion of the mean square value at the output that is contributed by the input at a certain frequency, showed medium to high correlations (r(2) = 0.50-0.90) between PPLL waveforms and invasively measured ICP waveforms at each harmonic wave components. Furthermore, there was a significant correlation (r(2) = 0.680, p < 0.01) in the harmonic distortion ratio (an index representing how much a given waveform is distorted from a pure sine wave) between PPLL waveforms and invasively measured ICP waveforms. In conclusion, PPLL technology enables the noninvasive evaluation of ICP dynamics in clinical settings. C1 Univ Calif San Diego, Dept Orthopaed Surg, San Diego, CA 92103 USA. NASA, Langley Res Ctr, Div Mat, Nondestruct Evaluat Sci Branch, Hampton, VA 23665 USA. RP Ueno, T (reprint author), Univ Calif San Diego, Dept Orthopaed Surg, San Diego, CA 92103 USA. EM tueno@med.teikyo-u.ac.jp NR 31 TC 6 Z9 6 U1 1 U2 6 PU AMER ASSOC NEUROLOGICAL SURGEONS PI CHARLOTTESVILLE PA UNIV VIRGINIA, 1224 WEST MAIN ST, STE 450, CHARLOTTESVILLE, VA 22903 USA SN 0022-3085 J9 J NEUROSURG JI J. Neurosurg. PD AUG PY 2005 VL 103 IS 2 BP 361 EP 367 DI 10.3171/jns.2005.103.2.0361 PG 7 WC Clinical Neurology; Surgery SC Neurosciences & Neurology; Surgery GA 957KI UT WOS:000231368300025 PM 16175869 ER PT J AU Lai, RJ Huang, N AF Lai, RJ Huang, N TI Investigation of vertical and horizontal momentum transfer in the Gulf of Mexico using empirical mode decomposition method SO JOURNAL OF PHYSICAL OCEANOGRAPHY LA English DT Article ID TOPOGRAPHIC ROSSBY WAVES; HILBERT SPECTRUM; FREQUENCY AB Data from a series of deep mooring stations in the Gulf of Mexico (GOM) have been analyzed with the newly developed empirical mode decomposition and Hilbert spectral analysis method, abbreviated as Hilbert-Huang transformation (HHT). The flows in the GOM near the shelf/slope region are treated as a two-layer system, with the 800-m permanent thermocline as the dividing depth. When the data are treated with HHT, motions of different temporal scales are identified. The top layer (depth less than 800 m) is controlled by inertia flow with episodic Loop Current eddies, while the lower layer (depth greater than 800 m) is controlled primarily by the topographic Rossby waves and small-scale cyclonic and anticyclonic eddies. Using a cross-correlation analysis between the appropriate intrinsic mode components from the data, the wavelength, the phase velocity, and the vertical trapping depth for the topographic Rossby waves were determined. Observations are in general agreement with the modeled results by Oey and Lee. C1 US Dept Interior, Minerals Management Serv, Environm Sci Branch, Herndon, VA USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lai, RJ (reprint author), US Dept Interior, Minerals Management Serv, Environm Sci Branch, 381 Elden St,MS 4041, Herndon, VA USA. EM ronald.lai@mms.gov NR 17 TC 10 Z9 10 U1 1 U2 6 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 AUG PY 2005 VL 35 IS 8 BP 1383 EP 1402 DI 10.1175/JPO2755.1 PG 20 WC Oceanography SC Oceanography GA 961ZS UT WOS:000231701400007 ER PT J AU Tai, CK Fu, LL AF Tai, CK Fu, LL TI The 25-day-period large-scale oscillations in the Argentine Basin revisited SO JOURNAL OF PHYSICAL OCEANOGRAPHY LA English DT Article ID SATELLITE; WAVES AB From sea surface height measurements made by the Ocean Topography Experiment (TOPEX)/Poseidon satellite, Fu et al. found and described large-scale oscillations at the period of 25 days in the Argentine Basin of the South Atlantic Ocean. These oscillations were previously hinted at by in situ observations. Only the extensive space-time sampling capability of TOPEX/Poseidon, however, was able to give a complete description of the phenomenon as a counterclockwise-rotating dipole centered at 45 degrees S, 317 degrees E over the Zapiola Rise. Fu et al. also undertook theoretical and numerical studies to suggest that the phenomenon is a resonantly excited barotropic normal mode of the locally closed f/H contour. In a simulation study, however, they also found that the space-time smoothing scheme employed would probably lower the amplitude of the estimated phenomenon by 30%-40%. By reprocessing the data using a different method and showing the amplitude to be almost 2 times as large, in this note it is confirmed that this is indeed the case. The original 5-yr study has also been extended to nearly 10 yr, demonstrating that the same phenomenon has persisted for almost 10 yr. C1 NOAA, Natl Environm Satellite Data & Informat Serv, Camp Springs, MD 20746 USA. CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Tai, CK (reprint author), NOAA, Natl Environm Satellite Data & Informat Serv, 5200 Auth Rd,E-RA3, Camp Springs, MD 20746 USA. EM ek.tai@noaa.gov RI Tai, C.K./F-5628-2010 NR 14 TC 9 Z9 9 U1 0 U2 3 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-3670 J9 J PHYS OCEANOGR JI J. Phys. Oceanogr. PD AUG PY 2005 VL 35 IS 8 BP 1473 EP 1479 DI 10.1175/JPO2766.1 PG 7 WC Oceanography SC Oceanography GA 961ZS UT WOS:000231701400012 ER PT J AU Toth, RA AF Toth, RA TI Measurements and analysis (using empirical functions for widths) of air- and self-broadening parameters of H2O SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE H2O; measured widths; analysis ID DIODE-LASER MEASUREMENTS; VAPOR LINE PARAMETERS; 720-NM WAVELENGTH REGION; 1.39 MU-M; WATER-VAPOR; CM(-1) REGION; SPECTRAL REGION; HIGH-RESOLUTION; NU-2 BAND; N2-BROADENING COEFFICIENTS AB High-resolution spectra of H2O were recorded with the McMath Fourier-transform spectrometer at the National Solar Observatory located at Kitt Peak, AZ. Seventeen laboratory spectra of water plus air mixtures were recorded at a spectral resolution of 0.01 cm(-1) covering the region between 2800 and 8000 cm(-1). Over 4000 linewidth and pressure-induced frequency shift coefficients were derived from the spectral data with sample temperatures near or at room temperature (296 K). The measurements include transitions of H-2 (16)0, H-2 O-17, and H-2 O-18 with the rare oxygen species observed in normal H2O gas samples. The measurements were analyzed with consideration of collision-narrowing effects. The analysis required a knowledge of the self-broadened linewidth coefficients, and the data measured and reported in the previous study were used along with earlier results for this purpose. The self-broadened and air-broadened measured linewidth coefficients obtained here as well as those reported in earlier studies covering the 600-2400 cm(-1), were fitted to an empirical expression which contains up to 28 terms. Two fitting procedures were used: one considered the fit of families of transitions and the other was more global in scope. The computed linewidth coefficients derived from the fitted parameters are compared statistically to measurements in this work as well as other studies. (C) 2004 Elsevier Ltd. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Toth, RA (reprint author), CALTECH, Jet Prop Lab, MS 183-301, Pasadena, CA 91109 USA. EM toth@caesar.jpl.nasa.gov NR 50 TC 31 Z9 32 U1 3 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD AUG 1 PY 2005 VL 94 IS 1 BP 1 EP 50 DI 10.1016/j.jqsrt.2004.08.041 PG 50 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 900DO UT WOS:000227195800001 ER PT J AU Toth, RA AF Toth, RA TI Measurements of positions, strengths and self-broadened widths of H2O from 2900 to 8000cm(-1): line strength analysis of the 2nd triad bands SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE H2O; infrared; laboratory; spectroscopy ID DIODE-LASER MEASUREMENTS; EXPERIMENTAL ENERGY-LEVELS; HYDROGEN FLAME SPECTRA; RO-VIBRATIONAL LEVELS; MU-M REGION; WATER-VAPOR; INTERACTING STATES; CM-1 REGION; HOT BANDS; V2&V3 BANDS AB High-resolution spectra of H2O were recorded with a Fourier-transform spectrometer covering H2O transitions from 2900 to 8000 cm(-1). Over 13,000 absorptions were measured to determine line positions, strengths and self-broadened half-width coefficients. The H-2 O-16 line strengths of the (030)-(010),(110)-(010), (011)-(010) and (030)-(000), (110)-(000), (011)-(000) bands were fitted to a quantum mechanical model which involves the interactions between the (030), (110), and (011) vibrational states. Also fitted were experimental strengths of the hot bands; (120)-(010) and (021)-(010). The model includes 14 dipole matrix elements for B- and A-type transitions. The measured line positions were used along with hot water emission measurements (for the (030), (040), and (050) states of H-2 O-16) in an analysis to obtain high-accuracy energy level values in the (030), (1 10), (011), (040), (120), (021), (200), (101). (002), and (050) vibrational states of H-2 O-16 and the (110) and (011) states of H-2 O-17. Also included were measurements and analysis of self-broadened half-widths for over 4700 absorptions between 4405 and 7729 cm(-1). The results from this investigation provide new information for the noted H-2 O-17 bands and present a more accurate representation of the measured H-2 O-16 bands. (C) 2004 Elsevier Ltd. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Toth, RA (reprint author), CALTECH, Jet Prop Lab, MS 183-301, Pasadena, CA 91109 USA. EM toth@caesar.jpl.nasa.gov NR 45 TC 57 Z9 59 U1 2 U2 9 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 AUG 1 PY 2005 VL 94 IS 1 BP 51 EP 107 DI 10.1016/j.jqsrt.2004.08.042 PG 57 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 900DO UT WOS:000227195800002 ER PT J AU Leventis, N Palczer, A McCorkle, L Zhang, GH Sotiriou-Leventis, C AF Leventis, N Palczer, A McCorkle, L Zhang, GH Sotiriou-Leventis, C TI Nanoengineered silica-polymer composite aerogels with no need for supercritical fluid drying SO JOURNAL OF SOL-GEL SCIENCE AND TECHNOLOGY LA English DT Article DE aerogel; crosslinked; composite; ambient pressure; drying ID AMBIENT-PRESSURE; MONOLITHS; FILMS; OXIDE AB Owing to their low density, dielectric constant, thermal conductivity, high porosity and chemical inertness, monolithic aerogels could be useful in a variety of electronic, optical and chemical applications [1]. However, practical implementation has been slow, because aerogels are fragile, environmentally sensitive (hydrophilic) and most importantly, the final stage of their preparation involves supercritical fluid (SCF) extraction [1c]. It is reported herewith that for a nominal 3-fold increase in density, typical polymer crosslinked silica aerogels are not only stronger (> 300x) and less hydrophilic (< 10x) than the underlying silica backbone, but they can also withstand the capillary forces exerted upon their nanostructured framework by the residing meniscus of selected solvents, and thus they can be dried under ambient pressure without need for supercritical fluid (SCF) extraction. The best solvent identified for that purpose is pentane, and the resulting aerogels are both microscopically and macroscopically identical to their SCF-CO2 dried counterparts. Being able to dry monolithic crosslinked aerogels without SCF extraction is expected to facilitate their commercial application. C1 NASA, Glenn Res Ctr, Div Mat, Polymers Branch, Cleveland, OH 44135 USA. Univ Missouri, Dept Chem, Rolla, MO 65409 USA. RP Leventis, N (reprint author), NASA, Glenn Res Ctr, Div Mat, Polymers Branch, 21000 Brookpk Rd,MS 49-1, Cleveland, OH 44135 USA. EM Nicholas.Leventis@nasa.gov; cslevent@umr.edu NR 21 TC 43 Z9 45 U1 7 U2 39 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0928-0707 J9 J SOL-GEL SCI TECHN JI J. Sol-Gel Sci. Technol. PD AUG PY 2005 VL 35 IS 2 BP 99 EP 105 DI 10.1007/s10971-005-1372-7 PG 7 WC Materials Science, Ceramics SC Materials Science GA 956DZ UT WOS:000231280700002 ER PT J AU Roth, DJ Verrilli, MJ Martin, RE Cosgriff, LM AF Roth, DJ Verrilli, MJ Martin, RE Cosgriff, LM TI Initial attempt to characterize oxidation damage in C/Sic composite using an ultrasonic guided wave method SO JOURNAL OF THE AMERICAN CERAMIC SOCIETY LA English DT Article AB An ultrasonic guided wave scan system was used to non-destructively monitor damage over time and position in a C/enhanced SiC sample that was creep tested to failure at 1200 degrees C in air at a stress of 69 MPa (10 ksi). The use of the guided wave scan system for mapping evolving oxidation profiles (via porosity gradients resulting from oxidation) along the sample length and predicting failure location was explored. The creep-rupture tests were interrupted for ultrasonic evaluation every two hours until failure at similar to 17.5 cumulative hours. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. Cleveland State Univ, Cleveland, OH 44115 USA. RP Roth, DJ (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM donald.j.roth@nasa.gov NR 13 TC 0 Z9 0 U1 0 U2 1 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0002-7820 J9 J AM CERAM SOC JI J. Am. Ceram. Soc. PD AUG PY 2005 VL 88 IS 8 BP 2164 EP 2168 DI 10.1111/j.1551-2916.2005.00395.x PG 5 WC Materials Science, Ceramics SC Materials Science GA 950PR UT WOS:000230870000024 ER PT J AU Harstad, K AF Harstad, K TI Trend analysis for atmospheric hydrocarbon partitioning using continuous thermodynamics SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID POLYCYCLIC AROMATIC-HYDROCARBONS; SEMIVOLATILE ORGANIC-COMPOUNDS; DILUTION ACTIVITY-COEFFICIENTS; SATURNS ATMOSPHERE; MODEL; GAS; EQUILIBRIA; AEROSOLS; SOLUTES; OIL AB The partitioning of atmospheric hydrocarbons into vapor and condensed phases when the species count is large is considered using the formalism of continuous thermodynamics. The vapor saturation pressures and condensate species distribution are parameterized using the species normal boiling temperatures. Qualitative trends in activity coefficient values and phase equilibrium. behavior that are relevant to the outer planets and Titan are discussed in terms of a much simplified perspective on these aspects of partitioning. The trends found are generally consistent with those from other published atmospheric model results. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Harstad, K (reprint author), CALTECH, Jet Prop Lab, M-S 125-109,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Kenneth.G.Harstad@jpl.nasa.gov NR 22 TC 1 Z9 1 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 J9 J ATMOS SCI JI J. Atmos. Sci. PD AUG PY 2005 VL 62 IS 8 BP 2977 EP 2987 DI 10.1175/JAS3518.1 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 961OS UT WOS:000231672300021 ER PT J AU Phabhakara, C Iacovazzi, R Yoo, JM Kim, KM AF Phabhakara, C Iacovazzi, R Yoo, JM Kim, KM TI A model for estimation of rain rate on tropical land from TRMM microwave imager radiometer observations SO JOURNAL OF THE METEOROLOGICAL SOCIETY OF JAPAN LA English DT Article ID STRATIFORM PRECIPITATION; PROFILING ALGORITHM; RADAR; PHASE; HYDROMETEORS AB Over the tropical land regions scatter plots of the rain rate (R-PR), deduced from the TRMM Precipitation Radar (PR) versus the observed 85 GHz brightness temperature (T-85v) made by the TRMM Microwave Imager (TMI) radiometer, for a period of a season over a given geographic region of 3 degrees x 5 degrees (lat x lon), indicate that there are two maxima in rain rate. One strong maximum occurs when T-85v has a value of about 220 K, and the other weaker one when T-85v is much colder similar to 150 K. Also these two maxima are vividly revealed in plots of R-PR vs. (T-19v-T-37v). The strong maximum occurs when (T-19v-T-37v) is similar to 20 K and the weaker maximum when it is greater than similar to 40 K. Together with the help of a) earlier investigations based on airborne Doppler Radar observations and b) radiative transfer theoretical simulations, we infer the strong maximum is a result of relatively weak scattering due to super cooled rain drops and water coated ice hydrometeors associated with a developing thunderstorm (Cb) that has a strong updraft. The other maximum is associated with strong scattering due to ice particles that are formed when the updraft collapses and the rain from the Cb is transitioning from convective type to stratiform type. Incorporating these ideas with a view to improve the estimation of rain rate from existing operational method applicable to the tropical land areas, we have developed a rain retrieval model. This model utilizes two parameters, that have a horizontal scale of similar to 20 km, deduced from the TMI measurements at 10, 19, 21 and 37 GHz (T-10v, T-19v, T-21v, T-37v). The third parameter in the model, namely the mean horizontal gradient < dT(85v)/dr > (K km(-1)) within the 20 km scale, is deduced from TMI measurements at 85 GHz that have the scale of similar to 5 km. Utilizing these parameters our retrieval model is formulated to yield instantaneous rain rate on a scale of 20 km. This retrieval model is initially tuned with the help of a limited amount of PR rain rate. After initial tuning, the model is applied to widely different tropical land areas, and for different seasons. Our estimates of instantaneous rain rate, on a scale of 20 km, and seasonal averages on a scale of 3 degrees x 5 degrees (lat x lon) agree better with PR than that given by the operational TMI rain retrievals. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Ctr Res Changing Earth Syst, Columbia, MD USA. EWHA Womans Univ, Seoul, South Korea. Sci Syst & Appl Inc, Lanham, MD USA. RP Phabhakara, C (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. EM Cuddapah@climate.gsfc.nasa.gov RI Iacovazzi Jr, Robert/G-3867-2010; Kim, Kyu-Myong/G-5398-2014 NR 18 TC 0 Z9 0 U1 1 U2 1 PU METEOROLOGICAL SOC JPN PI TOKYO PA C/O JPN METEOROL AGENCY 1-3-4 OTE-MACHI, CHIYODA-KU, TOKYO, JAPAN SN 0026-1165 J9 J METEOROL SOC JPN JI J. Meteorol. Soc. Jpn. PD AUG PY 2005 VL 83 IS 4 BP 595 EP 609 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 974CK UT WOS:000232568700009 ER PT J AU Klippel, A Tappe, H Kulik, L Lee, PU AF Klippel, A Tappe, H Kulik, L Lee, PU TI Wayfinding choremes - a language for modeling conceptual route knowledge SO JOURNAL OF VISUAL LANGUAGES AND COMPUTING LA English DT Article ID SPATIAL DISCOURSE; ONTOLOGIES AB The emergent interest in ontological and conceptual approaches to modeling route information results from new information technologies as well as from a multidisciplinary interest in spatial cognition. Linguistics investigates verbal route directions; cartography carries out research on route maps and on the information needs of map users; and computer science develops formal representations of routes with the aim to build new wayfinding applications. In concert with geomatics, ontologies of spatial domain knowledge are assembled while sensing technologies for location-aware wayfinding aids are developed simultaneously (e.g. cell phones, GPS-enabled devices or PDAs). These joint multidisciplinary efforts have enhanced cognitive approaches for route directions. In this article, we propose an interdisciplinary approach to modeling route information, the wayfinding choreme theory. Wayfinding choremes are mental conceptualizations of functional wayfinding and route direction elements. With the wayfinding choreme theory, we propose a formal treatment of (mental) conceptual route knowledge that is based on qualitative calculi and refined by behavioral experimental research. This contribution has three parts: First, we introduce the theory of wayfinding choremes. Second, we present terms rewriting rules that are grounded in cognitive principles and can tailor route directions to different user requirements. Third, we exemplify various application scenarios for our approach. (c) 2005 Elsevier Ltd. All rights reserved. C1 Univ Melbourne, Dept Geomat, Cooperat Res Ctr Spatial Informat, Melbourne, Vic 3010, Australia. Univ KwaZulu Natal, Linguist Programme, Durban, South Africa. Univ Melbourne, Dept Comp Sci & Software Engn, Melbourne, Vic 3010, Australia. San Jose State Univ, NASA, Ames Res Ctr, Moffett Field, CA USA. RP Univ Melbourne, Dept Geomat, Cooperat Res Ctr Spatial Informat, Melbourne, Vic 3010, Australia. EM aklippel@unimelb.edu.au NR 52 TC 27 Z9 29 U1 0 U2 10 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 1045-926X EI 1095-8533 J9 J VISUAL LANG COMPUT JI J. Vis. Lang. Comput. PD AUG PY 2005 VL 16 IS 4 BP 311 EP 329 DI 10.1016/j.jvlc.2004.11.004 PG 19 WC Computer Science, Software Engineering SC Computer Science GA 952XJ UT WOS:000231039100004 ER PT J AU Nowinski, JL Dismukes, RK AF Nowinski, JL Dismukes, RK TI Effects of ongoing task context and target typicality on prospective memory performance: The importance of associative cueing SO MEMORY LA English DT Article ID ENVIRONMENTAL CONTEXT; OLDER ADULTS; INTENTIONS; RECOGNITION; FAMILIARITY; COMPLEXITY; YOUNGER; RECALL AB Two experiments examined whether prospective memory performance is influenced by contextual cues. In our automatic activation model, any information available at encoding and retrieval should aid recall of the prospective task. The first experiment demonstrated an effect of the ongoing task context; performance was better when information about the ongoing task present at retrieval was available at encoding. Performance was also improved by a strong association between the prospective memory target as it was presented at retrieval and the intention as it was encoded. Experiment 2 demonstrated boundary conditions of the ongoing task context effect, which implicate the association between the ongoing and prospective tasks formed at encoding as the source of the context effect. The results of this study are consistent with predictions based on automatic activation of intentions. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Nowinski, JL (reprint author), NASA, Ames Res Ctr, Mail Stop 262-4, Moffett Field, CA 94035 USA. EM Jessica.L.Nowinski@nasa.gov NR 39 TC 37 Z9 38 U1 0 U2 5 PU PSYCHOLOGY PRESS PI HOVE PA 27 CHURCH RD, HOVE BN3 2FA, EAST SUSSEX, ENGLAND SN 0965-8211 J9 MEMORY JI Memory PD AUG PY 2005 VL 13 IS 6 BP 649 EP 657 DI 10.1080/09658210444000313 PG 9 WC Psychology, Experimental SC Psychology GA 965LU UT WOS:000231952800007 PM 16076678 ER PT J AU ten Kate, IL Garry, JRC Peeters, Z Quinn, R Foing, B Ehrenfreund, P AF ten Kate, IL Garry, JRC Peeters, Z Quinn, R Foing, B Ehrenfreund, P TI Amino acid photostability on the Martian surface SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID L-ALANINE; ORGANIC-COMPOUNDS; INFRARED-SPECTRA; MARS; GLYCINE; SOIL; PHOTOELECTRON; SPECTROSCOPY; DEGRADATION; METEORITES AB In the framework of international planetary exploration programs, several space missions are planned to search for organics and bio-signatures on Mars. Previous attempts have not detected any organic compounds in the Martian regolith. It is therefore critical to investigate the processes that may affect organic molecules on and below the planet's surface. Laboratory simulations can provide useful data about the reaction pathways of organic material at Mars' surface. We have studied the stability of amino acid thin films against ultraviolet (UV) irradiation and use those data to predict the survival time of these compounds on and in the Martian regolith. We show that thin films of glycine and D-alanine are expected to have half-lives of 22 +/- 5 hr and of 3 +/- 1 hr, respectively, when irradiated with Mars-like UV flux levels. Modelling shows that the half-lives of the amino acids are extended to the order of 107 years when embedded in regolith. These data suggest that subsurface sampling must be a key component of future missions to Mars dedicated to organic detection. C1 Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. Leiden Univ, Leiden Inst Chem, Astrobiol Lab, NL-2300 RA Leiden, Netherlands. NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. Estec, SCISR, ESA, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. RP ten Kate, IL (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM tenkate@strw.leidenuniv.nl NR 29 TC 71 Z9 72 U1 2 U2 12 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2005 VL 40 IS 8 BP 1185 EP 1193 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 976SH UT WOS:000232753100006 ER PT J AU Feng, K Hsu, FL Bota, K Bu, XR AF Feng, K Hsu, FL Bota, K Bu, XR TI A potential fluorescent Hg(II) chemosensor SO MICROCHEMICAL JOURNAL LA English DT Article DE imidazole; thiazole; mercury complex; fluorescence; copper complex; molecular probe ID NONLINEAR-OPTICAL CHROMOPHORES; CRYSTAL-STRUCTURES; METAL-COMPLEXES; DERIVATIVES; MERCURY(II); THIAZOLE AB An imidazole-based ligand has been evaluated for a potential fluorescent Hg(II) sensing probe. In water-acetonitrite solvent system, the ligand exhibits a unique selectivity towards Hg(II), which not only modulates fluorescence intensity but also shifts the emission band. The fluorescence reduction and the emission shift correlate with Hg(II) concentrations. (c) 2005 Elsevier B.V. All rights reserved. C1 Clark Atlanta Univ, Dept Chem, Lab Electroopt Mat, Atlanta, GA 30314 USA. Clark Atlanta Univ, NASA, Ctr High Performance Polymers & Mat, Atlanta, GA 30314 USA. USA, Edgewood Chem & Biol Ctr, Aberdeen Proving Ground, MD 21010 USA. RP Bu, XR (reprint author), Clark Atlanta Univ, Dept Chem, Lab Electroopt Mat, Atlanta, GA 30314 USA. EM xbu@cau.edu NR 13 TC 19 Z9 19 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0026-265X J9 MICROCHEM J JI Microchem J. PD AUG PY 2005 VL 81 IS 1 BP 23 EP 27 DI 10.1016/j.microc.2005.01.021 PG 5 WC Chemistry, Analytical SC Chemistry GA 942EA UT WOS:000230264500006 ER PT J AU Jonker, PG Campana, S Steeghs, D Torres, MAP Galloway, DK Markwardt, CB Chakrabarty, D Swank, J AF Jonker, PG Campana, S Steeghs, D Torres, MAP Galloway, DK Markwardt, CB Chakrabarty, D Swank, J TI Chandra observations of the millisecond X-ray pulsar IGR J00291+5934 in quiescence SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion : accretion discs; binaries : general; stars : individual : IGR J00291+5934; stars : neutron; X-rays : binaries ID NEUTRON-STAR; THERMAL EMISSION; AQUILA X-1; XMM-NEWTON; TRANSIENT; SPECTRUM; KS-1731-260; VARIABILITY; DISCOVERY AB In this paper we report on our analysis of three Chandra observations of the accretion-powered millisecond X-ray pulsar IGR J00291+5934 obtained during the late stages of the 2004 outburst. We also report the serendipitous detection of the source in quiescence by ROSAT during MID 48830-48839 (1992 July 26-August 4). The detected 0.3-10 keV source count rates varied significantly between the Chandra observations from (7.2 +/- 1.2) x 10(-3), (6.8 +/- 0.9) x 10(-3) and (1.4 +/- 0. 1) x 10(-2) counts s(-1) for the first, second and third Chandra observations, on MJD 53371.88 (2005 January 1), 53383.99 (2005 January 13) and 53407.57 (2005 February 6), respectively. The count rate for the third observation is 2.0 +/- 0.4 times as high as that of the average of the first two observations. The unabsorbed 0.5-10 keV source fluxes for the bestfitting power-law model to the source spectrum were (7.9 +/- 2.5) x 10(-14), (7.3 +/- 2.0) x 10(-14), and (1.17 +/- 0.22) x 10(-13) erg cm(-2) s(-1) for the first, second and third Chandra observations, respectively. We find that this source flux is consistent with that found by ROSAT [ approximate to (5.4 +/- 2.4) x 10(-14) erg cm(-2) s(-1)]. Under the assumption that the interstellar extinction, NH, does not vary between the observations, we find that the blackbody temperature during the second Chandra observation is significantly higher than that during the first and third observations. Furthermore, the effective temperature of the neutron star derived from fitting an absorbed blackbody or neutron star atmosphere model to the data is rather high in comparison with many other neutron star soft X-ray transients in quiescence, even during the first and third observations. If we assume that the source quiescent luminosity is similar to that measured for two other accretion powered millisecond pulsars in quiescence, the distance to IGR J00291+5934 is 2.6-3.6 kpc. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. SRON, Natl Inst Space Res, NL-3584 CA Utrecht, Netherlands. Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. MIT, Ctr Space Res, Cambridge, MA 02139 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pjonker@cfa.harvard.edu RI Swank, Jean/F-2693-2012; Steeghs, Danny/C-5468-2009; OI Steeghs, Danny/0000-0003-0771-4746; Galloway, Duncan/0000-0002-6558-5121 NR 38 TC 22 Z9 22 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 1 PY 2005 VL 361 IS 2 BP 511 EP 516 DI 10.1111/j.1365-2966.2005.09171.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 952JT UT WOS:000231000500015 ER PT J AU Lee, U Strohmayer, TE AF Lee, U Strohmayer, TE TI Light curves of oscillating neutron stars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars : neutron; stars : oscillations; stars : rotation ID X-RAY-BURSTS; MILLISECOND OSCILLATIONS; R-MODES; NONRADIAL OSCILLATIONS; HOT-SPOTS; FREQUENCY; STABILITY; EVOLUTION; PULSARS; BINARY AB We calculate light curves produced by tau modes with small azimuthal wavenumbers, m, propagating in the surface fluid ocean of rotating neutron stars. We include relativistic effects due to rapid rotation, and propagate photons from the stellar surface to a distant observer using the Schwarzschild metric. The wave motions of the surface r modes are confined to the equatorial region of the star, and the surface pattern of the temperature variation can be either symmetric (for even modes) or antisymmetric (for odd modes) with respect to the equator. Because for the surface r modes the oscillation frequency in the corotating frame of the star is much smaller than the rotation frequency, Omega, we employ the approximation in which the oscillation frequency in the inertial frame, or, is given by sigma = -m Omega. We find that the even, m = I r mode produces the largest light variations. The dominant Fourier component in the light curves of these modes is the fundamental having sigma = -Omega, and the first harmonic component having sigma = -2 Omega is always negligible in comparison. The dominant Fourier component of the even, m = 2 r modes is the first harmonic. Although the odd r modes produce smaller amplitude light variations compared with the even modes, the light curves of the former have a stronger first harmonic component. If both m = 1 and 2 r modes are excited simultaneously, a rich variety of light curves is possible, including those having an appreciable first harmonic component. We show that the phase difference, delta - delta(E), between the bolometric light curve and that at a particular photon energy can possibly be used as a probe of the stellar compactness, RIM, where R and M are the radius and mass of the star. We find that hard leads are expected in general rather than hard lags, although there exists a parameter space of R and the inclination angle i that produces hard lags for the odd modes. C1 Tohoku Univ, Inst Astron, Sendai, Miyagi 9808578, Japan. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Lee, U (reprint author), Tohoku Univ, Inst Astron, Sendai, Miyagi 9808578, Japan. EM lee@astr.tohoku.ac.jp; stroh@clarence.gsfc.nasa.gov NR 43 TC 19 Z9 19 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 1 PY 2005 VL 361 IS 2 BP 659 EP 672 DI 10.1111/j.1365-2966.2005.09198.x PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 952JT UT WOS:000231000500029 ER PT J AU Edge, WRT Coe, MJ Galache, JL McBride, VA Corbet, RHD Okazaki, AT Laycock, S Markwardt, CB Marshall, FE Udalski, A AF Edge, WRT Coe, MJ Galache, JL McBride, VA Corbet, RHD Okazaki, AT Laycock, S Markwardt, CB Marshall, FE Udalski, A TI The binary period and outburst behaviour of the Small Magellanic Cloud X-ray binary pulsar system SXP504 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars : emission-line, Be; Magellanic Clouds; X-rays : binaries ID NEUTRON-STAR; SMC AB A probable binary period has been detected in the optical counterpart to the X-ray source CXOUJ005455.6-724510 = RXJ0054.9-7245 = AXJ0054.8-7244 = SXP504 in the Small Magellanic Cloud. This source was detected by Chandra on 2002 July 4 and subsequently observed by XMM-Newton on 2003 December 18. The source is coincident with an Optical Gravitational Lensing object in the light curves of which several optical outburst peaks are visible at similar to 268-d intervals. Timing analysis shows a period of 268.6 +/- 0.1 d at > 99 per cent significance. Archival Rossi X-ray Timing Explorer data for the 504-s pulse-period have revealed detections which correspond closely with predicted or actual peaks in the optical data. The relationship between this orbital period and the pulse period of 504 s is within the normal variance found in the Corbet diagram. C1 Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Space Res Assoc, Columbia, MD 21044 USA. Hokkai Gakuen Univ, Fac Engn, Sapporo, Hokkaido, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Edge, WRT (reprint author), Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. EM wrte@astro.soton.ac.uk NR 19 TC 5 Z9 5 U1 0 U2 1 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 1 PY 2005 VL 361 IS 2 BP 743 EP 747 DI 10.1111/j.1365-2966.2005.09205.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 952JT UT WOS:000231000500037 ER PT J AU Borovikov, A Rienecker, MM Keppenne, CL Johnson, GC AF Borovikov, A Rienecker, MM Keppenne, CL Johnson, GC TI Multivariate error covariance estimates by Monte Carlo simulation for assimilation studies in the Pacific Ocean SO MONTHLY WEATHER REVIEW LA English DT Article ID ENSEMBLE KALMAN FILTER; GENERAL-CIRCULATION MODEL; QUASI-GEOSTROPHIC MODEL; TROPICAL PACIFIC; ANALYSIS SYSTEM; EL-NINO; TEMPERATURE; PRECIPITATION; PREDICTION; ATLANTIC AB One of the most difficult aspects of ocean-state estimation is the prescription of the model forecast error covariances. The paucity of ocean observations limits our ability to estimate the covariance structures from model-observation differences. In most practical applications, simple covariances are usually prescribed. Rarely are cross covariances between different model variables used. Here a comparison is made between a univariate optimal interpolation (UOI) scheme and a multivariate OI algorithm (MvOI) in the assimilation of ocean temperature profiles. In the UOI case only temperature is updated using a Gaussian covariance function. In the MvOL salinity, zonal, and meridional velocities as well as temperature are updated using an empirically estimated multivariate covariance matrix. Earlier studies have shown that a univariate 01 has a detrimental effect on the salinity and velocity fields of the model. Apparently, in a sequential framework it is important to analyze temperature and salinity together. For the MvOI an estimate of the forecast error statistics is made by Monte Carlo techniques from an ensemble of model forecasts. An important advantage of using an ensemble of ocean states is that it provides a natural way to estimate cross covariances between the fields of different physical variables constituting the model-state vector, at the same time incorporating the model's dynamical and thermodynamical constraints as well as the effects of physical boundaries. Only temperature observations from the Tropical Atmosphere-Ocean array have been assimilated in this study. To investigate the efficacy of the multivariate scheme, two data assimilation experiments are validated with a large independent set of recently published subsurface observations of salinity, zonal velocity, and temperature. For reference, a control run with no data assimilation is used to check how the data assimilation affects systematic model errors. While the performance of the UOI and MvOI is similar with respect to the temperature field, the salinity and velocity fields are greatly improved when the multivariate correction is used, as is evident from the analyses of the rms differences between these fields and independent observations. The MvOI assimilation is found to improve upon the control run in generating water masses with properties close to the observed, while the UOI fails to maintain the temperature and salinity structure. C1 NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. SAIC, Beltsville, MD USA. NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA. RP Borovikov, A (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610-1, Greenbelt, MD 20771 USA. EM ayb@mohawk.gsfc.nasa.gov RI Johnson, Gregory/I-6559-2012 OI Johnson, Gregory/0000-0002-8023-4020 NR 53 TC 17 Z9 17 U1 0 U2 2 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0027-0644 J9 MON WEATHER REV JI Mon. Weather Rev. PD AUG PY 2005 VL 133 IS 8 BP 2310 EP 2334 DI 10.1175/MWR2984.1 PG 25 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 955TM UT WOS:000231250500013 ER PT J AU Vaddiraju, S Mohite, A Chin, A Meyyappan, M Sumanasekera, G Alphenaar, BW Sunkara, MK AF Vaddiraju, S Mohite, A Chin, A Meyyappan, M Sumanasekera, G Alphenaar, BW Sunkara, MK TI Mechanisms of 1D crystal growth in reactive vapor transport: Indium nitride nanowires SO NANO LETTERS LA English DT Article ID GAN(0001) SURFACE; OXIDE; RECONSTRUCTIONS; SILICON; ROUTE; INN; GAN AB Indium nitride (InN) nanowire synthesis using indium (In) vapor transport in a dissociated ammonia environment (reactive vapor transport) is studied in detail to understand the nucleation and growth mechanisms involved with the so-called "self-catalysis" schemes. The results show that the nucleation of InN crystal occurs first on the substrate. Later, In droplets are formed on top of the InN crystals because of selective wetting of In onto InN crystals. Further growth via liquid-phase epitaxy through In droplets leads the growth in one dimension (1D), resulting in the formation of InN nanowires. The details about the nucleation and growth aspects within these self-catalysis schemes are rationalized further by demonstrating the growth of heteroepitaxially oriented nanowire arrays on single-crystal substrates and "tree-like" morphologies on a variety of substrates. However, the direct nitridation of In droplets using dissociated ammonia results in the spontaneous nucleation and basal growth of nanowires directly from the In melt surface, which is quite different from the above-mentioned nucleation mechanism with the reactive vapor transport case. The InN nanowires exhibit a band gap of 0.8 ell, whereas the mixed phase of InN and In2O3 nanowires exhibit a peak at similar to 1.9 eV in addition to that at 0.8 eV. C1 Univ Louisville, Dept Chem Engn, Louisville, KY 40292 USA. Univ Louisville, Dept Elect & Comp Engn, Louisville, KY 40292 USA. Univ Louisville, Dept Phys, Louisville, KY 40292 USA. NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Sunkara, MK (reprint author), Univ Louisville, Dept Chem Engn, Louisville, KY 40292 USA. EM mahendra@louisville.edu RI Sunkara, Mahendra/A-3033-2008 NR 29 TC 126 Z9 126 U1 2 U2 51 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1530-6984 J9 NANO LETT JI Nano Lett. PD AUG PY 2005 VL 5 IS 8 BP 1625 EP 1631 DI 10.1021/nl0505804 PG 7 WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA 955FQ UT WOS:000231211300018 PM 16089500 ER PT J AU Knuth, KH AF Knuth, KH TI Lattice duality: The origin of probability and entropy SO NEUROCOMPUTING LA English DT Article DE probability; entropy; lattice; information theory; Bayesian inference; inquiry ID INFORMATION; SEPARATION AB Bayesian probability theory is an inference calculus, which originates from a generalization of inclusion on the Boolean lattice of logical assertions to a degree of inclusion represented by a real number. Dual to this lattice is the distributive lattice of questions constructed from the ordered set of down-sets of assertions, which forms the foundation of the calculus of inquiry-a generalization of information theory. In this paper we introduce this novel perspective on these spaces in which machine learning is performed and discuss the relationship between these results and several proposed generalizations of information theory in the literature. Published by Elsevier B.V. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Knuth, KH (reprint author), NASA, Ames Res Ctr, Mail Stop 269-3, Moffett Field, CA 94035 USA. EM kevin.h.knuth@nasa.gov NR 50 TC 26 Z9 26 U1 0 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0925-2312 J9 NEUROCOMPUTING JI Neurocomputing PD AUG PY 2005 VL 67 BP 245 EP 274 DI 10.1016/j.neucom.2004.11.039 PG 30 WC Computer Science, Artificial Intelligence SC Computer Science GA 958HW UT WOS:000231436300010 ER PT J AU Stahl, HP Rowell, GH Reese, G Byberg, A AF Stahl, HP Rowell, GH Reese, G Byberg, A TI Multivariable parametric cost model for ground optical telescope assembly SO OPTICAL ENGINEERING LA English DT Article DE cost modeling; segmentation factor; ground-based telescopes AB A parametric cost model for ground-based telescopes is developed using multivariable statistical analysis of both engineering and performance parameters. While diameter continues to be the dominant cost driver, diffraction-limited wavelength is found to be a secondary driver. Other parameters such as radius of curvature are examined. The model includes an explicit factor for primary mirror segmentation and/or duplication (i.e., multi-telescope phased-array systems). Additionally, single variable models based on aperture diameter are derived. (c) 2005 Society of Photo-Optical Instrumentation Engineers. C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Qualis Corp, Huntsville, AL 35806 USA. Middle Tennessee State Univ, Dept Math Sci, Murfreesboro, TN 37128 USA. SAIC, Huntsville, AL 35806 USA. Lockheed Martin Integrated Syst & Solut, St Petersburg 191011, Russia. RP Stahl, HP (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM H.Philip.Stahl@msfc.nasa.gov; rowell@mtsu.edu; Gayle.D.Reese@saic.com NR 23 TC 5 Z9 5 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 AUG PY 2005 VL 44 IS 8 AR 083001 DI 10.1117/1.2031216 PG 9 WC Optics SC Optics GA 974MN UT WOS:000232596000006 ER PT J AU Summers, DP AF Summers, DP TI Ammonia formation by the reduction of nitrite/nitrate by FeS: Ammonia formation under acidic conditions SO ORIGINS OF LIFE AND EVOLUTION OF THE BIOSPHERE LA English DT Article DE ammonia; ammonium; aqueous; iron (II); iron sulfide FeS; nitrate; nitrite; nitrogen fixation; non-reducing atmosphere; prebiotic synthesis; reduction ID EARTHS EARLY ATMOSPHERE; BANDED IRON FORMATIONS; CARBON-DIOXIDE; OXIDATION-STATE; EVOLUTION; NITROGEN; OXYGEN; FIXATION; IMPACTS; OCEANS AB One issue for the origin of life under a non-reducing atmosphere is the availability of the reduced nitrogen necessary for amino acids, nucleic acids, etc. One possible source of this nitrogen is the formation of ammonia from the reduction of nitrates and nitrites produced by the shock heating of the atmosphere and subsequent chemistry. Ferrous ions will reduce these species to ammonium, but not under acidic conditions. We wish to report results on the reduction of nitrite and nitrate by another source of iron (II), ferrous sulfide, FeS. FeS reduces nitrite to ammonia at lower pHs than the corresponding reduction by aqueous Fe+2 stop. The reduction follows a first order decay, in nitrite concentration, with a half-life of about 150 min (room temperature, CO2, pH 6.25). The highest product yield of ammonia measured was 53%. Under CO2, the product yield decreases from pH 5.0 to pH 6.9. The increasing concentration of bicarbonate, at higher pH, interferes with the reaction. Comparing experiments under N-2 CO2 shows the interference of bicarbonate. The reaction proceeds well in the presence of such species as chloride, sulfate, and phosphate, though the yield drops significantly with phosphate. FeS also reduces nitrate and, unlike with Fe+2 stop, the reduction shows more reproducibility. Again, the product yield decreases with increasing pH, from 7% at pH 4.7 to 0% at pH 6.9. It appears that nitrate is much more sensitive to the presence of added species, perhaps not competing as well for binding sites on the FeS surface. This may be the cause of the lack of reproducibility of nitrate reduction by Fe+2 stop (which also can be sensitive to binding by certain species). C1 NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. RP Summers, DP (reprint author), NASA, Ames Res Ctr, SETI Inst, M-S,239-4, Moffett Field, CA 94035 USA. EM dsummers@mail.arc.nasa.gov NR 32 TC 26 Z9 27 U1 5 U2 36 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0169-6149 J9 ORIGINS LIFE EVOL B JI Orig. Life Evol. Biosph. PD AUG PY 2005 VL 35 IS 4 BP 299 EP 312 DI 10.1007/s11084-005-2040-1 PG 14 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 974TI UT WOS:000232613900002 PM 16228644 ER PT J AU Apel, CL Deamer, DW AF Apel, CL Deamer, DW TI The formation of glycerol monodecanoate by a dehydration/condensation reaction: Increasing the chemical complexity of amphiphiles on the early earth SO ORIGINS OF LIFE AND EVOLUTION OF THE BIOSPHERE LA English DT Article DE amphiphiles; ester bond; membranes; prebiotic; vesicles ID ENCAPSULATION; VESICLES AB Dehydration/condensation reactions between organic molecules in the prebiotic environment increased the inventory and complexity of organic compounds available for self-assembly into primitive cellular organisms. As a model of such reactions and to demonstrate this principle, we have investigated the esterification reaction between glycerol and decanoic acid that forms glycerol monodecanoate (GMD). This amphiphile enhances robustness of self-assembled membranous structures of carboxylic acids to the potentially disruptive effects of pH, divalent cation binding and osmotic stress. Experimental variables included temperature, water activity and hydrolysis of the resulting ester product, providing insights into the environmental conditions that would favor the formation and stability of this more evolved amphiphile. At temperatures exceeding 50 degrees C, the ester product formed even in the presence of bulk water, suggesting that the reaction occurs at the liquid interface of the two reactants and that the products segregate in the two immiscible layers, thereby reducing hydrolytic back reactions. This implies that esterification reactions were likely to be common in the prebiotic environment as reactants underwent cycles of wetting and drying on rare early landmasses at elevated temperatures. C1 NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. Univ Calif Santa Cruz, Dept Chem & Biochem, Santa Cruz, CA 95064 USA. RP Apel, CL (reprint author), NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. EM capel@mail.arc.nasa.gov NR 8 TC 23 Z9 24 U1 2 U2 13 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0169-6149 J9 ORIGINS LIFE EVOL B JI Orig. Life Evol. Biosph. PD AUG PY 2005 VL 35 IS 4 BP 323 EP 332 DI 10.1007/s11084-005-2046-8 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 974TI UT WOS:000232613900004 PM 16228646 ER PT J AU Kimura, Y Kaito, C AF Kimura, Y Kaito, C TI Formation of carbon nanotubes from mixture film of carbon and titanium SO PHYSICA E-LOW-DIMENSIONAL SYSTEMS & NANOSTRUCTURES LA English DT Article DE transmission electron microscopy; carbon nanotubes; catalytic properties; titanium ID LAYER AB It was shown that a carbon nanotube was selectively formed from carbon film containing Ti, supported by a standard Mo transmission electron microscopic grid, by heating at 800 degrees C in vacuum. With heating above 950 degrees C, graphite and rutile crystals of TiO2 predominately appeared. The formation of oxide is due to the supply of oxygen from the Mo grid. The formation mechanism of the carbon nanotubes was discussed on the basis of the heat of combustion due to the oxidation of titanium. The present result will lead to the development of an efficient method of production of carbon nanotubes. (c) 2005 Elsevier B.V. All rights reserved. C1 Ritsumeikan Univ, Dept Phys, Shiga 5258577, Japan. RP NASA, Goddard Space Flight Ctr, Astrochem Lab, Solar Syst Explorat Div, Code 691, Greenbelt, MD 20771 USA. EM rp092955@se.ritsumei.ac.jp RI Kimura, Yuki/J-9635-2014 OI Kimura, Yuki/0000-0002-9218-7663 NR 9 TC 5 Z9 5 U1 0 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1386-9477 EI 1873-1759 J9 PHYSICA E JI Physica E PD AUG PY 2005 VL 28 IS 3 BP 281 EP 285 DI 10.1016/j.physe.2005.03.015 PG 5 WC Nanoscience & Nanotechnology; Physics, Condensed Matter SC Science & Technology - Other Topics; Physics GA 947EY UT WOS:000230627400012 ER PT J AU Citrin, DS Maslov, AV AF Citrin, DS Maslov, AV TI Interband optical spectra of magnetoexcitons in semiconductor nanorings: Electron-hole spatial correlation SO PHYSICAL REVIEW B LA English DT Article ID RINGS AB An analytic model [R. A. Romer and M. E. Raikh, Phys. Rev. B 62, 7045 (2000); K. Moulopoulos and M. Constantinou, ibid. 70, 235327 (2004)] for magnetoexcitons in nanoscale semiconductor rings is extended to calculate directly the linear optical properties. The spectroscopic properties exhibit pronounced Phi(0)=hc/e excitonic Aharonov-Bohm oscillations in the threading magnetic flux Phi when the ring radius R is less than the effective exciton Bohr radius a(0). The electron-hole spatial correlation induced by an optical field as a function of nanoring radius and threading magnetic flux is studied. C1 Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. Georgia Tech Lorraine, F-57070 Metz, France. NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Citrin, DS (reprint author), Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. EM citrin@ece.gatech.edu RI Maslov, Alexey/E-5158-2011 OI Maslov, Alexey/0000-0002-7835-2474 NR 19 TC 3 Z9 3 U1 0 U2 0 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 J9 PHYS REV B JI Phys. Rev. B PD AUG PY 2005 VL 72 IS 7 AR 073302 DI 10.1103/PhysRevB.72.073302 PG 4 WC Physics, Condensed Matter SC Physics GA 960BF UT WOS:000231564500020 ER PT J AU Schurmans, M Luyten, J Creemers, C Bozzolo, G AF Schurmans, M Luyten, J Creemers, C Bozzolo, G TI Order-disorder transition temperatures and concentration dependence of the heat of formation via quantum approximate methods SO PHYSICAL REVIEW B LA English DT Article ID ALLOY PROPERTIES; METALS; CU; NI AB Model calculations combining the Monte Carlo method and a suitable energy model are widely used to complement experiments in order to gain insight on solid-state properties. One such energy model, the Bozzolo-Ferrante-Smith method for alloys, balances accuracy with simplicity in order to describe a wide range of materials. When combined with Monte Carlo simulations, it is seen that in cases of large lattice mismatch between the alloy components the method is bound to overestimate ordering tendencies, translating into deviations in the corresponding order-disorder transition temperatures. In this paper, the method is extended to take localized strain into account, thus improving its range of application to systems with arbitrary lattice mismatch and providing accurate estimates of order-disorder transition temperatures, heats of formation, and equilibrium lattice parameters. C1 Katholieke Univ Leuven, Dept Chem Engn, B-3001 Heverlee, Belgium. Ohio Aerosp Inst, Cleveland, OH 44142 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Creemers, C (reprint author), Katholieke Univ Leuven, Dept Chem Engn, W De Croylaan 46, B-3001 Heverlee, Belgium. EM claude.creemers@cit.kuleuven.be NR 19 TC 3 Z9 3 U1 0 U2 0 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 J9 PHYS REV B JI Phys. Rev. B PD AUG PY 2005 VL 72 IS 6 AR 064202 DI 10.1103/PhysRevB.72.064202 PG 8 WC Physics, Condensed Matter SC Physics GA 960BE UT WOS:000231564400054 ER PT J AU Smelyanskiy, VN Petukhov, AG Osipov, VV AF Smelyanskiy, VN Petukhov, AG Osipov, VV TI Quantum computing on long-lived donor states of Li in Si SO PHYSICAL REVIEW B LA English DT Article ID LITHIUM DONORS; SILICON; DOTS AB We predict a gigantically long lifetime of the first excited state of an interstitial lithium donor in silicon. The nature of this effect roots in the anomalous level structure of the 1s Li manifold under external stress. Namely, the coupling between the lowest two states of the opposite parity is very weak and occurs via intervalley phonon transitions only. We propose to use these states under the controlled ac and dc stress to process quantum information. We find an unusual form of the elastic-dipole interaction between different donors. This interaction scales with the interdonor distance R as R-3 or R-5 for the transitions between the states of the same or opposite parity, respectively. The long-range R-3 interaction provides a high fidelity mechanism for two-qubit operations. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. S Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA. LLC, El Segundo, CA 90245 USA. RP Smelyanskiy, VN (reprint author), NASA, Ames Res Ctr, Mail Stop 269-3, Moffett Field, CA 94035 USA. NR 21 TC 27 Z9 27 U1 0 U2 9 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 J9 PHYS REV B JI Phys. Rev. B PD AUG PY 2005 VL 72 IS 8 AR 081304 DI 10.1103/PhysRevB.72.081304 PG 4 WC Physics, Condensed Matter SC Physics GA 960BG UT WOS:000231564600007 ER PT J AU Svizhenko, A Anantram, MP AF Svizhenko, A Anantram, MP TI Effect of scattering and contacts on current and electrostatics in carbon nanotubes SO PHYSICAL REVIEW B LA English DT Article ID CURRENT-CARRYING CAPACITY; ELECTRICAL-TRANSPORT; CURRENT SATURATION; NANOTRANSISTORS AB We computationally study the electrostatic potential profile and current carrying capacity of carbon nanotubes as a function of length and diameter. Our study is based on solving the nonequilibrium Green's function and Poisson equations self-consistently, including the effect of electron-phonon scattering. A transition from the ballistic to diffusive regime of electron transport with an increase of applied bias is manifested by qualitative changes in the potential profiles, differential conductance, and electric field in a nanotube. In the low-bias ballistic limit, most of the applied voltage drop occurs near the contacts. In addition, the electric field at the tube center increases proportionally with diameter. In contrast, at high biases, most of the applied voltage drops across the nanotube, and the electric field at the tube center decreases with an increase in diameter. We find that the differential conductance can increase or decrease with bias as a result of an interplay of nanotube length, diameter, and a quality factor of the contacts. From an application viewpoint, we find that the current carrying capacity of nanotubes increases with an increase in diameter. Finally, we investigate the role of inner tubes in affecting the current carried by the outermost tube of a multiwalled nanotube. C1 NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. NASA, Ames Res Ctr, NASA, Adv Supercomp Div, Moffett Field, CA 94035 USA. RP Svizhenko, A (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, 229-1 Moffett Field, Moffett Field, CA 94035 USA. EM svizhenk@nas.nasa.gov; anant@mail.arc.nasa.gov NR 23 TC 21 Z9 21 U1 0 U2 4 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 J9 PHYS REV B JI Phys. Rev. B PD AUG PY 2005 VL 72 IS 8 AR 085430 DI 10.1103/PhysRevB.72.085430 PG 10 WC Physics, Condensed Matter SC Physics GA 960BG UT WOS:000231564600157 ER PT J AU Abbott, B Abbott, R Adhikari, R Ageev, A Allen, B Amin, R Anderson, SB Anderson, WG Araya, M Armandula, H Ashley, M Asiri, F Aufmuth, P Aulbert, C Babak, S Balasubramanian, R Ballmer, S Barish, BC Barker, C Barker, D Barnes, M Barr, B Barton, MA Bayer, K Beausoleil, R Belczynski, K Bennett, R Berukoff, SJ Betzwieser, J Bhawal, B Bilenko, IA Billingsley, G Black, E Blackburn, K Blackburn, L Bland, B Bochner, B Bogue, L Bork, R Bose, S Brady, PR Braginsky, VB Brau, JE Brown, DA Bullington, A Bunkowski, A Buonanno, A Burgess, R Busby, D Butler, WE Byer, RL Cadonati, L Cagnoli, G Camp, JB Cannizzo, JK Cantley, CA Cardenas, L Carter, K Casey, MM Castiglione, J Chandler, A Chapsky, J Charlton, P Chatterji, S Chelkowski, S Chen, Y Chickarmane, V Chin, D Christensen, N Churches, D Cokelaer, T Colacino, C Coldwell, R Coles, M Cook, D Corbitt, T Coyne, D Creighton, JDE Creighton, TD Crooks, DRM Csatorday, P Cusack, BJ Cutler, C D'Ambrosio, E Danzmann, K Daw, E DeBra, D Delker, T Dergachev, V DeSalvo, R Dhurandhar, S Credico, AD Diaz, M Ding, H Drever, RWP Dupuis, RJ Edlund, JA Ehrens, P Elliffe, EJ Etzel, T Evans, M Evans, T Fairhurst, S Fallnich, C Farnham, D Fejer, MM Findley, T Fine, M Finn, LS Franzen, KY Freise, A Frey, R Fritschel, P Frolov, VV Fyffe, M Ganezer, KS Garofoli, J Giaime, JA Gillespie, A Goda, K Gonzalez, G Gossler, S Grandclement, P Grant, A Gray, C Gretarsson, AM Grimmett, D Grote, H Grunewald, S Guenther, M Gustafson, E Gustafson, R Hamilton, WO Hammond, M Hanson, J Hardham, C Harms, J Harry, G Hartunian, A Heefner, J Hefetz, Y Heinzel, G Heng, IS Hennessy, M Hepler, N Heptonstall, A Heurs, M Hewitson, M Hild, S Hindman, N Hoang, P Hough, J Hrynevych, M Hua, W Ito, M Itoh, Y Ivanov, A Jennrich, O Johnson, B Johnson, WW Johnston, WR Jones, DI Jones, L Jungwirth, D Kalogera, V Katsavounidis, E Kawabe, K Kawamura, S Kells, W Kern, J Khan, A Killbourn, S Killow, CJ Kim, C King, C King, P Klimenko, S Koranda, S Kotter, K Kovalik, J Kozak, D Krishnan, B Landry, M Langdale, J Lantz, B Lawrence, R Lazzarini, A Lei, M Leonor, I Libbrecht, K Libson, A Lindquist, P Liu, S Logan, J Lormand, M Lubinski, M Luck, H Lyons, TT Machenschalk, B MacInnis, M Mageswaran, M Mailand, K Majid, W Malec, M Mann, F Marin, A Marka, S Maros, E Mason, J Mason, K Matherny, O Matone, L Mavalvala, N McCarthy, R McClelland, DE McHugh, M McNabb, JWC Mendell, G Mercer, RA Meshkov, S Messaritaki, E Messenger, C Mitrofanov, VP Mitselmakher, G Mittleman, R Miyakawa, O Miyoki, S Mohanty, S Moreno, G Mossavi, K Mueller, G Mukherjee, S Murray, P Myers, J Nagano, S Nash, T Nayak, R Newton, G Nocera, F Noel, JS Nutzman, P Olson, T O'Reilly, B Ottaway, DJ Ottewill, A Ouimette, D Overmier, H Owen, BJ Pan, Y Papa, MA Parameshwaraiah, V Parameswariah, C Pedraza, M Penn, S Pitkin, M Plissi, M Prix, R Quetschke, V Raab, F Radkins, H Rahkola, R Rakhmanov, M Rao, SR Rawlins, K Ray-Majumder, S Re, V Redding, D Regehr, MW Regimbau, T Reid, S Reilly, KT Reithmaier, K Reitze, DH Richman, S Riesen, R Riles, K Rivera, B Rizzi, A Robertson, DI Robertson, NA Robison, L Roddy, S Rollins, J Romano, JD Romie, J Rong, H Rose, D Rotthoff, E Rowan, S Rudiger, A Russell, P Ryan, K Salzman, I Sandberg, V Sanders, GH Sannibale, V Sathyaprakash, B Saulson, PR Savage, R Sazonov, A Schilling, R Schlaufman, K Schmidt, V Schnabel, R Schofield, R Schutz, BF Schwinberg, P Scott, SM Seader, SE Searle, AC Sears, B Seel, S Seifert, F Sengupta, AS Shapiro, CA Shawhan, P Shoemaker, DH Shu, QZ Sibley, A Siemens, X Sievers, L Sigg, D Sintes, AM Smith, JR Smith, M Smith, MR Sneddon, PH Spero, R Stapfer, G Steussy, D Strain, KA Strom, D Stuver, A Summerscales, T Sumner, MC Sutton, PJ Sylvestre, J Takamori, A Tanner, DB Tariq, H Taylor, I Taylor, R Taylor, R Thorne, KA Thorne, KS Tibbits, M Tilav, S Tinto, M Tokmakov, KV Torres, C Torrie, C Traylor, G Tyler, W Ugolini, D Ungarelli, C Vallisneri, M van Putten, M Vass, S Vecchio, A Veitch, J Vorvick, C Vyachanin, SP Wallace, L Walther, H Ward, H Ware, B Watts, K Webber, D Weidner, A Weiland, U Weinstein, A Weiss, R Welling, H Wen, L Wen, S Whelan, JT Whitcomb, SE Whiting, BF Wiley, S Wilkinson, C Willems, PA Williams, PR Williams, R Willke, B Wilson, A Winjum, BJ Winkler, W Wise, S Wiseman, AG Woan, G Wooley, R Worden, J Wu, W Yakushin, I Yamamoto, H Yoshida, S Zaleski, KD Zanolin, M Zawischa, I Zhang, L Zhu, R Zotov, N Zucker, M Zweizig, J AF Abbott, B Abbott, R Adhikari, R Ageev, A Allen, B Amin, R Anderson, SB Anderson, WG Araya, M Armandula, H Ashley, M Asiri, F Aufmuth, P Aulbert, C Babak, S Balasubramanian, R Ballmer, S Barish, BC Barker, C Barker, D Barnes, M Barr, B Barton, MA Bayer, K Beausoleil, R Belczynski, K Bennett, R Berukoff, SJ Betzwieser, J Bhawal, B Bilenko, IA Billingsley, G Black, E Blackburn, K Blackburn, L Bland, B Bochner, B Bogue, L Bork, R Bose, S Brady, PR Braginsky, VB Brau, JE Brown, DA Bullington, A Bunkowski, A Buonanno, A Burgess, R Busby, D Butler, WE Byer, RL Cadonati, L Cagnoli, G Camp, JB Cannizzo, JK Cantley, CA Cardenas, L Carter, K Casey, MM Castiglione, J Chandler, A Chapsky, J Charlton, P Chatterji, S Chelkowski, S Chen, Y Chickarmane, V Chin, D Christensen, N Churches, D Cokelaer, T Colacino, C Coldwell, R Coles, M Cook, D Corbitt, T Coyne, D Creighton, JDE Creighton, TD Crooks, DRM Csatorday, P Cusack, BJ Cutler, C D'Ambrosio, E Danzmann, K Daw, E DeBra, D Delker, T Dergachev, V DeSalvo, R Dhurandhar, S Credico, AD Diaz, M Ding, H Drever, RWP Dupuis, RJ Edlund, JA Ehrens, P Elliffe, EJ Etzel, T Evans, M Evans, T Fairhurst, S Fallnich, C Farnham, D Fejer, MM Findley, T Fine, M Finn, LS Franzen, KY Freise, A Frey, R Fritschel, P Frolov, VV Fyffe, M Ganezer, KS Garofoli, J Giaime, JA Gillespie, A Goda, K Gonzalez, G Gossler, S Grandclement, P Grant, A Gray, C Gretarsson, AM Grimmett, D Grote, H Grunewald, S Guenther, M Gustafson, E Gustafson, R Hamilton, WO Hammond, M Hanson, J Hardham, C Harms, J Harry, G Hartunian, A Heefner, J Hefetz, Y Heinzel, G Heng, IS Hennessy, M Hepler, N Heptonstall, A Heurs, M Hewitson, M Hild, S Hindman, N Hoang, P Hough, J Hrynevych, M Hua, W Ito, M Itoh, Y Ivanov, A Jennrich, O Johnson, B Johnson, WW Johnston, WR Jones, DI Jones, L Jungwirth, D Kalogera, V Katsavounidis, E Kawabe, K Kawamura, S Kells, W Kern, J Khan, A Killbourn, S Killow, CJ Kim, C King, C King, P Klimenko, S Koranda, S Kotter, K Kovalik, J Kozak, D Krishnan, B Landry, M Langdale, J Lantz, B Lawrence, R Lazzarini, A Lei, M Leonor, I Libbrecht, K Libson, A Lindquist, P Liu, S Logan, J Lormand, M Lubinski, M Luck, H Lyons, TT Machenschalk, B MacInnis, M Mageswaran, M Mailand, K Majid, W Malec, M Mann, F Marin, A Marka, S Maros, E Mason, J Mason, K Matherny, O Matone, L Mavalvala, N McCarthy, R McClelland, DE McHugh, M McNabb, JWC Mendell, G Mercer, RA Meshkov, S Messaritaki, E Messenger, C Mitrofanov, VP Mitselmakher, G Mittleman, R Miyakawa, O Miyoki, S Mohanty, S Moreno, G Mossavi, K Mueller, G Mukherjee, S Murray, P Myers, J Nagano, S Nash, T Nayak, R Newton, G Nocera, F Noel, JS Nutzman, P Olson, T O'Reilly, B Ottaway, DJ Ottewill, A Ouimette, D Overmier, H Owen, BJ Pan, Y Papa, MA Parameshwaraiah, V Parameswariah, C Pedraza, M Penn, S Pitkin, M Plissi, M Prix, R Quetschke, V Raab, F Radkins, H Rahkola, R Rakhmanov, M Rao, SR Rawlins, K Ray-Majumder, S Re, V Redding, D Regehr, MW Regimbau, T Reid, S Reilly, KT Reithmaier, K Reitze, DH Richman, S Riesen, R Riles, K Rivera, B Rizzi, A Robertson, DI Robertson, NA Robison, L Roddy, S Rollins, J Romano, JD Romie, J Rong, H Rose, D Rotthoff, E Rowan, S Rudiger, A Russell, P Ryan, K Salzman, I Sandberg, V Sanders, GH Sannibale, V Sathyaprakash, B Saulson, PR Savage, R Sazonov, A Schilling, R Schlaufman, K Schmidt, V Schnabel, R Schofield, R Schutz, BF Schwinberg, P Scott, SM Seader, SE Searle, AC Sears, B Seel, S Seifert, F Sengupta, AS Shapiro, CA Shawhan, P Shoemaker, DH Shu, QZ Sibley, A Siemens, X Sievers, L Sigg, D Sintes, AM Smith, JR Smith, M Smith, MR Sneddon, PH Spero, R Stapfer, G Steussy, D Strain, KA Strom, D Stuver, A Summerscales, T Sumner, MC Sutton, PJ Sylvestre, J Takamori, A Tanner, DB Tariq, H Taylor, I Taylor, R Taylor, R Thorne, KA Thorne, KS Tibbits, M Tilav, S Tinto, M Tokmakov, KV Torres, C Torrie, C Traylor, G Tyler, W Ugolini, D Ungarelli, C Vallisneri, M van Putten, M Vass, S Vecchio, A Veitch, J Vorvick, C Vyachanin, SP Wallace, L Walther, H Ward, H Ware, B Watts, K Webber, D Weidner, A Weiland, U Weinstein, A Weiss, R Welling, H Wen, L Wen, S Whelan, JT Whitcomb, SE Whiting, BF Wiley, S Wilkinson, C Willems, PA Williams, PR Williams, R Willke, B Wilson, A Winjum, BJ Winkler, W Wise, S Wiseman, AG Woan, G Wooley, R Worden, J Wu, W Yakushin, I Yamamoto, H Yoshida, S Zaleski, KD Zanolin, M Zawischa, I Zhang, L Zhu, R Zotov, N Zucker, M Zweizig, J CA LIGO Sci Collaboration TI Search for gravitational waves associated with the gamma ray burst GRB030329 using the LIGO detectors SO PHYSICAL REVIEW D LA English DT Article ID 25 APRIL 1998; ROTATIONAL CORE COLLAPSE; 29 MARCH 2003; OPTICAL AFTERGLOW; UNUSUAL SUPERNOVA; MASSIVE STARS; BLACK-HOLES; EXPLORER; GRB-030329; RADIATION AB We have performed a search for bursts of gravitational waves associated with the very bright gamma ray burst GRB030329, using the two detectors at the LIGO Hanford Observatory. Our search covered the most sensitive frequency range of the LIGO detectors (approximately 80--2048 Hz), and we specifically targeted signals shorter than similar or equal to 150 ms. Our search algorithm looks for excess correlated power between the two interferometers and thus makes minimal assumptions about the gravitational waveform. We observed no candidates with gravitational-wave signal strength larger than a predetermined threshold. We report frequency-dependent upper limits on the strength of the gravitational waves associated with GRB030329. Near the most sensitive frequency region, around similar or equal to 250 Hz, our root-sum-square (RSS) gravitational-wave strain sensitivity for optimally polarized bursts was better than h(RSS)similar or equal to 6x10(-21) Hz(-1/2). Our result is comparable to the best published results searching for association between gravitational waves and gamma ray bursts. C1 Albert Einstein Inst, Max Planck Inst Gravitationsphys, D-30167 Hannover, Germany. Australian Natl Univ, Canberra, ACT 0200, Australia. CALTECH, Pasadena, CA 91125 USA. Calif State Univ Dominguez Hills, Carson, CA 90747 USA. CALTECH, CaRT, Pasadena, CA 91125 USA. Cardiff Univ, Cardiff CF2 3YB, Wales. Carleton Coll, Northfield, MN 55057 USA. Hobart & William Smith Coll, Geneva, NY 14456 USA. Inter Univ Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. Albert Einstein Inst, Max Planck Inst Gravitat Phys, D-14476 Golm, Germany. MIT, LIGO, Cambridge, MA 02139 USA. Hanford Observ, LIGO, Richland, WA 99352 USA. Livingston Observ, LIGO, Livingston, LA 70754 USA. Louisiana State Univ, Baton Rouge, LA 70803 USA. Louisiana Tech Univ, Ruston, LA 71272 USA. Loyola Univ, New Orleans, LA 70118 USA. Max Plank Inst Quantenopt, D-85748 Garching, Germany. Moscow MV Lomonosov State Univ, Moscow 119992, Russia. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Natl Astron Observ, Tokyo 1818588, Japan. Northwestern Univ, Evanston, IL 60208 USA. Salish Kootenai Coll, Pablo, MT 59855 USA. SE Louisiana Univ, Hammond, LA 70402 USA. Stanford Univ, Stanford, CA 94305 USA. Syracuse Univ, Syracuse, NY 13244 USA. Penn State Univ, University Pk, PA 16802 USA. Univ Texas, Brownsville, TX 78520 USA. Texas Southmost Coll, Brownsville, TX 78520 USA. Trinity Univ, San Antonio, TX 78712 USA. Leibniz Univ Hannover, D-30167 Hannover, Germany. Univ Illes Balears, E-07122 Palma de Mallorca, Spain. Univ Birmingham, Birmingham B15 2TT, W Midlands, England. Univ Florida, Gainesville, FL 32611 USA. Univ Glasgow, Glasgow G12 8QQ, Lanark, Scotland. Univ Michigan, Ann Arbor, MI 48109 USA. Univ Oregon, Eugene, OR 97403 USA. Univ Rochester, Rochester, NY 14627 USA. Univ Wisconsin, Milwaukee, WI 53201 USA. Washington State Univ, Pullman, WA 99164 USA. Inst Astrophys, CNRS, GReCO, F-75014 Paris, France. Columbia Univ, New York, NY 10027 USA. Univ Tokyo, Inst Cosm Ray Res, Tokyo, Japan. Univ Coll Dublin, Dublin 2, Ireland. Jet Prop Lab, Pasadena, CA USA. RP CALTECH, LIGO, Pasadena, CA 91125 USA. RI Raab, Frederick/E-2222-2011; Rowan, Sheila/E-3032-2010; Lueck, Harald/F-7100-2011; Freise, Andreas/F-8892-2011; Kawabe, Keita/G-9840-2011; Ottewill, Adrian/A-1838-2016; Frey, Raymond/E-2830-2016; Barker, David/A-5671-2013; Mitrofanov, Valery/D-8501-2012; Finn, Lee Samuel/A-3452-2009; Messaritaki, Eirini/D-7393-2016; Liu, Sheng/K-2815-2013; Pitkin, Matthew/I-3802-2013; Vyatchanin, Sergey/J-2238-2012; Chen, Yanbei/A-2604-2013; Bilenko, Igor/D-5172-2012; Harms, Jan/J-4359-2012; Agresti, Juri/G-8168-2012; Sylvestre, Julien/A-8610-2009; Casey, Morag/C-9703-2010; Sigg, Daniel/I-4308-2015; van Putten, Maurice/F-5237-2011; Beausoleil, Raymond/C-5076-2009; Allen, Bruce/K-2327-2012; Hild, Stefan/A-3864-2010; McClelland, David/E-6765-2010; Vecchio, Alberto/F-8310-2015; Strain, Kenneth/D-5236-2011; Ottaway, David/J-5908-2015; Schutz, Bernard/B-1504-2010 OI Zweizig, John/0000-0002-1521-3397; Russell, Pamela/0000-0002-3995-1239; Fairhurst, Stephen/0000-0001-8480-1961; Taylor, Ian/0000-0001-5040-0772; Freise, Andreas/0000-0001-6586-9901; Whiting, Bernard F/0000-0002-8501-8669; Lueck, Harald/0000-0001-9350-4846; Ottewill, Adrian/0000-0003-3293-8450; Frey, Raymond/0000-0003-0341-2636; Whelan, John/0000-0001-5710-6576; Stuver, Amber/0000-0003-0324-5735; Finn, Lee Samuel/0000-0002-3937-0688; Pitkin, Matthew/0000-0003-4548-526X; Agresti, Juri/0000-0001-6119-2470; Sylvestre, Julien/0000-0001-8136-4348; Sigg, Daniel/0000-0003-4606-6526; Allen, Bruce/0000-0003-4285-6256; McClelland, David/0000-0001-6210-5842; Vecchio, Alberto/0000-0002-6254-1617; Strain, Kenneth/0000-0002-2066-5355; NR 70 TC 146 Z9 145 U1 3 U2 10 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD AUG PY 2005 VL 72 IS 4 AR 042002 DI 10.1103/PhysRevD.72.042002 PG 17 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 960BK UT WOS:000231565000003 ER PT J AU Alcubierre, M Brugmann, B Diener, P Guzman, FS Hawke, I Hawley, S Herrmann, F Koppitz, M Pollney, D Seidel, E Thornburg, J AF Alcubierre, M Brugmann, B Diener, P Guzman, FS Hawke, I Hawley, S Herrmann, F Koppitz, M Pollney, D Seidel, E Thornburg, J TI Dynamical evolution of quasicircular binary black hole data SO PHYSICAL REVIEW D LA English DT Article ID APPARENT HORIZON FINDERS; 3D NUMERICAL RELATIVITY; GRAVITATIONAL-WAVES; EVENT HORIZONS; 3+1 DIMENSIONS; NORMAL-MODES; INITIAL DATA; SPACETIMES; COLLISION; MECHANICS AB We study the fully nonlinear dynamical evolution of binary black hole data, whose orbital parameters are specified via the effective potential method for determining quasicircular orbits. The cases studied range from the Cook-Baumgarte innermost stable circular orbit (ISCO) to significantly beyond that separation. In all cases we find the black holes to coalesce (as determined by the appearance of a common apparent horizon) in less than half an orbital period. The results of the numerical simulations indicate that the initial holes are not actually in quasicircular orbits, but that they are in fact nearly plunging together. The dynamics of the final horizon are studied to determine physical parameters of the final black hole, such as its spin, mass, and oscillation frequency, revealing information about the inspiral process. We show that considerable resolution is required to extract accurate physical information from the final black hole formed in the merger process, and that the quasinormal modes of the final hole are strongly excited in the merger process. For the ISCO case, by comparing physical measurements of the final black hole formed to the initial data, we estimate that less than 3% of the total energy is radiated in the merger process. C1 Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico. Univ Jena, Inst Theoret Phys, D-07743 Jena, Germany. Louisiana State Univ, Ctr Computat Technol, Baton Rouge, LA 70803 USA. Univ Michoacana, Inst Fis & Matemat, Morelia 58040, Michoacan, Mexico. Albert Einstein Inst, Max Planck Inst Gravitat Phys, D-14476 Golm, Germany. Univ Southampton, Sch Math, Southampton SO17 1BJ, Hants, England. Univ Texas, Ctr Relativ, Austin, TX 78712 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. RP Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, AP 70-543, Mexico City 04510, DF, Mexico. RI Guzman, Francisco/D-8309-2012 NR 59 TC 41 Z9 41 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD AUG PY 2005 VL 72 IS 4 AR 044004 DI 10.1103/PhysRevD.72.044004 PG 14 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 960BK UT WOS:000231565000053 ER PT J AU Vallisneri, M AF Vallisneri, M TI Geometric time delay interferometry SO PHYSICAL REVIEW D LA English DT Article ID GRAVITATIONAL-RADIATION; LASER-INTERFEROMETER; PROJECT; SEARCH; BAND AB The space-based gravitational-wave observatory LISA, a NASA-ESA mission to be launched after 2012, will achieve its optimal sensitivity using time delay interferometry (TDI), a LISA-specific technique needed to cancel the otherwise overwhelming laser noise in the interspacecraft phase measurements. The TDI observables of the Michelson and Sagnac types have been interpreted physically as the virtual measurements of a synthesized interferometer. In this paper, I present Geometric TDI, a new and intuitive approach to extend this interpretation to all TDI observables. Unlike the standard algebraic formalism, Geometric TDI provides a combinatorial algorithm to explore exhaustively the space of second-generation TDI observables (i.e., those that cancel laser noise in LISA-like interferometers with time-dependent arm lengths). Using this algorithm, I survey the space of second-generation TDI observables of length (i.e., number of component phase measurements) up to 24, and I identify alternative, improved forms of the standard second-generation TDI observables. The alternative forms have improved high-frequency gravitational-wave sensitivity in realistic noise conditions (because they have fewer nulls in the gravitational-wave and noise response functions), and are less susceptible to instrumental gaps and glitches (because their component phase measurements span shorter time periods). C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 36 TC 20 Z9 20 U1 1 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD AUG PY 2005 VL 72 IS 4 AR 042003 DI 10.1103/PhysRevD.72.042003 PG 18 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 960BK UT WOS:000231565000004 ER PT J AU Luchinsky, DG Millonas, MM Smelyanskiy, VN Pershakova, A Stefanovska, A McClintock, PVE AF Luchinsky, DG Millonas, MM Smelyanskiy, VN Pershakova, A Stefanovska, A McClintock, PVE TI Nonlinear statistical modeling and model discovery for cardiorespiratory data SO PHYSICAL REVIEW E LA English DT Article ID HEART-RATE-VARIABILITY; CHAOTIC DYNAMICAL-SYSTEMS; CARDIOVASCULAR-SYSTEM; PARAMETER-ESTIMATION; BLOOD-PRESSURE; IDENTIFICATION; OSCILLATIONS; HUMANS; NOISE; FLUCTUATIONS AB We present a Bayesian dynamical inference method for characterizing cardiorespiratory (CR) dynamics in humans by inverse modeling from blood pressure time-series data. The technique is applicable to a broad range of stochastic dynamical models and can be implemented without severe computational demands. A simple nonlinear dynamical model is found that describes a measured blood pressure time series in the primary frequency band of the CR dynamics. The accuracy of the method is investigated using model-generated data with parameters close to the parameters inferred in the experiment. The connection of the inferred model to a well-known beat-to-beat model of the baroreflex is discussed. C1 Newstead Miss Crit Technol Inc, E Beverly Hills, CA 90212 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Lancaster, Dept Phys, Lancaster LA1 4YB, England. Univ Ljubljana, Fac Elect Engn, Ljubljana 1000, Slovenia. RP Luchinsky, DG (reprint author), Newstead Miss Crit Technol Inc, 9100 Wilshire Blvd,Suite 540, E Beverly Hills, CA 90212 USA. RI Luchinsky, Dmitry/N-4177-2014 FU Wellcome Trust [074437, ] NR 70 TC 16 Z9 16 U1 0 U2 6 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1539-3755 J9 PHYS REV E JI Phys. Rev. E PD AUG PY 2005 VL 72 IS 2 AR 021905 DI 10.1103/PhysRevE.72.021905 PN 1 PG 10 WC Physics, Fluids & Plasmas; Physics, Mathematical SC Physics GA 960BA UT WOS:000231564000069 PM 16196602 ER PT J AU Smelyanskiy, VN Luchinsky, DG Timucin, DA Bandrivskyy, A AF Smelyanskiy, VN Luchinsky, DG Timucin, DA Bandrivskyy, A TI Reconstruction of stochastic nonlinear dynamical models from trajectory measurements SO PHYSICAL REVIEW E LA English DT Article ID TIME-SERIES; SYSTEMS; NOISE AB An algorithm is presented for reconstructing stochastic nonlinear dynamical models from noisy time-series data. The approach is analytical; consequently, the resulting algorithm does not require an extensive global search for the model parameters, provides optimal compensation for the effects of dynamical noise, and is robust for a broad range of dynamical models. The strengths of the algorithm are illustrated by inferring the parameters of the stochastic Lorenz system and comparing the results with those of earlier research. The efficiency and accuracy of the algorithm are further demonstrated by inferring a model for a system of five globally and locally coupled noisy oscillators. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Lancaster, Dept Phys, Lancaster LA1 4YB, England. RP Smelyanskiy, VN (reprint author), NASA, Ames Res Ctr, Mail Stop 269-2, Moffett Field, CA 94035 USA. EM Vadim.N.Smelyanskiy@nasa.gov RI Luchinsky, Dmitry/N-4177-2014 NR 29 TC 17 Z9 17 U1 0 U2 6 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1539-3755 J9 PHYS REV E JI Phys. Rev. E PD AUG PY 2005 VL 72 IS 2 AR 026202 DI 10.1103/PhysRevE.72.026202 PN 2 PG 12 WC Physics, Fluids & Plasmas; Physics, Mathematical SC Physics GA 960BB UT WOS:000231564100056 PM 16196679 ER PT J AU Lodhi, MAK Diaz, AB Wilson, TL AF Lodhi, MAK Diaz, AB Wilson, TL TI Simplified solar modulation model of inner trapped belt proton flux as a function of atmospheric density SO RADIATION MEASUREMENTS LA English DT Article ID SPACE-SHUTTLE; STATION AB No simple algorithm seems to exist for calculating proton fluxes and lifetimes in the Earth's inner, trapped radiation belt throughout the solar cycle. Most models of the inner trapped belt in use depend upon AP8 which only describes the radiation environment at solar maximum and solar minimum in Cycle 20. One exception is NOAAPRO which incorporates flight data from the TIROS/NOAA polar orbiting spacecraft. The present study discloses yet another, simple formulation for approximating proton fluxes at any time in a given solar cycle, in particular between solar maximum and solar minimum. It is derived from AP8 using a regression algorithm technique from nuclear physics. From flux and its time integral fluence, one can then approximate dose rate and its time integral dose. It has already been published in this journal that the absorbed dose rate, D, in the trapped belts exhibits a power law relationship, D = Arho(-n), where A is a constant, rho is the atmospheric density, and the index n is weakly dependent upon shielding. However, that method does not work for flux and fluence. Instead, we extend this idea by showing that the power law approximation for flux J is actually bivariant in energy E as well as density rho. The resulting relation is J(E, rho) similar to Sigma A(E-n)rho(-n), with A itself a power law in E. This provides another method for calculating approximate proton flux and lifetime at any time in the solar cycle. These in turn can be used to predict the associated dose and dose rate. (C) 2004 Elsevier Ltd. All rights reserved. C1 Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Lodhi, MAK (reprint author), Texas Tech Univ, Dept Phys, MS 1051, Lubbock, TX 79409 USA. EM a.lodhi@ttu.edu NR 27 TC 2 Z9 3 U1 1 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1350-4487 J9 RADIAT MEAS JI Radiat. Meas. PD AUG PY 2005 VL 39 IS 4 BP 391 EP 399 DI 10.1016/j.radmeas.2004.10.005 PG 9 WC Nuclear Science & Technology SC Nuclear Science & Technology GA 899GY UT WOS:000227134100005 ER PT J AU Emfietzoglou, D Cucinotta, FA Nikjoo, H AF Emfietzoglou, D Cucinotta, FA Nikjoo, H TI A complete dielectric response model for liquid water: A solution of the Bethe Ridge problem SO RADIATION RESEARCH LA English DT Article ID LOW-ENERGY ELECTRONS; X-RAY-SCATTERING; SWIFT CHARGED-PARTICLES; MONTE-CARLO-SIMULATION; MEAN FREE-PATH; CONDENSED MATTER; STOPPING POWER; INELASTIC-SCATTERING; OPTICAL-SPECTRA; CROSS-SECTIONS AB We present a complete yet computationally simple model for the dielectric response function of liquid water over the energy-momentum plane, which, in contrast to earlier models, is consistent with the recent inelastic X-ray scattering spectroscopy data at both zero and finite momentum transfer values. The model follows Ritchie's extended-Drude algorithm and is particularly effective at the region of the Bethe ridge, substantially improving previous models. The present development allows for a more accurate simulation of the inelastic scattering and energy deposition process of low-energy electrons in liquid water and other biomaterials. As an example, we calculate the stopping power of liquid water for electrons over the 0.1-10 keV range where direct experimental measurements are still impractical and the Bethe stopping formula is inaccurate. The new stopping power values are up to 30-40% lower than previous calculations. Within the range of validity of the first Born approximation, the new values are accurate to within the experimental uncertainties (a few percent). At the low end, the introduction of Born corrections raises the uncertainty to perhaps similar to 10%. Thus the present model helps extend the ICRU electron stopping power database for liquid water down to about two orders of magnitude with a comparable level of uncertainty. (c) 2005 by Radiation Research Society. C1 NASA, Johnson Space Ctr, Ctr Adv Space Studies, USRA, Houston, TX 77058 USA. NASA, Johnson Space Ctr, Houston, TX 77058 USA. Univ Ioannina, Sch Med, Med Phys Lab, GR-45110 Ioannina, Greece. RP Emfietzoglou, D (reprint author), NASA, Johnson Space Ctr, Ctr Adv Space Studies, USRA, NASA Rd 1, Houston, TX 77058 USA. EM Hooshang.nikjoo@jsc.nasa.gov RI Emfietzoglou, Dimitris/G-7168-2012 NR 44 TC 90 Z9 90 U1 1 U2 8 PU RADIATION RESEARCH SOC PI LAWRENCE PA 810 E TENTH STREET, LAWRENCE, KS 66044 USA SN 0033-7587 J9 RADIAT RES JI Radiat. Res. PD AUG PY 2005 VL 164 IS 2 BP 202 EP 211 DI 10.1667/RR3399 PG 10 WC Biology; Biophysics; Radiology, Nuclear Medicine & Medical Imaging SC Life Sciences & Biomedicine - Other Topics; Biophysics; Radiology, Nuclear Medicine & Medical Imaging GA 949OR UT WOS:000230798500011 PM 16038591 ER PT J AU Vasavada, AR Showman, AP AF Vasavada, AR Showman, AP TI Jovian atmospheric dynamics: an update after Galileo and Cassini SO REPORTS ON PROGRESS IN PHYSICS LA English DT Review ID GREAT-RED-SPOT; SHALLOW-WATER TURBULENCE; BETA-PLANE TURBULENCE; JUPITERS CLOUD BANDS; 2-DIMENSIONAL DECAYING TURBULENCE; GENERALIZED ELIASSEN-PALM; 6-YEAR 1994-2000 SURVEY; ZONAL FLOW DRIVEN; PROBE ENTRY SITE; WHITE OVAL BC AB The Galileo and Cassini spacecrafts have greatly enhanced the observational record of Jupiter's tropospheric dynamics, particularly through returning high spatial resolution, multi-spectral and global imaging data with episodic coverage over periods of months to years. These data, along with those from Earth-based telescopes, have revealed the stability of Jupiter's zonal jets, captured the evolution of vortices and equatorial waves, and mapped the distributions of lightning and moist convection. Because no observations of Jupiter's interior exist, a forward modelling approach has been used to relate observations at cloud level to models of shallow or deep jet structure, shallow or deep jet forcing and energy transfer between turbulence, vortices and jets. A range of observed phenomena can be reproduced in shallow models, though the Galileo probe winds and jet stability arguments hint at the presence of deep jets. Many deep models, however, fail to reproduce Jupiter-like non-zonal features (e.g. vortices). Jupiter's dynamics likely include both deep and shallow processes, requiring an integrated approach to future modelling-an important goal for the post-Galileo and Cassini era. C1 CALTECH, Jet Propuls Lab, Pasadena, CA 91109 USA. Univ Arizona, Phys Planetary Sci & Lunar & Planetary Lab, Tucson, AZ 85721 USA. RP Vasavada, AR (reprint author), CALTECH, Jet Propuls Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ashwin.r.vasavada@jpl.nasa.gov NR 216 TC 150 Z9 152 U1 6 U2 18 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0034-4885 EI 1361-6633 J9 REP PROG PHYS JI Rep. Prog. Phys. PD AUG PY 2005 VL 68 IS 8 BP 1935 EP 1996 DI 10.1088/0034-4885/68/8/R06 PG 62 WC Physics, Multidisciplinary SC Physics GA 960FS UT WOS:000231576200006 ER PT J AU Anderson, DE Cahalan, RF AF Anderson, DE Cahalan, RF TI The Solar Radiation and Climate Experiment (SORCE) mission for the NASA Earth Observing System (EOS) SO SOLAR PHYSICS LA English DT Article AB The NASA Earth Observing System (EOS) is an advanced study of Earth's long-term global changes of solid Earth, its atmosphere, and oceans and includes a coordinated collection of satellites, data systems, and modeling. The EOS program was conceived in the 1980s as part of NASA's Earth System Enterprise (ESE). The Solar Radiation and Climate Experiment (SORCE) is one of about 20 missions planned for the EOS program, and the SORCE measurement objectives include the total solar irradiance (TSI) and solar spectral irradiance (SSI) that are two of the 24 key measurement parameters defined for the EOS program. The SORCE satellite was launched in January 2003, and its observations are improving the understanding and generating new inquiry regarding how and why solar variability occurs and how it affects Earth's energy balance, atmosphere, and long-term climate changes. C1 NASA Headquarters, Washington, DC USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Anderson, DE (reprint author), NASA Headquarters, Washington, DC USA. EM Donald.Anderson-1@nasa.gov; Robert.F.Cahalan@nasa.gov RI Cahalan, Robert/E-3462-2012 OI Cahalan, Robert/0000-0001-9724-1270 NR 2 TC 12 Z9 12 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD AUG PY 2005 VL 230 IS 1-2 BP 3 EP 6 DI 10.1007/s11207-005-1592-6 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 991FH UT WOS:000233797200002 ER PT J AU Sparn, TP Rottman, G Woods, TN Boyle, BD Kohnert, R Ryan, S Davis, R Fulton, R Ochs, W AF Sparn, TP Rottman, G Woods, TN Boyle, BD Kohnert, R Ryan, S Davis, R Fulton, R Ochs, W TI The SORCE spacecraft and operations SO SOLAR PHYSICS LA English DT Article ID EXPLORER AB The Solar Radiation and Climate Experiment, SORCE, is a satellite carrying four scientific instruments that measure the total solar irradiance and the spectral irradiance from the ultraviolet to the infrared. The instruments were all developed by the Laboratory for Atmospheric and Space Physics (LASP) at the University of Colorado, Boulder. The spacecraft carrying and accommodating the instruments was developed by Orbital Sciences Corporation in Dulles, Virginia. It is three-axis stabilized with a control system to point the instruments at the Sun, as well as the stars for calibration. SORCE was successfully launched from the Kennedy Space Center in Florida on 25 January 2003 aboard a Pegasus XL rocket. The anticipated lifetime is 5 years, with a goal of 6 years. SORCE is operated from the Mission Operations Center at LASP where all data are collected, processed, and distributed. This paper describes the SORCE spacecraft, integration and test, mission operations, and ground data system. C1 Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. Orbital Sci Corp, Dulles, VA USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Sparn, TP (reprint author), Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA. EM sparn@lasp.colorado.edu; rottman@lasp.colorado.edu NR 6 TC 3 Z9 3 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD AUG PY 2005 VL 230 IS 1-2 BP 71 EP 89 DI 10.1007/s11207-005-1584-6 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 991FH UT WOS:000233797200006 ER PT J AU Hancock, R AF Hancock, R TI Provisions of the commercial space launch act (CSLA) SO SPACE POLICY LA English DT Article AB In an acknowledgement that private spaceflight is becoming a reality, the USA has enacted legislation, in the form of the CSLA, to assist the development of commercial, including passenger-carrying, launch vehicles. This report describes the salient features of the new act and explains the steps necessary for the obtention of a commercial launch license. (c) 2005 Published by Elsevier Ltd. C1 NASA, Shuttle Safety & Miss Assurance, Kennedy Space Ctr, FL 32899 USA. RP Hancock, R (reprint author), NASA, Shuttle Safety & Miss Assurance, Kennedy Space Ctr, FL 32899 USA. EM randy.hancock-1@ksc.nasa.gov NR 1 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 0265-9646 J9 SPACE POLICY JI Space Policy PD AUG PY 2005 VL 21 IS 3 BP 227 EP 229 DI 10.1016/j.spacepol.2005.05.004 PG 3 WC International Relations; Social Sciences, Interdisciplinary SC International Relations; Social Sciences - Other Topics GA 966TM UT WOS:000232044800007 ER PT J AU Tratt, DM Whiteman, DN Demoz, BB Farley, RW Wessel, JE AF Tratt, DM Whiteman, DN Demoz, BB Farley, RW Wessel, JE TI Active Raman sounding of the earth's water vapor field SO SPECTROCHIMICA ACTA PART A-MOLECULAR AND BIOMOLECULAR SPECTROSCOPY LA English DT Article; Proceedings Paper CT 6th International Conference on Raman Spectroscopy Applied to the Earth and Planetary Sciences CY JUN 06-11, 2004 CL Honolulu, HI SP US Natl Sci Fdn, Univ Hawaii DE Raman lidar; water vapor; aerosols ID PHYSICAL PARTICLE PROPERTIES; TROPICAL INDIAN-OCEAN; LIDAR MEASUREMENTS; CIRRUS CLOUDS; EXTINCTION; AEROSOLS AB The typically weak cross-sections characteristic of Raman processes has historically limited their use in atmospheric remote sensing to nighttime application. However, with advances in instrumentation and techniques, it is now possible to apply Raman lidar to the monitoring of atmospheric water vapor, aerosols and clouds throughout the diurnal cycle. Upper tropospheric and lower stratospheric measurements of water vapor using Raman lidar are also possible but are limited to nighttime and require long integration times. However, boundary layer studies of water vapor variability can now be performed with high temporal and spatial resolution. This paper will review the current state-of-the-art of Raman lidar for high-resolution measurements of the atmospheric water vapor, aerosol and cloud fields. In particular, we describe the use of Raman lidar for mapping the vertical distribution and variability of atmospheric water vapor, aerosols and clouds throughout the evolution of dynamic meteorological events. The ability of Raman lidar to detect and characterize water in the region of the tropopause and the importance of high-altitude water vapor for climate-related studies and meteorological satellite performance are discussed. (c) 2005 Elsevier B.V. All rights reserved. C1 NASA, Earth Sci Technol Off, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Aerosp Corp, Los Angeles, CA 90009 USA. RP Tratt, DM (reprint author), NASA, Earth Sci Technol Off, Code 661, Greenbelt, MD 20771 USA. EM dtratt@esto.gsfc.nasa.gov RI Tratt, David/A-7884-2009; Demoz, Belay/N-4130-2014 OI Tratt, David/0000-0002-3942-6848; NR 17 TC 4 Z9 4 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1386-1425 J9 SPECTROCHIM ACTA A JI Spectroc. Acta Pt. A-Molec. Biomolec. Spectr. PD AUG PY 2005 VL 61 IS 10 BP 2335 EP 2341 DI 10.1016/j.saa.2005.02.032 PG 7 WC Spectroscopy SC Spectroscopy GA 952TE UT WOS:000231027600008 PM 16029854 ER PT J AU Moody, CD Villar, SEJ Edwards, HGM Hodgson, DA Doran, PT Bishop, JL AF Moody, CD Villar, SEJ Edwards, HGM Hodgson, DA Doran, PT Bishop, JL TI Biogeological Raman spectroscopic studies of Antarctic lacustrine sediments SO SPECTROCHIMICA ACTA PART A-MOLECULAR AND BIOMOLECULAR SPECTROSCOPY LA English DT Article; Proceedings Paper CT 6th International Conference on Raman Spectroscopy Applied to the Earth and Planetary Sciences CY JUN 06-11, 2004 CL Honolulu, HI SP US Natl Sci Fdn, Univ Hawaii DE lacustrine sediments; Antarctica; Mars; Raman spectroscopy AB Analysis of lacustrine sediments is an accepted method for deciphering the palaeoenvironment of a lake's catchment area, as each strata of the sediment gives information about the rock type it was eroded from and also the state of the lake, i.e. oxic or anoxic. Antarctica has long been accepted as a putative analogue for Mars, so the analysis of Antarctic material may give results that can be compared to sediments on Mars. Raman spectroscopy has been selected as the method of analysis as it does not destroy the sample, can be used in situ and requires very little sample preparation. It is a suitable method for analysing both inorganic and organic matter and a miniature spectrometer is currently being developed for use in the field. The results from the spectrometers can serve as a guide for analysing sediments on Mars. It has been shown that Raman spectroscopy can detect and differentiate between oxic and anoxic sediments. Both 1064 and 785 nm wavelengths are suitable for laser excitation of organic and inorganic matter. (c) 2005 Elsevier B.V. All rights reserved. C1 Univ Bradford, Dept Chem & Forens Sci, Bradford BD7 1DP, W Yorkshire, England. Univ Burgos, Dept Humanidades & Educ, Area Geodinam Interna, Burgos 09001, Spain. British Antarctic Survey, Cambridge CB3 0ET, England. Univ Illinois, Dept Earth & Environm Sci, Chicago, IL 60607 USA. NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Edwards, HGM (reprint author), Univ Bradford, Dept Chem & Forens Sci, Bradford BD7 1DP, W Yorkshire, England. EM h.g.m.edwards@bradford.ac.uk OI Jorge-Villar, Susana/0000-0003-1676-4438 NR 7 TC 4 Z9 5 U1 1 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1386-1425 J9 SPECTROCHIM ACTA A JI Spectroc. Acta Pt. A-Molec. Biomolec. Spectr. PD AUG PY 2005 VL 61 IS 10 BP 2413 EP 2417 DI 10.1016/j.saa.2005.02.023 PG 5 WC Spectroscopy SC Spectroscopy GA 952TE UT WOS:000231027600019 PM 15876550 ER PT J AU Sen, S Kar, SK Catalina, AV Stefanescu, DM Dhindaw, BK AF Sen, S Kar, SK Catalina, AV Stefanescu, DM Dhindaw, BK TI Evolution of in-situ generated reinforcement precipitates in metal matrix composites SO TRANSACTIONS OF THE INDIAN INSTITUTE OF METALS LA English DT Article; Proceedings Paper CT 2nd International Conference on Solidification Science and Processing CY NOV 17-20, 2004 CL Bangalore, INDIA SP Indian Inst Technol Kharagpur ID DIRECTIONAL DENDRITIC SOLIDIFICATION; PARTICLE ENGULFMENT; DEFORMATION; 1300-K; SLURRY AB Due to certain inherent advantages, in-situ production of Metal Matrix Composites (MMCs) have received considerable attention in the recent past. In-situ techniques typically involve a chemical reaction that results in precipitation of a ceramic reinforcement phase. The size and spatial distribution of these precipitates ultimately determine the mechanical properties of these MMCs. In this paper we will investigate the validity of extending the mathematical expression derived to quantify the interaction between an inert particle and a planar solid-liquid interface (SLI) to predict the spatial evolution of the in-situ generated precipitates within an equiaxed grain. Measurements made on size and distribution of TiC precipitates in a Ni3Al matrix will be presented to test the validity of such an approach. C1 NASA, George C Marshall Space Flight Ctr, BAE Sys SD 46, Huntsville, AL 35812 USA. Ohio State Univ, Columbus, OH 43210 USA. Caterpillar Inc, Peoria, IL 61629 USA. Univ Alabama, Tuscaloosa, AL USA. Indian Inst Technol, Kharagpur 721302, W Bengal, India. RP Sen, S (reprint author), NASA, George C Marshall Space Flight Ctr, BAE Sys SD 46, Huntsville, AL 35812 USA. EM sisen@knology.net RI Stefanescu, Doru/G-8101-2012; OI Stefanescu, Doru M./0000-0001-5544-8396; Dhindaw, Brij Kumar/0000-0001-6991-9793 NR 22 TC 0 Z9 0 U1 0 U2 4 PU INDIAN INST METALS PI CALCUTTA PA METAL HOUSE, PLOT 13/4, BLOCK AQ, SECTOR V, SALT LAKE, CALCUTTA 700 091, INDIA SN 0019-493X J9 T INDIAN I METALS JI Trans. Indian Inst. Met. PD AUG PY 2005 VL 58 IS 4 BP 709 EP 714 PG 6 WC Metallurgy & Metallurgical Engineering SC Metallurgy & Metallurgical Engineering GA 970TO UT WOS:000232332700029 ER PT J AU Royce, TE Rozowsky, JS Bertone, P Samanta, M Stolc, V Weissman, S Snyder, M Gerstein, M AF Royce, TE Rozowsky, JS Bertone, P Samanta, M Stolc, V Weissman, S Snyder, M Gerstein, M TI Issues in the analysis of oligonucleotide tiling microarrays for transcript mapping SO TRENDS IN GENETICS LA English DT Review ID CDNA MICROARRAY; BACKGROUND CORRECTION; BINDING SITES; GENOME; ARRAYS; HUMAN-CHROMOSOME-22; IDENTIFICATION; NORMALIZATION; SEQUENCES; MODEL AB Traditional microarrays use probes complementary to known genes to quantitate the differential gene expression between two or more conditions. Genomic tiling microarray experiments differ in that probes that span a genomic region at regular intervals are used to detect the presence or absence of transcription. This difference means the same sets of biases and the methods for addressing them are unlikely to be relevant to both types of experiment. We introduce the informatics challenges arising in the analysis of tiling microarray experiments as open problems to the scientific community and present initial approaches for the analysis of this nascent technology. C1 Yale Univ, Dept Mol Biophys & Biochem, New Haven, CT 06520 USA. Yale Univ, Program Computat Biol & Bioinformat, New Haven, CT 06520 USA. Yale Univ, Dept Mol Cellular & Dev Biol, New Haven, CT 06520 USA. Systemix Inc, Cupertino, CA 95014 USA. NASA, Ames Res Ctr, Genome Res Facil, Moffett Field, CA 94035 USA. Yale Univ, Dept Genet, New Haven, CT 06520 USA. Yale Univ, Dept Comp Sci, New Haven, CT 06520 USA. RP Gerstein, M (reprint author), Yale Univ, Dept Mol Biophys & Biochem, New Haven, CT 06520 USA. EM mark.gerstein@yale.edu RI Bertone, Paul/A-6600-2013; OI Bertone, Paul/0000-0001-5059-4829; Rozowsky, Joel/0000-0002-3565-0762 FU NHGRI NIH HHS [P50 HG 02357, P50 HG002357] NR 35 TC 73 Z9 82 U1 0 U2 5 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 0168-9525 J9 TRENDS GENET JI Trends Genet. PD AUG PY 2005 VL 21 IS 8 BP 466 EP 475 DI 10.1016/j.tig.2005.06.007 PG 10 WC Genetics & Heredity SC Genetics & Heredity GA 955EW UT WOS:000231209200010 PM 15979196 ER PT J AU DellaCorte, C AF DellaCorte, C TI Today's kids are smarter and better educated 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. EM cdellacorte@stle.org NR 0 TC 0 Z9 0 U1 0 U2 1 PU SOC TRIBOLOGISTS & LUBRICATION ENGINEERS PI PARK RIDGE PA 840 BUSSE HIGHWAY, PARK RIDGE, IL 60068 USA SN 0024-7154 J9 TRIBOL LUBR TECHNOL JI Tribol. Lubr. Technol. PD AUG PY 2005 VL 61 IS 8 BP 6 EP 6 PG 1 WC Engineering, Mechanical SC Engineering GA 952DP UT WOS:000230982600002 ER PT J AU Manning, RM AF Manning, RM TI An extended parabolic equation and its application to the calculation of transverse and longitudinal mutual coherence functions in atmospheric turbulence SO WAVES IN RANDOM AND COMPLEX MEDIA LA English DT Article ID REFRACTIVE INDEX; PROPAGATION; WAVES; INHOMOGENEITIES; APPROXIMATION; LIGHT; MEDIA AB An extended, Wide forward angle scattering version of the parabolic equation is considered and an operator expression for the solution of the generalized ninth moment of the electromagnetic wave field is obtained. Here, 'generalized' connotes the consideration of both the transverse as well as the longitudinal spatial moments of the wave field. A unified Solution for the generalized second-order moment, i.e. the Mutual coherence function (MCF), is found. The solution is applied to the case of Kolmogorov turbulent fluctuations Within the atmosphere. In addition to demonstrating,in interesting decaying oscillatory behaviour of the longitudinal MCF in atmospheric turbulence, it is found that the use of the extended parabolic equation yields negligible corrections to the transverse MCF, as calculated from the parabolic equation in the paraxial approximation. C1 NASA, Cleveland, OH 44135 USA. RP Manning, RM (reprint author), NASA, MS 54-8,21000 Brookpk Rd, Cleveland, OH 44135 USA. EM Robert.M.Manning@nasa.gov NR 19 TC 1 Z9 1 U1 0 U2 3 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 1745-5030 J9 WAVE RANDOM COMPLEX JI Waves Random Complex Media PD AUG PY 2005 VL 15 IS 3 BP 405 EP 416 DI 10.1080/17455030500297966 PG 12 WC Physics, Multidisciplinary SC Physics GA 996IW UT WOS:000234168600008 ER PT J AU Chen, JL Rodell, M Wilson, CR Famiglietti, JS AF Chen, JL Rodell, M Wilson, CR Famiglietti, JS TI Low degree spherical harmonic influences on Gravity Recovery and Climate Experiment (GRACE) water storage estimates SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID VARIABILITY; SYSTEM AB We estimate terrestrial water storage variations using time variable gravity changes observed by the Gravity Recovery and Climate Experiment ( GRACE) satellites during the first 2 years of the mission. We examine how treatment of low-degree gravitational changes and geocenter variations affect GRACE based estimates of basin-scale water storage changes, using independently derived low-degree harmonics from Earth rotation (EOP) and satellite laser ranging (SLR) observations. GRACE based water storage changes are compared with estimates from NASA's Global Land Data Assimilation System (GLDAS). Results from the 22 GRACE monthly gravity solutions, covering the period April 2002 to July 2004, show remarkably good agreement with GLDAS in the Mississippi, Amazon, Ganges, Ob, Zambezi, and Victoria basins. Combining GRACE observations with EOP and SLR degree-2 spherical harmonic coefficient changes and SLR observed geocenter variations significantly affects and apparently improves the estimates, especially in the Mississippi, Ob, and Victoria basins. C1 Univ Texas, Ctr Space Res, Austin, TX 78759 USA. NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. Univ Texas, Dept Geol Sci, Austin, TX 78712 USA. Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. RP Chen, JL (reprint author), Univ Texas, Ctr Space Res, Austin, TX 78759 USA. EM chen@csr.utexas.edu RI Rodell, Matthew/E-4946-2012 OI Rodell, Matthew/0000-0003-0106-7437 NR 13 TC 82 Z9 93 U1 5 U2 22 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 JUL 30 PY 2005 VL 32 IS 14 AR L14405 DI 10.1029/2005GL022964 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 951MR UT WOS:000230935100003 ER PT J AU Koren, I Kaufman, YJ Rosenfeld, D Remer, LA Rudich, Y AF Koren, I Kaufman, YJ Rosenfeld, D Remer, LA Rudich, Y TI Aerosol invigoration and restructuring of Atlantic convective clouds SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID WATER-VAPOR; MODIS; PRODUCTS; AMAZON AB Clouds and precipitation play crucial roles in the Earth's energy balance, global atmospheric circulation and the availability of fresh water. Aerosols may modify cloud properties and precipitation formation by modifying the concentration and size of cloud droplets, and consequently the strength of cloud convection, and height of glaciation levels thus affecting precipitation patterns. Here we evaluate the aerosol effect on clouds, using large statistics of daily satellite data over the North Atlantic Ocean. We found a strong correlation between the presence of aerosols and the structural properties of convective clouds. These correlations suggest systematic invigoration of convective clouds by pollution, desert dust and biomass burning aerosols. On average increase in the aerosol concentration from a baseline to the average values is associated with a 0.05 +/- 0.01 increase in the cloud fraction and a 40 +/- 5mb decrease in the cloud top pressure. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, JCET, Baltimore, MD 21228 USA. Hebrew Univ Jerusalem, Inst Earth Sci, IL-91904 Jerusalem, Israel. Weizmann Inst Sci, Dept Environm Sci, IL-76100 Rehovot, Israel. RP Koren, I (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM ilank@climate.gsfc.nasa.gov RI Rudich, Yinon/K-1498-2012; Koren, Ilan/K-1417-2012; Rosenfeld, Daniel/F-6077-2016; OI Koren, Ilan/0000-0001-6759-6265; Rosenfeld, Daniel/0000-0002-0784-7656; Rudich, Yinon/0000-0003-3149-0201 NR 17 TC 228 Z9 232 U1 2 U2 21 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 30 PY 2005 VL 32 IS 14 AR L14828 DI 10.1029/2005GL023187 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 951MR UT WOS:000230935100004 ER PT J AU Su, WY Charlock, TP Rose, FG AF Su, WY Charlock, TP Rose, FG TI Deriving surface ultraviolet radiation from CERES surface and atmospheric radiation budget: Methodology SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID ENERGY SYSTEM CERES; AEROSOL RETRIEVALS; TOTAL OZONE; TROPOSPHERIC AEROSOL; SATELLITE ESTIMATION; OPTICAL-PROPERTIES; SIZE DISTRIBUTION; UV-RADIATION; CLOUDS; TOMS AB We describe an algorithm that retrieves the surface UVB (280-315 nm) and UVA (315-400 nm) irradiances from the Surface and Atmosphere Radiation Budget (SARB) product of Clouds and the Earth's Radiant Energy System (CERES). The SARB product we use here routinely calculates the vertical profiles of shortwave, longwave, and window channel irradiances with inputs of retrievals from imagers collocated with CERES. The top of the atmosphere broadband irradiance from SARB is constrained by CERES broadband irradiance. The shortwave spectrum in the SARB calculation is divided into 15 bands, and the two ultraviolet spectral bands, band 5 (298.5-322.5 nm) and band 6 (322.5-357.5 nm), are used to generate surface UVB and UVA irradiances. In this study, we develop a set of ratio lookup tables to derive surface UVB and UVA irradiances from SARB band 5 and band 6 outputs. We show that the ratio of band 5 to UVB irradiance is sensitive to total column ozone, solar zenith angle, surface albedo, and the atmospheric profile in cloud-free conditions; in cloudy conditions, the ratio of band 5 to UVB irradiance is also sensitive to cloud optical depth and height. Additionally, we show that the ratio of band 6 to UVA irradiance is sensitive to solar zenith angle, surface albedo, and cloud optical depth. We also derive a UV index from the UVB irradiance. Our algorithm may be applied at any surface elevation or surface type, including snow and ice. Surface UV irradiances derived from the lookup table that we created agree well with those computed by the high-resolution, multistream radiative transfer code, with differences ranging from -10% to +4% for UVB and UVA irradiances. The relative differences for the UV index are higher, ranging from -26% to +16%. C1 Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. Analyt Serv & Mat Inc, Hampton, VA 23666 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Su, WY (reprint author), Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. EM w.su@larc.nasa.gov OI Rose, Fred G/0000-0003-0769-0772 NR 60 TC 13 Z9 13 U1 1 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 JUL 30 PY 2005 VL 110 IS D14 AR D14209 DI 10.1029/2005JD005794 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 951OZ UT WOS:000230941500006 ER PT J AU Burlaga, LF Vinas, AF AF Burlaga, LF Vinas, AF TI Tsallis distributions of the large-scale magnetic field strength fluctuations in the solar wind from 7 to 87 AU SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID STATISTICAL-MECHANICS; LEVY DISTRIBUTIONS; RANDOM-WALKS; SUPERSTATISTICS; FOUNDATION; ENTROPIES; ELECTRONS; STATE AB [1] The solar wind is a driven nonlinear, nonequilibrium system with large jumps and fluctuations in the temporal profiles of the magnetic field strength B. Relatively large clusters of strong fields ("merged interaction regions,'' MIRs) form beyond 1 AU, grow out to approximate to 5 - 30 AU, and decay slowly between approximate to 30 AU and at least 90 AU. We analyze the probability distribution functions (PDFs) of fluctuations of B observed by Voyager 1 between 7 and 87 AU on scales from 1 to 128 days during each of four years ( 1980, 1991, 2001, and 2002). The 32 PDFs of the increments of B can be described by a single function, the q-exponential distribution of the nonextensive Tsallis statistical mechanics. The tails of the PDFs are described by the entropic index q, which is scale dependent. The Tsallis distribution has a finite variance when q < 5/3 and a divergent moment when q >= 5/3. For the 1980 and 1991 data ( near 8 and 45 AU, respectively), q >= 5/3 at all scales, owing to large tails of the PDFs caused by large fluctuations and jumps in B(t). For the 2001 and 2002 data ( between 80 and 87 AU), q < 5/3, and q approaches 1 ( the PDF tends to a Gaussian) at large scales. The standard deviation and kurtosis of the observed increments of B vary with the scale of the fluctuations. The transition from q > 5/3 at < 45 AU to q < 5/3 at > 80 AU suggests the possibility of a phase transition in the distant heliosphere. C1 NASA, Goddard Space Flight Ctr, Lab Solar & Space Phys, Heliospher Phys Branch, Greenbelt, MD 20771 USA. RP Burlaga, LF (reprint author), NASA, Goddard Space Flight Ctr, Lab Solar & Space Phys, Heliospher Phys Branch, Mail Code 612-2,Bldg 21,Room 244, Greenbelt, MD 20771 USA. EM Leonard.F.Burlaga@nasa.gov; adolfo.figueroa-vinas.l@nasa.gov NR 39 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-SPACE JI J. Geophys. Res-Space Phys. PD JUL 30 PY 2005 VL 110 IS A7 AR A07110 DI 10.1029/2005JA011132 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 951QJ UT WOS:000230945200002 ER PT J AU Roy, DP Jin, Y Lewis, PE Justice, CO AF Roy, DP Jin, Y Lewis, PE Justice, CO TI Prototyping a global algorithm for systematic fire-affected area mapping using MODIS time series data SO REMOTE SENSING OF ENVIRONMENT LA English DT Review DE fire; fire-affected area; burned area; change detection; BRDF; MODIS; time series ID SURFACE BIDIRECTIONAL REFLECTANCE; BURNED AREAS; EOS-MODIS; BOREAL FORESTS; CENTRAL-AFRICA; SATELLITE DATA; AVHRR DATA; LAND; VEGETATION; ALBEDO AB The remote sensing of Earth surface changes is an active research field aimed at the development of methods and data products needed by scientists, resource managers, and policymakers. Fire is a major cause of surface change and occurs in most vegetation zones across the world. The identification and delineation of fire-affected areas, also known as burned areas or fire scars, may be considered a change detection problem. Remote sensing algorithms developed to map fire-affected areas are difficult to implement reliably over large areas because of variations in both the surface state and those imposed by the sensing system. The availability of robustly calibrated, atmospherically corrected, cloud-screened, geolocated data provided by the latest generation of moderate resolution remote sensing systems allows for major advances in satellite mapping of fire-affected area. This paper describes an algorithm developed to map fire-affected areas at a global scale using Moderate Resolution Imaging Spectroradiometer (MODIS) surface reflectance time series data. The algorithm is developed from the recently published Bi-Directional Reflectance Model-Based Expectation change detection approach and maps at 500 in the location and approximate day of burning. Improvements made to the algorithm for systematic global implementation are presented and the algorithm performance is demonstrated for southern African, Australian, South American, and Boreal fire regimes. The algorithm does not use training data but rather applies a wavelength independent threshold and spectral constraints defined by the noise characteristics of the reflectance data and knowledge of the spectral behavior of burned vegetation and spectrally confusing changes that are not associated with burning. Temporal constraints are applied capitalizing on the spectral persistence of fire-affected areas. Differences between mapped fire-affected areas and cumulative MODIS active fire detections are illustrated and discussed for each fire regime. The results reveal a coherent spatio-temporal mapping of fire-affected area and indicate that the algorithm shows potential for global application. (C) 2005 Elsevier Inc. All rights reserved. C1 Univ Maryland, Dept Geog, College Pk, MD 20742 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. UCL, Remote Sensing Unit, London WC1H 0AP, England. UCL, NERC, Ctr Terr Carbon Dynam, Dept Geog, London WC1H 0AP, England. RP Roy, DP (reprint author), Univ Maryland, Dept Geog, 1113 LeFrak Hall, College Pk, MD 20742 USA. EM droy@kratmos.gsfe.nasa.gov RI Lewis, Philip/C-1588-2008 OI Lewis, Philip/0000-0002-8562-0633 NR 101 TC 227 Z9 239 U1 9 U2 53 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD JUL 30 PY 2005 VL 97 IS 2 BP 137 EP 162 DI 10.1016/j.rse.2005.04.007 PG 26 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 955NM UT WOS:000231232700001 ER PT J AU Wang, HQ Zurek, RW Richardson, MI AF Wang, HQ Zurek, RW Richardson, MI TI Relationship between frontal dust storms and transient eddy activity in the northern hemisphere of Mars as observed by Mars Global Surveyor SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID MID-LATITUDE DISTURBANCES; GENERAL-CIRCULATION MODEL; TES NADIR DATA; MARTIAN ATMOSPHERE; ORBITER CAMERA; SURFACE PRESSURE; TRAVELING-WAVES; POLAR HOOD; VARIABILITY; PACIFIC AB [1] We have compiled a catalog of frontal dust storms in the northern hemisphere using Mars Orbiter Camera daily global maps spanning similar to 2.3 Martian years of Mars Global Surveyor (MGS) observations ( from 1999 to 2003). The most vigorous frontal storms that flush dust to the low latitudes occur in early-mid fall and mid-late winter, away from the northern winter solstice. While many streaks are observed in the polar hood during the winter solstice period, no frontal dust storms are observed in the vicinity of the north polar region. We have also analyzed simultaneous MGS Thermal Emission Spectrometer (TES) temperature data and found statistically significant negative temperature anomalies associated with frontal storms. In the lowest scale height of the atmosphere, the geographical and seasonal distributions of temperature standard deviations associated with transient variations agree well with the distributions of frontal storms. The correlation deteriorates with increasing altitude, suggesting that lower-level temperature waves are associated with the frontal dust storms. Specifically, eastward traveling m = 3 waves with periods of 2 - 3 sols appear to be closely related to the development of flushing frontal storms. C1 CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Wang, HQ (reprint author), CALTECH, Div Geol & Planetary Sci, MS 150-21, Pasadena, CA 91125 USA. EM hqw@gps.caltech.edu NR 40 TC 37 Z9 37 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-PLANET JI J. Geophys. Res.-Planets PD JUL 29 PY 2005 VL 110 IS E7 AR E07005 DI 10.1029/2005JE002423 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 951PO UT WOS:000230943000001 ER PT J AU Messenger, S Keller, LP Lauretta, DS AF Messenger, S Keller, LP Lauretta, DS TI Supernova olivine from cometary dust SO SCIENCE LA English DT Article ID MOLECULAR-CLOUD MATERIAL; SOLAR-SYSTEM FORMATION; PRESOLAR SIC GRAINS; GIANT BRANCH STARS; INTERPLANETARY DUST; ISOTOPIC COMPOSITIONS; INTERSTELLAR DUST; ISO SPECTROSCOPY; SILICON-CARBIDE; MASSIVE STARS AB An interplanetary dust particle contains a submicrometer crystalline silicate aggregate of probable supernova origin. The grain has a pronounced enrichment in O-18/O-16 (13 times the solar value) and depletions in O-17/O-16 (one-third solar) and Si-29/Si-28 (<0.8 times solar), indicative of formation from a type 11 supernova. The aggregate contains olivine (forsterite 83) grains <100 nanometers in size, with microstructures that are consistent with minimal thermal alteration. This unusually iron-rich olivine grain could have formed by equilibrium condensation from cooling supernova ejecta if several different nucleosynthetic zones mixed in the proper proportions. The supernova grain is also partially encased in nitrogen-15-rich organic matter that likely formed in a presolar cold molecular cloud. C1 NASA, Lyndon B Johnson Space Ctr, Robert M Walker Lab Space Sci, Houston, TX 77058 USA. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. RP Messenger, S (reprint author), NASA, Lyndon B Johnson Space Ctr, Robert M Walker Lab Space Sci, Mail Code KR, Houston, TX 77058 USA. EM scott.r.messenger@nasa.gov NR 63 TC 95 Z9 95 U1 1 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 JUL 29 PY 2005 VL 309 IS 5735 BP 737 EP 741 DI 10.1126/science.1109602 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 951NU UT WOS:000230938200040 PM 15994379 ER PT J AU Filipiak, MJ Harwood, RS Jiang, JH Li, QB Livesey, NJ Manney, GL Read, WG Schwartz, MJ Waters, JW Wu, DL AF Filipiak, MJ Harwood, RS Jiang, JH Li, QB Livesey, NJ Manney, GL Read, WG Schwartz, MJ Waters, JW Wu, DL TI Carbon monoxide measured by the EOS Microwave Limb Sounder on Aura: First results SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID UARS AB Atmospheric carbon monoxide (CO) is measured by the EOS Microwave Limb Sounder (MLS) on NASA's recently-launched Aura satellite. Descent has been observed in the 2004-2005 Northern Hemisphere winter polar mesosphere and upper stratosphere. During August and September 2004 enhanced CO was observed in the upper troposphere over India and Tibet. The MLS CO measurements are described and the radiance signal due to the enhanced CO in the upper troposphere is demonstrated. C1 Univ Edinburgh, Sch Geosci, Inst Atmospher & Environm Sci, Edinburgh EH9 3JN, Midlothian, Scotland. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. New Mexico Highlands Univ, Dept Nat Sci, Las Vegas, NM 87701 USA. RP Filipiak, MJ (reprint author), Univ Edinburgh, Sch Geosci, Inst Atmospher & Environm Sci, Crew Bldg,Kings Bldg,Mayfield Rd, Edinburgh EH9 3JN, Midlothian, Scotland. EM mjf@met.ed.ac.uk RI Schwartz, Michael/F-5172-2016; Wu, Dong/D-5375-2012 OI Schwartz, Michael/0000-0001-6169-5094; NR 5 TC 41 Z9 46 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 28 PY 2005 VL 32 IS 14 AR L14825 DI 10.1029/2005GL022765 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 951MM UT WOS:000230934600003 ER PT J AU Li, QB Jiang, JH Wu, DL Read, WG Livesey, NJ Waters, JW Zhang, YS Wang, B Filipiak, MJ Davis, CP Turquety, S Wu, SL Park, RJ Yantosca, RM Jacob, DJ AF Li, QB Jiang, JH Wu, DL Read, WG Livesey, NJ Waters, JW Zhang, YS Wang, B Filipiak, MJ Davis, CP Turquety, S Wu, SL Park, RJ Yantosca, RM Jacob, DJ TI Convective outflow of South Asian pollution: A global CTM simulation compared with EOS MLS observations SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID AIR-POLLUTION; MODEL; EMISSIONS; AEROSOL AB A global 3-D chemical transport model is used to analyze observations of carbon monoxide (CO) and upper tropospheric clouds from the EOS Microwave Limb Sounder (MLS). MLS observations during 25 August-6 September 2004 reveal elevated CO and dense high clouds in the upper troposphere over the Tibetan plateau and southwest China, collocating with the upper level Tibetan anticyclone. Model simulations indicate the transport of boundary layer pollution by Asian summer monsoon (ASM) convection and orographic lifting to the upper troposphere over South Asia, where simulated distributions of CO resemble MLS observations. Model results also show elevated aerosols in the anticyclone region. Analysis of model simulated CO and aerosols indicate that the Tibetan anticyclone could 'trap' anthropogenic emissions lifted from northeast India and southwest China. These aerosols may be responsible for the formation of some of the dense high clouds. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Int Pacific Res Ctr, Honolulu, HI 96822 USA. Univ Hawaii Manoa, Dept Meteorol, Honolulu, HI 96822 USA. Univ Edinburgh, Sch Geosci, Inst Atmospher & Environm Sci, Edinburgh EH9 3JZ, Midlothian, Scotland. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 183-501, Pasadena, CA 91109 USA. EM qinbin.li@jpl.nasa.gov RI Yantosca, Robert/F-7920-2014; Park, Rokjin/I-5055-2012; Wu, Dong/D-5375-2012 OI Yantosca, Robert/0000-0003-3781-1870; Park, Rokjin/0000-0001-8922-0234; NR 22 TC 110 Z9 117 U1 3 U2 20 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 28 PY 2005 VL 32 IS 14 AR L14826 DI 10.1029/2005GL022762 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 951MM UT WOS:000230934600002 ER PT J AU Arnoldy, RL Engebretson, MJ Denton, RE Posch, JL Lessard, MR Maynard, NC Ober, DM Farrugia, CJ Russell, CT Scudder, JD Torbert, RB Chen, SH Moore, TE AF Arnoldy, RL Engebretson, MJ Denton, RE Posch, JL Lessard, MR Maynard, NC Ober, DM Farrugia, CJ Russell, CT Scudder, JD Torbert, RB Chen, SH Moore, TE TI Pc 1 waves and associated unstable distributions of magnetospheric protons observed during a solar wind pressure pulse SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ION-CYCLOTRON WAVES; STORM SUDDEN COMMENCEMENTS; MAGNETIC-FIELD; GEOMAGNETIC-PULSATIONS; PLASMA INSTRUMENT; POLAR SATELLITE; INSTABILITY; ELECTRON; DENSITY; MODULATION AB [1] We present observations of Pc 1 waves ( similar to 0.6 Hz) that occurred shortly after a strong (> 20 nPa) compression of Earth's magnetosphere at 1321 UT, 18 March 2002. Intense Pc 1 waves were observed at several high-latitude ground stations in Antarctica and Greenland from 1321 UT to beyond 1445 UT. Two wave bursts were recorded at the Polar satellite at 1338 and 1343 - 1344 UT as it passed outbound in the Southern Hemisphere at 1154 local time (SM magnetic latitude of - 22 degrees and near L = 7.5) in good magnetic conjunction with the Antarctic. The pressure increase created a significant population of protons between a few hundred eV and several keV, whose fluxes were mostly perpendicular to B. These protons seem to have replaced the quiescent stream of protons ( presumably convected from the plasma sheet) that existed before this increase. There was also a nearly two-order-of-magnitude increase in the population of thermal/suprathermal (0.32 - 410 eV) protons. The generation of ion cyclotron waves is expected to limit the proton temperature anisotropy A, defined as T-perpendicular to/T-parallel to - 1. The ion cyclotron instability driven by the observed hot ion temperature anisotropy is studied using two models, with and without the presence of cold background plasma. Peaks in the calculated instability as a function of time show excellent agreement with the times of the Polar wave bursts, which were measured a few tens of seconds after maxima in the instability calculation. The time delay is consistent with the propagation time to the spacecraft from a source nearer to the equatorial plane. The hot proton population at Polar appears to be driven back to stability by a sudden increase in very field-aligned protons having energies less than the hot perpendicular population, suggesting a different source for the two populations. These observations confirm the importance of both the energization and/or increase in population of protons transverse to B in the several keV range ( possibly betatron acceleration as a result of the pressure pulse), and the presence of greatly increased fluxes of lower energy protons (100s of eV to a few keV), predominantly aligned along B, in determining whether the particle population is unstable at a given time. C1 Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. Augsburg Coll, Dept Phys, Minneapolis, MN USA. Dartmouth Coll, Dept Phys, Hanover, NH 03755 USA. ATK Miss Res, Nashua, NH USA. Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. Univ Iowa, Dept Phys, Iowa City, IA USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. EM roger.arnoldy@unh.edu; engebret@augsburg.edu; richard.e.denton@dartmouth.edu; posch@augsburg.edu; marc.lessard@unh.edu; nelson.maynard@atk.com; dan.ober@atk.com; charlie.farrugia@unh.ed; ctrussell@igpp.ucla.edu; jds@space-theory.physics.uiowa.edu; roy.torbert@unh.edu; sheng-hsien.chen@gsfc.nasa.gov; thomas.e.moore@nasa.gov RI Moore, Thomas/D-4675-2012; Scudder, Jack/D-8417-2013 OI Moore, Thomas/0000-0002-3150-1137; Scudder, Jack/0000-0001-7975-5630 NR 48 TC 37 Z9 37 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUL 28 PY 2005 VL 110 IS A7 AR A07229 DI 10.1029/2005JA011041 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 951QE UT WOS:000230944700003 ER PT J AU Miller, Y Chaban, GM Gerber, RB AF Miller, Y Chaban, GM Gerber, RB TI Ab initio vibrational calculations for H(2)SO(4) and H(2)SO(4)center dot H(2)O: Spectroscopy and the nature of the anharmonic couplings SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID SELF-CONSISTENT-FIELD; DENSITY-FUNCTIONAL THEORY; SULFURIC-ACID AEROSOLS; INFRARED-SPECTRA; BIOLOGICAL MOLECULES; EMPIRICAL POTENTIALS; POLYATOMIC SYSTEMS; MATRIX-ISOLATION; STATES; VAPOR AB Vibrational frequencies for fundamental, overtone, and combination excitations of sulfuric acid (H(2)SO(4)) and of sulfuric acid monohydrate cluster (H(2)SO(4)(.)H(2)O) are computed directly from ab initio MP2/TZP potential surface points using the correlation-corrected vibrational self-consistent field (CC-VSCF) method, which includes anharmonic effects. The results are compared with experiment. The computed transitions show in nearly all cases good agreement with experimental data and consistent improvement over the harmonic approximation. The CC-VSCF improvements over the harmonic approximation are largest for the overtone and combination excitations and for the OH stretching fundamental. The agreement between the calculations and experiment also supports the validity of the MP2/TZP potential surfaces. Anharmonic coupling between different vibrational modes is found to significantly affect the vibrational frequencies. Analysis of the mean magnitude of the anharmonic coupling interactions between different pairs of normal modes is carried out. The results suggest possible mechanisms for the internal flow of vibrational energy in H(2)SO(4) and H(2)SO(4)(.) H(2)O. C1 Hebrew Univ Jerusalem, Dept Phys Chem, IL-91904 Jerusalem, Israel. Hebrew Univ Jerusalem, Fritz Haber Res Ctr, IL-91904 Jerusalem, Israel. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Calif Irvine, Dept Chem, Irvine, CA 92697 USA. RP Gerber, RB (reprint author), Hebrew Univ Jerusalem, Dept Phys Chem, IL-91904 Jerusalem, Israel. EM benny@fh.huji.ac.il RI Young, Nigel/B-5472-2010 NR 66 TC 75 Z9 75 U1 2 U2 19 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 J9 J PHYS CHEM A JI J. Phys. Chem. A PD JUL 28 PY 2005 VL 109 IS 29 BP 6565 EP 6574 DI 10.1021/jp058110l PG 10 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 948DK UT WOS:000230696000022 PM 16834003 ER PT J AU Creilson, JK Fishman, J Wozniak, AE AF Creilson, JK Fishman, J Wozniak, AE TI Arctic Oscillation - induced variability in satellite-derived tropospheric ozone SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID EXTRATROPICAL CIRCULATION; ANNULAR MODES; POLLUTION; RESIDUALS; TRANSPORT; CLIMATE; TRENDS AB The Arctic Oscillation (AO) has been identified as the dominant mode of near-surface climate variability in the Northern Hemisphere. In this study, we examine the interaction between the AO and the distribution of tropospheric ozone derived from satellite observations. Our analysis shows that there is a statistically significant correlation between the AO and the springtime tropospheric ozone distribution over the northeastern Atlantic, but not over the Pacific. This finding is consistent with our understanding of the differing effect that the AO has on the Atlantic versus Pacific basins and the strong influence that the El Nino phenomenon has in the Pacific. The insight gained from this study will contribute to the growing use of teleconnections as a forecast tool, providing insight into the interaction between prevailing meteorological conditions and the formation of significant pollution events. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. Sci Applicat Int Corp, Hampton, VA USA. RP Creilson, JK (reprint author), NASA, Langley Res Ctr, MS 927,1 Enterprise Pkwy, Hampton, VA 23681 USA. EM j.k.creilson@larc.nasa.gov NR 20 TC 12 Z9 13 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 27 PY 2005 VL 32 IS 14 AR L14822 DI 10.1029/2005GL023016 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 951ML UT WOS:000230934500007 ER PT J AU Klimas, AJ Uritsky, VM Vassiliadis, D Baker, DN AF Klimas, AJ Uritsky, VM Vassiliadis, D Baker, DN TI A mechanism for the loading-unloading substorm cycle missing in MHD global magnetospheric simulation models SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID RECONNECTION; SHEET AB A 2-dimensional numerical driven current-sheet model has been developed that incorporates an idealized current-driven instability with a resistive MHD system. Under steady loading, the model exhibits a global loading-unloading cycle. The specific mechanism for producing the loading-unloading cycle is discussed. It is shown that scale-free avalanching of electromagnetic energy through the model, from loading to unloading, is carried by repetitive bursts of localized reconnection. Each burst leads, somewhat later, to a field configuration that is capable of exciting a reconnection burst again. This process repeats itself in an intermittent manner while the total field energy in the system falls. The total field energy is reduced to well below that necessary to initiate an unloading event and, thus, a loading-unloading cycle results. It is shown that, in this model, it is the topology of bursty localized reconnection that is responsible for the appearance of the loading-unloading cycle. C1 NASA, Goddard Space Flight Ctr, Lab Solar & Space Phys, Greenbelt, MD 20771 USA. St Petersburg State Univ, Inst Phys, St Petersburg, Russia. St Petersburg State Univ, Dept Phys, St Petersburg, Russia. NASA, Goddard Space Flight Ctr, Sarissa Technol, Greenbelt, MD 20771 USA. Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. RP Klimas, AJ (reprint author), NASA, Goddard Space Flight Ctr, Lab Solar & Space Phys, Greenbelt, MD 20771 USA. EM alex.klimas@gsfc.nasa.gov 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 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 27 PY 2005 VL 32 IS 14 AR L14108 DI 10.1029/2005GL022916 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 951ML UT WOS:000230934500005 ER PT J AU Webber, WR Cummings, AC Stone, EC McDonald, FB Lal, N Heikkila, B AF Webber, WR Cummings, AC Stone, EC McDonald, FB Lal, N Heikkila, B TI Differences in the spectra of anomalous cosmic ray helium nuclei in two solar magnetic polarity cycles SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID OUTER HELIOSPHERE; ENERGY-SPECTRA; ENHANCEMENTS; MODULATION; COMPONENT; HYDROGEN; NITROGEN; OXYGEN; SHOCK; LESS AB [1] We compare the spectra of anomalous He nuclei measured in the heliosphere by the IMP, Voyager, and Pioneer spacecraft at heliospheric distances ranging from 1 to over 80 AU in the time period from 1977 to 2003. Striking differences in the energy spectra of these nuclei are found between positive and negative solar magnetic polarity cycles. These differences are such that the spectra observed in negative polarity cycles appear to be greatly deficient in particles with energies of less than similar to 15 MeV but have an excess intensity above > 25 MeV, relative to the spectra observed in positive cycles. These spectral differences are complex and may be related to both solar modulation effects inside of the heliospheric termination shock as well as differences occurring at or near the termination shock itself. At the modulation minimum in 1998 when V2 was at a distance of 56 AU and V1 at 71 AU, a high intensity of low-energy anomalous He particles was observed with a peak in the spectrum at similar to 5 MeV/nuc. In late 2001 after the solar magnetic polarity had changed from positive to negative and the 11-year solar modulation had increased, the previous high intensities of the anomalous He nuclei seen in 1998 were greatly reduced at both V1 and V2, and the energy of the peak intensity had moved up to similar to 20 - 25 MeV/nuc. However, in both polarity periods the highest-energy part of this spectrum above similar to 30 MeV/ nuc is similar with a slope of - 2.8 +/- 0.2. The details of these complex spectral changes are described in this paper. C1 New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. CALTECH, Downs Lab, Pasadena, CA USA. Univ Maryland, Inst Phys Sci & Technol, College Pk, MD 20742 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Webber, WR (reprint author), New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. EM bwebber@nmsu.edu NR 27 TC 4 Z9 4 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUL 27 PY 2005 VL 110 IS A7 AR A07106 DI 10.1029/2005JA011123 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 951QC UT WOS:000230944500002 ER PT J AU Petersen, WA Christian, HJ Rutledge, SA AF Petersen, WA Christian, HJ Rutledge, SA TI TRMM observations of the global relationship between ice water content and lightning SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID RADAR REFLECTIVITY; PRECIPITATION AB This study uses TRMM lightning and radar observations to study the fundamental relationship between precipitation ice mass and lightning flash density. The results indicate that the physical assumptions of precipitation-based charging and mixed phase precipitation development are robust and that on a global scale, the relationship between precipitation ice water path and lightning flash density is relatively invariant between land, ocean and coastal regimes. Hence lightning data may be a useful variable for inclusion in combined space borne algorithms designed to retrieve ice water content. C1 Univ Alabama, Ctr Earth Syst Sci, Huntsville, AL 35899 USA. Univ Alabama, NSSTC, Huntsville, AL 35899 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. RP Univ Alabama, Ctr Earth Syst Sci, Huntsville, AL 35899 USA. EM walt.petersen@msfc.nasa.gov OI Peterson, WK/0000-0002-1513-6096 NR 14 TC 92 Z9 97 U1 1 U2 12 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 JUL 26 PY 2005 VL 32 IS 14 AR L14819 DI 10.1029/2005GL023236 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 951MJ UT WOS:000230934300008 ER PT J AU Bills, BG Neumann, GA Smith, DE Zuber, MT AF Bills, BG Neumann, GA Smith, DE Zuber, MT TI Improved estimate of tidal dissipation within Mars from MOLA observations of the shadow of Phobos SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Review ID ORBITER LASER ALTIMETER; MARTIAN SATELLITES; SECULAR ACCELERATION; VISCOELASTIC MODELS; EARTHS ROTATION; GRAVITY-FIELD; UPPER-MANTLE; SOLAR-WIND; EVOLUTION; IO AB [1] We report on new observations of the orbital position of Phobos, the innermost natural satellite of Mars, and show that these observations provide an improved estimate of the rate of tidal dissipation within Mars. The observations were made with the Mars Orbiter Laser Altimeter instrument on the Mars Global Surveyor spacecraft. The secular acceleration in along-track orbital motion is conventionally expressed in terms of a quadratic term in mean orbital longitude, which yields s = (dn/dt)/2 = (136.7 +/- 0.6) x 10(-5) deg/yr(2), where n is the mean motion. The corresponding fractional rate of change in orbital angular velocity is (dn/dt)/ n = (6.631 +/- 0.029) x 10(-9)/ yr, the highest measured for any natural satellite in the solar system. The energy dissipation rate is (3.34 +/- 0.01) MW. Because Phobos is so close to Mars, there are nonnegligible contributions to the tidal evolution from harmonic degrees 2, 3, and 4. However, the elastic tidal Love numbers are observationally constrained only at degree two. The observed acceleration is consistent with that for a homogeneous Maxwell viscoelastic model of Mars with effective viscosity of (8.7 +/- 0.6) x 10(14) Pa s. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. MIT, Cambridge, MA 02139 USA. RP Bills, BG (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM bbills@ucsd.edu RI Bills, Bruce/C-1156-2008 NR 101 TC 54 Z9 53 U1 9 U2 24 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUL 26 PY 2005 VL 110 IS E7 AR E07004 DI 10.1029/2004JE002376 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 951PN UT WOS:000230942900001 ER PT J AU Dass, A Leventis, N AF Dass, A Leventis, N TI Non-additive voltammetric currents from multicomponent systems of redox-active substances SO ELECTROCHIMICA ACTA LA English DT Article DE voltammetric; analysis; multicomponent; non-additive; ultramicroelectrodes ID POTENTIAL STEP CHRONOAMPEROMETRY; ELECTRON-TRANSFER; CONCENTRATION PROFILES; DIFFUSIONAL PATHWAYS AB Mixtures of two redox-active compounds with dissimilar diffusion coefficients produce non-additive mass-transfer limited currents. Similarly, in the potential range where three redox-active species, decamethylferrocene (dMeFc), ferrocene (Fc) and N-methylphenothiazine (MePTZ), are oxidized simultaneously (E-MePTZ(o') > E-Fc(o') > E-dMeFc(o')) with rates controlled by linear diffusion, electrogenerated radicals diffusing outwards from the electrode react with original species diffusing towards the electrode from the bulk; thus, Fc(center dot+) reacts with dMeFc producing Fc and dMeFc(center dot+), while MePTZ(center dot+) reacts with both Fc and dMeFc producing MePTZ together with Fc(center dot+) and dMeFc(center dot+). These processes replace the flux of dMeFc with Fc at the second current plateau (referring to normal pulse voltammetry), and the fluxes of both dMeFc and Fc with MePTZ at the third plateau. Analogous results have been obtained and analyzed with two other multicomponent systems undergoing multiple sequential electron transfers, namely dMeFc/Fc/TPTA and dMeFc/TTF (TPTA: tri-N-p-tolylamine; TTF: tetrathiafulvalene). Since the diffusion coefficients of the three species are different, the mass-transfer limited currents of the second and third oxidation waves are not equal to the sum of the currents that each component would have produced if it were in the solution alone. Numerical simulations of the experimental voltammograms using diffusion coefficients measured independently support this mechanism. Multicomponent systems are encountered frequently in practice and our results identify one significant (similar to 10%) source of error in quantitative voltammetric analysis. Ways around the problem are summarized in the conclusions section. (c) 2005 Elsevier Ltd. All rights reserved. C1 NASA, Glenn Res Ctr, Div Mat, Cleveland, OH 44135 USA. Univ Missouri, Dept Chem, Rolla, MO 65401 USA. RP Leventis, N (reprint author), NASA, Glenn Res Ctr, Div Mat, 21000 Brookpk Rd MS 49-1, Cleveland, OH 44135 USA. EM nicholas.leventis@nasa.gov RI Dass, Amal/A-2520-2011; Dass, Amala/H-4729-2012 OI Dass, Amala/0000-0001-6942-5451 NR 14 TC 3 Z9 3 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0013-4686 J9 ELECTROCHIM ACTA JI Electrochim. Acta PD JUL 25 PY 2005 VL 50 IS 20 BP 4134 EP 4139 DI 10.1016/j.electacta.2005.01.030 PG 6 WC Electrochemistry SC Electrochemistry GA 948GT UT WOS:000230704800013 ER PT J AU Rogers, MM AF Rogers, MM TI Turbulent plane wakes subjected to successive strains SO JOURNAL OF FLUID MECHANICS LA English DT Article ID UNIFORM DISTORTION; MIXING LAYERS; SHEAR AB Six direct numerical simulations of turbulent time-evolving strained plane wakes have been examined to investigate the response of a wake to successive irrotational plane strains of opposite sign. The orientation of the applied strain field has been selected so that the flow is the time-developing analogue of a spatially developing wake evolving in the presence of either a favourable or an adverse streamwise pressure gradient. The magnitude of the applied strain rate a is constant in time t until the total strain eat reaches about 4. At this point, a new simulation is begun with the sign of the applied strain being reversed (the original simulation is continued as well). When the total strain is reduced back to its original value of 1, yet another simulation is begun with the strain again being reversed back to its original sign. This is done for both initially 'favourable' and initially 'adverse' strains, providing simulations for each of these strain types from three different initial conditions. The evolution of the wake mean velocity deficit and width is found to be similar for all the 'adversely' strained cases, with both measures rapidly achieving exponential growth at the rate associated with the cross-stream expansive strain e a,. In the Tavourably' strained cases, the wake widths approach a constant and the velocity deficits ultimately decay rapidly as e(-2at). Although all three of these cases do exhibit the same asymptotic exponential behaviour, the time required to achieve this is longer for the cases that have been previously adversely strained (by at 1). The evolution described above is not consistent with the predictions of classical self-similar analysis; a more general 'equilibrium similarity solution' is required to describe the results. Examination of these simulations confirms that the wake width and mean velocity deficit evolutions observed in Rogers (2002) are not a result of the particular initial condition used in that work. At least for the cases considered here, the wake Reynolds number and the ratio of the turbulent kinetic energy to the square of the wake mean velocity deficit are determined nearly entirely by the total strain. For these measures, the order in which the strains are applied does not matter and the changes brought about by the strain are nearly reversible. The wake mean velocity deficit and width, on the other hand, differ by about a factor of 3 when the total strain returns to 1, depending on whether the wake was first Tavourably' or 'adversely' strained. The strain history is important for predicting the evolution of these quantities. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Rogers, MM (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 24 TC 4 Z9 4 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0022-1120 J9 J FLUID MECH JI J. Fluid Mech. PD JUL 25 PY 2005 VL 535 BP 215 EP 243 DI 10.1017/S0022112005004775 PG 29 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA 955DJ UT WOS:000231205100008 ER PT J AU Israel, MH Binns, WR Cummings, AC Leske, RA Mewaldt, RA Stone, EC von Rosenvinge, TT Wiedenbeck, ME AF Israel, MH Binns, WR Cummings, AC Leske, RA Mewaldt, RA Stone, EC von Rosenvinge, TT Wiedenbeck, ME TI Isotopic composition of cosmic rays: Results from the Cosmic Ray Isotope Spectrometer on the ACE spacecraft SO NUCLEAR PHYSICS A LA English DT Article; Proceedings Paper CT 8th International Symposium on Nucle in the Cosmos (NIC8) CY JUL 19-23, 2004 CL Vancouver, CANADA ID SUPERNOVA-REMNANTS; ACCELERATION; ABUNDANCES; SOLAR; NUCLEOSYNTHESIS; CONSTRAINTS; ELEMENTS; ORIGIN AB The Cosmic Ray Isotope Spectrometer on the ACE spacecraft measures the isotopic composition of cosmic-ray elements from Li through Zn with an unprecedented combination of excellent mass resolution and high statistics. The results indicate a cosmic-ray source whose composition is remarkably similar to that of the solar system, but which is enriched in material that may have originated in Wolf-Rayet stars. The lack of Ni-59 is strong indication that the cosmic rays are accelerated at least 10(5) years after nucleosynthesis. We examine these results in the context of the superbubble model of cosmic-ray origin that has been described by Higdon and Lingenfelter. C1 Washington Univ, Dept Phys, St Louis, MO 63130 USA. Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA. CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Israel, MH (reprint author), Washington Univ, Dept Phys, St Louis, MO 63130 USA. NR 21 TC 6 Z9 6 U1 0 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0375-9474 J9 NUCL PHYS A JI Nucl. Phys. A PD JUL 25 PY 2005 VL 758 SI SI BP 201C EP 208C DI 10.1016/j.nuclphysa.2005.05.038 PG 8 WC Physics, Nuclear SC Physics GA 947QG UT WOS:000230660500046 ER PT J AU Kurth, WS Hospodarsky, GB Gurnett, DA Cecconi, B Louarn, P Lecacheux, A Zarka, P Rucker, HO Boudjada, M Kaiser, ML AF Kurth, WS Hospodarsky, GB Gurnett, DA Cecconi, B Louarn, P Lecacheux, A Zarka, P Rucker, HO Boudjada, M Kaiser, ML TI High spectral and temporal resolution observations of Saturn kilometric radiation SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID RADIO-EMISSION; INSTABILITY; GENERATION; MODEL; BAND AB This paper presents the first high- resolution dynamic spectra of Saturn kilometric radiation acquired upon Cassini's approach and first orbits of Saturn. The emissions display upward and downward drifting features with bandwidths down to similar to 200 Hz and drift rates of a few kHz per second. At other times, the emissions are much more diffuse or continuous, showing little spectral structure on scales of 10 or 20 kHz. The fine structure is strikingly similar to Earth's auroral kilometric radiation ( AKR) and Jovian auroral radio emissions in many respects. The dynamic spectral features provide insight into the highly nonlinear nature of the cyclotron maser instability believed to generate the emissions. We use ideas developed to explain the fine structures at Earth to suggest features and processes in the auroral acceleration region which may result in Saturn's fine structures. C1 Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Observ Paris, F-92195 Meudon, France. CNRS, CESR, F-31028 Toulouse, France. RP Kurth, WS (reprint author), Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. EM william-kurth@uiowa.edu; george-hospodarsky@uiowa.edu; donald-gurnett@uiowa.edu; baptiste-cecconi@uiowa.edu; philippe.louarn@cesr.fr; alain.lecacheux@obspm.fr; philippe.zarka@obspm.fr; helmut.rucker@oeaw.ac.at; mohammed.boudjada@oeaw.ac.at; michael.kaiser@nasa.gov OI Hospodarsky, George/0000-0001-9200-9878; Kurth, William/0000-0002-5471-6202 NR 19 TC 4 Z9 4 U1 1 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 23 PY 2005 VL 32 IS 20 AR L20S07 DI 10.1029/2005GL022648 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 951GK UT WOS:000230917300001 ER PT J AU Miller, CE Onorato, RM Liang, MC Yung, YL AF Miller, CE Onorato, RM Liang, MC Yung, YL TI Extraordinary isotopic fractionation in ozone photolysis SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID HEAVY OZONE; ATMOSPHERE; OXYGEN; PHOTOCHEMISTRY; SPECTROSCOPY; STRATOSPHERE; ENRICHMENT; SPECTRA; SYSTEM; UV AB Analysis of experimental ozone absorption spectra reveals that ultraviolet photolysis within the structured Huggins band yields extraordinary wavelength-dependent isotopic fractionation, oscillating between complete enrichment and complete depletion for changes of less than 2 nm in the excitation wavelength. Visible photolysis yields wavelength-dependent fractionation that varies from -300 parts per thousand to +300 parts per thousand. Photochemical modeling demonstrates photolysis contributes fractionation up to +45 parts per thousand to the heavy ozone anomaly in the middle stratosphere with measurable O-17 and O-18 isotopologue-dependent variations as a function of altitude despite the fact that the extraordinary photolysis-induced isotopic fractionation effect is dampened in the atmosphere due to the integration over all excitation wavelengths. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Miller, CE (reprint author), CALTECH, Jet Prop Lab, MS 183-501,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM charles.e.miller@jpl.nasa.gov NR 23 TC 15 Z9 15 U1 2 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 23 PY 2005 VL 32 IS 14 AR L14814 DI 10.1029/2005GL023160 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 951GI UT WOS:000230917000006 ER PT J AU Bell, N Koch, D Shindell, DT AF Bell, N Koch, D Shindell, DT TI Impacts of chemistry-aerosol coupling on tropospheric ozone and sulfate simulations in a general circulation model SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SURFACE OZONE; HETEROGENEOUS CHEMISTRY; GODDARD-INSTITUTE; NORTH-AMERICA; AIR-POLLUTION; UNITED-STATES; SULFUR CYCLE; TRANSPORT; OXIDANTS; SPACE AB We have implemented fully interactive tropospheric gas-phase chemistry and sulfate aerosol modules into the new generation state-of the-art Goddard Institute for Space Studies (GISS) modelE general circulation model (GCM). The code has been developed with a unique flexibility to perform simulations in coupled or off-line (decoupled) mode. Both modes use identical chemical calculations, but the decoupled simulation relies on previously saved off-line oxidant and aerosol concentration fields whereas the coupled simulation is fully interactive. Here we describe the application of the model to isolate the impacts of the two-way chemistry-aerosol coupling on the predictions of sulfate aerosol and ozone pollution and to provide insights into the mechanisms that drive the different predictions between coupled and off-line models. On annual and global scales, the differences between the coupled and off-line simulations are small, but larger deviations do occur on regional and seasonal scales. The chemistry-aerosol coupling leads to similar to 20% increases in surface sulfate over SO2 source regions in the northern hemisphere summer due to higher H2O2 levels and aqueous-phase oxidation rates in the coupled model. Compensating sulfate decreases occur in downwind regions and in the upper troposphere due to depleted SO2. At middle to high tropospheric altitudes in the northern hemisphere, ozone and OH are increased in the coupled model relative to the off- line model by similar to 10% due to reductions in sulfate loading and subsequent suppression of N2O5 heterogeneous hydrolysis. The use of off- line versus coupled models has implications for the simulation of the intercontinental transport of pollutants and their precursors. C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Columbia Univ, New York, NY 10025 USA. RP NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM nbell@giss.nasa.gov RI Shindell, Drew/D-4636-2012; Unger, Nadine/M-9360-2015 NR 29 TC 37 Z9 38 U1 0 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 23 PY 2005 VL 110 IS D14 AR D14305 DI 10.1029/2004JD005538 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 951GT UT WOS:000230918200004 ER PT J AU Stenchikov, G Pickering, K DeCaria, A Tao, WK Scala, J Ott, L Bartels, D Matejka, T AF Stenchikov, G Pickering, K DeCaria, A Tao, WK Scala, J Ott, L Bartels, D Matejka, T TI Simulation of the fine structure of the 12 July 1996 Stratosphere-Troposphere Experiment: Radiation, Aerosols and Ozone ( STERAO-A) storm accounting for effects of terrain and interaction with mesoscale flow SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID (STERAO)-DEEP CONVECTION EXPERIMENT; GENERATED MOIST CONVECTION; BIOMASS BURNING EMISSIONS; NUMERICAL SIMULATIONS; SQUALL LINES; PART I; MODEL; TRANSPORT; PARAMETERIZATION; THUNDERSTORM AB Vertical mixing of chemical tracers and optically active constituents by deep convection affects regional and global chemical balances in the troposphere and lower stratosphere. This important process is not explicitly resolved in global and regional models and has to be parameterized. However, mixing depends strongly on the spatial structure, strength, and temporal evolution of the particular storm, complicating parameterization of this important effect in the large-scale models. To better quantify dynamic fields and associated mixing processes, we simulate a thunderstorm observed on 12 July 1996 during the STERAO-A (Stratosphere-Troposphere Experiment: Radiation, Aerosols, and Ozone) Deep Convection field project using the Goddard Cloud Ensemble (GCE) model. The 12 July STERAO-A storm had very complex temporal and spatial structure. The meteorological environment and evolution of the storm were significantly different than those of the 10 July STERAO-A storm extensively discussed in previous studies. Our 2-D and 3-D GCE model runs with uniform one-sounding initialization were unable to reproduce the full life cycle of the 12 July storm observed by the CHILL radar system. To describe the storm evolution, we modified the 3-D GCE model to include the effects of terrain and the capability of using nonuniform initial fields. We conducted a series of numerical experiments and reproduced the observed life cycle and fine spatial structure of the storm. The main characteristics of the 3-D simulation of the 12 July storm were compared with observations, with 2-D simulations of the same storm, and with the evolution of the 10 July storm. The simulated 3-D convection appears to be stronger and more realistic than in our 2-D simulations. Having developed in a less unstable environment than the 10 July 1996 STERAO-A storm, our simulation of the 12 July storm produced weaker but sustainable convection that was significantly fed by wind shear instability in the lower troposphere. The time evolution, direction, and speed of propagation of the storm were determined by interaction with the nonuniform background mesoscale flow. For example, storm intensity decreased drastically when the storm left the region with large convective available potential energy. The model appears to be successful in reproducing the rectangular four-cell structure of the convection. The distributions of convergence, vertical vorticity, and position of the inflow level in the later single-cell regime compare favorably with the airborne Doppler radar observations. This analysis allowed us to better understand the role of terrain and mesoscale circulation in the development of a midlatitude deep convective system and associated convective mixing. Wind, temperature, hydrometeor, and turbulent diffusion coefficient data from the cloud model simulations were provided for off-line 3-D cloud-scale chemical transport simulations discussed in the companion paper by DeCaria et al. (2005). C1 Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ 08901 USA. Univ Maryland, Dept Meteorol, College Pk, MD 20742 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Millersville Univ Pennsylvania, Dept Earth Sci, Millersville, PA 17551 USA. NOAA, Natl Severe Storms Lab, NCAR, Boulder, CO 80307 USA. RP Stenchikov, G (reprint author), Rutgers State Univ, Dept Environm Sci, 14 Coll Farm Rd, New Brunswick, NJ 08901 USA. EM gera@envsci.rutgers.edu; pickerin@atmos.umd.edu; alex.decaria@millersville.edu; tao@agnes.gsfc.nasa.gov; john.scala@millersville.edu; leo@atmos.umd.edu; diana.bartels@noaa.gov RI Ott, Lesley/E-2250-2012; Pickering, Kenneth/E-6274-2012; Georgiy, Stenchikov/J-8569-2013 NR 58 TC 8 Z9 8 U1 2 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 22 PY 2005 VL 110 IS D14 AR D14304 DI 10.1029/2004JD005582 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 951GS UT WOS:000230918100003 ER PT J AU Altobelli, N Kempf, S Kruger, H Landgraf, M Roy, M Grun, E AF Altobelli, N Kempf, S Kruger, H Landgraf, M Roy, M Grun, E TI Interstellar dust flux measurements by the Galileo dust instrument between the orbits of Venus and Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID SOLAR-SYSTEM; ULYSSES; HELIOSPHERE; DETECTOR; GRAINS; STREAM AB [1] We present an analysis of the data obtained by the Galileo in situ dust instrument for interstellar dust (ISD). Between December 1989 and the end of 1993, three orbit segments were favorable for the detection of ISD at less than 3 AU heliocentric distance. After removing background events from the data sample, which were mostly due to interplanetary dust impactors, we infer that the flux of ISD grains between 0.7 AU and 3 AU is about 4 x 10(-5) m(-2) s(-1). This result is compatible with the ISD flux of 3 x 10(-5) m(-2) s(-1) (grain size approximate to 0.4 mu m) derived from the Cassini measurements at about 1 AU. Using a new concept called "ISD beta spectroscopy,'' we are able to estimate at different locations in the inner solar system the ISD flux alteration resulting from the competing effects of radiation pressure and gravitation. In particular, we confirm results of previous Ulysses dust data analysis showing that radiation pressure prevents smaller ISD grains ( radius smaller than approximate to 0.3 mu m) from reaching the innermost region of the solar system. Furthermore, our analysis shows the relevance of gravitational focusing in the dynamics of bigger ISD grains ( micron-sized grains). The Galileo measurements were performed 10 years before the Cassini measurements. Thus the available ISD data now cover almost a full 11-year solar cycle. Nonetheless, the flux of ISD grains with radius bigger than 0.4 mu m shows no significant temporal variation. This suggests that the dynamics of these ISD grains is not influenced much by the interaction with the time-dependent solar magnetic field. C1 Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. European Space Agcy, European Space Operat Ctr, D-64293 Darmstadt, Germany. Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. RP Altobelli, N (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,230-205, Pasadena, CA 91109 USA. EM nicolas.altobelli@jpl.nasa.gov NR 22 TC 24 Z9 24 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 JUL 22 PY 2005 VL 110 IS A7 AR A07102 DI 10.1029/2004JA010772 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 951HT UT WOS:000230920900004 ER PT J AU Manley, S Davidovitch, B Davies, NR Cipelletti, L Bailey, AE Christianson, RJ Gasser, U Prasad, V Segre, PN Doherty, MP Sankaran, S Jankovsky, AL Shiley, B Bowen, J Eggers, J Kurta, C Lorik, T Weitz, DA AF Manley, S Davidovitch, B Davies, NR Cipelletti, L Bailey, AE Christianson, RJ Gasser, U Prasad, V Segre, PN Doherty, MP Sankaran, S Jankovsky, AL Shiley, B Bowen, J Eggers, J Kurta, C Lorik, T Weitz, DA TI Time-dependent strength of colloidal gels SO PHYSICAL REVIEW LETTERS LA English DT Article ID AGGREGATION; TRANSITION; DYNAMICS; SURFACES; FEATURES AB Colloidal silica gels are shown to stiffen with time, as demonstrated by both dynamic light scattering and bulk rheological measurements. Their elastic moduli increase as a power law with time, independent of particle volume fraction; however, static light scattering indicates that there are no large-scale structural changes. We propose that increases in local elasticity arising from bonding between neighboring colloidal particles can account for the strengthening of the network, while preserving network structure. C1 Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Harvard Univ, DEAS, Cambridge, MA 02138 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. Zin Technol Inc, Brookpark, OH 44142 USA. RP Manley, S (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RI Manley, Suliana/D-3818-2012; Sankaran, Subramanian/L-8416-2013 OI Manley, Suliana/0000-0002-4755-4778; Sankaran, Subramanian/0000-0002-8990-4107 NR 22 TC 6 Z9 6 U1 5 U2 20 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 JUL 22 PY 2005 VL 95 IS 4 AR 048302 DI 10.1103/PhysRevLett.95.048302 PG 4 WC Physics, Multidisciplinary SC Physics GA 947XG UT WOS:000230680000066 ER PT J AU Ogbuji, LU AF Ogbuji, LU TI Oxidation behavior of Cu-Cr environmental barrier coatings on Cu-8Cr-4Nb SO SURFACE & COATINGS TECHNOLOGY LA English DT Article DE Cu-Cr coatings; Cu-8Cr-4Nb substrate; oxidation behavior; Cr2O3 growth ID ALLOYS; COPPER AB Oxidation behavior of some Cu-Cr alloys (with 8.5-25.6 wt.% Cr, in both stand-alone coupons and spray coatings on Cu-8Cr-4Nb) was studied by TGA and cyclic oxidation. Judging by the more stringent cyclic oxidation results, protection of the substrate Cu-8Cr-4Nb was effective for the whole 10-h duration of testing up to 750 degrees C only for coatings with 21% or higher Cr. Similar protection was exhibited by Cu-17Cr only up to 650 degrees C, and only for < 3 h at 750 degrees C. In all cases the Cr2O3 subscale nucleated discretely (and always under a non-adherent scale of Cu oxides), and passive protection did not start until the nuclei joined into a continuous barrier and parabolic oxidation kinetics set in. The only protection achieved before that stage of Cr2O3 coalescence was via sacrificial oxidation of the coating. (c) 2005 Elsevier B.V. All rights reserved. C1 NASA, Glenn Res Ctr, QSS Inc, Cleveland, OH 44135 USA. RP Ogbuji, LU (reprint author), NASA, Glenn Res Ctr, QSS Inc, MS 106-1, Cleveland, OH 44135 USA. EM linus@ogbuji.net NR 19 TC 7 Z9 7 U1 0 U2 1 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0257-8972 J9 SURF COAT TECH JI Surf. Coat. Technol. PD JUL 22 PY 2005 VL 197 IS 2-3 BP 327 EP 335 DI 10.1016/j.surfcoat.2005.01.116 PG 9 WC Materials Science, Coatings & Films; Physics, Applied SC Materials Science; Physics GA 933XJ UT WOS:000229665900027 ER PT J AU Melott, AL Thomas, BC Hogan, DP Ejzak, LM Jackman, CH AF Melott, AL Thomas, BC Hogan, DP Ejzak, LM Jackman, CH TI Climatic and biogeochemical effects of a galactic gamma ray burst SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID LATE ORDOVICIAN; 2-DIMENSIONAL MODEL; ULTRAVIOLET-RADIATION; ATMOSPHERIC PCO(2); OZONE DEPLETION; MASS EXTINCTION; GLACIATION; TRANSPORT; EVENTS AB It is likely that one or more gamma ray bursts within our galaxy have strongly irradiated the Earth in the last Gy. This produces significant atmospheric ionization and dissociation, resulting in ozone depletion and DNA-damaging ultraviolet solar flux reaching the surface for up to a decade. Here we show the first detailed computation of two other significant effects. Visible opacity of NO2 is sufficient to reduce solar energy at the surface up to a few percent, with the greatest effect at the poles, which may be sufficient to initiate glaciation. Rainout of dilute nitric acid could have been important for a burst nearer than our conservative " nearest burst''. These results support the hypothesis that the characteristics of the Late Ordovician mass extinction are consistent with GRB initiation. C1 Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. NASA, Atmospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Melott, AL (reprint author), Univ Kansas, Dept Phys & Astron, 1251 Wescoe Hall Dr 1082, Lawrence, KS 66045 USA. EM melott@ku.edu RI Jackman, Charles/D-4699-2012 NR 30 TC 19 Z9 19 U1 3 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 21 PY 2005 VL 32 IS 14 AR L14808 DI 10.1029/2005GL023073 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 951GF UT WOS:000230916700004 ER PT J AU Colbert, EJM Strickland, DK Veilleux, S Weaver, KA AF Colbert, EJM Strickland, DK Veilleux, S Weaver, KA TI Extranuclear X-ray emission in the edge-on Seyfert galaxy NGC 2992 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 2992); galaxies : Seyfert; galaxies : spiral; X-rays : galaxies ID LARGE-SCALE OUTFLOWS; GRATING SPECTROMETER OBSERVATIONS; ACTIVE GALACTIC NUCLEI; NARROW-LINE REGION; NGC 2992; XMM-NEWTON; H-ALPHA; CHANDRA OBSERVATIONS; SPIRAL GALAXIES; HOT GAS AB We observed the edge-on Seyfert 1.9 galaxy NGC 2992 with the ACIS CCD array on the Chandra X-Ray Observatory and found several extranuclear (r greater than or similar to 3 '') X-ray nebulae within 4000 (6.3 kpc for our assumed distance of 32.5 Mpc) of the nucleus. The net X-ray luminosity from the extranuclear sources is similar to 2-3 x 10(39) ergs s(-1) in the 0.3-8.0 keV band. The X-ray core itself (r less than or similar to 1 '') is positioned at R.A. 9(h)45(m)41(s). 95, decl. -14 degrees 19'34 ''.8 (J2000.0) and has a remarkably simple power-law spectrum with photon index Gamma = 1.86 and intrinsic N-H = 7 x 10(21) cm(-2). The near-nuclear (3 '' less than or similar to r less than or similar to 18 '') Chandra spectrum is best modeled by three components: (1) a direct active galactic nucleus (AGN) component from the wings of the point-spread function or an electron-scattered AGN component, with Gamma fixed at 1.86, (2) cold Compton reflection of the AGN component with intrinsic absorption N-H similar to 10(22) cm(-2), with approximately the same 0.3-8.0 keV flux as the direct component, and (3) a 0.5 keV low-abundance (Z < 0.03 Z circle dot) thermal plasma, with similar to 10% of the flux of either of the first two components. The X-ray luminosity of the third component (the "soft excess'') is approximate to 1.4 x 10(40) ergs s(-1), or similar to 5 times that of all of the detected extranuclear X-ray sources. We suggest that most (similar to 75%-80%) of the soft excess emission originates from a region between radii of 100 and 300, which is not imaged in our observation due to severe CCD pileup. We also require the cold reflector to be positioned at least 100 (158 pc) from the nucleus, since there is no reflection component in the X-ray core spectrum. Much of the extranuclear X-ray emission is coincident with radio structures (nuclear radio bubbles and large-scale radio features), and its soft X-ray luminosity is generally consistent with luminosities expected from a starburst-driven wind (with the starburst scaled from L-FIR). However, the AGN in NGC 2992 seems equally likely to power the galactic wind in that object. Furthermore, AGN photoionization and photoexcitation processes could dominate the soft excess, especially the similar to 75%-80% that is not imaged by our observations. C1 Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Colbert, EJM (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Homewood Campus,3400 N Charles St, Baltimore, MD 21218 USA. NR 64 TC 10 Z9 10 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2005 VL 628 IS 1 BP 113 EP 128 DI 10.1086/430734 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 948MR UT WOS:000230720500009 ER PT J AU Chandar, R Leitherer, C Tremonti, CA Calzetti, D Aloisi, A Meurer, GR de Mello, D AF Chandar, R Leitherer, C Tremonti, CA Calzetti, D Aloisi, A Meurer, GR de Mello, D TI The stellar content of nearby star-forming galaxies. III. Unravelling the nature of the diffuse ultraviolet light SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : starburst; galaxies : stellar content; ultraviolet : galaxies ID SPECTRAL ENERGY-DISTRIBUTION; SPACE-TELESCOPE OBSERVATIONS; INITIAL MASS FUNCTION; EVOLUTIONARY SEQUENCES; POSTSTARBURST GALAXY; RADIATIVE OPACITIES; MAGELLANIC CLOUDS; MOLECULAR CLOUDS; HIGH-REDSHIFT; CLUSTERS AB We investigate the nature of the diffuse intracluster ultraviolet light seen in 12 local starburst galaxies, using long-slit ultraviolet spectroscopy obtained with the Space Telescope Imaging Spectrograph (STIS) aboard the Hubble Space Telescope (HST). We take this faint intracluster light to be the field in each galaxy and compare its spectroscopic signature with Starburst99 evolutionary synthesis models and with neighboring star clusters. Our main result is that the diffuse ultraviolet light in 11 of the 12 starbursts lacks the strong O star wind features that are clearly visible in spectra of luminous clusters in the same galaxies. The difference in stellar features dominating cluster and field spectra indicates that the field light comes primarily from a different stellar population and not from scattering of UV photons originating in the massive clusters. A cut along the spatial direction of the UV spectra establishes that the field light is not smooth but rather shows numerous "bumps and wiggles.'' Roughly 30%-60% of these faint peaks seen in field regions of the closest (< 4 Mpc) starbursts appear to be resolved, suggesting a contribution from superpositions of stars and/or faint star clusters. Complementary WFPC2 UVI imaging for the three nearest target galaxies, NGC 4214, NGC 4449, and NGC 5253, is used to obtain a broader picture and establish that all three galaxies have a dispersed population of unresolved, luminous blue sources. Because the field spectra are dominated by B stars, we suggest that the individual sources observed in the WFPC2 images are individual B stars (rather than O stars) or small star clusters. We consider several scenarios to understand the lack of observed massive stars in the field and their implications for the origin of the field stellar population. If the field stellar populations formed in situ, the field must have either an IMF that is steeper than Salpeter (alpha similar to -3.0 to -3.5) or a Salpeter slope with an upper mass cutoff of 30-50 M circle dot. If star formation occurs primarily in star clusters, the field could be composed of older, faded clusters and/or a population that is coeval with the luminous clusters but lower in mass. We use these benchmark populations to place constraints on the field stellar population origin. Although the field probably includes stars of different ages, the UV light is dominated by the youngest stellar populations in the field. If the field is composed of older, dissolving clusters, we estimate that star clusters (regardless of mass) need to dissolve on timescales 7-10 Myr to create the field. If the field is composed of young clusters that fall below the detection limit of individual sources in our spectroscopy, they would have to be several hundred solar masses or less, in order to be deficient in O stars, despite their extreme youth. C1 Space Telescope Sci Inst, Baltimore, MD 21218 USA. Steward Observ, Tucson, AZ 85721 USA. Johns Hopkins Univ, Baltimore, MD 21218 USA. Goddard Space Flight Ctr, Lab Astron & Solar Phys, Greenbelt, MD 20771 USA. Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. RP Chandar, R (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM rupali@stsci.edu NR 62 TC 43 Z9 43 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2005 VL 628 IS 1 BP 210 EP 230 DI 10.1086/430592 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 948MR UT WOS:000230720500017 ER PT J AU Young, KE Harvey, PM Brooke, TY Chapman, N Kauffmann, J Bertoldi, F Lai, SP Alcala, J Bourke, TL Spiesman, W Allen, LE Blake, GA Evans, NJ Koerner, DW Mundy, LG Myers, PC Padgett, DL Salinas, A Sargent, AI Stapelfeldt, KR Teuben, P van Dishoeck, EF Wahhaj, Z AF Young, KE Harvey, PM Brooke, TY Chapman, N Kauffmann, J Bertoldi, F Lai, SP Alcala, J Bourke, TL Spiesman, W Allen, LE Blake, GA Evans, NJ Koerner, DW Mundy, LG Myers, PC Padgett, DL Salinas, A Sargent, AI Stapelfeldt, KR Teuben, P van Dishoeck, EF Wahhaj, Z TI The Spitzer c2d survey of large, nearby, interstellar clouds. I. Chamaeleon II observed with MIPS SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; ISM : clouds; stars : formation ID MULTIBAND IMAGING PHOTOMETER; YOUNG STELLAR OBJECTS; MAIN-SEQUENCE STARS; DARK-CLOUD; MOLECULAR CLOUDS; REDUCTION ALGORITHMS; T-TAURI; HH 54; CORES; DUST AB We present maps of over 1.5 deg(2) in Chamaeleon (Cha) II at 24, 70, and 160 mu m observed with the Spitzer Space Telescope Multiband Imaging Photometer for Spitzer (MIPS) and a 1.2 deg(2) millimeter map from SIMBA on the Swedish-ESO Submillimetre Telescope (SEST). The c2d Spitzer Legacy Team's data reduction pipeline is described in detail. Over 1500 24 mu m sources and 41 70 mu m sources were detected by MIPS with fluxes greater than 10 sigma. More than 40 potential YSOs are identified with a MIPS and 2MASS color-color diagram and by their spectral indices, including two previously unknown sources with 24 mu m excesses. Our new SIMBA millimeter map of Cha II shows that only a small fraction of the gas is in compact structures with high column densities. The extended emission seen by MIPS is compared with previous CO observations. Some selected interesting sources, including two detected at 1 mm, associated with Cha II are discussed in detail, and their SEDs are presented. The classification of these sources using MIPS data is found to be consistent with that of previous studies. C1 Univ Texas, Dept Astron, Austin, TX 78712 USA. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Univ Bonn, Inst Radioastron, D-53121 Bonn, Germany. Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. Spitzer Sci Ctr, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Young, KE (reprint author), Univ Texas, Dept Astron, 1 Univ Stn C1400, Austin, TX 78712 USA. EM kaisa@astro.as.utexas.edu; pmh@astro.as.utexas.edu; tyb@astro.caltech.edu; chapman@astro.umd.edu; jkauffma@mpifr-bonn.mpg.de; bertoldi@uni-bonn.de; slai@astro.umd.edu; jmae@sun1.na.astro.it; tbourke@cfa.harvard.edu; spies@astro.as.utexas.edu; leallen@cfa.harvard.edu; gab@gps.caltech.edu; nje@astro.as.utexas.edu; koerner@physics.nau.edu; lgm@astro.umd.edu; pmyers@cfa.harvard.edu; dlp@ipac.caltech.edu; afs@astro.caltech.edu; krs@exoplanet.jpl.nasa.gov; zwahhaj@physics.nau.edu RI Stapelfeldt, Karl/D-2721-2012 NR 50 TC 44 Z9 44 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 JUL 20 PY 2005 VL 628 IS 1 BP 283 EP 297 DI 10.1086/430597 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 948MR UT WOS:000230720500023 ER PT J AU Shaklan, SB Green, JJ AF Shaklan, SB Green, JJ TI Low-order aberration sensitivity of eighth-order coronagraph masks SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; planetary systems; techniques : high angular resolution ID PLANET-FINDER CORONAGRAPH; NOTCH-FILTER MASKS; OPTICAL ABERRATIONS; DESIGNS; PUPIL AB In a recent paper, Kuchner, Crepp, and Ge describe new image-plane coronagraph mask designs that reject to eighth order the leakage of starlight caused by image motion at the mask, resulting in a substantial relaxation of image centroiding requirements compared to previous fourth-order and second-order masks. They also suggest that the new masks are effective at rejecting leakage caused by low-order aberrations (e.g., focus, coma, and astigmatism). In this paper, we derive the sensitivity of eighth-order masks to aberrations of any order and provide simulations of coronagraph behavior in the presence of optical aberrations. We find that the masks leak light as the fourth power of focus, astigmatism, coma, and trefoil. This has tremendous performance advantages for the Terrestrial Planet Finder Coronagraph. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Shaklan, SB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM stuart.shaklan@jpl.nasa.gov; joseph.j.green@jpl.nasa.gov NR 17 TC 26 Z9 26 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 JUL 20 PY 2005 VL 628 IS 1 BP 474 EP 477 DI 10.1086/430204 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 948MR UT WOS:000230720500039 ER PT J AU Su, KYL Rieke, GH Misselt, KA Stansberry, JA Moro-Martin, A Stapelfeldt, KR Werner, MW Trilling, DE Bendo, GJ Gordon, KD Hines, DC Wyatt, MC Holland, WS Marengo, M Megeath, ST Fazio, GG AF Su, KYL Rieke, GH Misselt, KA Stansberry, JA Moro-Martin, A Stapelfeldt, KR Werner, MW Trilling, DE Bendo, GJ Gordon, KD Hines, DC Wyatt, MC Holland, WS Marengo, M Megeath, ST Fazio, GG TI The vega debris disk: A surprise from Spitzer SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared : stars; planetary systems; stars : individual (Vega) ID MULTIBAND IMAGING PHOTOMETER; MAIN-SEQUENCE STARS; RADIATION PRESSURE; SPACE-TELESCOPE; REDUCTION ALGORITHMS; ACCRETION DISKS; SOLAR-SYSTEM; DUSTY DEBRIS; GRAINS; SUBMILLIMETER AB We present high spatial resolution mid- and far-infrared images of the Vega debris disk obtained with the Multiband Imaging Photometer for Spitzer ( MIPS). The disk is well resolved, and its angular size is much larger than found previously. The radius of the disk is at least 43" (330 AU), 70" (543 AU), and 105" (815 AU) in extent at 24, 70, and 160 mu m, respectively. The disk images are circular, smooth, and without clumpiness at all three wavelengths. The radial surface brightness profiles follow radial power laws of r(-3) or r(-4) and imply an inner boundary at a radius of 11" +/- 2" (86 AU). Assuming an amalgam of amorphous silicate and carbonaceous grains, the disk can be modeled as an axially symmetric and geometrically thin disk, viewed face-on, with the surface particle number density following an inverse radial power law. The disk radiometric properties are consistent with a range of models using grains of sizes similar to 1 to similar to 50 mu m. The exact minimum and maximum grain size limits depend on the adopted grain composition. However, all of these models require an r(-1) surface number density profile and a total mass of (3 +/- 1.5) x 10(-3) M-circle plus in grains. We find that a ring, containing grains larger than 180 mu m and at radii of 86 - 200 AU from the star, can reproduce the observed 850 mu m flux, while its emission does not violate the observed MIPS profiles. This ring could be associated with a population of larger asteroidal bodies analogous to our own Kuiper Belt. Cascades of collisions starting with encounters among these large bodies in the ring produce the small debris that is blown outward by radiation pressure to much larger distances, where we detect its thermal emission. The relatively short lifetime (< 1000 yr) of these small grains and the observed total mass, similar to 3 x 10(-3) M-circle plus, set a lower limit on the dust production rate, similar to 10(15) g s(-1). This rate would require a very massive asteroidal reservoir for the dust to be produced in a steady state throughout Vega's life. Instead, we suggest that the disk we imaged is ephemeral and that we are witnessing the aftermath of a large and relatively recent collisional event, and a subsequent collisional cascade. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Space Sci Inst, Boulder, CO 80301 USA. Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Su, KYL (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM ksu@as.arizona.edu RI Stapelfeldt, Karl/D-2721-2012; OI Su, Kate/0000-0002-3532-5580 NR 41 TC 144 Z9 144 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 JUL 20 PY 2005 VL 628 IS 1 BP 487 EP 500 DI 10.1086/430819 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 948MR UT WOS:000230720500041 ER PT J AU Halasinski, TM Salama, F Allamandola, LJ AF Halasinski, TM Salama, F Allamandola, LJ TI Investigation of the ultraviolet, visible, and near-infrared absorption spectra of hydrogenated polycyclic aromatic hydrocarbons and their cations SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM : lines and bands; ISM : molecules; methods : laboratory; molecular data; ultraviolet : ISM ID DIFFUSE INTERSTELLAR BANDS; PAH CATIONS; GAS-PHASE; ASTROPHYSICAL IMPLICATIONS; NAPHTHALENE CATION; ELECTRONIC-SPECTRA; SPECTROSCOPY; EMISSION; IONS; EXTINCTION AB The formation and the presence of PAHs containing excess H atoms, or hydrogenated PAHs (H-n-PAHs) in interstellar clouds has recently been discussed. It has been suggested that H-n-PAHs contribute to the IR emission bands and that they might be among the molecular precursors of the carbon particles that cause the interstellar UV extinction curve. The spectroscopy of H-n-PAHs is investigated, and the implications for interstellar spectra are discussed. The UV, visible, and near-IR absorption spectra of a series of H-n-PAHs and their photoproducts formed by vacuum UV irradiation were measured for the first time in inert-gas (neon) matrices at 5 K. It is shown that the spectra of both the neutral H-n-PAH and cationic H-n-PAH(+) species exhibit vibronic band systems with similar spectral positions and relative spectral intensities to their nonhydrogenated PAH chromophore counterparts. The results are discussed in the context of the nature of the origin of the diffuse interstellar bands. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Salama, F (reprint author), NASA, Ames Res Ctr, Mail Stop 245-6, Moffett Field, CA 94035 USA. EM farid.salama@nasa.gov RI Salama, Farid/A-8787-2009 OI Salama, Farid/0000-0002-6064-4401 NR 51 TC 30 Z9 30 U1 2 U2 25 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 JUL 20 PY 2005 VL 628 IS 1 BP 555 EP 566 DI 10.1086/430631 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 948MR UT WOS:000230720500047 ER PT J AU Engelbracht, CW Gordon, KD Rieke, GH Werner, MW Dale, DA Latter, WB AF Engelbracht, CW Gordon, KD Rieke, GH Werner, MW Dale, DA Latter, WB TI Metallicity effects on mid-infrared colors and the 8 mu m PAH emission in galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : ISM; infrared : galaxies ID SPITZER-SPACE-TELESCOPE; STAR-FORMING GALAXIES; SPECTRAL ENERGY-DISTRIBUTION; INFRARED SPECTROGRAPH IRS; BLUE COMPACT GALAXIES; METAL-POOR GALAXY; 24 MICRON SOURCES; ELEMENT ABUNDANCES; 1ST-LOOK SURVEY; DWARF GALAXIES AB We examine colors from 3.6 to 24 mm as a function of metallicity (O/H) for a sample of 34 galaxies. The galaxies range over 2 orders of magnitude in metallicity. They display an abrupt shift in the 8 mu m-to-24 mu m color for metallicities between one-third and one-fifth of the solar value. The mean 8-to-24 mu m flux density ratio below and above 12 + log (O/H) p 8.2 is 0.08 +/- 0.04 and 0.70 +/- 0.53, respectively. We use mid-IR colors and spectroscopy to demonstrate that the shift is primarily due to a decrease in the 8 mm flux density, as opposed to an increase in the 24 mm flux density. This result is most simply interpreted as being due to a weakening at low metallicity of the mid-IR emission bands usually attributed to PAHs (polycyclic aromatic hydrocarbons) relative to the small-grain dust emission. However, existing empirical spectral energy distribution models cannot account for the observed short-wavelength (below 8 mm) colors of the low-metallicity galaxies merely by reducing the strength of the PAH features; some other emission source (e. g., hot dust) is required. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Jet Prop Lab, Pasadena, CA 91109 USA. Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RP Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM cengelbracht@as.arizona.edu NR 56 TC 170 Z9 169 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 JUL 20 PY 2005 VL 628 IS 1 BP L29 EP L32 DI 10.1086/432613 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 948MU UT WOS:000230720800008 ER PT J AU Davis, CP Wu, DL Emde, C Jiang, JH Cofield, RE Harwood, RS AF Davis, CP Wu, DL Emde, C Jiang, JH Cofield, RE Harwood, RS TI Cirrus induced polarization in 122 GHz aura Microwave Limb Sounder radiances SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID RADIATIVE-TRANSFER; ICE; ORIENTATION; SCATTERING; PARTICLE; CLOUDS AB Previous simulation studies have outlined the possibility of significant polarization signals in microwave limb sounding due to horizontally aligned ice crystals in cirrus clouds. From the recently launched Aura MLS instrument, we present the first polarized microwave limb sounding observations of cirrus clouds. We also present polarized radiative transfer simulations, which show qualitative agreement with these observations, and indicate the limits to which aligned non-spherical particles are influencing bulk optical properties of cirrus clouds at microwave wavelengths. Although 122 GHz is not ideal for cloud measurements due to strong O-2 absorption, data and simulations suggest that preferential crystal orientation is causing small, but noticeable, partial vertical polarization, which can be replicated in simulations by considering all particles as horizontally aligned oblate spheroids with aspect ratios of around 1.2 +/- 0.15. C1 Univ Edinburgh, Inst Atmospher & Environm Sci, Edinburgh EH9 3JZ, Midlothian, Scotland. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Bremen, Inst Environm Phys, D-28359 Bremen, Germany. RP Davis, CP (reprint author), Univ Edinburgh, Inst Atmospher & Environm Sci, Edinburgh EH9 3JZ, Midlothian, Scotland. EM cdavis@staffmail.ed.ac.uk RI Emde, Claudia/B-5447-2010; Wu, Dong/D-5375-2012 NR 13 TC 19 Z9 20 U1 1 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 20 PY 2005 VL 32 IS 14 AR L14806 DI 10.1029/2005GL022681 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 951GE UT WOS:000230916600002 ER PT J AU Vogel, SW Tulaczyk, S Kamb, B Engelhardt, H Carsey, FD Behar, AE Lane, AL Joughin, I AF Vogel, SW Tulaczyk, S Kamb, B Engelhardt, H Carsey, FD Behar, AE Lane, AL Joughin, I TI Subglacial conditions during and after stoppage of an Antarctic Ice Stream: Is reactivation imminent? SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID WEST ANTARCTICA; SURGE MECHANISM; SHEET; STAGNATION; BENEATH; OSCILLATIONS; SEDIMENTS; GLACIERS; BALANCE; REGIONS AB Borehole observations from the base of the West-Antarctic Ice Sheet (WAIS) reveal the presence of a 10 to 15 m thick accretionary basal ice layer in the upstream area of Kamb Ice Stream (KIS). This ice layer has formed over a time of several thousand years by freeze-on of subglacial water to the ice base and has recorded during this time basal conditions upstream of its current location. Analysis of samples and videos sequences from boreholes drilled to the bottom of KIS confirms that KIS-stoppage was due to basal freeze-on and that relubrication of the ice stream is well underway. These results further suggest that ice stream cyclicity may be shorter than expected (1000s of years) and that a restart of KIS may be imminent within decades to centuries. C1 Univ Calif Santa Cruz, Dept Earth Sci, Santa Cruz, CA 95064 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Vogel, SW (reprint author), Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH 43210 USA. EM svogel@geol.niu.edu RI Joughin, Ian/A-2998-2008; Vogel, Stefan/I-1963-2014; OI Joughin, Ian/0000-0001-6229-679X; Vogel, Stefan W./0000-0002-4350-7130 NR 30 TC 36 Z9 35 U1 0 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 JUL 20 PY 2005 VL 32 IS 14 AR L14502 DI 10.1029/2005GL022563 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 951GE UT WOS:000230916600001 ER PT J AU Siegel, DA Maritorena, S Nelson, NB Behrenfeld, MJ AF Siegel, DA Maritorena, S Nelson, NB Behrenfeld, MJ TI Independence and interdependencies among global ocean color properties: Reassessing the bio-optical assumption SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID CHLOROPHYLL-A; SARGASSO SEA; LIGHT-SCATTERING; ORGANIC-MATTER; CASE-1 WATERS; TIME-SERIES; PHYTOPLANKTON; MODEL; ABSORPTION; SPECTRA AB [1] The bio-optical assumption states that ocean optical properties should covary with the chlorophyll concentration. However, chlorophyll is not the only constituent capable of absorbing and scattering light as phytoplankton, detrital particles, colored dissolved organic material ( CDOM), and suspended solids all contribute independently to ocean color. Here we employ a semi-analytical ocean color algorithm, the Garver-Siegel-Maritorena model (GSM01), to decompose ocean color imagery from the Sea-viewing Wide Field of view Sensor (SeaWiFS) into optically relevant components for phytoplankton absorption ( related to the chlorophyll concentration, Chl), colored non-algal absorption and particulate backscatter. Semi-analytical Chl retrievals are consistent with available open ocean observations but show important differences compared with the standard SeaWiFS algorithm (OC4v4). These differences may be accounted for by the absorption due to colored detrital materials (CDM; the sum of colored dissolved organic material and detrital particulates). Values of CDM are a large and variable fraction of the total non-water absorption at 440 nm varying from 30 to 40% in the subtropical gyres to more than 60% at high latitudes. Retrievals of particulate backscatter (BBP) vary comparatively little. In the tropical and subtropical oceans, changes in BBP are largely unrelated to Chl, while at higher latitudes, BBP increases mirror changes in Chl. For much of the ocean, alterations in the relationship between BBP and Chl are consistent with a physiological response by phytoplankton to changes in mixed layer light, nutrients, and temperature. Regional scale correspondences among the three ocean color properties illustrate both independent and interdependent variations which can be explained by assessing the regional scale forcing mechanisms driving changes in ocean color properties. C1 Univ Calif Santa Barbara, Inst Computat Earth Syst Sci, Santa Barbara, CA 93106 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Siegel, DA (reprint author), Univ Calif Santa Barbara, Inst Computat Earth Syst Sci, Santa Barbara, CA 93106 USA. EM davey@icess.ucsb.edu RI Siegel, David/C-5587-2008; Nelson, Norman/B-7343-2014 OI Nelson, Norman/0000-0003-1767-7598 NR 50 TC 98 Z9 99 U1 5 U2 18 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 JUL 20 PY 2005 VL 110 IS C7 AR C07011 DI 10.1029/2004JC002527 PG 14 WC Oceanography SC Oceanography GA 951GX UT WOS:000230918600001 ER PT J AU Bjerklie, DM Moller, D Smith, LC Dingman, SL AF Bjerklie, DM Moller, D Smith, LC Dingman, SL TI Estimating discharge in rivers using remotely sensed hydraulic information SO JOURNAL OF HYDROLOGY LA English DT Article DE remote sensing of river discharge; river channel hydraulics; synthetic aperture radar; discharge estimates from water-surface velocity; discharge estimates from channel width and slope ID IMAGERY AB A methodology to estimate in-bank river discharge exclusively from remotely sensed hydraulic data is developed. Water-surface width and maximum channel width measured from 26 aerial and digital orthophotos of 17 single channel rivers and 41 SAR images of three braided rivers were coupled with channel slope data obtained from topographic maps to estimate the discharge. The standard error of the discharge estimates were within a factor of 1.5-2 (50-100%) of the observed, with the mean estimate accuracy within 10%. This level of accuracy was achieved using calibration functions developed from observed discharge. The calibration functions use reach specific geomorphic variables, the maximum channel width and the channel slope, to predict a correction factor. The calibration functions are related to channel type. Surface velocity and width information, obtained from a single C-band image obtained by the Jet Propulsion Laboratory's (JPL's) AirSAR was also used to estimate discharge for a reach of the Missouri River. Without using a calibration function, the estimate accuracy was +72% of the observed discharge, which is within the expected range of uncertainty for the method. However, using the observed velocity to calibrate the initial estimate improved the estimate accuracy to within +10% of the observed. Remotely sensed discharge estimates with accuracies reported in this paper could be useful for regional or continental scale hydrologic studies, or in regions where ground-based data is lacking. (c) 2004 Elsevier B.V. All rights reserved. C1 Univ New Hampshire, Dept Earth Sci, Durham, NH USA. CALTECH, Jet Propuls Lab, Pasadena, CA USA. Univ Calif Berkeley, Dept Geog, Berkeley, CA 94720 USA. RP Bjerklie, DM (reprint author), US Geol Survey, 101 Pitkin St, E Hartford, CT 06108 USA. EM dmbjerkl@usgs.gov; delwyn.k.moller@jpl.nasa.gov; lsmith@geog.ucla.edu; ldingman@cisunix.unh.edu RI Smith, Laurence/E-7785-2012 OI Smith, Laurence/0000-0001-6866-5904 NR 35 TC 85 Z9 88 U1 1 U2 17 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-1694 J9 J HYDROL JI J. Hydrol. PD JUL 19 PY 2005 VL 309 IS 1-4 BP 191 EP 209 DI 10.1016/j.jhydrol.2004.11.022 PG 19 WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources SC Engineering; Geology; Water Resources GA 938SR UT WOS:000230023700014 ER PT J AU Nguyen, P Ng, HT Meyyappan, M AF Nguyen, P Ng, HT Meyyappan, M TI Catalyst metal selection for synthesis of inorganic nanowires SO ADVANCED MATERIALS LA English DT Article ID FIELD-EFFECT TRANSISTOR; MOLTEN GALLIUM; OXIDE NANOWIRE; GROWTH; TRANSPORT AB Growth of inorganic nanowires mediated by alternatives to gold using a vapor-liquid-solid mechanism is reported. Fifteen metals have been studied as catalysts, with several of them yielding nanowires (see Figure). The nanowire growth density is a function of melting temperature of the catalyst metals, as the catalyst material serves as the soft template for incorporation of the vapor species into the nanowire. C1 NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Meyyappan, M (reprint author), Univ So Calif, Keck Sch Med, Los Angeles, CA 90033 USA. EM meyya@orbit.arc.nasa.gov NR 19 TC 66 Z9 67 U1 1 U2 14 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0935-9648 J9 ADV MATER JI Adv. Mater. PD JUL 18 PY 2005 VL 17 IS 14 BP 1773 EP + DI 10.1002/adma.200401717 PG 6 WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA 947ZE UT WOS:000230685000015 ER PT J AU Gutsev, GL Mochena, MD Bauschlicher, CW AF Gutsev, GL Mochena, MD Bauschlicher, CW TI Interaction of water with small Fe-n clusters SO CHEMICAL PHYSICS LA English DT Article DE iron clusters; water; density functional theory; dissociation ID WALLED CARBON NANOTUBES; DENSITY-FUNCTIONAL THEORY; COLLISION-INDUCED DISSOCIATION; METAL POSITIVE-IONS; GAUSSIAN-BASIS SETS; GAS-PHASE; BINDING-ENERGIES; IONIZATION ENERGIES; HYDROGEN-PRODUCTION; MATRIX-ISOLATION AB The electronic and geometrical structures of clusters formed by a single water molecule and small iron clusters Fe., Fe-n(-) and Fe-n(+)', for n = 1-4, are studied using density functional theory. We found that FeH2O and Fe2H2O possess a large number of isomers with different geometries, which are close in total energy to the corresponding ground states. In accord with previous computations, the ground state of FeH2O has an inserted HFeOH geometry and water remains intact in the ground state of the FeH2O+ cation. Beginning with Fe2H2O, the lowest energy states correspond to isomers with a fully dissociated water molecule, except for the ground state of the Fe2H2O+ cation that contains an OH group. Except for FeH2O+ and Fe4H2O+, the hydrogen desorption energies (FenH2O -> FenO + H-2) are smaller than the water desorption energies (FenH2O -> Fe-n + H2O) for all neutral and ionic species considered and are relatively low, being about 1.5 eV. (c) 2005 Elsevier B.V. All rights reserved. C1 Florida A&M Univ, Dept Phys, Tallahassee, FL 32307 USA. NASA Ames Res Ctr, Moffett Field, CA 94035 USA. RP Gutsev, GL (reprint author), Florida A&M Univ, Dept Phys, Tallahassee, FL 32307 USA. EM gennady.gutsev@famu.edu NR 51 TC 15 Z9 15 U1 0 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0301-0104 J9 CHEM PHYS JI Chem. Phys. PD JUL 18 PY 2005 VL 314 IS 1-3 BP 291 EP 298 DI 10.1016/j.chemphys.2005.03.014 PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 930CD UT WOS:000229392500028 ER PT J AU Meyerowitz, EM Reddy, V Heisler, M Jonsson, H Shapiro, B Mjolsness, E AF Meyerowitz, EM Reddy, V Heisler, M Jonsson, H Shapiro, B Mjolsness, E TI Dynamic genetics: A new view of plant growth. SO DEVELOPMENTAL BIOLOGY LA English DT Meeting Abstract CT 64th Annual Meeting of the Society-for-Development-Biology CY JUL 27-AUG 01, 2005 CL San Francisco, CA SP Soc Dev Biol C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. Lund Univ, Lund, Sweden. Univ Calif Irvine, Irvine, CA USA. RI Meyerowitz, Elliot/A-7118-2009 NR 0 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 0012-1606 J9 DEV BIOL JI Dev. Biol. PD JUL 15 PY 2005 VL 283 IS 2 MA 64 BP 587 EP 588 PG 2 WC Developmental Biology SC Developmental Biology GA 947YS UT WOS:000230683800085 ER PT J AU Sylvester, TA Dali, LA Domingo, CR AF Sylvester, TA Dali, LA Domingo, CR TI An analysis of pluripotency of the dorsal ectoderm and mesoderm in Xenopus. SO DEVELOPMENTAL BIOLOGY LA English DT Meeting Abstract CT 64th Annual Meeting of the Society-for-Development-Biology CY JUL 27-AUG 01, 2005 CL San Francisco, CA SP Soc Dev Biol C1 San Francisco State Univ, San Francisco, CA 94132 USA. NASA, Ames Res Ctr, Moffatt Field, CA USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0012-1606 J9 DEV BIOL JI Dev. Biol. PD JUL 15 PY 2005 VL 283 IS 2 MA 263 BP 629 EP 629 PG 1 WC Developmental Biology SC Developmental Biology GA 947YS UT WOS:000230683800283 ER PT J AU Torrejon, ME Gupta, R Walter, K Gennuso, S Reinsch, S AF Torrejon, ME Gupta, R Walter, K Gennuso, S Reinsch, S TI The KIAA0888 homolog of Xenopus tropicalis is essential for early embryogenesis. SO DEVELOPMENTAL BIOLOGY LA English DT Meeting Abstract CT 64th Annual Meeting of the Society-for-Development-Biology CY JUL 27-AUG 01, 2005 CL San Francisco, CA SP Soc Dev Biol C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0012-1606 J9 DEV BIOL JI Dev. Biol. PD JUL 15 PY 2005 VL 283 IS 2 MA 572 BP 692 EP 692 PG 1 WC Developmental Biology SC Developmental Biology GA 947YS UT WOS:000230683800588 ER PT J AU Szego, K Bebesi, Z Erdos, G Foldy, L Crary, F McComas, DJ Young, DT Bolton, S Coates, AJ Rymer, AM Hartle, RE Sittler, EC Reisenfeld, D Bethelier, JJ Johnson, RE Smith, HT Hill, TW Vilppola, J Steinberg, J Andre, N AF Szego, K Bebesi, Z Erdos, G Foldy, L Crary, F McComas, DJ Young, DT Bolton, S Coates, AJ Rymer, AM Hartle, RE Sittler, EC Reisenfeld, D Bethelier, JJ Johnson, RE Smith, HT Hill, TW Vilppola, J Steinberg, J Andre, N TI The global plasma environment of Titan as observed by Cassini Plasma Spectrometer during the first two close encounters with Titan SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MHD MODEL; VOYAGER-1 AB The Cassini spacecraft flew by Titan on October 26, 2004 and December 13, 2004. In both cases it entered the ionosphere of Titan, allowing exploration of its plasma environment. Using observations from the Cassini Plasma Spectrometer (CAPS) and the Cassini magnetometer along the inbound legs of both flybys, we examine Titan's global plasma environment. On both occasions CAPS detected plasma populations distinct from those of the Kronian magnetosphere at about 1 - 1.5 Saturn radii from the moon. Closer to Titan CAPS observed drifting ion ring distributions originating from Titan and, in addition, a corotating flow that was significantly decelerated around the moon due to mass loading. Near the moon, but above the ionosphere, very cold plasma was dominant. We also compare the CAPS data to those of Voyager 1. C1 KFKI Res Inst Particle & Nucl Phys, H-1121 Budapest, Hungary. SW Res Inst, San Antonio, TX 78228 USA. UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Montana, Dept Phys & Astron, Missoula, MT 59812 USA. Ctr Etud Environm Terr & Planetaires, F-94100 St Maur des Fosses, France. Univ Virginia, Charlottesville, VA 22903 USA. Rice Univ, Dept Space Phys & Astron, Houston, TX 77005 USA. Univ Oulu, FIN-90014 Oulu, Finland. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France. RP Szego, K (reprint author), KFKI Res Inst Particle & Nucl Phys, Konkoly Thege Str 29-33,Bldg 3, H-1121 Budapest, Hungary. EM szego@rmki.kfki.hu RI Coates, Andrew/C-2396-2008; Reisenfeld, Daniel/F-7614-2015; Smith, Howard/H-4662-2016 OI Coates, Andrew/0000-0002-6185-3125; Smith, Howard/0000-0003-3537-3360 NR 13 TC 31 Z9 31 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 JUL 15 PY 2005 VL 32 IS 20 AR L20S05 DI 10.1029/2005GL022646 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 950CF UT WOS:000230834500001 ER PT J AU Boccippio, DJ Petersen, WA Cecil, DJ AF Boccippio, DJ Petersen, WA Cecil, DJ TI The tropical convective spectrum. Part I: Archetypal vertical structures SO JOURNAL OF CLIMATE LA English DT Article ID OPTICAL TRANSIENT DETECTOR; TRMM PRECIPITATION RADAR; ICE-SCATTERING SIGNATURE; PASSIVE MICROWAVE; LIGHTNING CHARACTERISTICS; PROFILING ALGORITHM; TOGA COARE; VARIABILITY; RAINFALL; SYSTEMS AB A taxonomy of tropical convective and stratiform vertical structures is constructed through cluster analysis of 3 yr of Tropical Rainfall Measuring Mission (TRMM) "warm-season" (surface temperature greater than 10 degrees C) precipitation radar (PR) vertical profiles, their surface rainfall, and associated radar-based classifiers (convective/stratiform and brightband existence). Twenty-five archetypal profile types are identified, including nine convective types, eight stratiform types, two mixed types, and six anvil/fragment types (nonprecipitating anvils and sheared deep convective profiles). These profile types are then hierarchically clustered into 10 similar families, which can be further combined, providing an objective and physical reduction of the highly multivariate PR data space that retains vertical structure information. The taxonomy allows for description of any storm or local convective spectrum by the profile types or families. The analysis provides a quasi-independent corroboration of the TRMM 2A23 convective/stratiform classification. The global frequency of occurrence and contribution to rainfall for the profile types are presented, demonstrating primary rainfall contribution by midlevel glaciated convection (27%) and similar depth decaying/stratiform stages (28%-31%). Profiles of these types exhibit similar 37- and 85-GHz passive microwave brightness temperatures but differ greatly in their frequency of occurrence and mean rain rates, underscoring the importance to passive microwave rain retrieval of convective/stratiform discrimination by other means, such as polarization or texture techniques, or incorporation of lightning observations. Close correspondence is found between deep convective profile frequency and annualized lightning production, and pixel-level lightning occurrence likelihood directly tracks the estimated mean ice water path within profile types. C1 NASA, George C Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Dept Earth Sci, Huntsville, AL 35812 USA. Univ Alabama, Huntsville, AL 35899 USA. RP Boccippio, DJ (reprint author), NASA, George C Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Dept Earth Sci, SD-60, Huntsville, AL 35812 USA. EM Dennis.Boccippio@nasa.gov NR 36 TC 18 Z9 18 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 JUL 15 PY 2005 VL 18 IS 14 BP 2744 EP 2769 DI 10.1175/JCLI3335.1 PG 26 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 955TV UT WOS:000231251400015 ER PT J AU Minnis, P AF Minnis, P TI Contrails, cirrus trends, and climate - Reply SO JOURNAL OF CLIMATE LA English DT Editorial Material ID TEMPERATURE TRENDS; IMPACT C1 NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA. RP Minnis, P (reprint author), NASA, Langley Res Ctr, Climate Sci Branch, MS 420, Hampton, VA 23681 USA. EM p.minis@nasa.gov RI Minnis, Patrick/G-1902-2010 OI Minnis, Patrick/0000-0002-4733-6148 NR 12 TC 2 Z9 2 U1 1 U2 1 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 JUL 15 PY 2005 VL 18 IS 14 BP 2783 EP 2784 DI 10.1175/JCLI3434.1 PG 2 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 955TV UT WOS:000231251400021 ER PT J AU Rastatter, L Hesse, M Kuznetsova, M Sigwarth, JB Raeder, J Gombosi, TI AF Rastatter, L Hesse, M Kuznetsova, M Sigwarth, JB Raeder, J Gombosi, TI TI Polar cap size during 14-16 July 2000 (Bastille Day) solar coronal mass ejection event: MHD modeling and satellite imager observations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID INTERPLANETARY MAGNETIC-FIELD; EXPLORER 12 OBSERVATIONS; GLOBAL SIMULATION; MAGNETOSPHERE; IONOSPHERE; SUBSTORM; MAGNETOHYDRODYNAMICS; RECONNECTION; SPACECRAFT; CHALLENGE AB This study investigates the development of the polar cap area as simulated by global magnetohydrodynamic models of the Earth's magnetosphere during the 14-16 July 2000 (Bastille Day) event. Around 1440 UT on 15 July, a magnetic cloud hit the magnetosphere and in the following hours high levels of activity in the magnetosphere and ionosphere were driven by the frequent changes in solar wind conditions. We compare the size of the polar cap ( region of open magnetic field lines) as computed with two MHD models (UCLA-GGCM and BATSRUS) with observation data obtained from the IMAGE and Polar satellites. The two models in general reproduce the changes of the polar cap size that are seen by the satellite imagers. The range of modeled polar cap sizes, however, is limited to about 50-80% of the size range seen by the imagers and the shapes of the polar caps sometimes differ considerably among the models and compared to the observations. We found that a smoothing of solar wind parameters occurs, suggesting that solar wind inputs are stored in the magnetospheric system over a certain "memory'' timescale. Cross-correlations are computed between smoothed solar wind input and the time history of the resulting polar cap size. Modeled magnetospheric "memory'' timescales are estimated to be less than 12 min, whereas the satellite image data suggest a timescale of more than 20 min. The driver of magnetospheric activity in the models was found to be the B-z (north-south) component of the solar wind magnetic field and to a lesser degree, the Akasofu epsilon parameter which is closely related to Bz but is also influenced by the solar wind velocity V-x and magnetic field B-y. N, V-x, and P-dyn proportional to NVx2 show some degree of anticorrelation with observed polar cap sizes, but anticorrelations are barely significant for polar caps computed from either model. Memory timescales and reaction time delays could be derived from some of the parameters within the limits of statistical significance of the correlation coefficients. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. Univ Michigan, Dept Engn, Ann Arbor, MI 48109 USA. RP NASA, Goddard Space Flight Ctr, Code 696, Greenbelt, MD 20771 USA. EM lr@waipio.gsfc.nasa.gov RI Hesse, Michael/D-2031-2012; Rastaetter, Lutz/D-4715-2012; Kuznetsova, Maria/F-6840-2012; Gombosi, Tamas/G-4238-2011 OI Rastaetter, Lutz/0000-0002-7343-4147; Gombosi, Tamas/0000-0001-9360-4951 NR 34 TC 6 Z9 6 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUL 15 PY 2005 VL 110 IS A7 AR A07212 DI 10.1029/2004JA010672 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 950DR UT WOS:000230838300002 ER PT J AU Trigwell, S Selvaduray, G AF Trigwell, S Selvaduray, G TI Effects of welding on the passive oxide film of electropolished 316L stainless steel SO JOURNAL OF MATERIALS PROCESSING TECHNOLOGY LA English DT Article DE electropolished 316L stainless steel; heat-affected zone; Auger electron spectroscopy ID INTERGRANULAR CORROSION AB In semiconductor manufacture the corrosive fluid delivery systems are subjected to the same scrutiny as the chemicals and gases used, to prevent any contribution to contamination, corrosion, or particle generation. Electropolished 316L stainless steel has become the industry standard due to its superior corrosion resistance and the passive oxide layer formed by the electropolishing. However, welding of the tubing often leads to discoloration in the heat-affected zone (HAZ) leading to corrosion. In this study, specimens from various heat lots were welded under identical parameters, with varying concentrations of oxygen leaked into the argon purge gas during the welding. The chemical composition and thickness of the discoloration in the HAZ and a clean reference area were analyzed by Auger electron spectroscopy. The of the discoloration was due to iron diffusing through the chromium oxide layer in the HAZ in the sensitizing temperature range and forming an iron oxide layer, the thickness of which depended upon the concentration of oxygen available in the purge gas. The composition of the original steel was found to be only a minor contributor to the extent of the discoloration. (c) 2004 Elsevier B.V. All rights reserved. C1 NASA, Kennedy Spade Ctr, Electrostat & Surface Phys Lab, Kennedy Space Ctr, FL 32899 USA. San Jose State Univ, Dept Chem & Mat Engn, San Jose, CA 95192 USA. RP Trigwell, S (reprint author), NASA, Kennedy Spade Ctr, Electrostat & Surface Phys Lab, YA-CT-2, Kennedy Space Ctr, FL 32899 USA. EM steve.trigwell@physics.org NR 36 TC 8 Z9 8 U1 1 U2 4 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0924-0136 J9 J MATER PROCESS TECH JI J. Mater. Process. Technol. PD JUL 15 PY 2005 VL 166 IS 1 BP 30 EP 43 DI 10.1016/j.jmatprotec.2004.07.091 PG 14 WC Engineering, Industrial; Engineering, Manufacturing; Materials Science, Multidisciplinary SC Engineering; Materials Science GA 963ZM UT WOS:000231845400004 ER PT J AU Cath, TY Gormly, S Beaudry, EG Flynn, MT Adams, VD Childress, AE AF Cath, TY Gormly, S Beaudry, EG Flynn, MT Adams, VD Childress, AE TI Membrane contactor processes for wastewater reclamation in space Part I. Direct osmotic concentration as pretreatment for reverse osmosis SO JOURNAL OF MEMBRANE SCIENCE LA English DT Article DE forward osmosis; osmotic distillation; reverse osmosis; wastewater reclamation; life support system ID RO MEMBRANE; DISTILLATION; FILTRATION AB An innovative system that combines three different membrane processes for reclamation and reuse of wastewater in future space missions was evaluated. The direct osmotic concentration (DOC) system consists of an array of five reverse osmosis (RO) elements, a direct osmosis (DO) pretreatment process. and a combined direct osmosis/osmotic distillation (DO/OD) pretreatment process. Optimized operating conditions, including RO pressures, salt load in the brine loop, and flow velocities were determined for the three subsystems. Mass and heat transfer in the pretreatment processes were measured. Water flux in the DO process was found to be strongly dependent on the type of membrane used; it ranged from 10 to 251/(m(2)h) for a cellulose triacetate membrane specifically designed for this application and from 0.5 to 2 for commercially available RO membrane. Water flux through the dual DO/OD process was also found to be highly dependent on temperature gradient across the membranes-increasing with increasing temperature gradient. The conditions for minimum energy consumption of the system were determined and used in estimating the specific energy cost of treating the wastewater generated in space. The weight of salt resupply for continuous operation was also estimated. When compared to alternative technologies, the DOC system provides high wastewater recovery (> 95%), at low energy cost (< 90 x 10(3) J/l (25 Wh/l)), with minimal resupply (< 20 kg/year). (c) 2005 Elsevier B.V. All rights reserved. C1 Univ Nevada, Dept Civil & Environm Engn, Reno, NV 89557 USA. Osmotek Inc, Corvallis, OR 97339 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Childress, AE (reprint author), Univ Nevada, Dept Civil & Environm Engn, Reno, NV 89557 USA. EM amyec@unr.edu RI Cath, Tzahi/H-6458-2011 NR 29 TC 122 Z9 134 U1 7 U2 72 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0376-7388 J9 J MEMBRANE SCI JI J. Membr. Sci. PD JUL 15 PY 2005 VL 257 IS 1-2 BP 85 EP 98 DI 10.1016/j.memsci.2004.08.039 PG 14 WC Engineering, Chemical; Polymer Science SC Engineering; Polymer Science GA 938YC UT WOS:000230038300008 ER PT J AU Ripoll, JF Wray, AA AF Ripoll, JF Wray, AA TI A half-moment model for radiative transfer in a 3D gray medium and its reduction to a moment model for hot, opaque sources SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE radiation; radiative transfer equation; maximum entropy closure; moving directional space; half-moment; M-1(1/2) model; M-1(+) model; M-1 model ID ENTROPY EDDINGTON FACTORS; MULTIPLE-SCATTERING; CLOSURE; PARAMETERIZATION AB We present in this paper a new 3D half-moment model for radiative transfer in a gray medium, called the M-1(1/2) model, which uses maximum entropy closure. This model is a generalization to 3D of the I D version recently proposed in (J. Comp. Phys. 180 (2002) 584). The direction space Omega is divided into two pieces, Omega(+) and Omega(-), in a dynamical way by the plane perpendicular to the total radiative flux, and the half moments are defined from these subspaces. The model closure and the integrations of the radiative transfer equation performed on the moving Omega(-) spaces are detailed. ID planar results, which have motivated the extension of the model of (J. Comp. Phys. 180 (2002) 584) to multi-dimensions, are shown. These results are very good. The model is thereafter derived for 3D spherically symmetric geometry, where the correctness of the non-trivial border terms can be checked. Two 3D spherically symmetric problems are numerically solved in order to show the accuracy of the closure and the role of the border terms. Once again, compared to the solution obtained with a ray tracing solver, results are very good. From the 3D half-moment model, a new moment model, called M-1(+), is derived for the particular case of a 3D hot and opaque source radiating into a cold medium, for applications such as simulations of stellar atmospheres and fires. Two-dimensional numerical results are presented and compared to those obtained solving the RTE and with other moment models. They demonstrate the very good accuracy of the M-1(+) model, its good convergence properties, and better prediction compared to all other existing moment models in its domain of applicability. (C) 2004 Elsevier Ltd. All rights reserved. C1 Stanford Univ, Ctr Turbulence Res, Dept Mech Engn, Stanford, CA 94305 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Ripoll, JF (reprint author), Stanford Univ, Ctr Turbulence Res, Dept Mech Engn, 488 Escondido,Bldg 500-500A, Stanford, CA 94305 USA. EM ripoll@ctr.stanford.edu; wray@nas.nasa.gov NR 27 TC 9 Z9 10 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 JUL 15 PY 2005 VL 93 IS 4 BP 473 EP 519 DI 10.1016/j.jqrst.2004.09.040 PG 47 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 901XQ UT WOS:000227316000006 ER PT J AU Hunton, DE Viggiano, AA Miller, TM Ballenthin, JO Reeves, JM Wilson, JC Lee, SH Anderson, BE Brune, WH Harder, H Simpas, JB Oskarsson, N AF Hunton, DE Viggiano, AA Miller, TM Ballenthin, JO Reeves, JM Wilson, JC Lee, SH Anderson, BE Brune, WH Harder, H Simpas, JB Oskarsson, N TI In-situ aircraft observations of the 2000 Mt. Hekla volcanic cloud: Composition and chemical evolution in the Arctic lower stratosphere SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH LA English DT Article DE volcano cloud composition; in-situ measurements; trace gas; aerosol; SO2 oxidation kinetics ID AIRBORNE OBSERVATIONS; PINATUBO VOLCANO; PARTICLE-SIZE; ST-HELENS; TROPOSPHERE; EMISSIONS; SO2; ERUPTIONS; OZONE; PLUME AB An instrumented NASA aircraft made comprehensive, in-situ measurements of trace gas concentrations and aerosol properties while flying through the eruptive cloud from Mt. Hekla in February and March, 2000. The data reveal novel aspects of the properties and evolution of the volcanic cloud in the lower arctic stratosphere. Thirty-five hours after the initial, sub-Plinian explosion on February 26, 2000, the aircraft intersected the cloud at an altitude of 11.3 km. SO2 concentrations in the cloud exceeded 1 ppmv, but no H2S was observed. Large HF concentrations of similar to 50 ppbv were nearly equal to the HCl concentration, the same ratio of halogen species adsorbed on fallen ash. Although reactive nitrogen species are rarely detected in volcanic clouds, significant HNO3 concentrations of 3 ppbv above background were measured. A bimodal aerosol size distribution with total number densities exceeding 8000 particles/cm(3) and total aerosol volume of 65 mu m(3)/cm(3) was observed. Approximately 1/3 of the fine aerosol particles were non-volatile (volcanic ash) and the remaining 2/3 were volatile (sulfate aerosol and ice). The volcanic cloud was highly structured with clearly delineated boundaries. In the 18-day period following the initial eruption, increases in SO2, sulfate aerosol, HCl, and HF volume mixing ratios were again detected. Analysis of the partitioning of sulfur between the gas and aerosol phases in these later cloud encounters shows that the rate Of SO2 oxidation to sulfuric acid was broadly consistent with changing OH concentrations at the time of the vernal equinox. Published by Elsevier B.V. C1 USAF, Res Lab, Space Vehicles Directorate, Hanscom AFB, MA 01731 USA. Univ Denver, Dept Engn, Denver, CO 80208 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Penn State Univ, Dept Meteorol, State Coll, PA 16802 USA. Nord Volcanol Inst, Reykjavik, Iceland. RP Hunton, DE (reprint author), USAF, Res Lab, Space Vehicles Directorate, Hanscom AFB, MA 01731 USA. EM donald.hunton@hanscom.af.mil RI Lee, Shan-Hu/F-9913-2014 NR 45 TC 28 Z9 28 U1 1 U2 13 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0377-0273 J9 J VOLCANOL GEOTH RES JI J. Volcanol. Geotherm. Res. PD JUL 15 PY 2005 VL 145 IS 1-2 BP 23 EP 34 DI 10.1016/j.jvolgeores.2005.01.005 PG 12 WC Geosciences, Multidisciplinary SC Geology GA 953CP UT WOS:000231054100002 ER PT J AU Greenberg, JA Dobrowski, SZ Ustin, SL AF Greenberg, JA Dobrowski, SZ Ustin, SL TI Shadow allometry: Estimating tree structural parameters using hyperspatial image analysis SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE biomass; allometry; DBH; crown area; stem density; trees; shadow; vectorization; forestry; hyperspatial imagery; IKONOS; Lake Tahoe Basin ID RESOLUTION AERIAL IMAGES; SPECIES CLASSIFICATION; FORESTS; DELINEATION; BASIN; MODEL AB We present a novel approach to generating regional scale aboveground biomass estimates for tree species of the Lake Tahoe Basin using hyperspatial (<1 m(2) ground resolution) remote sensing imagery. Tree crown shadows were identified and delineated as individual polygons. The area of shadowed vegetation for each tree was related to two tree structural parameters, diameter-at-breast height (DBH) and crown area. We found we could detect DBH and crown area with reasonable accuracy (field measured to image derived cross correlation results were 0.67 and 0.77 for DBH and crown area, respectively). Furthermore, the counts of the delineated polygons in a region generated overstory stem densities validated to manually photointerpreted stem densities (photointerpreted vs. image-derived stem densities correlation was 0.87). We demonstrate with accurate classification maps and allometric equations relating DBH or crown area to biomass, that these crown-level parameters can be used to generate regional scale biomass estimates without the signal saturation common to coarse-scale optical and RADAR sensors. (C) 2005 Elsevier Inc. All rights reserved. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Calif Davis, Calspace, Davis, CA 95616 USA. RP Greenberg, JA (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM jgreenberg@arc.nasa.gov OI Greenberg, Jonathan/0000-0001-8435-9077 NR 31 TC 38 Z9 40 U1 1 U2 12 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD JUL 15 PY 2005 VL 97 IS 1 BP 15 EP 25 DI 10.1016/j.rse.2005.02.015 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 955DE UT WOS:000231204600002 ER PT J AU Dong, JR Walker, JP Houser, PR AF Dong, JR Walker, JP Houser, PR TI Factors affecting remotely sensed snow water equivalent uncertainty SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE snow water equivalent (SWE); Scanning Multichannei Microwave Radiometer (SMMR); error analysis; uncertainty ID NORTHERN GREAT-PLAINS; COVER VARIABILITY; CLIMATE; DEPTH; LAND; PARAMETERS; FOREST; TIME AB State-of-the-art passive microwave remote sensing-based snow water equivalent (SWE) algorithms correct for factors believed to most significantly affect retrieved SWE bias and uncertainty. For example, a recently developed semi-empirical SWE retrieval algorithm accounts for systematic and random error caused by forest cover and snow morphology (crystal size - a function of location and time of year). However, we have found that climate and land surface complexities lead to significant systematic and random error uncertainties in remotely sensed SWE retrievals that are not included in current SWE estimation algorithms. Joint analysis of independent meteorological records, ground SWE measurements, remotely sensed SWE estimates, and land surface characteristics have provided a unique look at the error structure of these recently developed satellite SWE products. We considered satellite-derived SWE errors associated with the snow pack mass itself, the distance to significant open water bodies, liquid water in the snow pack and/or morphology change due to melt and refreeze, forest cover, snow class, and topographic factors such as large scale root mean square roughness and dominant aspect. Analysis of the nine-year Scanning Multichannel Microwave Radiometer (SMMR) SWE data set was undertaken for Canada where many in-situ measurements are available. It was found that for SMMR pixels with 5 or more ground stations available, the remote sensing product was generally unbiased with a seasonal maximum 20 mm average root mean square error for SWE values less than 100 mm. For snow packs above 100 mm, the SWE estimate bias was linearly related to the snow pack mass and the root mean square error increased to around 150 mm. Both the distance to open water and average monthly mean air temperature were found to significantly influence the retrieved SWE product uncertainty. Apart from maritime snow class, which had the greatest snow class affect on root mean square error and bias, all other factors showed little relation to observed uncertainties. Eliminating the drop-in-the-bucket averaged gridded remote sensing SWE data within 200 km of open water bodies, for monthly mean temperatures greater than -2 degrees C, and for snow packs greater than 100 mm, has resulted in a remotely sensed SWE product that is useful for practical applications. (C) 2005 Elsevier Inc. All rights reserved. C1 NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21250 USA. Univ Melbourne, Dept Civil & Environm Engn, Parkville, Vic 3010, Australia. George Mason Univ, Calverton, MD 20705 USA. Ctr Res Environm & Water, Calverton, MD 20705 USA. RP Dong, JR (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Code 974, Greenbelt, MD 20771 USA. EM jiarui@hsb.gsfc.nasa.gov RI Walker, Jeffrey/D-2624-2009; Houser, Paul/J-9515-2013 OI Houser, Paul/0000-0002-2991-0441 NR 32 TC 65 Z9 67 U1 1 U2 11 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD JUL 15 PY 2005 VL 97 IS 1 BP 68 EP 82 DI 10.1016/j.rse.2005.04.010 PG 15 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 955DE UT WOS:000231204600006 ER PT J AU Maule, CF Purucker, ME Olsen, N Mosegaard, K AF Maule, CF Purucker, ME Olsen, N Mosegaard, K TI Heat flux anomalies in Antarctica revealed by satellite magnetic data SO SCIENCE LA English DT Article ID ICE-SHEET; SUBGLACIAL LAKES; BASAL MELT; STABILITY; BOREHOLE; STREAMS AB The geothermal heat flux is an important factor in the dynamics of ice sheets; it affects the occurrence of subglacial takes, the onset of ice streams, and mass tosses from the ice sheet base. Because direct heat flux measurements in ice-covered regions are difficult to obtain, we developed a method that uses satellite magnetic data to estimate the heat flux underneath the Antarctic ice sheet We found that the heat flux underneath the ice sheet varies from 40 to 185 megawatts per square meter and that areas of high heat flux coincide with known current volcanism and some areas known to have ice streams. C1 Ctr Planetary Sci, DK-2100 Copenhagen, Denmark. NASA, Goddard Space Flight Ctr, Raytheon Co, Greenbelt, MD 20771 USA. RP Maule, CF (reprint author), Ctr Planetary Sci, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark. EM foxmaule@gfy.ku.dk RI Olsen, Nils/H-1822-2011 OI Olsen, Nils/0000-0003-1132-6113 NR 25 TC 79 Z9 81 U1 2 U2 25 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 JUL 15 PY 2005 VL 309 IS 5733 BP 464 EP 467 DI 10.1126/science.1106888 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 946LY UT WOS:000230574900046 PM 15947138 ER PT J AU Lauenstein, JM Barth, JL Sibeck, DG AF Lauenstein, JM Barth, JL Sibeck, DG TI Introduction to special section on International Working Group Meeting on New Standard Radiation Belt and Space Plasma Models for Spacecraft Engineering SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Editorial Material C1 Muniz Engn Inc, Lanham, MD 20706 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lauenstein, JM (reprint author), Muniz Engn Inc, Lanham, MD 20706 USA. EM Jean.Marie.Lauenstein@gsfc.nasa.gov RI Sibeck, David/D-4424-2012 NR 0 TC 1 Z9 1 U1 0 U2 1 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 JUL 15 PY 2005 VL 3 IS 7 AR S07B01 DI 10.1029/2005SW000159 PG 1 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 953YA UT WOS:000231120100001 ER PT J AU Jackman, CH DeLand, MT Labow, GJ Fleming, EL Weisenstein, DK Ko, MKW Sinnhuber, M Russell, JM AF Jackman, CH DeLand, MT Labow, GJ Fleming, EL Weisenstein, DK Ko, MKW Sinnhuber, M Russell, JM TI Neutral atmospheric influences of the solar proton events in October-November 2003 SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID EARTHS MIDDLE ATMOSPHERE; 2-DIMENSIONAL MODEL; ODD NITROGEN; NITRIC-OXIDE; OZONE MEASUREMENTS; PARTICLE EVENTS; STRATOSPHERE; MESOSPHERE; CHEMISTRY; DEPLETION AB The large solar storms in October-November 2003 caused solar proton events (SPEs) at the Earth and impacted the middle atmospheric polar cap regions. Although occurring near the end of the maximum of solar cycle 23, the fourth largest period of SPEs measured in the past 40 years happened 28-31 October 2003. The highly energetic protons associated with the SPEs produced ionizations, excitations, dissociations, and dissociative ionizations of the background constituents, which led to the production of odd hydrogen (HOx) and odd nitrogen (NOy). NOx (NO + NO2) was observed by the UARS HALOE instrument to increase over 20 ppbv throughout the Southern Hemisphere polar lower mesosphere. The NOAA 16 SBUV/2 instrument measured a short-term ozone depletion of 40% in the Southern Hemisphere polar lower mesosphere, probably a result of the HOx increases. SBUV/2 observations showed ozone depletions of 5-8% in the southern polar upper stratosphere lasting days beyond the events, most likely a result of the NOy enhancements. Longer-term Northern Hemisphere polar total ozone decreases of >0.5% were predicted to last for over 8 months past the events with the Goddard Space Flight Center two-dimensional model. Although the production of NOy constituents is the same in both hemispheres, the NOy constituents have a much larger impact in the northern than the southern polar latitudes because of the seasonal differences between the two hemispheres. These observations and model computations illustrate the substantial impact of solar protons on the polar neutral middle atmosphere. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Sci Syst & Applicat Inc, Lanham, MD 20706 USA. Atmospher & Environm Res Inc, Lexington, MA 02421 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Univ Bremen, Inst Environm Phys, D-2800 Bremen, Germany. Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. RP Jackman, CH (reprint author), NASA, Goddard Space Flight Ctr, Code 916,Greenbelt Rd, Greenbelt, MD 20771 USA. EM charles.h.jackman@nasa.gov; matthew_deland@ssaihq.com; labow@qhearts.gsfc.nasa.gov; fleming@kahuna.gsfc.nasa.gov; weisenstein@aer.com; malcolm.k.ko@nasa.gov; miriam@iup.physik.uni-bremen.de; james.russell@hamptonu.edu RI Sinnhuber, Miriam/A-7252-2013; Jackman, Charles/D-4699-2012; Ko, Malcolm/D-5898-2015 NR 36 TC 97 Z9 98 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUL 14 PY 2005 VL 110 IS A9 AR A09S27 DI 10.1029/2004JA010888, PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 950DV UT WOS:000230838700001 ER PT J AU Deck, RT Amar, JG Fralick, G AF Deck, RT Amar, JG Fralick, G TI Nuclear size corrections to the energy levels of single-electron and -muon atoms SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID DEEP DIRAC LEVELS; ISOTOPE SHIFT; DEUTERIUM; HYDROGEN; TRANSITIONS; PROGRAM AB We formulate an analytic method which accounts for the finite size of the nucleus by treating it as a boundary value problem. The method is used to obtain solutions of the Dirac equation for a central potential that is proportional to 1/r only for values of the radial coordinate greater than a given value R. Our results are applied to a non-perturbative calculation of the nuclear size corrections to the energy levels of single-electron and single-muon atoms. For values of the nuclear charge number Z greater than 40 in the case of electronic atoms, and greater than 1 in the case of muonic atoms, we find large discrepancies between our results for the atomic energy levels and those obtained from first-order relativistic perturbation theory. C1 Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Deck, RT (reprint author), Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. NR 11 TC 3 Z9 4 U1 1 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 JUL 14 PY 2005 VL 38 IS 13 BP 2173 EP 2186 DI 10.1088/0953-4075/38/13/010 PG 14 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 951ES UT WOS:000230912500013 ER PT J AU Wang, MH Shi, W AF Wang, MH Shi, W TI Estimation of ocean contribution at the MODIS near-infrared wavelengths along the east coast of the US: Two case studies SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ATMOSPHERIC CORRECTION; COLOR IMAGERY; SEAWIFS; WATER AB Atmospheric correction for the ocean color products derived from the Moderate Resolution Imaging Spectroradiometer (MODIS) uses two near-infrared (NIR) bands centered at 748 and 869 nm. Ocean is usually assumed to be black at these two NIR wavelengths. For Case-2 and high productive Case-1 waters, however, ocean could have significant contributions in the NIR, leading to significant under-estimation of the MODIS-derived water-leaving radiances. This is often the case in coastal regions. In this paper, measurements from the MODIS Terra at the short wave infrared (SWIR) wavelengths (1240 and 1640 nm) are used to evaluate the ocean contributions at wavelengths 748 and 869 nm. The ocean is black in coastal regions in these SWIR bands due to much stronger water absorption. Studies of two MODIS granules off the east coast of the U. S. show that the ocean could have reflectance values of similar to 3.1% and similar to 1.8% at the top of atmosphere (TOA) for bands 748 and 869 nm in the Outer Banks, while these values are similar to 0.15% and similar to 0.1% in the Chesapeake Bay region. Thus, for the turbid waters, it is important to accurately account for the ocean contributions in the NIR bands for the atmospheric correction of ocean color remote sensing. C1 Univ Maryland Baltimore Cty, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Wang, MH (reprint author), Natl Environm Satellite Data & Informat Serv, NOAA, Off Res & Applicat, E-RA3,Room 102,5200 Auth Rd, Camp Springs, MD 20746 USA. EM menghua.wang@noaa.gov RI Shi, Wei/F-5625-2010; Wang, Menghua/F-5631-2010 OI Wang, Menghua/0000-0001-7019-3125 NR 6 TC 116 Z9 121 U1 4 U2 18 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 JUL 13 PY 2005 VL 32 IS 13 AR L13606 DI 10.1029/2005GL022917 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 950BT UT WOS:000230833300001 ER PT J AU Han, QY Zeng, J Kuo, KS Chen, H Smith, E AF Han, QY Zeng, J Kuo, KS Chen, H Smith, E TI Effect of particle size distributions on the retrieval of ice cloud properties SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SINGLE-SCATTERING PROPERTIES; CIRRUS CLOUDS; RADIATIVE PROPERTIES; OPTICAL-PROPERTIES; CLIMATE MODELS; ACCURATE PARAMETERIZATION; PLANETARY ATMOSPHERES; CRYSTAL SIZE; WATER CLOUDS; LIGHT AB Various measured size distributions obtained from aircraft measurements at different regions and seasons are used in the retrieval algorithms for ice cloud properties by several major satellite instruments such as MODIS, CERES and VIIRS. These measured size distributions are characterized by one parameter: effective size ( diameter or radius). This study shows that the adoption of such measured size distributions leads to inconsistent results in retrieved cloud properties because neglecting the effect of effective variances causes non-monotonic relations between crystal size and single scattering properties. We also show that single scattering properties of most observed size distributions of hexagonal columns can be adequately characterized by effective radius and effective variance. Therefore, in remote sensing of ice cloud properties, theoretical size distributions with explicitly assumed effective variances should be used, similar to the practice adopted for water clouds. C1 Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35805 USA. Caelum Res Corp, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Serenet Inc, Englewood, CO 80112 USA. RP Han, QY (reprint author), Univ Alabama, Dept Atmospher Sci, 320 Sparkman Dr, Huntsville, AL 35805 USA. EM han@nsstc.uah.edu NR 21 TC 3 Z9 3 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 JUL 12 PY 2005 VL 32 IS 13 AR L13818 DI 10.1029/2005GL022659 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 950BR UT WOS:000230833100004 ER PT J AU Alexandrov, MD Carlson, BE Lacis, AA Cairns, B AF Alexandrov, MD Carlson, BE Lacis, AA Cairns, B TI Separation of fine and coarse aerosol modes in MFRSR data sets SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OPTICAL-PROPERTIES; CHEMICAL-COMPOSITION; SIZE DISTRIBUTIONS; ALGORITHM; SULFATE; MASS; PARAMETERIZATION; RETRIEVAL; EVOLUTION; INVERSION AB A new MFRSR data analysis algorithm is presented. Our earlier algorithm assumed a monomodal aerosol size distribution, while the new algorithm allows us to partition the aerosol optical thickness into fine and coarse aerosol modes. In addition, we retrieve the fine mode effective radius and Angstrom exponent. A bimodal gamma distribution is used to describe the aerosol particle size distribution. The algorithm has been tested using a multi-year data set from the local MFRSR network at the DOE Atmospheric Radiation Measurement (ARM) Program site in Southern Great Plains (SGP). Our retrieved aerosol optical thicknesses (total, fine, and coarse) are compared with the corresponding AERONET almucantar retrieval results derived from a CIMEL sunphotometer co-located with the MFRSR at the SGP Central Facility. A constrained variant of the algorithm (zero NO2 column values) has been used to define the range of physically justified values of the fine mode effective radius, and for comparison with AERONET particle size retrievals. We use the multiple MFRSR measurements obtained during the year 2000 at the SGP Extended Facilities to examine geographical and seasonal variability of aerosol properties. A correspondence has been found between the geographical variation in the fine mode particle size and aerosol composition ( nitrates versus sulfates) as measured by National Atmospheric Deposition Program. We similarly find good correspondence between our retrieved aerosol sizes and the PM2.5 to PM10 ratios obtained from EPA AirData monitoring. Examination of the data from the SGP Central Facility obtained for the period 1993 - 1997 reveals a decreasing trend in coarse mode aerosol optical thickness during the 1993 - 1995 period, consistent with the decay of the stratospheric aerosol following the 1991 eruption of Mt. Pinatubo. In contrast, fine mode optical thickness exhibits only seasonal variability with summer maxima during this period. C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Alexandrov, MD (reprint author), Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA. EM malexandrov@giss.nasa.gov RI Lacis, Andrew/D-4658-2012; Carlson, Barbara/D-8319-2012; OI Cairns, Brian/0000-0002-1980-1022 NR 27 TC 8 Z9 8 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 12 PY 2005 VL 110 IS D13 AR D13204 DI 10.1029/2004JD005226 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 950CQ UT WOS:000230835600002 ER PT J AU Natarajan, M Deaver, LE Thompson, E Magill, B AF Natarajan, M Deaver, LE Thompson, E Magill, B TI Impact of twilight gradients on the retrieval of mesospheric ozone from HALOE SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OCCULTATION EXPERIMENT; STRATOSPHERE; VALIDATION AB Solar occultation measurement of atmospheric species with short photochemical lifetimes poses some difficulties if sharp gradients are present in the species concentrations near sunrise/sunset conditions. These photochemically induced variations introduce asymmetries in the species distribution along the line of sight that need to be taken into account in the retrieval process in order to prevent inaccuracies. Correction factors derived from photochemical model calculations have been routinely applied to the retrievals of stratospheric NO and NO2 by HALOE and ATMOS experiments. Mesospheric ozone, because of its twilight variations, also belongs to the group of species which require a correction procedure. Results from our mesospheric diurnal photochemical model indicate that proper accounting of diurnal variations leads to more than 20% increase in the ozone column along the line of sight for sunrise conditions near 0.1 hPA at the equator in January. Correspondingly, the retrieved ozone at the tangent point will be lower if these twilight variations are considered. The effects under sunset conditions are smaller. The current HALOE retrieval algorithm uses an approximate correction for mesospheric ozone. We have developed a new database of twilight gradients for the entire altitude range of HALOE measurements based on the results from a contemporary diurnal photochemical model. HALOE scans for January 29, 1992, have been reprocessed using the new diurnal correction factors. Sunrise ozone mixing ratios near 0.1 hPa are smaller by more than 20% compared to the HALOE V19 data. The differences between the corrections for sunrise and sunset retrievals suggest that, with the new diurnal corrections, the sunrise to sunset ozone ratios near 0.1 hPa obtained from approximately coincident HALOE data will be in much better agreement with the values derived from photochemical theory. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. GATS Inc, Newport News, VA 23606 USA. RP NASA, Langley Res Ctr, 21 Langley Blvd, Hampton, VA 23681 USA. EM murali.natarajan@.nasa.gov; l.e.deaver@larc.nasa.gov; r.e.thompson@gats-inc.com; b.e.magill@gats-inc.com NR 15 TC 9 Z9 9 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 12 PY 2005 VL 110 IS D13 AR D13305 DI 10.1029/2004JD005719 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 950CQ UT WOS:000230835600010 ER EF