FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Ergun, RE Malaspina, DM Cairns, IH Goldman, MV Newman, DL Robinson, PA Eriksson, S Bougeret, JL Briand, C Bale, SD Cattell, CA Kellogg, PJ Kaiser, ML AF Ergun, R. E. Malaspina, D. M. Cairns, Iver H. Goldman, M. V. Newman, D. L. Robinson, P. A. Eriksson, S. Bougeret, J. L. Briand, C. Bale, S. D. Cattell, C. A. Kellogg, P. J. Kaiser, M. L. TI Eigenmode structure in solar-wind Langmuir waves SO PHYSICAL REVIEW LETTERS LA English DT Article ID RADIO-BURSTS; PLASMA-WAVES; TURBULENCE; FREQUENCY; COLLAPSE; ELECTRONS; CORONA AB We show that observed spatial- and frequency-domain signatures of intense solar-wind Langmuir waves can be described as eigenmodes trapped in a parabolic density well. Measured solar-wind electric field spectra and waveforms are compared with 1D linear solutions and, in many cases, can be represented by 1-3 low-order eigenstates. To our knowledge, this report is the first observational confirmation of Langmuir eigenmodes in space. These results suggest that linear eigenmodes may be the starting point of the nonlinear evolution, critical for producing solar type II and type III radio bursts. C1 [Ergun, R. E.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Ergun, R. E.; Malaspina, D. M.; Eriksson, S.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. [Cairns, Iver H.; Robinson, P. A.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. [Goldman, M. V.; Newman, D. L.] Univ Colorado, Ctr Integrated Plasma Studies, Boulder, CO 80309 USA. [Bougeret, J. L.; Briand, C.] Univ Paris Diderot, UPMC, CNRS, Observ Paris,LESIA, F-92190 Meudon, France. [Bale, S. D.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Cattell, C. A.; Kellogg, P. J.] Univ Minnesota, Dept Phys & Astron, Minneapolis, MN 55455 USA. [Kaiser, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ergun, RE (reprint author), Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. RI Bale, Stuart/E-7533-2011; OI Bale, Stuart/0000-0002-1989-3596; Cattell, Cynthia/0000-0002-3805-320X; Cairns, Iver/0000-0001-6978-9765; Eriksson, Stefan/0000-0002-5619-1577 NR 27 TC 51 Z9 51 U1 2 U2 3 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD AUG 1 PY 2008 VL 101 IS 5 AR 051101 DI 10.1103/PhysRevLett.101.051101 PG 4 WC Physics, Multidisciplinary SC Physics GA 336SK UT WOS:000258384700010 PM 18764383 ER PT J AU Klimas, A Hesse, M Zenitani, S AF Klimas, Alex Hesse, Michael Zenitani, Seiji TI Particle-in-cell simulation of collisionless reconnection with open outflow boundaries SO PHYSICS OF PLASMAS LA English DT Article ID MAGNETIC RECONNECTION; ACCELERATION; MAGNETOTAIL AB A new method for applying open boundary conditions in particle-in-cell (PIC) simulations is utilized to study magnetic reconnection. Particle distributions are assumed to have zero normal derivatives at the boundaries. Advantages and possible limitations of this method for PIC simulations are discussed. Results from a reconnection simulation study are presented. For the purpose of this investigation, a 2 1/2-dimensional electromagnetic PIC simulation using open conditions at the outflow boundaries and simple reflecting boundaries to the inflow regions is discussed. The electron diffusion region is defined as that region where the out-of-plane electron inertial electric field is positive indicating acceleration and flux transfer; the evolution of this region is analyzed. It is found that this region varies in the range 2.5-4 local electron inertial lengths in total width and in the range 10-15 local electron inertial lengths in total length for the mass ratio 25. The reconnection rate is investigated in terms of the aspect ratio of the electron diffusion region plus inflow and outflow measures at its boundaries. It is shown that a properly measured aspect ratio predicts the flux transfer rate, scaled to account for the decline in field strength and electron density at the inflow boundary to the electron diffusion region. It is concluded that this electron diffusion region either adjusts its aspect ratio for compatibility with the flux transfer rate that is set elsewhere, as in the Hall reconnection model, or that it is this region that controls the reconnection flux transfer rate. (C) 2008 American Institute of Physics. C1 [Klimas, Alex] NASA, Goddard Space Flight Ctr, UMBC, Greenbelt, MD 20771 USA. [Zenitani, Seiji] NASA, Goddard Space Flight Ctr, ORAU, Greenbelt, MD 20771 USA. RP Klimas, A (reprint author), NASA, Goddard Space Flight Ctr, UMBC, Greenbelt, MD 20771 USA. RI Hesse, Michael/D-2031-2012; Zenitani, Seiji/D-7988-2013; NASA MMS, Science Team/J-5393-2013 OI Zenitani, Seiji/0000-0002-0945-1815; NASA MMS, Science Team/0000-0002-9504-5214 NR 35 TC 34 Z9 34 U1 0 U2 4 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-664X J9 PHYS PLASMAS JI Phys. Plasmas PD AUG PY 2008 VL 15 IS 8 AR 082102 DI 10.1063/1.2965826 PG 9 WC Physics, Fluids & Plasmas SC Physics GA 351TN UT WOS:000259448900007 ER PT J AU Parks, GK Lee, E Teste, A Wilber, M Lin, N Canu, P Dandouras, I Reme, H Fu, SY Goldstein, ML AF Parks, G. K. Lee, E. Teste, A. Wilber, M. Lin, N. Canu, P. Dandouras, I. Reme, H. Fu, S. Y. Goldstein, M. L. TI Transport of transient solar wind particles in Earth's cusps SO PHYSICS OF PLASMAS LA English DT Article ID HIGH-ALTITUDE CUSP; MAGNETOSPHERIC CUSPS; BERNSTEIN WAVES; BOW SHOCK; CLUSTER; REGION; PLASMA; SPACECRAFT; FIELDS AB An important problem in space physics still not understood well is how the solar wind enters the Earth's magnetosphere. Evidence is presented that transient solar wind particles produced by solar disturbances can appear in the Earth's mid-altitude (similar to 5 R(E) geocentric) cusps with densities nearly equal to those in the magnetosheath. That these are magnetosheath particles is established by showing they have the same "flattop" electron distributions as magnetosheath electrons behind the bow shock. The transient ions are moving parallel to the magnetic field (B) toward Earth and often coexist with ionospheric particles that are flowing out. The accompanying waves include electromagnetic and broadband electrostatic noise emissions and Bernstein mode waves. Phase-space distributions show a mixture of hot and cold electrons and multiple ion species including field-aligned ionospheric O(+) beams. (C) 2008 American Institute of Physics. C1 [Parks, G. K.; Lee, E.; Teste, A.; Wilber, M.; Lin, N.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Canu, P.] CETP, Velizy Villacoublay, France. [Dandouras, I.; Reme, H.] Univ Toulouse 3, Ctr Etud Spatiale Rayonnement, F-31062 Toulouse, France. [Fu, S. Y.] Peking Univ, Sch Earth & Space Sci, Beijing, Peoples R China. [Goldstein, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. RP Parks, GK (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM parks@ssl.berkeley.edu RI Goldstein, Melvyn/B-1724-2008; Lee, Ensang/E-2356-2013; Fu, Suiyan/E-9178-2013; OI Dandouras, Iannis/0000-0002-7121-1118 FU NASA [NNG04GF23G] FX The research at UC Berkeley is performed under NASA Grant No. NNG04GF23G. NR 25 TC 2 Z9 2 U1 0 U2 4 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-664X J9 PHYS PLASMAS JI Phys. Plasmas PD AUG PY 2008 VL 15 IS 8 AR 080702 DI 10.1063/1.2965825 PG 4 WC Physics, Fluids & Plasmas SC Physics GA 351TN UT WOS:000259448900003 ER PT J AU Zenitani, S Hesse, M AF Zenitani, S. Hesse, M. TI The role of the Weibel instability at the reconnection jet front in relativistic pair plasma reconnection (vol 15, artn no 022101, 2008) SO PHYSICS OF PLASMAS LA English DT Correction C1 [Zenitani, S.; Hesse, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Zenitani, S (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM zenitani@lssp-mail.gsfc.nasa.gov RI Hesse, Michael/D-2031-2012; NASA MMS, Science Team/J-5393-2013 OI NASA MMS, Science Team/0000-0002-9504-5214 NR 2 TC 0 Z9 0 U1 1 U2 1 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-664X J9 PHYS PLASMAS JI Phys. Plasmas PD AUG PY 2008 VL 15 IS 8 AR 089901 DI 10.1063/1.2965501 PG 1 WC Physics, Fluids & Plasmas SC Physics GA 351TN UT WOS:000259448900075 ER PT J AU Bailey, J Chamberlain, S Crisp, D Meadows, VS AF Bailey, Jeremy Chamberlain, S. Crisp, D. Meadows, V. S. TI Near infrared imaging spectroscopy of Venus with the Anglo-Australian Telescope SO PLANETARY AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Symposium on Ground-Based and Venus Express Coordinated Campaign CY DEC 17-19, 2007 CL Noordwijk, NETHERLANDS DE Venus; Venus atmosphere; Near-infrared spectroscopy; Airglow ID ESA/VENUS EXPRESS MISSION; DARK SIDE; UPPER-ATMOSPHERE; AIRGLOW; VIRTIS; SPECTROMETER; NIGHTSIDE; DYNAMICS; LAYER AB We have obtained full-disk spatially resolved spectra of the Venus nightside at near-infrared wavelengths during July 2007 using the Anglo-Australian Telescope and Infrared Imager and Spectrograph 2 (IRIS2). The data have been used to map the intensity and rotational temperature of the O-2 (a(1)Delta(g)) airglow band at 1.27 mu m. The temperatures agree with those obtained in earlier IRIS2 observations and are significantly higher than expected from the Venus International Reference Atmosphere (VIRA) profile. We also report the detection of the corresponding nu = 0-1 O-2 airglow band at 1.58 mu m with a similar spatial distribution to the 1.27 mu m nu = 0-0 band. Observations in the 1.18 mu m thermal window have been used to image surface topography using two different methods of cloud correction. We have also obtained 2.3 mu m images that can be used to study cloud motion. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Bailey, Jeremy; Chamberlain, S.] Macquarie Univ, Dept Phys, N Ryde, NSW 2109, Australia. [Crisp, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Meadows, V. S.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. RP Bailey, J (reprint author), Macquarie Univ, Dept Phys, N Ryde, NSW 2109, Australia. EM jbailey@els.mq.edu.au NR 19 TC 12 Z9 12 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD AUG PY 2008 VL 56 IS 10 SI SI BP 1385 EP 1390 DI 10.1016/j.pss.2008.03.006 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 369UA UT WOS:000260718200007 ER PT J AU Sornig, M Livengood, T Sonnabend, G Kroetz, P Stupar, D Kostiuk, T Schieder, R AF Sornig, M. Livengood, T. Sonnabend, G. Kroetz, P. Stupar, D. Kostiuk, T. Schieder, R. TI Venus upper atmosphere winds from ground-based heterodyne spectroscopy of CO2 at 10 mu m wavelength SO PLANETARY AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Symposium on Ground-Based and Venus Express Coordinated Campaign CY DEC 17-19, 2007 CL Noordwijk, NETHERLANDS DE Venus; Planetary atmospheres; Non-LTE; Mid-infrared; Heterodyne; Dynamics ID GLOBAL CIRCULATION; UPPER MESOSPHERE; EMISSION-LINES; NATURAL LASER; MARS; THERMOSPHERE; VELOCITIES; DISCOVERY; (CO)-C-12; DYNAMICS AB We report observations of Venus atmospheric wind near 110 km altitude by means of high-resolution mid-infrared spectroscopy. Data were acquired May 28-June 4, 2007 at the McMath-Pierce Solar Telescope (Kitt Peak, Arizona, USA), during a coordinated groundbased observing campaign in support of Venus Express. The Cologne Tuneable Heterodyne Infrared Spectrometer (THIS) was used to measure the Doppler shift of fully resolved non-LTE emission lines Of CO2 at 959.3917 cm(-1) (10.423 mu m) to determine wind velocity. Spatial resolution was similar to 1.7 arcsec on Venus' apparent diameter of 20-22 arcsec. Zonal wind velocities were retrieved at six different latitudes close to the west limb. Retrieved zonal velocities-parallel to Venus' retrograde solid body rotation-range 3 +/- 7 m/s (1 sigma) at the equator to a maximum of 32 +/- 4 m/s (1 sigma) at southern mid-latitude (45 degrees S), decreasing at higher latitudes and thus suggesting a retrograde double jet structure for the zonal component. The subsolar-to-antisolar circulation component was measured at one position, 45 degrees towards the sunlit limb from the central meridian, on the equator. The retrieved subsolar-to-antisolar component at this position implies a cross-terminator velocity of 52 +/- 18 m/s (1 sigma). Retrieved velocities are lower than previous results, suggesting spatial and/or temporal variability of dynamics in the mesosphere/thermosphere of Venus. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Sornig, M.; Sonnabend, G.; Kroetz, P.; Stupar, D.; Schieder, R.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Livengood, T.; Kostiuk, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Livengood, T.] USRA, Columbia, MD 21044 USA. RP Sonnabend, G (reprint author), Univ Cologne, Inst Phys 1, Zuelpicher Str 77, D-50937 Cologne, Germany. EM samstag@ph1.uni-koeln.de RI Livengood, Timothy/C-8512-2012; Kostiuk, Theodor/A-3077-2014 NR 31 TC 21 Z9 21 U1 2 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD AUG PY 2008 VL 56 IS 10 SI SI BP 1399 EP 1406 DI 10.1016/j.pss.2008.05.006 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 369UA UT WOS:000260718200009 ER PT J AU Sonnabend, G Sornig, M Schieder, R Kostiuk, T Delgado, J AF Sonnabend, G. Sornig, M. Schieder, R. Kostiuk, T. Delgado, J. TI Temperatures in Venus upper atmosphere from mid-infrared heterodyne spectroscopy of CO2 around 10 mu m wavelength SO PLANETARY AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Symposium on Ground-Based and Venus Express Coordinated Campaign CY DEC 17-19, 2007 CL Noordwijk, NETHERLANDS DE Venus; Observation; Temperature; Mesosphere; Spectroscopy ID NATURAL LASER-EMISSION; MARS; MESOSPHERES; LINES AB We report observations of temperatures in the Venus upper mesosphere/lower thermosphere. Data were acquired between 22 and 24 October 2007 at the NASA Infrared Telescope Facility on Mauna Kea, Hawaii using the NASA Goddard Space Flight Center Heterodyne Instrument for Planetary Wind and Composition (HIPWAC). Fully resolved non-thermal emission (non-LTE) lines in the 10.6 mu m band Of CO2 from various rotational levels were used to study rotational and kinetic temperatures on the Venus dayside. From models the emission is assumed to originate in the range of similar to 100-120 km altitude. Rotational temperatures were derived from the intensity distribution of the CO2 lines measured at the equator/45 degrees east, mid-latitudes (45 degrees north and south)/45 degrees cast, and 70 degrees south/30 degrees east. Retrieved values (171-236K) disagree with the observed kinetic temperatures in all but one point (45 degrees north/45 degrees east). In addition, the measured intensities show a large dispersion originating most likely in the Venus atmosphere. Information on kinetic temperatures was extracted from the widths of the emission lines. Temperature values range from 224 to 236 K and were retrieved at the equator/45 degrees east, mid-latitudes (45 degrees north and south)/45 degrees east, and 70 degrees south/30 degrees east, and along the equator at various longitudes with an accuracy of up to 2 K. These values are higher than the Venus International Reference Atmosphere model predicts. The longitudinal scan shows kinetic temperatures of similar to 230-250K from the subsolar point to 40 degrees offset from the terminator followed by a decrease to similar to 120 K close to the terminator. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Sonnabend, G.; Sornig, M.; Schieder, R.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Kostiuk, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Delgado, J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Sonnabend, G (reprint author), Univ Cologne, Inst Phys 1, Zuelpicher Str 77, D-50937 Cologne, Germany. EM samstag@ph1.uni-koeln.de RI Kostiuk, Theodor/A-3077-2014 NR 18 TC 10 Z9 10 U1 1 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD AUG PY 2008 VL 56 IS 10 SI SI BP 1407 EP 1413 DI 10.1016/j.pss.2008.05.008 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 369UA UT WOS:000260718200010 ER PT J AU Wirz, R Goebel, D AF Wirz, Richard Goebel, Dan TI Effects of magnetic field topography on ion thruster discharge performance SO PLASMA SOURCES SCIENCE & TECHNOLOGY LA English DT Article ID PLASMA AB Traditional magnetic field design techniques for dc ion thrusters typically focus on closing a sufficiently high maximum closed magnetic contour, B(cc), inside the discharge chamber. In this study, detailed computational analysis of several modified NSTAR thruster 3-ring and 4-ring magnetic field geometries reveals that the magnetic field line shape as well as Bcc determines important aspects of dc ion thruster performance (i.e. propellant efficiency, beam flatness and double ion content). The DC-ION ion thruster model results show that the baseline NSTAR configuration traps the primary electrons on-axis, which leads to the high on-axis plasma density peak and high double ion content observed in experimental measurements. These problems are further exacerbated by simply increasing Bcc and not changing the field line shape. Changing the field line shape to prevent on-axis confinement ( while maintaining the NSTAR baseline Bcc) improves thruster performance, improves plasma uniformity and lowers double ion content. For these favorable field line geometries, we observe further improvements to performance with increased Bcc, while maintaining plasma uniformity and low double ion content. These improvements derive from the fact that the field lines guide the high-energy primaries to regions where they are most efficiently used to create ions while a higher Bcc prevents the loss of ions to the anode walls. Therefore, it is recommended that the ion thruster designer first establish a divergent field line shape that ensures favorable beam flatness, low double ion content and reasonable performance; then the designer may adjust the Bcc to attain desirable performance and stability for the target discharge plasma conditions. C1 [Wirz, Richard; Goebel, Dan] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Wirz, R (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 23 TC 6 Z9 6 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0963-0252 J9 PLASMA SOURCES SCI T JI Plasma Sources Sci. Technol. PD AUG PY 2008 VL 17 IS 3 AR 035010 DI 10.1088/0963-0252/17/3/035010 PG 11 WC Physics, Fluids & Plasmas SC Physics GA 333HV UT WOS:000258144500011 ER PT J AU Hou, TH Jensen, BJ AF Hou, T. H. Jensen, B. J. TI Double-vacuum-bag technology for volatile management in composite fabrication SO POLYMER COMPOSITES LA English DT Article ID POLYIMIDE COMPOSITES AB A nonautoclave vacuum bag process using atmospheric pressure alone that eliminates the need for external pressure supplied normally by an autoclave or a press is an attractive method for composite fabrication. This type of process does not require large capital expenditures for tooling and processing equipment. The traditional single-vacuum-bag (SVB) process is best suited for molding epoxy matrix-based composites because of their superior flow and the absence of reaction byproducts or other volatiles. This is not the case for other classes of materials such as polyimides and phenolics. Polyimides and phenolics are cured by condensation reactions which generate water as a reaction byproduct. In addition, these materials are commonly synthesized as oligomers using solvents to facilitate processability. Volatiles (solvents and reaction byproducts) management therefore becomes a critical issue. SVB molding, without additional pressure, normally fails to yield void-free quality composites for these classes of resin systems. A double-vacuum-bag (DVB) process for volatile management in composite fabrication using common molding equipment was designed and built at the NASA Langley Research Center. This experimental DVB process affords superior volatiles management compared with the traditional SVB process. Void-free composites are consistently fabricated as measured by C-scan and optical photo-microscopy for high-performance polyimide and phenolic resins. C1 [Hou, T. H.; Jensen, B. J.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Hou, TH (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM tan-hung.hou-1@nasa.gov NR 13 TC 10 Z9 10 U1 0 U2 5 PU JOHN WILEY & SONS INC PI HOBOKEN PA 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0272-8397 J9 POLYM COMPOSITE JI Polym. Compos. PD AUG PY 2008 VL 29 IS 8 BP 906 EP 914 DI 10.1002/pc.20475 PG 9 WC Materials Science, Composites; Polymer Science SC Materials Science; Polymer Science GA 329YT UT WOS:000257907200010 ER PT J AU Danehy, PM Alderfer, DW Inman, JA Berger, KT Buck, GM Schwartz, RJ AF Danehy, P. M. Alderfer, D. W. Inman, J. A. Berger, K. T. Buck, G. M. Schwartz, R. J. TI Fluorescence imaging and streakline visualization of hypersonic flow over rapid prototype wind-tunnel models SO PROCEEDINGS OF THE INSTITUTION OF MECHANICAL ENGINEERS PART G-JOURNAL OF AEROSPACE ENGINEERING LA English DT Article DE laser-induced fluorescence; planar laser-induced fluorescence; hypersonic; rapid prototype; stereolithography; wake flow; flow visualization; streamline; streakline ID TEMPERATURE; VELOCIMETRY AB The use of planar laser-induced fluorescence (PLIF) of nitric oxide (NO) was investigated for use in visualizing wake flowfields downstream of rapid prototyping models in a hypersonic wind tunnel. The re-entry models for use in this study were fabricated using a stereo-lithography apparatus. These models were produced in one day or less, which is a significant time savings compared with the manufacture of ceramic or metal models. The models were tested in the NASA Langley Research Center 31-Inch Mach 10 Air Tunnel. Pure NO was either seeded through tubes plumbed into the model or via a tube attached to the strut holding the model, which provided localized addition of NO into the model's wake through a porous metal cylinder attached to the end of the tube. Various entry capsule model types and configurations and NO-seeding methods were used, including a new streamwise visualization method based on PLIF Virtual diagnostics interface technology, developed at NASA Langley Research Center, was used to visualize the datasets in post-processing. The use of calibration 'dotcards' was investigated to correct for camera perspective and lens distortions in the PLIF images. C1 [Danehy, P. M.; Alderfer, D. W.; Inman, J. A.] NASA, Langley Res Ctr, Adv Sensing & Opt Measurements Branch, Hampton, VA 23681 USA. [Berger, K. T.; Buck, G. M.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23665 USA. [Schwartz, R. J.] ATK Space Div, Hampton, VA USA. RP Danehy, PM (reprint author), NASA, Langley Res Ctr, Adv Sensing & Opt Measurements Branch, MS 493, Hampton, VA 23681 USA. EM Paul.M.Danehy@nasa.gov FU NASA Langley Research Center; NASA Fundamental Aeronautics Hypersonics Program FX The authors wish to acknowledge the contribution to this project from the NASA Langley Research Center 31-Inch Mach 10 Air Tunnel technicians and engineers including Kevin Hollingsworth, Paul Tucker Tony Robbins, Henry Fitzgerald, and Johnny Ellis. For model fabrication and coating, the authors wish to acknowledge Gary Wainwright, Mike Powers, Pete Vasquez, and Steve Nevins. This work was supported by the NASA Fundamental Aeronautics Hypersonics Program. The current work is based on a prior, un-refereed conference paper [13]. NR 19 TC 11 Z9 11 U1 2 U2 8 PU PROFESSIONAL ENGINEERING PUBLISHING LTD PI WESTMINISTER PA 1 BIRDCAGE WALK, WESTMINISTER SW1H 9JJ, ENGLAND SN 0954-4100 J9 P I MECH ENG G-J AER JI Proc. Inst. Mech. Eng. Part G-J. Aerosp. Eng. PD AUG PY 2008 VL 222 IS G5 BP 637 EP 651 DI 10.1243/09544100JAERO295 PG 15 WC Engineering, Aerospace; Engineering, Mechanical SC Engineering GA 346GU UT WOS:000259057600007 ER PT J AU Georgiadis, NJ AF Georgiadis, Nicholas J. TI Large-eddy simulation-Current capabilities and areas of needed research Introduction SO PROGRESS IN AEROSPACE SCIENCES LA English DT Editorial Material C1 NASA, Glenn Res Ctr, Cleveland, OH USA. RP Georgiadis, NJ (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA. EM Georgiadis@nasa.gov NR 0 TC 2 Z9 2 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0376-0421 J9 PROG AEROSP SCI JI Prog. Aeosp. Sci. PD AUG PY 2008 VL 44 IS 6 BP 379 EP 380 DI 10.1016/j.paerosci.2008.07.001 PG 2 WC Engineering, Aerospace SC Engineering GA 358CJ UT WOS:000259893900001 ER PT J AU Laird, JS Chen, Y Scheick, L Vo, T Johnston, A AF Laird, Jamie Stuart Chen, Yuan Scheick, Leif Vo, Tuan Johnston, Allan TI Scanning picosecond tunable laser system for simulating MeV heavy ion-induced charge collection events as a function of temperature SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article ID ELECTRON-HOLE-PAIR; P-N-JUNCTIONS; HIGH-SPEED SI; PULSED-LASER; 2-PHOTON ABSORPTION; GAAS-MESFETS; AUGER RECOMBINATION; INTEGRATED-CIRCUITS; ENERGY DEPOSITION; INDUCED LATCHUP AB A new methodology for using scanning picosecond laser microscopy to simulate cosmic ray induced radiation effects as a function of temperature is described in detail. The built system is centered on diffraction-limited focusing of the output from a broadband (690-960 nm) ultrafast Ti:sapphire Tsunami laser pumped by a 532 nm Millennia laser. An acousto-optic modulator is used to provide pulse picking down to event rates necessary for the technologies and effects under study: The temperature dependence of the charge generation process for ions and photons is briefly reviewed and the need for wavelength tunability is discussed. An appropriate wavelength selection is critical for proper emulation of ion events over a wide temperature range. The system developed is detailed and illustrated by way of example on a deep-submicron complementary metal-oxide semiconductor test structure. (C) 2008 American Institute of Physics. C1 [Laird, Jamie Stuart; Chen, Yuan; Scheick, Leif; Vo, Tuan; Johnston, Allan] NASA, CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Laird, JS (reprint author), Univ Melbourne, Sch Phys, Div Explorat & Min, Commonwealth Sci & Ind Res Org, Parkville, Vic 3101, Australia. RI Laird, Jamie/A-7683-2011 NR 77 TC 1 Z9 1 U1 0 U2 4 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0034-6748 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD AUG PY 2008 VL 79 IS 8 AR 083705 DI 10.1063/1.2965262 PG 10 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 350SX UT WOS:000259374500026 PM 19044355 ER PT J AU Martin, V Chevalier, V Ceccato, P Anyamba, A De Simone, L Lubroth, J de la Rocque, S Domenech, J AF Martin, V. Chevalier, V. Ceccato, P. Anyamba, A. De Simone, L. Lubroth, J. de la Rocque, S. Domenech, J. TI The impact of climate change on the epidemiology and control of Rift Valley fever SO REVUE SCIENTIFIQUE ET TECHNIQUE-OFFICE INTERNATIONAL DES EPIZOOTIES LA English DT Article DE climate change; early warning system; Rift Valley fever; vector-borne disease ID VECTOR COMPETENCE; SAUDI-ARABIA; ENVIRONMENTAL-TEMPERATURE; SOUTHERN MAURITANIA; VIRUS; DIPTERA; KENYA; CULICIDAE; SENEGAL; ENCEPHALITIS AB Climate change is likely to change the frequency of extreme weather events, such as tropical cyclones, floods, droughts and hurricanes, and may destabilise and weaken the ecosystem services upon which human society depends. Climate change is also expected to affect animal, human and plant health via indirect pathways: it is likely that the geography of infectious diseases and pests will be altered, including the distribution of vector-borne diseases, such as Rift Valley fever, yellow fever, malaria and dengue, which are highly sensitive to climatic conditions. Extreme weather events might then create the necessary conditions for Rift Valley fever to expand its geographical range northwards and cross the Mediterranean and Arabian seas, with an unexpected impact on the animal and human health of newly affected countries. Strengthening global, regional and national early warning systems is crucial, as are co-ordinated research programmes and subsequent prevention and intervention measures. C1 [Martin, V.] FAO, Emergency Ctr Contol Transboundary Anim Dis ECTAD, Beijing, Peoples R China. [Chevalier, V.] Ctr Cooperat Int Rech Agron Dev CIRAD, Montpellier, France. [Ceccato, P.] Columbia Univ, Earth Inst, Int Res Inst Climate & Soc, Palisades, NY USA. [Anyamba, A.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. [De Simone, L.; Lubroth, J.; de la Rocque, S.; Domenech, J.] Food & Agr Org United Nations FAO, Infect Dis Grp, Anim Hlth Serv, Rome, Italy. RP Martin, V (reprint author), FAO, Emergency Ctr Contol Transboundary Anim Dis ECTAD, Beijing, Peoples R China. EM Vincent.Martin@fao.org RI Hensens, Hanka/A-4187-2010 NR 39 TC 57 Z9 65 U1 4 U2 35 PU OFFICE INT EPIZOOTIES PI PARIS PA 12 RUE DE PRONY, 75017 PARIS, FRANCE SN 0253-1933 J9 REV SCI TECH OIE JI Rev. Sci. Tech. Off. Int. Epizoot. PD AUG PY 2008 VL 27 IS 2 BP 413 EP 426 PG 14 WC Veterinary Sciences SC Veterinary Sciences GA 350LJ UT WOS:000259353700011 PM 18819669 ER PT J AU Levine, BD Stray-Gundersen, J Mehta, RD AF Levine, B. D. Stray-Gundersen, J. Mehta, R. D. TI Effect of altitude on football performance SO SCANDINAVIAN JOURNAL OF MEDICINE & SCIENCE IN SPORTS LA English DT Article; Proceedings Paper CT Consensus Meeting on Football at High Altitude CY OCT 25-27, 2007 CL Zurich, SWITZERLAND SP FIFA, F MARC DE hypoxia; exercise; hypobaria; soccer ID ACUTE MODERATE HYPOXIA; MAXIMAL OXYGEN-UPTAKE; EXERCISE PERFORMANCE; THEORETICAL-ANALYSIS; SUBMAXIMAL EXERCISE; ANAEROBIC CAPACITY; SIMULATED ALTITUDE; PHYSICAL MODEL; SEA-LEVEL; ACCLIMATIZATION AB Altitude will impact football performance through two separate and parallel pathways related to the hypobaric (physical) and hypoxic (physiological) components of terrestrial altitude: (a) the decrease in partial pressure of oxygen reduces maximal oxygen uptake and impairs "aerobic" performance by reducing maximal aerobic power, increasing the relative intensity of any given absolute level of work, and delaying recovery of high-energy phosphates between high-intensity "interval" type efforts; (b) the decrease in air density reduces air resistance which will facilitate high-velocity running, but will also alter drag and lift thereby impairing sensorimotor skills. These effects appear to have their greatest impact very early in the altitude exposure, and their physiological/neurosensory consequences are ameliorated by acclimatization, though the extent of restoration of sea level type performance depends on the absolute magnitude of the competing and living altitudes. C1 [Levine, B. D.] Univ Texas SW Med Ctr Dallas, Presbyterian Hosp, Inst Exercise & Environm Med, Dallas, TX 75231 USA. [Stray-Gundersen, J.] Cooper Clin, Dallas, TX USA. [Mehta, R. D.] NASA, Ames Res Ctr, Fluid Mech Lab, Mountain View, CA USA. RP Levine, BD (reprint author), Univ Texas SW Med Ctr Dallas, Presbyterian Hosp, Inst Exercise & Environm Med, 7232 Greenville Ave,Suite 435, Dallas, TX 75231 USA. EM benjaminlevine@texashealth.org NR 56 TC 34 Z9 35 U1 2 U2 13 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0905-7188 J9 SCAND J MED SCI SPOR JI Scand. J. Med. Sci. Sports PD AUG PY 2008 VL 18 SU 1 BP 76 EP 84 DI 10.1111/j.1600-0838.2008.00835.x PG 9 WC Sport Sciences SC Sport Sciences GA 327AE UT WOS:000257700300010 PM 18665955 ER PT J AU Smith, CE Morscher, GN Xia, ZH AF Smith, Craig E. Morscher, Gregory N. Xia, Z. H. TI Monitoring damage accumulation in ceramic matrix composites using electrical resistivity SO SCRIPTA MATERIALIA LA English DT Article DE ceramic matrix composites (CMC); electrical properties; fracture; non-destructive testing ID COMBUSTOR AB The electric resistance of woven SiC fiber-reinforced SiC matrix composites were measured under tensile loading conditions. The results show that the electrical resistance is closely related to damage and that real-time information about the damage state can be obtained through monitoring of the resistance. Such self-sensing capability provides the possibility of on-board/in situ damage detection and accurate life prediction for high-temperature ceramic matrix composites. (C) 2008 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved. C1 [Smith, Craig E.; Xia, Z. H.] Univ Akron, Dept Mech Engn, Akron, OH 44325 USA. [Morscher, Gregory N.] NASA Glenn Res Ctr, Ohio Aersosp Inst, Ceram Branch, Cleveland, OH 44224 USA. RP Xia, ZH (reprint author), Univ Akron, Dept Mech Engn, Akron, OH 44325 USA. EM zxia@uakron.edu NR 22 TC 31 Z9 31 U1 1 U2 11 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1359-6462 J9 SCRIPTA MATER JI Scr. Mater. PD AUG PY 2008 VL 59 IS 4 BP 463 EP 466 DI 10.1016/j.scriptamat.2008.04.033 PG 4 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA 325VF UT WOS:000257615700024 ER PT J AU Woods, TN Chamberlin, PC Peterson, WK Meier, RR Richards, PG Strickland, DJ Lu, G Qian, LY Solomon, SC Iijima, BA Mannucci, AJ Tsurutani, BT AF Woods, Thomas N. Chamberlin, Phillip C. Peterson, W. K. Meier, R. R. Richards, Phil G. Strickland, Douglas J. Lu, Gang Qian, Liying Solomon, Stanley C. Iijima, B. A. Mannucci, A. J. Tsurutani, B. T. TI XUV Photometer System (XPS): Improved solar irradiance algorithm using CHIANTI spectral models SO SOLAR PHYSICS LA English DT Article ID X-RAY IRRADIANCE; CHROMOSPHERIC STRUCTURES; EXTREME-ULTRAVIOLET; ATOMIC DATABASE; ELECTRON-IMPACT; EMISSION-LINES; SORCE MISSION; EUV; VARIABILITY; CALIBRATIONS AB Solar soft X-ray (XUV) radiation is highly variable on all time scales and strongly affects Earth's ionosphere and upper atmosphere; consequently, the solar XUV irradiance is important for atmospheric studies and for space weather applications. Although there have been several recent measurements of the solar XUV irradiance, detailed understanding of the solar XUV irradiance, especially its variability during flares, has been hampered by the broad bands measured in the XUV range. In particular, the simple conversion of the XUV photometer signal into irradiance, in which a static solar spectrum is assumed, overestimates the flare variations by more than a factor of two as compared to the atmospheric response to the flares. To address this deficiency in the simple conversion, an improved algorithm using CHIANTI spectral models has been developed to process the XUV Photometer System (XPS) measurements with its broadband photometers. Model spectra representative of quiet Sun, active region, and flares are combined to match the signals from the XPS and produce spectra from 0.1 to 40 nm in 0.1-nm intervals for the XPS Level 4 data product. The two XPS instruments are aboard NASA's Solar Radiation and Climate Experiment (SORCE) and Thermosphere, Ionosphere, Mesosphere, Energetics, and Dynamics (TIMED) satellites. In addition, the XPS responsivities have been updated for the latest XPS data processing version. The new XPS results are consistent with daily variations from the previous simple conversion technique used for XPS and are also consistent with spectral measurements made at wavelengths longer than 27 nm. Most importantly, the XPS flare variations are reduced by factors of 2-4 at wavelengths shorter than 14 nm and are more consistent, for the first time, with atmospheric response to solar flares. Along with the details of the new XPS algorithm, several comparisons to dayglow and photoelectron measurements and model results are also presented to help verify the accuracy of the new XUV irradiance spectra. C1 [Woods, Thomas N.; Chamberlin, Phillip C.; Peterson, W. K.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA. [Meier, R. R.; Richards, Phil G.] George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA. [Strickland, Douglas J.] Computat Phys Inc, Springfield, VA 22151 USA. [Lu, Gang; Qian, Liying; Solomon, Stanley C.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80309 USA. [Iijima, B. A.; Mannucci, A. J.; Tsurutani, B. T.] Jet Prop Lab, Pasadena, CA 91109 USA. RP Woods, TN (reprint author), Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA. EM tom.woods@lasp.colorado.edu; phil.chamberlin@lasp.colorado.edu; bill.peterson@lasp.colorado.edu; rmeier@gmu.edu; prichar1@gmu.edu; dstrick@cpi.com; gang.lu@hao.ucar.edu; lqian@ucar.edu; stans@ucar.edu; byron.a.iijima@jpl.nasa.gov; anthony.j.mannucci@jpl.nasa.gov; bruce.t.tsurutani@jpl.nasa.gov RI Lu, Gang/A-6669-2011; Chamberlin, Phillip/C-9531-2012; Solomon, Stanley/J-4847-2012; Qian, Liying/D-9236-2013; Meier, Robert/G-4749-2014; Peterson, WK/A-8706-2009 OI Chamberlin, Phillip/0000-0003-4372-7405; Solomon, Stanley/0000-0002-5291-3034; Qian, Liying/0000-0003-2430-1388; Meier, Robert/0000-0001-8497-7115; Peterson, WK/0000-0002-1513-6096 NR 65 TC 37 Z9 37 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD AUG PY 2008 VL 250 IS 2 BP 235 EP 267 DI 10.1007/s11207-008-9196-6 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 332OV UT WOS:000258093200002 ER PT J AU Hathaway, DH Choudhary, DP AF Hathaway, David H. Choudhary, Debi Prasad TI Sunspot group decay SO SOLAR PHYSICS LA English DT Article DE Sun : sunspots; Sun : active regions ID SOLAR MAGNETIC-FIELD; FLUX; AREAS; IRRADIANCE; GROWTH; RATES; FLOW AB We examine daily records of sunspot group areas (measured in millionths of a solar hemisphere or mu Hem) for the last 130 years to determine the rate of decay of sunspot group areas. We exclude observations of groups when they are more than 60 degrees in longitude from the central meridian and only include data when at least three days of observations are available following the date of maximum area for a group's disk passage. This leaves data for over 18 000 measurements of sunspot group decay. We find that the decay rate increases linearly from 28 mu Hem day(-1) to about 140 mu Hem day(-1) for groups with areas increasing from 35 mu Hem to 1000 mu Hem. The decay rate tends to level off for groups with areas larger than 1000 mu Hem. This behavior is very similar to the increase in the number of sunspots per group as the area of the group increases. Calculating the decay rate per individual sunspot gives a decay rate of about 3.65 mu Hem day(-1) with little dependence upon the area of the group. This suggests that sunspots decay by a Fickian diffusion process with a diffusion coefficient of about 10 km(2) s(-1). Although the 18 000 decay rate measurements are lognormally distributed, this can be attributed to the lognormal distribution of sunspot group areas and the linear relationship between area and decay rate for the vast majority of groups. We find weak evidence for variations in decay rates from one solar cycle to another and for different phases of each sunspot cycle. However, the strongest evidence for variations is with latitude and the variations with cycle and phase of each cycle can be attributed to this variation. High latitude spots tend to decay faster than low latitude spots. C1 [Hathaway, David H.] NASA, George C Marshall Space Flight Ctr, NSSTC, Huntsville, AL 35812 USA. [Choudhary, Debi Prasad] Calif State Univ Northridge, San Fernando Observ, Dept Phys & Astron, Northridge, CA 91330 USA. RP Hathaway, DH (reprint author), NASA, George C Marshall Space Flight Ctr, NSSTC, Huntsville, AL 35812 USA. EM david.hathaway@nasa.gov; debiprasad.choudhary@csun.edu NR 26 TC 34 Z9 35 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 2008 VL 250 IS 2 BP 269 EP 278 DI 10.1007/s11207-008-9226-4 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 332OV UT WOS:000258093200003 ER PT J AU Thompson, WT Reginald, NL AF Thompson, W. T. Reginald, N. L. TI The radiometric and pointing calibration of SECCHI COR1 on STEREO SO SOLAR PHYSICS LA English DT Article DE instrumental effects; corona ID CORONAGRAPH AB COR1 is the innermost coronagraph of the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) instrument suite aboard the twin Solar Terrestrial Relations Observatory (STEREO) spacecraft. The paired COR1 telescopes observe the white-light K-corona from 1.4 to 4 solar radii in a waveband 22.5 nm wide centered on the H alpha line at 656 nm. An internal polarizer allows the measurement of both total and polarized brightness. The co-alignment of the two COR1 telescopes is derived from the star lambda Aquarii for the Ahead spacecraft, and from an occultation of the Sun by the Moon for Behind. Observations of the planet Jupiter are used to establish absolute photometric calibrations for each telescope. The intercalibration of the two COR1 telescopes are compared using coronal mass ejection observations made early in the mission, when the spacecraft were close together. Comparisons are also made with the Solar and Heliospheric Observatory (SOHO) Large Angle and Spectrometric Coronagraph (LASCO) C2 and Mauna Loa Solar Observatory Mk4 coronagraphs. C1 [Thompson, W. T.] NASA, Goddard Space Flight Ctr, Adnet Syst Inc, Greenbelt, MD 20771 USA. [Reginald, N. L.] Catholic Univ, NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Thompson, WT (reprint author), NASA, Goddard Space Flight Ctr, Adnet Syst Inc, Greenbelt, MD 20771 USA. EM William.T.Thompson@nasa.gov; Nelson.L.Reginald@nasa.gov RI Thompson, William/D-7376-2012 NR 9 TC 20 Z9 21 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD AUG PY 2008 VL 250 IS 2 BP 443 EP 454 DI 10.1007/s11207-008-9228-2 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 332OV UT WOS:000258093200014 ER PT J AU Bugos, GE Boyd, JW AF Bugos, Glenn E. Boyd, John W. TI Accelerating entrepreneurial space: The case for an NACA-style organization SO SPACE POLICY LA English DT Article AB The entrepreneurial space industry today faces challenges similar to those facing the commercial aircraft industry in the early part of the last century. At that time the National Advisory Committee for Aeronautics (NACA) helped develop many of the key technologies that enabled air travel to become effective, economical and safe. Today, in discussing how best to support the realization of a commercial space economy, we suggest revisiting what an NACA-style organization can contribute. This paper outlines the key concepts that made the NACA so successful: a committee structure, open source publication, a willingness to try any useful experimental method, and a focus on problem definition. (c) 2008 Elsevier Ltd. All rights reserved. C1 [Bugos, Glenn E.; Boyd, John W.] NASA, Ames Res Ctr, Ames Hist Off, Moffett Field, CA 94035 USA. RP Bugos, GE (reprint author), NASA, Ames Res Ctr, Ames Hist Off, MS 207-1, Moffett Field, CA 94035 USA. EM Glenn.E.Bugos@nasa.gov NR 17 TC 3 Z9 3 U1 0 U2 1 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 2008 VL 24 IS 3 BP 140 EP 147 DI 10.1016/j.spacepol.2008.06.003 PG 8 WC International Relations; Social Sciences, Interdisciplinary SC International Relations; Social Sciences - Other Topics GA 346OR UT WOS:000259078600005 ER PT J AU Witasse, O Cravens, T Mendillo, M Moses, J Kliore, A Nagy, AF Breus, T AF Witasse, O. Cravens, T. Mendillo, M. Moses, J. Kliore, A. Nagy, A. F. Breus, T. TI Solar System Ionospheres SO SPACE SCIENCE REVIEWS LA English DT Review DE Ionospheres; Planetology ID RADIO OCCULTATION MEASUREMENTS; SATURNS UPPER-ATMOSPHERE; MARS GLOBAL SURVEYOR; EQUATORIAL SPREAD-F; TO-DAY VARIABILITY; X-RAY-EMISSION; MAGNETIC-FIELD; MARTIAN IONOSPHERE; TITANS IONOSPHERE; VENUS IONOSPHERE AB This article reviews our understanding of the ionospheres in the solar system. It provides some basic information on the sources and sinks of the ionospheric plasma, its dynamics, the energetics and the coupling to the neutral atmosphere. Ionospheres in the solar system are reviewed and comparative ionospheric topics are discussed. C1 [Witasse, O.] European Space Agcy, NL-2200 AG Noordwijk, Netherlands. [Cravens, T.] Univ Kansas, Lawrence, KS 66045 USA. [Mendillo, M.] Boston Univ, Boston, MA 02215 USA. [Moses, J.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Kliore, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Nagy, A. F.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Breus, T.] Moscow Space Res Inst, Moscow 117810, Russia. RP Witasse, O (reprint author), European Space Agcy, POB 299, NL-2200 AG Noordwijk, Netherlands. EM owitasse@rssd.esa.int; cravens@ku.edu; mendillo@bu.edu; moses@lpi.usra.edu; akliore@jpl.nasa.gov; anagy@umich.edu; breus36@mail.ru RI Moses, Julianne/I-2151-2013; Mendillo, Michael /H-4397-2014 OI Moses, Julianne/0000-0002-8837-0035; NR 196 TC 26 Z9 27 U1 0 U2 8 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD AUG PY 2008 VL 139 IS 1-4 BP 235 EP 265 DI 10.1007/s11214-008-9395-3 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 362GB UT WOS:000260185100007 ER PT J AU Johnson, RE Combi, MR Fox, JL Ip, WH Leblanc, F McGrath, MA Shematovich, VI Strobel, DF Waite, JH AF Johnson, R. E. Combi, M. R. Fox, J. L. Ip, W. -H. Leblanc, F. McGrath, M. A. Shematovich, V. I. Strobel, D. F. Waite, J. H., Jr. TI Exospheres and Atmospheric Escape SO SPACE SCIENCE REVIEWS LA English DT Review DE Atmospheric escape; Planetary corona; Exobase; Exosphere ID SOLAR-WIND INTERACTION; COMET HALE-BOPP; SATURNS RING ATMOSPHERE; HOT OXYGEN-ATOMS; DIRECT STATISTICAL SIMULATION; VENUS RELATIVE CONTRIBUTIONS; NEUTRAL CLOUD DISTRIBUTION; IONOSPHERIC PLASMA ESCAPE; MARS GLOBAL SURVEYOR; NEAR-SURFACE LAYERS AB Aeronomy is a description of the physics and chemistry of the upper atmospheres and ionospheres of planetary bodies. In this chapter we consider those processes occurring in the upper atmosphere that determine the structure of the corona and lead to molecular escape. C1 [Johnson, R. E.] Univ Virginia, Charlottesville, VA 22904 USA. [Johnson, R. E.] NYU, Dept Phys, New York, NY 10003 USA. [Combi, M. R.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Fox, J. L.] Wright State Univ, Dept Phys, Dayton, OH 45435 USA. [Ip, W. -H.] Natl Cent Univ, Inst Astron, Chungli 32054, Taiwan. [Leblanc, F.] CNRS, Serv Aeron, Paris, France. [Leblanc, F.] Osserv Astron Trieste, F-34131 Trieste, France. [McGrath, M. A.] George C Marshall Space Flight Ctr, Huntsville, AL 35899 USA. [Shematovich, V. I.] RAS, Inst Astron, Moscow 119017, Russia. [Strobel, D. F.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Waite, J. H., Jr.] SW Res Inst, San Antonio, TX 78228 USA. RP Johnson, RE (reprint author), Univ Virginia, Charlottesville, VA 22904 USA. EM rej@virginia.edu; mcombi@umich.edu; Jane.Fox@wright.edu; wingip@astro.ncu.edu.tw; francois.leblanc@aerov.jussieu.fr; melissa.a.mcgrath@nasa.gov; shematov@inasan.ru; dstrobe1@jhu.edu; hwaite@swri.edu RI Combi, Michael/J-1697-2012; Shematovich, Valery/E-4670-2014 OI Combi, Michael/0000-0002-9805-0078; NR 310 TC 57 Z9 57 U1 2 U2 14 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD AUG PY 2008 VL 139 IS 1-4 BP 355 EP 397 DI 10.1007/s11214-008-9415-3 PG 43 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 362GB UT WOS:000260185100010 ER PT J AU D'Alimonte, D Cornford, D AF D'Alimonte, Davide Cornford, Dan TI Outlier detection with partial information: application to emergency mapping SO STOCHASTIC ENVIRONMENTAL RESEARCH AND RISK ASSESSMENT LA English DT Article ID NOVELTY DETECTION AB This paper, addresses the problem of novelty detection in the case that the observed data is a mixture of a known 'background' process contaminated with an unknown other process, which generates the outliers, or novel observations. The framework we describe here is quite general, employing univariate classification with incomplete information, based on knowledge of the distribution (the probability density function, pdf) of the data generated by the 'background' process. The relative proportion of this 'background' component (the prior 'background' probability), the pdf and the prior probabilities of all other components are all assumed unknown. The main contribution is a new classification scheme that identifies the maximum proportion of observed data following the known 'background' distribution. The method exploits the Kolmogorov-Smirnov test to estimate the proportions, and afterwards data are Bayes optimally separated. Results, demonstrated with synthetic data, show that this approach can produce more reliable results than a standard novelty detection scheme. The classification algorithm is then applied to the problem of identifying outliers in the SIC2004 data set, in order to detect the radioactive release simulated in the 'joker' data set. We propose this method as a reliable means of novelty detection in the emergency situation which can also be used to identify outliers prior to the application of a more general automatic mapping algorithm. C1 [Cornford, Dan] Aston Univ, Neural Comp Res Grp, Birmingham B4 7ET, W Midlands, England. [D'Alimonte, Davide] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Cornford, D (reprint author), Aston Univ, Neural Comp Res Grp, Birmingham B4 7ET, W Midlands, England. EM davide@ardbeg.gsfc.nasa.gov; d.cornford@aston.ac.uk RI D'Alimonte, Davide/I-6531-2013 OI D'Alimonte, Davide/0000-0001-7217-7057 NR 11 TC 1 Z9 1 U1 2 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1436-3240 J9 STOCH ENV RES RISK A JI Stoch. Environ. Res. Risk Assess. PD AUG PY 2008 VL 22 IS 5 BP 613 EP 620 DI 10.1007/s00477-007-0164-8 PG 8 WC Engineering, Environmental; Engineering, Civil; Environmental Sciences; Statistics & Probability; Water Resources SC Engineering; Environmental Sciences & Ecology; Mathematics; Water Resources GA 314RE UT WOS:000256825700003 ER PT J AU Liu, PCB Hansen, M Mukherjee, A AF Liu, Pei-chen Barry Hansen, Mark Mukherjee, Avijit TI Scenario-based air traffic flow management: From theory to practice SO TRANSPORTATION RESEARCH PART B-METHODOLOGICAL LA English DT Article DE air traffic flow management; ground delay program; ground holding problem; capacity scenarios; airport capacity; stochastic optimization; dynamic optimization ID GROUND-HOLDING PROBLEM; TREE GENERATION; OPTIMIZATION AB Recent developments in solving the single airport ground holding problem use static or dynamic optimization to manage uncertainty about how airport capacities will evolve. Both static and dynamic models involve the use of scenarios that depict different possible capacity evolutions. Dynamic models also require scenario trees featuring branch points where previously similar capacity profiles become distinct. In this paper, we present methodologies for generating and using scenario trees from empirical data and examine the performance of scenario-based models in a real-world setting. We find that most US airports have capacity profiles that can be classified into a small number of nominal scenarios, and for a number of airports these scenarios can be naturally combined into scenario trees. The costs incurred from applying scenario-based optimization, either static or dynamic, to these airports is considerably higher than the "theoretical" optimization results suggest because actual capacities vary around the nominal values assumed in the optimization, and because of uncertainty in navigating scenario trees that the idealized models ignore. Methods for tuning capacity scenarios and scenario trees to mitigate these problems are explored. (c) 2008 Elsevier Ltd. All rights reserved. C1 [Liu, Pei-chen Barry; Hansen, Mark] Univ Calif Berkeley, Natl Ctr Excellence Aviat Operat Res, Inst Transport Studies, Dept Civil & Environm Engn, Berkeley, CA 94720 USA. [Mukherjee, Avijit] Univ Calif Santa Cruz, NASA, Univ Affiliated Res Ctr, Santa Cruz, CA 94035 USA. RP Hansen, M (reprint author), Univ Calif Berkeley, Natl Ctr Excellence Aviat Operat Res, Inst Transport Studies, Dept Civil & Environm Engn, Berkeley, CA 94720 USA. EM barryliu@cal.berkeley.edu; hansen@ce.berkeley.edu; avijit@ucsc.edu NR 17 TC 34 Z9 39 U1 0 U2 13 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0191-2615 J9 TRANSPORT RES B-METH JI Transp. Res. Pt. B-Methodol. PD AUG PY 2008 VL 42 IS 7-8 BP 685 EP 702 DI 10.1016/j.trb.2008.01.002 PG 18 WC Economics; Engineering, Civil; Operations Research & Management Science; Transportation; Transportation Science & Technology SC Business & Economics; Engineering; Operations Research & Management Science; Transportation GA 324KL UT WOS:000257517400005 ER PT J AU Oswald, FB Jett, TR Predmore, RE Zaretsky, EV AF Oswald, Fred B. Jett, Timothy R. Predmore, Roamer E. Zaretsky, Erwin V. TI Probabilistic analysis of space shuttle body flap actuator ball bearings SO TRIBOLOGY & LUBRICATION TECHNOLOGY LA English DT Article; Proceedings Paper CT 62nd Annual Meeting of the Society-of-Tribologists-and-Lubrication-Engineers CY MAY 06-10, 2007 CL Philadelphia, PA SP Soc Tribologists Lubricat Engineers DE statistical analysis; weibull analysis; life prediction methods; wear; ball bearings; grease lubrication AB A probabilistic analysis, using the two-parameter Weibull-Johnson method, was performed on experimental lift test data from space shuttle actuator bearings. Experiments were performed on a test rig under simulated conditions to determine the life and failure mechanism of the grease lubricated bearings that support the input shaft of the space shuttle body flap actuators. The failure mechanism was wear that can cause loss of bearing preload. These tests established life and reliability data for both shuttle flight and ground operation. Test data were used to estimate the failure rate and reliability as a function of the number of shuttle missions flown. The Weibull analysis of the test data for the four actuators on one shuttle, each with a two-bearing shaft assembly, established a reliability level of 96.9% for a life of 12 missions. A probabilistic system analysis for four shuttles, each of which has four actuators, predicts a single bearing failure in one actuator Of one shuttle after 22 missions (a total of 88 missions for a four-shuttle fleet). This prediction is comparable with actual shuttle flight history in which a single actuator bearing was found to have failed by wear at 20 missions. C1 [Oswald, Fred B.; Zaretsky, Erwin V.] NASA Glenn Res Ctr, Cleveland, OH USA. [Jett, Timothy R.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Predmore, Roamer E.] Swales Aerosp, Greenbelt, MD USA. RP Oswald, FB (reprint author), NASA Glenn Res Ctr, Cleveland, OH USA. NR 20 TC 0 Z9 0 U1 0 U2 0 PU SOC TRIBOLOGISTS & LUBRICATION ENGINEERS PI PARK RIDGE PA 840 BUSSE HIGHWAY, PARK RIDGE, IL 60068 USA SN 1545-858X J9 TRIBOL LUBR TECHNOL JI Tribol. Lubr. Technol. PD AUG PY 2008 VL 64 IS 8 BP 36 EP 45 PG 10 WC Engineering, Mechanical SC Engineering GA 339FU UT WOS:000258564300010 ER PT J AU Fioletov, VE Labow, G Evans, R Hare, EW Koehler, U McElroy, CT Miyagawa, K Redondas, A Savastiouk, V Shalamyansky, AM Staehelin, J Vanicek, K Weber, M AF Fioletov, V. E. Labow, G. Evans, R. Hare, E. W. Koehler, U. McElroy, C. T. Miyagawa, K. Redondas, A. Savastiouk, V. Shalamyansky, A. M. Staehelin, J. Vanicek, K. Weber, M. TI Performance of the ground-based total ozone network assessed using satellite data SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID WFDOAS TOTAL OZONE; DOBSON NETWORK; BREWER; SPECTROPHOTOMETER; GOME; DRIFT; TOMS AB [1] Dobson and Brewer spectrophotometer and filter ozonometer data available from the World Ozone and Ultraviolet Data Centre ( WOUDC) were compared with satellite total ozone measurements from TOMS ( onboard Nimbus 7, Meteor 3, and Earth Probe satellites), OMI ( AURA satellite) and GOME ( ERS- 2 satellite) instruments. Five characteristics of the difference with satellite data were calculated for each site and instrument type: the mean difference, the standard deviation of daily differences, the standard deviation of monthly differences, the amplitude of the seasonal component of the difference, and the range of annual values. All these characteristics were calculated for five 5- year- long bins and for each site separately for direct sun ( DS) and zenith sky ( ZS) ozone measurements. The main percentiles were estimated for the five characteristics of the difference and then used to establish criteria for "suspect'' or "outlier'' sites for each characteristic. About 61% of Dobson, 46% of Brewer, and 28% of filter stations located between 60 degrees S and 60 degrees N have no "suspect'' or "outlier'' characteristics. In nearly 90% of all cases, Dobson and Brewer sites demonstrated 5- year mean differences with satellites to be within +/- 3% ( for DS observations). The seasonal median difference between all Brewer DS measurements at 25 degrees- 60 degrees N and GOME and OMI overpasses remained within +/- 0.5% over a period of more than 10 years. The satellite instrument performance was also analyzed to determine typical measurement uncertainties. It is demonstrated that systematic differences between the analyzed satellite instruments are typically within +/- 2% and very rarely are they outside the +/- 3% envelope. As the satellite instrument measurements appear to be better than +/- 3%, ground- based instruments with precision values worse than +/- 3% are not particularly useful for the analyses of long- term changes and comparison with numerical simulations. C1 [Fioletov, V. E.; Hare, E. W.; McElroy, C. T.; Savastiouk, V.] Environm Canada, ARQX, Toronto, ON M3H 5T4, Canada. [Koehler, U.] Meteorol Observ Hohenpeissenberg, German Weather Serv, D-82383 Hohenpeissenberg, Germany. [Labow, G.] Goddard Space Flight Ctr, NASA, Lanham, MD 20706 USA. [Labow, G.] Goddard Space Flight Ctr, SSAI Lanham, Lanham, MD 20706 USA. [Miyagawa, K.] Japan Meteorol Agcy, Aerol Observ, Ozone & Radiat Div, Tsukuba, Ibaraki 305, Japan. [Redondas, A.] Natl Inst Meteorol, Izana Observ, E-38071 Santa Cruz de Tenerife, Spain. [Shalamyansky, A. M.] Main Geophys Observ, St Petersburg 194018, Russia. [Staehelin, J.] Swiss Fed Inst Technol, Inst Atmospher & Climate Sci, CH-8092 Zurich, Switzerland. [Vanicek, K.] Czech Hydrometeorol Inst, Solar & Ozone Observ, Hradec Kralove 50008 8, Czech Republic. [Weber, M.] Univ Bremen, Inst Environm Phys & Remote Sensing, D-28359 Bremen, Germany. [Evans, R.] NOAA Earth Syst Res Lab, Global Monitoring Div, Boulder, CO 80305 USA. RP Fioletov, VE (reprint author), Environm Canada, ARQX, 4905 Dufferin St, Toronto, ON M3H 5T4, Canada. EM vitali.fioletov@ec.gc.ca RI Redondas, Alberto/L-9299-2015; OI Redondas, Alberto/0000-0002-4826-6823; Fioletov, Vitali/0000-0002-2731-5956 NR 36 TC 47 Z9 49 U1 1 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 31 PY 2008 VL 113 IS D14 AR D14313 DI 10.1029/2008JD009809 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 333KJ UT WOS:000258151100005 ER PT J AU Brown, RH Soderblom, LA Soderblom, JM Clark, RN Jaumann, R Barnes, JW Sotin, C Buratti, B Baines, KH Nicholson, PD AF Brown, R. H. Soderblom, L. A. Soderblom, J. M. Clark, R. N. Jaumann, R. Barnes, J. W. Sotin, C. Buratti, B. Baines, K. H. Nicholson, P. D. TI The identification of liquid ethane in Titan's Ontario Lacus SO NATURE LA English DT Article ID MU-M; SURFACE; ICE; SATELLITES; SATURN; SYSTEM; OCEAN; LAKES; SEAS AB Titan was once thought to have global oceans of light hydrocarbons on its surface(1-5), but after 40 close flybys of Titan by the Cassini spacecraft, it has become clear that no such oceans exist(6). There are, however, features similar to terrestrial lakes and seas(7), and widespread evidence for fluvial erosion(8,9), presumably driven by precipitation of liquid methane from Titan's dense, nitrogen-dominated atmosphere(10). Here we report infrared spectroscopic data, obtained by the Visual and Infrared Mapping Spectrometer(11) ( VIMS) on board the Cassini spacecraft, that strongly indicate that ethane, probably in liquid solution with methane, nitrogen and other low- molecular- mass hydrocarbons, is contained within Titan's Ontario Lacus. C1 [Brown, R. H.; Soderblom, J. M.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Soderblom, L. A.] US Geol Survey, Flagstaff, AZ 86001 USA. [Clark, R. N.] US Geol Survey, Lakewood, CO 80225 USA. [Jaumann, R.] Deutsch Zentrum Luft & Raumfahrt, D-12489 Berlin, Germany. [Barnes, J. W.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Sotin, C.; Buratti, B.; Baines, K. H.] CALTECH, Jet Prop Lab, Pasadena, CA 91107 USA. [Nicholson, P. D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Brown, RH (reprint author), Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. EM rhb@lpl.arizona.edu RI Barnes, Jason/B-1284-2009; OI Barnes, Jason/0000-0002-7755-3530; Soderblom, Jason/0000-0003-3715-6407 NR 29 TC 147 Z9 148 U1 5 U2 15 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JUL 31 PY 2008 VL 454 IS 7204 BP 607 EP 610 DI 10.1038/nature07100 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 331QC UT WOS:000258026500039 PM 18668101 ER PT J AU Wik, M Viljanen, A Pirjola, R Pulkkinen, A Wintoft, P Lundstedt, H AF Wik, M. Viljanen, A. Pirjola, R. Pulkkinen, A. Wintoft, P. Lundstedt, H. TI Calculation of geomagnetically induced currents in the 400 kV power grid in southern Sweden SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID ELEMENTARY CURRENT SYSTEMS; SPACE WEATHER; TRANSMISSION-SYSTEM; ELECTRIC-FIELDS; STORMS; RISKS; FLOW AB Sweden has experienced many geomagnetically induced current (GIC) events in the past, which is obviously due to the high-latitude location of the country. The largest GIC, almost 300 A, was measured in southern Sweden in the earthing lead of a 400 kV transformer neutral during the magnetic storm on 6 April 2000. On 30 October 2003, the city of Malmo at the southern coast suffered from a power blackout caused by GIC, leaving 50,000 customers without electricity for about 20-50 min. We have developed a model that enables calculation of GIC in the southern Swedish 400 kV power grid. This work constitutes the first modeling effort of GIC in Sweden. The model is divided into two parts. The electric field is first derived using a ground conductivity model and geomagnetic recordings from nearby stations. The conductivity model is determined from a least squares fit between measured and calculated GIC. GIC are calculated using a power grid model consisting of the topology of the system and of the transformer, transmission line, and station earthing resistances as well as of the coordinates of the stations. To validate the model, we have compared measured and calculated GIC from one site. In total, 24 events in 1998 to 2000 were used. In general the agreement is satisfactory as the correct GIC order of magnitude is obtained by the model, which is usually enough for engineering applications. C1 [Wik, M.; Wintoft, P.; Lundstedt, H.] Swedish Inst Space Phys, SE-22370 Lund, Sweden. [Wik, M.] Lund Univ, Dept Phys, Lund, Sweden. [Viljanen, A.; Pirjola, R.] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland. [Pulkkinen, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Pulkkinen, A.] Univ Maryland, Goddard Earth Sci & Technol Ctr, College Pk, MD 20742 USA. RP Wik, M (reprint author), Swedish Inst Space Phys, Scheelevagen 17, SE-22370 Lund, Sweden. EM magnus@lund.irf.se NR 29 TC 31 Z9 38 U1 2 U2 6 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 31 PY 2008 VL 6 IS 7 AR S07005 DI 10.1029/2007SW000343 PG 11 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 333MY UT WOS:000258157800001 ER PT J AU Tansel, B Sager, J Garland, J Xu, SH Levine, L Bisbee, P AF Tansel, Berrin Sager, John Garland, Jay Xu, Shaohua Levine, Lanfang Bisbee, Patricia TI Biofouling affinity of membrane surfaces under quiescent conditions SO DESALINATION LA English DT Article DE extracellular polymeric substances (EPS); soluble microbial products (SMP); biofouling; membrane morphology; atomic force microscopy (AFM); wetting angle ID SIZE-EXCLUSION CHROMATOGRAPHY; ACTIVATED-SLUDGE EXOPOLYMERS; SOLUBLE MICROBIAL PRODUCTS; BACTERIAL ADHESION; POLYSACCHARIDES AB Biofouling affinity of four thin film membranes was evaluated under quiescent conditions by exposing the membrane to the effluent from a membrane bioreactor. Coupons of the thin film membranes were left for 5 days in the bioreactor effluent Which was filtered through a 0.2 micron filter. The surface morphologies of the membranes before and after the exposure were evaluated by atomic force microscopy (AFM). All membranes showed significant amounts of deposits after the exposure. The easily disturbed nature of the deposits on the polyamide membrane indicated that these deposits were either entrapped within the surface crevices or loosely attached on the membrane. The extent of surface coverage and uniform appearance of the deposits on the polysulfone membrane were indicative Of Molecular adhesion by functional groups oil the membrane surface. Based on the wetting angle measurements, all clean membranes exhibited hydrophilic characteristics. After exposure to the bioreactor effluent, the membranes exhibited complete wetting characteristics. The use of AFM image analysis technique provided insight for the morphological changes and Substrate accumulation patterns on membrane surfaces. C1 [Tansel, Berrin] Florida Int Univ, Dept Civil & Environm Engn, Miami, FL 33199 USA. [Sager, John] Kennedy Space Ctr, NASA, Cape Canaveral, FL USA. [Garland, Jay; Levine, Lanfang; Bisbee, Patricia] Gen Dynam Corp, Kennedy Space Ctr, Cape Canaveral, FL USA. [Xu, Shaohua] Kennedy Space Ctr, Florida Space Res Inst, Cape Canaveral, FL USA. RP Tansel, B (reprint author), Florida Int Univ, Dept Civil & Environm Engn, Miami, FL 33199 USA. EM tanselb@fiu.edu NR 25 TC 11 Z9 11 U1 2 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0011-9164 J9 DESALINATION JI Desalination PD JUL 30 PY 2008 VL 227 IS 1-3 BP 264 EP 273 DI 10.1016/j.desal.2007.06.030 PG 10 WC Engineering, Chemical; Water Resources SC Engineering; Water Resources GA 338XK UT WOS:000258542500024 ER PT J AU Davila, AF Fairen, AG Gago-Duport, L Stoker, C Amils, R Bonaccorsi, R Zavaleta, J Lim, D Schulze-Makuch, D Mckay, CP AF Davila, Alfonso F. Fairen, Alberto G. Gago-Duport, Luis Stoker, Carol Amils, Ricardo Bonaccorsi, Rosalba Zavaleta, Jhony Lim, Darlene Schulze-Makuch, Dirk McKay, Christopher P. TI Subsurface formation of oxidants on Mars and implications for the preservation of organic biosignatures SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Mars; organic compounds; pyrite; aqueous oxidation; hydrogen peroxide ID AQUEOUS PYRITE OXIDATION; MERIDIANI-PLANUM; WEATHERING PRODUCTS; FERRIC IRON; SURFACE; ENVIRONMENT; ATMOSPHERE; MINERALOGY; LIFE; MECHANISM AB Hydrogen peroxide can form through the interaction of pyrite and anoxic water. The oxidation of pyrite results in the precipitation of sulfates and iron oxides, high redox potentials (similar to 1000 mV) and acidic pH (3-4). The oxidative potential of the resultant solution may be responsible for the oxidation of organic compounds, as observed in the subsurface of the Rio Tinto Mars analog. On Mars subsurface migration of groundwater interacting with volcanogenic massive pyrite deposits would have mobilized acidic and oxidizing fluids through large portions of the crust, resulting in the widespread deposition of sulfates and iron oxides. This groundwater could have leached substantial volumes of aquifer material and crustal rocks, thereby erasing any organic Compounds possibly down to depths of hundreds of meters. Therefore, the preservation of organic biosignatures must have been severely constrained in the portions of the ancient Martian crust that were exposed to aqueous processes, calling for a redefinition of the future targets in the search for biomolecular traces of life on Mars. (C) 2008 Elsevier B.V. All rights reserved. C1 [Davila, Alfonso F.; Fairen, Alberto G.; Stoker, Carol; Bonaccorsi, Rosalba; Zavaleta, Jhony; Lim, Darlene; McKay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Gago-Duport, Luis] Univ Vigo, Dpto Geociencias Marinas, Vigo 36200, Spain. [Amils, Ricardo] CSIC INTA, Ctr Astrobiol, Madrid 28850, Spain. [Schulze-Makuch, Dirk] Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99163 USA. RP Davila, AF (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM afernandez-davila@arc.nasa.gov RI Davila, Alfonso/A-2198-2013; OI Davila, Alfonso/0000-0002-0977-9909; Schulze-Makuch, Dirk/0000-0002-1923-9746 FU Oak Ridge Associated Universities; Centro de Astrobiologia; NASA ASTEP program FX AFD, AGF and RB wish to thank the Oak Ridge Associated Universities for financial Support. We wish to thank the MARTE team for obtaining the data of the project Used in this work and also the funds from the Centro de Astrobiologia and the NASA ASTEP program, devoted to the development of the project. We are also grateful to V. Chevrier and V. Baker for their valuable reviews. NR 48 TC 30 Z9 31 U1 0 U2 16 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD JUL 30 PY 2008 VL 272 IS 1-2 BP 456 EP 463 DI 10.1016/j.epsl.2008.05.015 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 347DD UT WOS:000259119900045 ER PT J AU Heinrich, JC Sajja, UK Felicelli, SD Westra, DG AF Heinrich, J. C. Sajja, U. K. Felicelli, S. D. Westra, D. G. TI Projection method for flows with large local density gradients: Application to dendritic solidification SO INTERNATIONAL JOURNAL FOR NUMERICAL METHODS IN FLUIDS LA English DT Article; Proceedings Paper CT 14th International Conference on Finite Elements in Flow Problems CY MAR 24-28, 2007 CL Santa Fe, NM DE mushy zone model; finite elements; dendritic solidification; projection method; channel formation; three-dimensional solidification ID NAVIER-STOKES EQUATIONS; BINARY ALLOY SOLIDIFICATION; FRACTIONAL-STEP METHOD; FINITE-ELEMENT-METHOD; VISCOUS INCOMPRESSIBLE-FLOW; PHASE-CHANGE PROBLEMS; DIRECTIONAL SOLIDIFICATION; FLUID-FLOW; VERTICAL SOLIDIFICATION; INTERDENDRITIC LIQUID AB Numerical models of solidification including a mushy zone are notoriously inefficient; most of them are based on formulations that require the coupled solution to the velocity components in the momentum equation greatly restricting the range of applicability of the models. Initial attempts at modeling directional solidification in the presence of a developing mushy zone using a projection formulation encountered difficulties once solidification starts, which were traced to the inability of the method to deal with large local density differences in the vicinity of the fluid-mush interface. A modified formulation of the projection method has been developed that maintains the coupling between the body force and the pressure gradient and is presented in this work. This formulation is shown to be robust and extremely efficient; reducing very significantly the necessary storage and the computational time required for the simulation of problems involving very large meshes when compared with previously published data. This is illustrated in this work through its application to simulations involving a Pb-Sn alloy. Copyright (C) 2008 John Wiley & Sons, Ltd. C1 [Heinrich, J. C.] Univ New Mexico, Dept Mech Engn, Albuquerque, NM 87131 USA. [Sajja, U. K.; Felicelli, S. D.] Mississippi State Univ, Dept Mech Engn, Mississippi State, MS 39762 USA. [Westra, D. G.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Heinrich, JC (reprint author), Univ New Mexico, Dept Mech Engn, Albuquerque, NM 87131 USA. EM heinrich@unm.edn NR 65 TC 7 Z9 7 U1 0 U2 7 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND SN 0271-2091 J9 INT J NUMER METH FL JI Int. J. Numer. Methods Fluids PD JUL 30 PY 2008 VL 57 IS 9 BP 1211 EP 1226 DI 10.1002/fld.1812 PG 16 WC Computer Science, Interdisciplinary Applications; Mathematics, Interdisciplinary Applications; Mechanics; Physics, Fluids & Plasmas SC Computer Science; Mathematics; Mechanics; Physics GA 332PT UT WOS:000258096300010 ER PT J AU Mannino, A Russ, ME Hooker, SB AF Mannino, Antonio Russ, Mary E. Hooker, Stanford B. TI Algorithm development and validation for satellite-derived distributions of DOC and CDOM in the US Middle Atlantic Bight SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID DISSOLVED ORGANIC-MATTER; INHERENT OPTICAL-PROPERTIES; COASTAL UPWELLING SYSTEM; WATER-LEAVING RADIANCES; CHESAPEAKE BAY; OCEAN COLOR; CONTINENTAL-SHELF; SURFACE WATERS; NORTH-ATLANTIC; ABOVE-WATER AB [1] Oceanographic cruises were conducted within the U. S. Middle Atlantic Bight ( MAB) to collect field measurements to develop algorithms to retrieve surface ocean colored dissolved organic matter ( CDOM) and dissolved organic carbon ( DOC) from NASA's MODIS- Aqua and SeaWiFS satellite sensors and to investigate the processes that influence the distributions of CDOM and DOC. In order to develop empirical algorithms for CDOM and DOC, the CDOM absorption coefficient ( aCDOM) was correlated with in situ remote sensing reflectance band ratios, and DOC was then derived from aCDOM through the aCDOM to DOC relationships. Our validation analyses demonstrate successful retrieval of DOC and CDOM using MODIS and SeaWiFS with mean absolute percent differences from field measurements of 9.3 +/- 7.3% for DOC, 19 +/- 14% for aCDOM( 355), 15.5 +/- 12% for aCDOM( 443), and 8.6 +/- 4.9% for the CDOM spectral slope. To our knowledge, the algorithms presented here represent the first validated algorithms for satellite retrieval of aCDOM, DOC, and CDOM spectral slope in the coastal ocean. Satellite imagery demonstrates the importance of riverine/ estuarine discharge from Chesapeake Bay and Delaware Bay to the export of CDOM and DOC to the coastal ocean. Between spring and summer, photooxidation has a significant impact on CDOM distributions resulting in a pronounced decrease in aCDOM between the midshelf and continental slope region of the MAB. The satellite- derived DOC products demonstrate the net ecosystem production of DOC of 12 to 34 mmol C L(-1) between spring and summer. The aCDOM algorithms presented here are applicable to other coastal regions and can also be used to retrieve DOC using region- specific aCDOM to DOC relationships. C1 [Mannino, Antonio; Russ, Mary E.; Hooker, Stanford B.] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA. [Russ, Mary E.] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. RP Mannino, A (reprint author), NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Mail Code 614-2, Greenbelt, MD 20771 USA. EM antonio.mannino@nasa.gov RI Hooker, Stanford/E-2162-2012; Mannino, Antonio/I-3633-2014 NR 81 TC 85 Z9 87 U1 7 U2 44 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 30 PY 2008 VL 113 IS C7 AR C07051 DI 10.1029/2007JC004493 PG 19 WC Oceanography SC Oceanography GA 333LX UT WOS:000258155100005 ER PT J AU Ebihara, Y Fok, MC Blake, JB Fennell, JF AF Ebihara, Y. Fok, M. -C. Blake, J. B. Fennell, J. F. TI Magnetic coupling of the ring current and the radiation belt SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID PITCH-ANGLE DISTRIBUTIONS; INNER MAGNETOSPHERE; ENERGETIC PARTICLE; TRAPPED PARTICLES; STORM; MODEL; FIELD; PRECIPITATION; MAGNETOTAIL; PROTONS AB The magnetic influence of the storm time ring current on high-energy particles is demonstrated by using a simulation of the ring current incorporating self-consistent magnetic and electric fields. Observations by the Polar satellite show that the magnetic field is occasionally depressed by 50% or more near the equatorial plane at < 6 R(E). We call them equatorially magnetic depression events ( EMDEs) and focus on the most intense EMDE observed during an intense storm on 22 October 1999. The simulation predicts that under a strong convection electric field, the magnetic field strength is highly depressed around L = 5 by newly injected ions of energy 80 keV or less. The depressed magnetic field causes a significant adiabatic decrease in the high-energy ion flux at pitch angles near 90 degrees to conserve the first adiabatic invariant. A more tail- like (shortened) magnetic field line causes an enhancement of the flux at pitch angles near 0 degrees and 180 degrees to conserve the second adiabatic invariant. Consequently, a butterfly- like pitch angle distribution (PAD) is formed, which agrees with the Polar observation. We propose that the adiabatic process could have acted not only on the high-energy component of the protons but also on relativistic electrons in the outer radiation belt. This notion is supported by simultaneous Polar observation of relativistic electron fluxes that show a decrease at pitch angles near 90 degrees and a slight increase at pitch angles near 0 degrees and 180 degrees. PADs of protons and electrons can be used to distinguish nonadiabatic processes acting selectively on electrons from adiabatic ones. C1 [Ebihara, Y.] Nagoya Univ, Inst Adv Res, Chikusa Ku, Nagoya, Aichi 4648601, Japan. [Blake, J. B.; Fennell, J. F.] Aerosp Corp, Dept Space Sci, Los Angeles, CA 90009 USA. [Fok, M. -C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ebihara, Y (reprint author), Nagoya Univ, Inst Adv Res, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648601, Japan. EM ebihara@stelab.nagoya-u.ac.jp RI Fok, Mei-Ching/D-1626-2012; Ebihara, Yusuke/D-1638-2013 OI Ebihara, Yusuke/0000-0002-2293-1557 NR 57 TC 20 Z9 22 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 JUL 30 PY 2008 VL 113 IS A7 AR A07221 DI 10.1029/2008JA013267 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 333MK UT WOS:000258156400007 ER PT J AU Kuang, W Jiang, W Wang, T AF Kuang, W. Jiang, W. Wang, T. TI Sudden termination of Martian dynamo?: Implications from subcritical dynamo simulations SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MAGNETIC-FIELD; THERMAL EVOLUTION; MARS; CORE; GEODYNAMO; CONVECTION AB [1] The crustal magnetism measured by the Mars Global Surveyor requires that Mars possessed a strong internal field generated by a core dynamo in its early history. We use a numerical model to simulate the early Martian dynamo, focusing on the minimum energy for sustaining an established dynamo. Our results show that near its end, the Martian dynamo could reverse frequently, and could be subcritical: the energy to sustain the dynamo is significantly less than that to excite the dynamo. In addition to a longer lifetime, the subcritical dynamo implies that it could be terminated suddenly with a very small perturbation and, once turned off, it could not be reactivated without substantial increase of the buoyancy force in the Martian core. C1 [Kuang, W.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Jiang, W.] Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. [Wang, T.] Chinese Acad Sci, Grad Univ, Sch Earth Sci, Beijing 10049, Peoples R China. RP Kuang, W (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Mail Stop 698, Greenbelt, MD 20771 USA. EM weijia.kuang-1@nasa.gov; jiangw@umbc.edu; tywang@mails.gucas.ac.cn RI Kuang, Weijia/K-5141-2012 OI Kuang, Weijia/0000-0001-7786-6425 NR 24 TC 34 Z9 36 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 29 PY 2008 VL 35 IS 14 AR L14204 DI 10.1029/2008GL034183 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 333JO UT WOS:000258149000003 ER PT J AU Remer, LA Kleidman, RG Levy, RC Kaufman, YJ Tanre, D Mattoo, S Martins, JV Ichoku, C Koren, I Yu, HB Holben, BN AF Remer, Lorraine A. Kleidman, Richard G. Levy, Robert C. Kaufman, Yoram J. Tanre, Didier Mattoo, Shana Martins, J. Vanderlei Ichoku, Charles Koren, Ilan Yu, Hongbin Holben, Brent N. TI Global aerosol climatology from the MODIS satellite sensors SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID RESOLUTION IMAGING SPECTRORADIOMETER; OPTICAL DEPTH; TROPOSPHERIC AEROSOLS; SPECTRAL RADIANCES; AIRBORNE SIMULATOR; SIZE DISTRIBUTION; OCEAN; RETRIEVALS; AERONET; ALGORITHM AB The recently released Collection 5 Moderate Resolution Imaging Spectroradiometer (MODIS) aerosol products provide a consistent record of the Earth's aerosol system. Comparing with ground-based AERONET observations of aerosol optical depth (AOD) we find that Collection 5 MODIS aerosol products estimate AOD to within expected accuracy more than 60% of the time over ocean and more than 72% of the time over land. This is similar to previous results for ocean and better than the previous results for land. However, the new collection introduces a 0.015 offset between the Terra and Aqua global mean AOD over ocean, where none existed previously. Aqua conforms to previous values and expectations while Terra is higher than what had been expected. The cause of the offset is unknown, but changes to calibration are a possible explanation. Even though Terra's higher ocean AOD is unexpected and unexplained, we present climatological analyses of data from both sensors. We find that the multiannual global mean AOD at 550 nm over oceans is 0.13 for Aqua and 0.14 for Terra, and over land it is 0.19 in both Aqua and Terra. AOD in situations with 80% cloud fraction are twice the global mean values, although such situations occur only 2% of the time over ocean and less than 1% of the time over land. Aerosol particle size associated with these very cloudy situations does not show a drastic change over ocean, but does over land. Regionally, aerosol amounts vary from polluted areas such as east Asia and India, to the cleanest regions such as Australia and the northern continents. As AOD increases over maritime background conditions, fine mode aerosol dominates over dust over all oceans, except over the tropical Atlantic downwind of the Sahara and during some months over the Arabian Sea. C1 [Remer, Lorraine A.; Kleidman, Richard G.; Levy, Robert C.; Mattoo, Shana; Martins, J. Vanderlei; Ichoku, Charles; Yu, Hongbin] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Holben, Brent N.] NASA, Goddard Space Flight Ctr, Terr Phys Lab, Greenbelt, MD 20771 USA. [Koren, Ilan] Weizmann Inst Sci, IL-76100 Rehovot, Israel. [Tanre, Didier] Univ Lille 1, Opt Atmospher Lab, F-59655 Villeneuve Dascq, France. [Kleidman, Richard G.; Levy, Robert C.; Mattoo, Shana] Sci Syst & Applicat Inc, Lanham, MD USA. [Martins, J. Vanderlei] Univ Maryland, Dept Phys, Baltimore, MD 21201 USA. [Ichoku, Charles] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Yu, Hongbin] Univ Maryland, Goddard Earth Sci & Technol Inst, Baltimore, MD 21201 USA. RP Remer, LA (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 613-2, Greenbelt, MD 20771 USA. EM lorraine.a.remer@nasa.gov RI Ichoku, Charles/E-1857-2012; Yu, Hongbin/C-6485-2008; Koren, Ilan/K-1417-2012; Levy, Robert/M-7764-2013 OI Ichoku, Charles/0000-0003-3244-4549; Yu, Hongbin/0000-0003-4706-1575; Koren, Ilan/0000-0001-6759-6265; Levy, Robert/0000-0002-8933-5303 NR 51 TC 283 Z9 289 U1 8 U2 55 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 29 PY 2008 VL 113 IS D14 AR D14S07 DI 10.1029/2007JD009661 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 333KG UT WOS:000258150800006 ER PT J AU Xia, XG Eck, TF Holben, BN Phillippe, G Chen, HB AF Xia, Xiangao Eck, Tom F. Holben, Brent N. Phillippe, Goloub Chen, Hongbin TI Analysis of the weekly cycle of aerosol optical depth using AERONET and MODIS data SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID RESOLUTION IMAGING SPECTRORADIOMETER; AIR-POLLUTANTS; NEW-YORK; NETWORK; PM2.5; LAND AB Multi-year Aerosol Robotic Network (AERONET) and Moderate Resolution Imaging Spectroradiometer (MODIS) aerosol optical depth (AOD) data are used to study AOD weekly variations at the global scale. A clear weekly cycle of AOD is observed in the United States (U. S.) and Central Europe. AOD during the weekday is larger than that during the weekend in 36 out of 43 AERONET sites in the U. S. The average U. S. weekend effect (the percent difference in AOD during the weekday and the weekend) is 3.8%. A weekly periodicity with lower AODs on Sunday and Monday and higher AODs from Wednesday until Saturday is revealed over Central Europe and the average weekend effect there is 4.0%. The weekly cycle in urban sites is greater than that in rural sites. AOD during the weekday is also significantly larger than that during the weekend in urban AERONET sites in South America and South Korea. However, a reversed AOD weekly cycle is observed in the Middle East and India. AODs on Thursday and Friday, the "weekend'' for Middle East cultures, are relatively lower than AODs on other days. There is no clear weekly variation of AOD over eastern China. The striking feature in this region is the occurrence of much higher AOD on Sunday and this phenomenon is independent of season. The analysis of MODIS aerosol data is in good agreement with that of AERONET data. C1 [Xia, Xiangao; Chen, Hongbin] Chinese Acad Sci, Inst Atmospher Phys, LAGEO, Beijing 100029, Peoples R China. [Eck, Tom F.; Holben, Brent N.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Phillippe, Goloub] Univ Sci & Tech Lille Flandres Artois, Opt Atmospher Lab, F-59655 Villeneuve Dascq, France. RP Xia, XG (reprint author), Chinese Acad Sci, Inst Atmospher Phys, LAGEO, 40 Huanyanbeili, Beijing 100029, Peoples R China. EM xiaxiangao2000@yahoo.com RI ECK, THOMAS/D-7407-2012; Xia, Xiangao/G-5545-2011 OI Xia, Xiangao/0000-0002-4187-6311 NR 32 TC 32 Z9 34 U1 0 U2 14 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 29 PY 2008 VL 113 IS D14 AR D14217 DI 10.1029/2007JD009604 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 333KG UT WOS:000258150800004 ER PT J AU Gutsev, GL Mochena, MD Bauschlicher, CW Zheng, WJ Thomas, OC Bowen, KH AF Gutsev, G. L. Mochena, M. D. Bauschlicher, Charles W., Jr. Zheng, W. -J. Thomas, O. C. Bowen, Kit H. TI Electronic and geometrical structure of Mn-13 anions, cations, and neutrals SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID DENSITY-FUNCTIONAL THEORY; MANGANESE CLUSTERS; SPIN-RESONANCE; ENERGY; SPECTROSCOPY; MOLECULES; TRIMER AB We have computed the electronic and geometrical structures of thirteen atom manganese clusters in all three charge states, Mn-13(-), Mn-13(+), and Mn-13 by using density functional theory with the generalized gradient approximation. Our results for Mn-13(-) are compared with our anion photoelectron spectrum of Mn-13(-), published in this paper. Our results for Mn-13(+) are compared with the previously published photoionization results of Knickelbein [J. Chem. Phys. 106, 9810 (1997)]. There is a good agreement between theoretical and experimental values of ionization and electron attachment energies. (C) 2008 American Institute of Physics. C1 [Gutsev, G. L.; Mochena, M. D.] Florida A&M Univ, Dept Phys, Tallahassee, FL 32307 USA. [Bauschlicher, Charles W., Jr.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Zheng, W. -J.; Thomas, O. C.; Bowen, Kit H.] Johns Hopkins Univ, Dept Chem, Baltimore, MD 21218 USA. [Zheng, W. -J.; Thomas, O. C.; Bowen, Kit H.] Johns Hopkins Univ, Dept Mat Sci, Baltimore, MD 21218 USA. RP Gutsev, GL (reprint author), Florida A&M Univ, Dept Phys, Tallahassee, FL 32307 USA. EM gennady.gutsev@famu.edu; kbowen@jbu.edu NR 38 TC 12 Z9 12 U1 0 U2 4 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD JUL 28 PY 2008 VL 129 IS 4 AR 044310 DI 10.1063/1.2956494 PG 5 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 333SB UT WOS:000258171500027 PM 18681649 ER PT J AU Huang, XC Lee, TJ AF Huang, Xinchuan Lee, Timothy J. TI A procedure for computing accurate ab initio quartic force fields: Application to HO2+ and H2O SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID POTENTIAL-ENERGY SURFACE; CORRELATED MOLECULAR CALCULATIONS; GAUSSIAN-BASIS SETS; VIBRATIONAL FREQUENCIES; ELECTRONIC-STRUCTURE; WATER; SPECTRUM; ISOTOPOMERS; COMPUTATION; PREDICTION AB A procedure for the calculation of molecular quartic force fields (QFFs) is proposed and investigated. The goal is to generate highly accurate ab initio QFFs that include many of the so-called "small" effects that are necessary to achieve high accuracy. The small effects investigated in the present study include correlation of the core electrons (core correlation), extrapolation to the one-particle basis set limit, correction for scalar relativistic contributions, correction for higher-order correlation effects, and inclusion of diffuse functions in the one-particle basis set. The procedure is flexible enough to allow for some effects to be computed directly, while others may be added as corrections. A single grid of points is used and is centered about an initial reference geometry that is designed to be as close as possible to the final ab initio equilibrium structure (with all effects included). It is shown that the least-squares fit of the QFF is not compromised by the added corrections, and the balance between elimination of contamination from higher-order force constants while retaining energy differences large enough to yield meaningful quartic force constants is essentially unchanged from the standard procedures we have used for many years. The initial QFF determined from the least-squares fit is transformed to the exact minimum in order to eliminate gradient terms and allow for the use of second-order perturbation theory for evaluation of spectroscopic constants. It is shown that this step has essentially no effect on the quality of the QFF largely because the initial reference structure is, by design, very close to the final ab initio equilibrium structure. The procedure is used to compute an accurate, purely ab initio QFF for the H2O molecule, which is used as a benchmark test case. The procedure is then applied to the ground and first excited electronic states of the HO2+ molecular cation. Fundamental vibrational frequencies and spectroscopic constants from these highly accurate QFFs are compared and contrasted with previous experiment and theory. It is concluded that the spectroscopic constants determined for the X(3)A' and A(1)A' states of HO2+ are the most accurately available. (C) 2008 American Institute of Physics. C1 [Huang, Xinchuan; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Lee, TJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM xinchuan.huang-1@nasa.gov; timothy.j.lee@nasa.gov RI HUANG, XINCHUAN/A-3266-2013; Lee, Timothy/K-2838-2012 NR 54 TC 70 Z9 70 U1 2 U2 12 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD JUL 28 PY 2008 VL 129 IS 4 AR 044312 DI 10.1063/1.2957488 PG 14 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 333SB UT WOS:000258171500029 PM 18681651 ER PT J AU Zeitlin, C Guetersloh, S Heilbronn, L Miller, J Elkhayari, N Empl, A LeBourgeois, M Mayes, BW Pinsky, L Christl, M Kuznetsov, E AF Zeitlin, C. Guetersloh, S. Heilbronn, L. Miller, J. Elkhayari, N. Empl, A. LeBourgeois, M. Mayes, B. W. Pinsky, L. Christl, M. Kuznetsov, E. TI Shielding experiments with high-energy heavy ions for spaceflight applications SO NEW JOURNAL OF PHYSICS LA English DT Article ID CROSS-SECTIONS; FRAGMENTATION; FE-56; MODEL AB Mitigation of radiation exposures received by astronauts on deep-space missions must be considered in the design of future spacecraft. The galactic cosmic rays (GCR) include high-energy heavy ions, many of which have ranges that exceed the depth of shielding that can be launched in realistic scenarios. Some of these ions are highly ionizing (producing a high dose per particle) and for some biological endpoints are more damaging per unit dose than sparsely ionizing radiation. The principal physical mechanism by which the dose and dose equivalent delivered by these particles can be reduced is nuclear fragmentation, the result of inelastic collisions between nuclei in the hull of the spacecraft and/or other materials. These interactions break the incident ions into lighter, less ionizing and less biologically effective particles. We have previously reported the tests of shielding effectiveness using many materials in a 1 GeV nucleon(-1) (56)Fe beam, and also reported results using a single polyethylene (CH(2)) target in a variety of beam ions and energies up to 1 GeV nucleon(-1). An important, but tentative, conclusion of those studies was that the average behavior of heavy ions in the GCR would be better simulated by heavy beams at energies above 1 GeV nucleon(-1). Following up on that work, we report new results using beams of (12)C, (28)Si and (56)Fe, each at three energies, 3, 5 and 10 GeV nucleon(-1), on carbon, polyethylene, aluminium and iron targets. C1 [Zeitlin, C.; Guetersloh, S.; Heilbronn, L.; Miller, J.] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. [Elkhayari, N.; Empl, A.; LeBourgeois, M.; Mayes, B. W.; Pinsky, L.] Univ Houston, Dept Phys, Houston, TX USA. [Christl, M.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Kuznetsov, E.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. RP Zeitlin, C (reprint author), Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. EM cjzeitlin@lbl.gov RI Heilbronn, Lawrence/J-6998-2013 OI Heilbronn, Lawrence/0000-0002-8226-1057 NR 13 TC 5 Z9 6 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1367-2630 J9 NEW J PHYS JI New J. Phys. PD JUL 28 PY 2008 VL 10 AR 075007 DI 10.1088/1367-2630/10/7/075007 PG 20 WC Physics, Multidisciplinary SC Physics GA 330TV UT WOS:000257966600005 ER PT J AU Lillis, RJ Frey, HV Manga, M AF Lillis, R. J. Frey, H. V. Manga, M. TI Rapid decrease in Martian crustal magnetization in the Noachian era: Implications for the dynamo and climate of early Mars SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ELECTRON REFLECTOMETRY; EVOLUTION; FIELD; HISTORY; ROCKS; SHOCK AB The magnetic signatures and crater retention ages of the 19 largest (> 1000 km diameter) impact basins on Mars are examined to constrain the history of the acquisition of crustal magnetization during the Noachian era. The 5 most clearly impact-demagnetized basins are younger than the 14 basins within which lies substantially re-magnetized crust. Poisson analysis shows that the most likely time of this magnetization cessation was 4.115-4.13 Ga ( model age) and that it occurred quickly, taking less than 20 Ma. A global decrease in effective crustal magnetic susceptibility due, e. g., to a decrease in the rate of hydrothermal alteration, is one possible explanation. Alternatively, the cessation of post-impact magnetization reflects the rapid death of the Martian dynamo. C1 [Lillis, R. J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Frey, H. V.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Manga, M.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. RP Lillis, RJ (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. EM rlillis@ssl.berkeley.edu RI Manga, Michael/D-3847-2013; Lillis, Robert/A-3281-2008; OI Lillis, Robert/0000-0003-0578-517X; Manga, Michael/0000-0003-3286-4682 NR 29 TC 73 Z9 75 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 26 PY 2008 VL 35 IS 14 AR L14203 DI 10.1029/2008GL034338 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 331EV UT WOS:000257996400006 ER PT J AU Loeb, NG Schuster, GL AF Loeb, Norman G. Schuster, Gregory L. TI An observational study of the relationship between cloud, aerosol and meteorology in broken low-level cloud conditions SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID ANGULAR-DISTRIBUTION MODELS; RADIATIVE FLUX ESTIMATION; ENERGY SYSTEM INSTRUMENT; PART I; OPTICAL-PROPERTIES; ATMOSPHERIC AEROSOL; LIGHT-SCATTERING; BOUNDARY-LAYER; SATELLITE; METHODOLOGY AB [1] Global satellite analyses showing strong correlations between aerosol optical depth and cloud cover have stirred much debate recently. While it is tempting to interpret the results as evidence of aerosol enhancement of cloud cover, other factors such as the influence of meteorology on both the aerosol and cloud distributions can also play a role, as both aerosols and clouds depend upon local meteorology. This study uses satellite observations to examine aerosol-cloud relationships for broken low-level cloud regions off the coast of Africa. The analysis approach minimizes the influence of large-scale meteorology by restricting the spatial and temporal domains in which the aerosol and cloud properties are compared. While distributions of several meteorological variables within 5 degrees x 5 degrees latitude-longitude regions are nearly identical under low and high aerosol optical depth, the corresponding distributions of single-layer low cloud properties and top-of-atmosphere radiative fluxes differ markedly, consistent with earlier studies showing increased cloud cover with aerosol optical depth. Furthermore, fine-mode fraction and Angstrom Exponent are also larger in conditions of higher aerosol optical depth, even though no evidence of systematic latitudinal or longitudinal gradients between the low and high aerosol optical depth populations are observed. When the analysis is repeated for all 5 degrees x 5 degrees latitude-longitude regions over the global oceans ( after removing cases in which significant meteorological differences are found between the low and high aerosol populations), results are qualitatively similar to those off the coast of Africa. C1 [Loeb, Norman G.; Schuster, Gregory L.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Loeb, NG (reprint author), NASA, Langley Res Ctr, Mail Stop 420,21 Langley Blvd, Hampton, VA 23681 USA. EM norman.g.loeb@nasa.gov NR 57 TC 64 Z9 67 U1 0 U2 20 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 26 PY 2008 VL 113 IS D14 AR D14214 DI 10.1029/2007JD009763 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 331FK UT WOS:000257997900003 ER PT J AU Marchiarullo, DJ Lim, JY Vaksman, Z Ferrance, JP Putcha, L Landers, JP AF Marchiarullo, Daniel J. Lim, Ji Y. Vaksman, Zalman Ferrance, Jerome P. Putcha, Lakshmi Landers, James P. TI Towards an integrated microfluidic device for spaceflight clinical diagnostics Microchip-based solid-phase extraction of hydroxyl radical markers SO JOURNAL OF CHROMATOGRAPHY A LA English DT Article DE microfluidic; solid-phase extraction; hydroxyl radical; spaceflight ID MICELLAR ELECTROKINETIC CHROMATOGRAPHY; CAPILLARY-ZONE-ELECTROPHORESIS; AMPEROMETRIC DETECTION; SEPARATION METHODS; DNA EXTRACTION; PROTEIN; SAMPLES; SYSTEM; ACID AB A microchip-based solid-phase extraction method for biological fluid small molecule analysis has been developed. Using a commercially available copolymer packed into a microchip channel, extraction and preconcentration of 2,3-dihydroxybenzoic acid (DHBA) and 2,5-DHBA from saliva was achieved. The metabolites, formed from salicylic acid by reactive oxygen species, can be used as markers of oxidative stress. The results show high recovery of both metabolites (> 90 +/- 15% for spiked saliva) with an 80-fold concentration enhancement possible. The eluent is directly analyzed using capillary electrophoresis, with good resolution for the two metabolites. This study demonstrates the feasibility of future integrated microdevices for spaceflight small molecule biomarker analysis. (c) 2008 Published by Elsevier B.V. C1 [Marchiarullo, Daniel J.; Lim, Ji Y.; Ferrance, Jerome P.; Landers, James P.] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA. [Vaksman, Zalman; Putcha, Lakshmi] NASA, Lyndon B Johnson Space Ctr, Life Sci Res Labs, Houston, TX 77058 USA. [Vaksman, Zalman] Wyle Labs, Div Life Sci, Houston, TX 77058 USA. [Landers, James P.] Univ Virginia, Dept Pathol, Charlottesville, VA 22908 USA. [Landers, James P.] Univ Virginia, Dept Mech Engn, Charlottesville, VA 22904 USA. RP Landers, JP (reprint author), Univ Virginia, Dept Chem, McCormick Rd,POB 400319, Charlottesville, VA 22904 USA. EM landers@virginia.edu OI Ferrance, Jerome/0000-0003-1020-8289 NR 24 TC 13 Z9 15 U1 1 U2 19 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0021-9673 J9 J CHROMATOGR A JI J. Chromatogr. A PD JUL 25 PY 2008 VL 1200 IS 2 BP 198 EP 203 DI 10.1016/j.chroma.2008.05.031 PG 6 WC Biochemical Research Methods; Chemistry, Analytical SC Biochemistry & Molecular Biology; Chemistry GA 330QX UT WOS:000257959000013 PM 18555260 ER PT J AU Brinksma, EJ Pinardi, G Volten, H Braak, R Richter, A Schonhardt, A van Roozendael, M Fayt, C Hermans, C Dirksen, RJ Vlemmix, T Berkhout, AJC Swart, DPJ Oetjen, H Wittrock, F Wagner, T Ibrahim, OW de Leeuw, G Moerman, M Curier, RL Celarier, EA Cede, A Knap, WH Veefkind, JP Eskes, HJ Allaart, M Rothe, R Piters, AJM Levelt, PF AF Brinksma, E. J. Pinardi, G. Volten, H. Braak, R. Richter, A. Schoenhardt, A. van Roozendael, M. Fayt, C. Hermans, C. Dirksen, R. J. Vlemmix, T. Berkhout, A. J. C. Swart, D. P. J. Oetjen, H. Wittrock, F. Wagner, T. Ibrahim, O. W. de Leeuw, G. Moerman, M. Curier, R. L. Celarier, E. A. Cede, A. Knap, W. H. Veefkind, J. P. Eskes, H. J. Allaart, M. Rothe, R. Piters, A. J. M. Levelt, P. F. TI The 2005 and 2006 DANDELIONS NO2 and aerosol intercomparison campaigns SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SPECTROSCOPY MAX-DOAS; OZONE MONITORING INSTRUMENT; ABSORPTION SPECTROSCOPY; RADIATIVE-TRANSFER; NITROGEN-DIOXIDE; SUN PHOTOMETER; NETWORK; MODELS AB [1] Dutch Aerosol and Nitrogen Dioxide Experiments for Validation of OMI and SCIAMACHY (DANDELIONS) is a project that encompasses validation of spaceborne measurements of NO2 by the Ozone Monitoring Instrument (OMI) and Scanning Imaging Absorption Spectrometer for Atmospheric Cartography (SCIAMACHY), and of aerosol by OMI and Advanced Along-Track Scanning Radiometer (AATSR), using an extensive set of ground-based and balloon measurements over the polluted area of the Netherlands. We present an extensive data set of ground-based, balloon, and satellite data on NO2, aerosols, and ozone obtained from two campaigns within the project, held during May-June 2005 and September 2006. We have used these data for first validation of OMI NO2, and the data are available through the Aura Validation Data Center website for use in other validation efforts. In this paper we describe the available data, and the methods and instruments used, including the National Institute of Public Health and the Environment (RIVM) NO2 lidar. We show that NO2 from Multi-Axis Differential Optical Absorption Spectroscopy (MAX-DOAS) compares well with in situ measurements. We show that different MAX-DOAS instruments, operating simultaneously during the campaign, give very similar results. We also provide unique information on the spatial homogeneity and the vertical and temporal variability of NO2, showing that during a number of days, the NO2 columns derived from measurements in different directions varied significantly, which implies that, under polluted conditions, measurements in one single azimuth direction are not always representative for the averaged field that the satellite observes. In addition, we show that there is good agreement between tropospheric NO2 from OMI and MAX-DOAS, and also between total NO2 from OMI and direct-sun observations. Observations of the aerosol optical thickness (AOT) show that values derived with three ground-based instruments correspond well with each other, and with aerosol optical thicknesses observed by OMI. C1 [Brinksma, E. J.; Volten, H.; Braak, R.; Dirksen, R. J.; Vlemmix, T.; Knap, W. H.; Veefkind, J. P.; Eskes, H. J.; Allaart, M.; Rothe, R.; Piters, A. J. M.; Levelt, P. F.] Royal Netherlands Meteorol Inst, Climate Res & Seismol Dept, NL-3730 AE De Bilt, Netherlands. [Pinardi, G.; van Roozendael, M.; Fayt, C.; Hermans, C.] Belgian Inst Space Aeron, B-1180 Brussels, Belgium. [Volten, H.; Berkhout, A. J. C.; Swart, D. P. J.] Netherlands Natl Inst Publ Hlth & Environm, RIVM, LVM, NL-3720 BA Bilthoven, Netherlands. [Richter, A.; Schoenhardt, A.; Oetjen, H.; Wittrock, F.] Univ Bremen, Inst Environm Phys, D-28334 Bremen, Germany. [Wagner, T.] Max Planck Inst Chem, D-55020 Mainz, Germany. [Wagner, T.; Ibrahim, O. W.] Heidelberg Univ, Inst Environm Phys, D-69120 Heidelberg, Germany. [de Leeuw, G.; Moerman, M.; Curier, R. L.] TNO, Def Secur & Safety, NL-2509 JG The Hague, Netherlands. [de Leeuw, G.] Finnish Meteorol Inst, Climate Change Unit, R&D, FIN-00101 Helsinki, Finland. [de Leeuw, G.] Univ Helsinki, Dept Phys Sci, Helsinki, Finland. [Celarier, E. A.] SGT Inc, Greenbelt, MD 20770 USA. [Cede, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Brinksma, EJ (reprint author), Royal Netherlands Meteorol Inst, Climate Res & Seismol Dept, POB 201, NL-3730 AE De Bilt, Netherlands. EM brinksma@knmi.nl; hester.volten@rivm.nl; stijn.berkhout@rivm.nl; daan.swart@rivm.nl; gerrit.deleeuw@tno.nl; lyana.curier@tno.nl; edward.a.celarier.1@gsfc.nasa.gov RI Richter, Andreas/C-4971-2008; Wittrock, Folkard/B-6959-2008; Oetjen, Hilke/H-3708-2016 OI Richter, Andreas/0000-0003-3339-212X; Wittrock, Folkard/0000-0002-3024-0211; Oetjen, Hilke/0000-0002-3542-1337 NR 39 TC 60 Z9 62 U1 1 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 25 PY 2008 VL 113 IS D16 AR D16S46 DI 10.1029/2007JD008808 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 331FM UT WOS:000257998100001 ER PT J AU Oreopoulos, L Platnick, S AF Oreopoulos, Lazaros Platnick, Steven TI Radiative susceptibility of cloudy atmospheres to droplet number perturbations: 2. Global analysis from MODIS SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID STRATOCUMULUS CLOUDS; GENERAL-CIRCULATION; AEROSOL; ALBEDO; PARAMETERIZATION; SCATTERING; SATELLITE; POLLUTION; PRODUCTS; MODELS AB Global distributions of albedo susceptibility for areas covered by liquid clouds are presented for 4 months in 2005. The susceptibility estimates are based on expanded definitions presented in a companion paper and include relative cloud droplet number concentration (CDNC) changes, perturbations in cloud droplet asymmetry parameter and single-scattering albedo, atmospheric/surface effects, and incorporation of the full solar spectrum. The cloud properties (optical thickness and effective radius) used as input in the susceptibility calculations come from MODIS Terra and Aqua Collection 5 gridded data. Geographical distributions of susceptibility corresponding to absolute ("absolute cloud susceptibility'') and relative ("relative cloud susceptibility'') CDNC changes are markedly different indicating that the detailed nature of the cloud microphysical perturbation is important for determining the radiative forcing associated with the first indirect aerosol effect. However, both types of susceptibility exhibit common characteristics such as significant reductions when perturbations in single- scattering properties are omitted, significant increases when atmospheric absorption and surface albedo effects are ignored, and the tendency to decrease with latitude, to be higher over ocean than over land, and to be statistically similar between the morning and afternoon MODIS overpasses. The satellite-based susceptibility analysis helps elucidate the role of present-day cloud and land surface properties in indirect aerosol forcing responses. Our realistic yet moderate CDNC perturbations yield forcings on the order of 1-2 W m(-2) for cloud optical property distributions and land surface spectral albedos observed by MODIS. Since susceptibilities can potentially be computed from model fields, these results have practical application in assessing the reasonableness of model-generated estimates of the aerosol indirect radiative forcing. C1 [Oreopoulos, Lazaros] Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. [Platnick, Steven] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Oreopoulos, L (reprint author), Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. EM steven.platnick@nasa.gov RI Oreopoulos, Lazaros/E-5868-2012; Platnick, Steven/J-9982-2014 OI Oreopoulos, Lazaros/0000-0001-6061-6905; Platnick, Steven/0000-0003-3964-3567 NR 25 TC 20 Z9 20 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 25 PY 2008 VL 113 IS D14 AR D14S21 DI 10.1029/2007JD009655 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 331FI UT WOS:000257997700005 ER PT J AU Platnick, S Oreopoulos, L AF Platnick, Steven Oreopoulos, Lazaros TI Radiative susceptibility of cloudy atmospheres to droplet number perturbations: 1. Theoretical analysis and examples from MODIS SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID EFFECTIVE RADIUS; STRATOCUMULUS CLOUDS; BOUNDARY-LAYER; SATELLITE DATA; AEROSOL; CLIMATE; ALBEDO; PARAMETERIZATION; MICROPHYSICS; PRODUCTS AB Theoretical and satellite-based assessments of the sensitivity of broadband shortwave radiative fluxes in cloudy atmospheres to small perturbations in the cloud droplet number concentration (N) of liquid water clouds under constant water conditions are performed. Two approaches to study this sensitivity are adopted: absolute increases in N, for which the radiative response is referred to as "absolute cloud susceptibility,'' and relative increases in N or "relative cloud susceptibility.'' Estimating the former is more challenging as it requires an assumed value for either cloud liquid water content or geometrical thickness; both susceptibilities require an assumed relationship between the droplet volume and effective radius. Expanding upon previous susceptibility studies, present radiative calculations include the effect of Delta N perturbations on droplet asymmetry parameter and single-scattering albedo, in addition to extinction. Absolute cloud susceptibility has a strong nonlinear dependence on the droplet effective radius as expected, while relative cloud susceptibility is primarily dependent on optical thickness. Molecular absorption and reflecting surfaces both reduce the relative contribution of the cloud to the top-of-atmosphere (TOA) flux and therefore also reduce the TOA albedo susceptibility. Transmittance susceptibilities are negative with absolute values similar to albedo susceptibility, while atmospheric absorptance susceptibilities are about an order of magnitude smaller than albedo susceptibilities and can be either positive or negative. Observation-based susceptibility calculations are derived from MODIS pixel-level retrievals of liquid water cloud optical thickness, effective radius, and cloud top temperature; two data granule examples are shown. Susceptibility quantifies the aerosol indirect effect sensitivity in a way that can be easily computed from model fields. As such, susceptibilities derived from MODIS observations provide a higher-order test of model cloud properties used for indirect effect studies. MODIS-derived global distributions of cloud susceptibility and radiative forcing calculations are presented in a companion paper. C1 [Platnick, Steven] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Oreopoulos, Lazaros] Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. RP Platnick, S (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. EM steven.platnick@nasa.gov RI Oreopoulos, Lazaros/E-5868-2012; Platnick, Steven/J-9982-2014 OI Oreopoulos, Lazaros/0000-0001-6061-6905; Platnick, Steven/0000-0003-3964-3567 NR 37 TC 13 Z9 13 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 25 PY 2008 VL 113 IS D14 AR D14S20 DI 10.1029/2007JD009654 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 331FI UT WOS:000257997700004 ER PT J AU Reid, JS Reid, EA Walker, A Piketh, S Cliff, S Al Mandoos, A Tsay, SC Eck, TF AF Reid, Jeffrey S. Reid, Elizabeth A. Walker, Annette Piketh, Stuart Cliff, Steve Al Mandoos, Abdulla Tsay, Si-Chee Eck, Thomas F. TI Dynamics of southwest Asian dust particle size characteristics with implications for global dust research SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MINERAL AEROSOL PRODUCTION; NONSPHERICAL PARTICLES; BOUNDARY-LAYER; PERSIAN-GULF; WIND EROSION; DISTRIBUTIONS; TRANSPORT; BEHAVIOR; DEPOSITION; ATLANTIC AB As part of the United Arab Emirates Unified Aerosol Experiment (UAE 2), the size distribution and chemistry of dust particles were measured for the months of August and September 2004 at an Arabian Gulf coastal site impacted by dust from several sources within southwest Asia. The characteristics of common mode dust (0.8 < d(p) < 10 mu m) were examined using an aerodynamic particle sizer (APS), a DRUM cascade impactor, and AERONET Sun/sky retrievals. While size properties from these distinct methods do correlate, accurate dust measurement is still an outstanding challenge. But when instruments are applied consistently in the correct context, the dynamics of dust particle size can be accurately studied. Here, observations are used to study the stability of dust size and chemistry characteristics. We found that dust particle size, chemistry, and morphology appear to be fairly static from individual sources, confirming preliminary hypotheses based on large-scale observations of Saharan dust. Thus, our data provide experimental evidence that on regional scales, common mode dust is not functionally impacted by production wind speed, but rather influenced by soil properties such as geomorphology or roughness length. Similarly, we found transport processes from the mesoscale to near synoptic scale do not significantly impact common mode dust size either. When combined with other APS observations around the world, the dust coarse mode is found to be fairly robust with a volume median diameter on the order of similar to 3.5 mu m +/- 30%. Finally, evidence for a strong submicron dust mode, suggested in previous studies, was inconclusive. C1 [Reid, Jeffrey S.; Reid, Elizabeth A.; Walker, Annette] USN, Res Lab, Marine Meteorol Div, Monterey, CA 93943 USA. [Piketh, Stuart] Univ Witwatersrand, Climatol Res Grp, ZA-2050 Johannesburg, South Africa. [Tsay, Si-Chee; Eck, Thomas F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cliff, Steve] Univ Calif Davis, Dept Land Air & Water Resources, Davis, CA 95616 USA. [Al Mandoos, Abdulla] Minist Presidential Affairs, Dept Atmospher Studies, Abu Dhabi, U Arab Emirates. RP Reid, JS (reprint author), USN, Res Lab, Marine Meteorol Div, 7 Grace Hopper Ave,Stop 2, Monterey, CA 93943 USA. EM jeffrey.reid@nrlmry.navy.mil RI ECK, THOMAS/D-7407-2012; Reid, Jeffrey/B-7633-2014; Tsay, Si-Chee/J-1147-2014 OI Reid, Jeffrey/0000-0002-5147-7955; NR 43 TC 44 Z9 45 U1 3 U2 16 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 25 PY 2008 VL 113 IS D14 AR D14212 DI 10.1029/2007JD009752 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 331FI UT WOS:000257997700006 ER PT J AU Reid, JS Piketh, SJ Walker, AL Burger, RP Ross, KE Westphal, DL Bruintjes, RT Holben, BN Hsu, C Jensen, TL Kahn, RA Kuciauskas, AP Al Mandoos, A Al Mangoosh, A Miller, SD Porter, JN Reid, EA Tsay, SC AF Reid, Jeffrey S. Piketh, Stuart J. Walker, Annette L. Burger, Roelof P. Ross, Kristy E. Westphal, Douglas L. Bruintjes, Roelof T. Holben, Brent N. Hsu, Christina Jensen, Tara L. Kahn, Ralph A. Kuciauskas, Arunas P. Al Mandoos, Abdulla Al Mangoosh, Abdulla Miller, Steven D. Porter, John N. Reid, Elizabeth A. Tsay, Si-Chee TI An overview of UAE(2) flight operations: Observations of summertime atmospheric thermodynamic and aerosol profiles of the southern Arabian Gulf SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID PERSIAN-GULF; BOUNDARY-LAYER; SUN PHOTOMETER; SAHARAN DUST; AIRCRAFT; SIZE; REGION AB In August through September 2004 the United Arab Emirates Unified Aerosol Experiment (UAE 2) was conducted in the southern Arabian Gulf region. We present atmospheric thermodynamic and aerosol data collected on 18 flights by the South African Aerocommander aircraft. In the first few kilometers, we observed high concentrations of both regional dust (from 100 to 300 mu g m(-3) in background, to over 1.5 mg m(-3) in events) and ubiquitous sulfate based pollution from the Gulf's prevalent petroleum industry (10-100 mu g m(-3)). Smoke and pollution from Europe and possibly Africa were found at levels between 1.5 and 5 km. Inland, classic deep over desert boundary layer characteristics were found. Over the Arabian Gulf, dust and pollution were most often either trapped below or sequestered above a strong stable boundary. However, there were cases where a well-distributed aerosol layer crossed the inversion uniformly. Data suggest that the observed vertical profiles can be explained by the rapid formation of stable marine boundary layers as air moves offshore. This can decouple aerosol layers from within the boundary layer to those aloft in regions of vertical wind shear. In the case of pollution, the ability of flaring plumes to penetrate the inversion may also in part determine layering. In coastal regions without vertical wind shear, uniform concentrations with height across the inversion are a result of internal boundary layer development. We conclude that the bulk of the observed variability in particle vertical distribution appear to be controlled by mesoscale and microscale processes, such as the sea/land breeze. C1 [Reid, Jeffrey S.; Walker, Annette L.; Westphal, Douglas L.; Kuciauskas, Arunas P.; Reid, Elizabeth A.] USN, Res Lab, Marine Meteorol Div, Monterey, CA 93943 USA. [Al Mandoos, Abdulla] Minist Presidential Affairs, Dept Atmospher Studies, Abu Dhabi, U Arab Emirates. [Bruintjes, Roelof T.; Jensen, Tara L.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Piketh, Stuart J.; Burger, Roelof P.; Ross, Kristy E.] Univ Witwatersrand, Climatol Res Grp, ZA-2050 Johannesburg, South Africa. [Holben, Brent N.; Hsu, Christina; Kahn, Ralph A.; Tsay, Si-Chee] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Miller, Steven D.] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA. [Porter, John N.] Univ Hawaii, Sch Ocean & Earth Sci & Technol, Honolulu, HI 96822 USA. RP Reid, JS (reprint author), USN, Res Lab, Marine Meteorol Div, 7 Grace Hopper Ave,Stop 2, Monterey, CA 93943 USA. EM reidj@nrlmry.navy.mil RI Hsu, N. Christina/H-3420-2013; Reid, Jeffrey/B-7633-2014; Kahn, Ralph/D-5371-2012; Tsay, Si-Chee/J-1147-2014 OI Reid, Jeffrey/0000-0002-5147-7955; Kahn, Ralph/0000-0002-5234-6359; NR 28 TC 18 Z9 18 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 25 PY 2008 VL 113 IS D14 AR D14213 DI 10.1029/2007JD009435 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 331FI UT WOS:000257997700003 ER PT J AU Tokar, RL Wilson, RJ Johnson, RE Henderson, MG Thomsen, MF Cowee, MM Sittler, EC Young, DT Crary, FJ McAndrews, HJ Smith, HT AF Tokar, R. L. Wilson, R. J. Johnson, R. E. Henderson, M. G. Thomsen, M. F. Cowee, M. M. Sittler, E. C., Jr. Young, D. T. Crary, F. J. McAndrews, H. J. Smith, H. T. TI Cassini detection of water-group pick-up ions in the Enceladus torus SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MAGNETOSPHERE; PLASMA; ATMOSPHERE; SATURN AB This study reports direct detection by the Cassini plasma spectrometer of freshly-produced water-group pick-up ions within the proposed Enceladus torus, a radially narrow toroidal region surrounding Saturn that contains a high density of water-group neutrals. This torus is produced by the icy plumes observed near the south pole of Enceladus. The ions are created by charge exchange collisions between water-group neutrals in the Enceladus torus and thermal ions corotating with Saturn. They are identified in the Cassini data via their characteristic ring-like signatures in ion velocity distributions. In the radial distance range of 4.0 to 4.5 R-S, the density of these non-thermalized ions is estimated to be at least 5.2 cm(-3), about 8% of the total ion density. The estimated density together with ionization, charge exchange, and loss times, yield an ion thermalization time of at least 3150 s, in reasonable agreement with hybrid particle simulations. C1 [Tokar, R. L.; Wilson, R. J.; Henderson, M. G.; Thomsen, M. F.; Cowee, M. M.; McAndrews, H. J.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Young, D. T.; Crary, F. J.] SW Res Inst, San Antonio, TX USA. [Johnson, R. E.] Univ Virginia, Charlottesville, VA USA. [Sittler, E. C., Jr.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Smith, H. T.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. RP Tokar, RL (reprint author), Los Alamos Natl Lab, POB 1663, Los Alamos, NM 87545 USA. EM rlt@lanl.gov RI Wilson, Rob/C-2689-2009; Smith, Howard/H-4662-2016; Henderson, Michael/A-3948-2011 OI Wilson, Rob/0000-0001-9276-2368; Smith, Howard/0000-0003-3537-3360; Henderson, Michael/0000-0003-4975-9029 NR 13 TC 37 Z9 37 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 24 PY 2008 VL 35 IS 14 AR L14202 DI 10.1029/2008GL034749 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 331ER UT WOS:000257996000002 ER PT J AU Douglass, AR Stolarski, RS Schoeberl, MR Jackman, CH Gupta, ML Newman, PA Nielsen, JE Fleming, EL AF Douglass, A. R. Stolarski, R. S. Schoeberl, M. R. Jackman, C. H. Gupta, M. L. Newman, P. A. Nielsen, J. E. Fleming, E. L. TI Relationship of loss, mean age of air and the distribution of CFCs to stratospheric circulation and implications for atmospheric lifetimes SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID 2-DIMENSIONAL MODEL; TRANSPORT MODEL; CLIMATE MODEL; OZONE; SENSITIVITY; TROPOSPHERE; AIRCRAFT; CHLORINE; TRACERS; VIEW AB Projections of the recovery of the ozone layer are made with global atmospheric models using a specified time series of mixing ratios of ozone depleting substances (ODSs) at the lower boundary. This time series is calculated using atmospheric mixing ratio observations, emission rates, and an estimate for the atmospheric lifetime. ODS destruction and simulated atmospheric-lifetime vary among models because they depend on the simulated stratospheric transport and mixing. We investigate the balance between the annual change in ODS burden, its atmospheric loss, and the annual ODS input to the atmosphere using several models. Some models produce realistic distributions for the mean age of air and some do not. Back trajectory calculations relate the fractional release (one minus the amount of ODS at a location relative to its stratospheric entry value) to the mean age through the age spectrum, showing that, for the individual spectrum elements, the maximum altitude and loss increase with age. Models with faster circulations produce "young'' distributions for the age of air and fail to reproduce the observed relationship between the mean age of air and the fractional release. Models with realistic mean age of air reproduce the observed relationship. These models yield a lifetime for CFCl3 of similar to 56 years, longer than the 45 year lifetime currently used to project future mixing ratios. Use of flux boundary conditions in assessment models would have several advantages, including consistency between the ODS evolution and simulated loss even if the simulated residual circulation changes due to climate change. C1 [Douglass, A. R.; Stolarski, R. S.; Schoeberl, M. R.; Jackman, C. H.; Newman, P. A.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Greenbelt, MD 20771 USA. [Fleming, E. L.] NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA. [Gupta, M. L.] AEE 300 Emiss Div, Fed Aviat Adm, Off Environm & Energy, Washington, DC 20591 USA. [Nielsen, J. E.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. RP Douglass, AR (reprint author), NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Code 6133, Greenbelt, MD 20771 USA. EM anne.r.douglass@nasa.gov RI Newman, Paul/D-6208-2012; Douglass, Anne/D-4655-2012; Jackman, Charles/D-4699-2012; Stolarski, Richard/B-8499-2013 OI Newman, Paul/0000-0003-1139-2508; Stolarski, Richard/0000-0001-8722-4012 NR 49 TC 40 Z9 40 U1 0 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 JUL 24 PY 2008 VL 113 IS D14 AR D14309 DI 10.1029/2007JD009575 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 331FG UT WOS:000257997500002 ER PT J AU Helber, RW Barron, CN Carnes, MR Zingarelli, RA AF Helber, Robert W. Barron, Charlie N. Carnes, Michael R. Zingarelli, Robert A. TI Evaluating the sonic layer depth relative to the mixed layer depth SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID ACOUSTIC TRANSMISSION; SURFACE DUCT; OCEAN; PROPAGATION; MODEL; SEA AB Using a global set of in situ temperature and salinity profile observations, the sonic layer depth (SLD) and the mixed layer depth (MLD) are analyzed and compared over the annual cycle. The SLD characterizes the potential of the upper ocean to trap acoustic energy in a surface duct while MLD characterizes upper ocean mixing. The SLD is computed from temperature and salinity profile pairs using a new tunable method while MLD is computed using recently developed methods and either temperature only profiles or temperature and salinity profile pairs. Both SLD and MLD estimates provide information on different and important aspects of the upper ocean. The SLD and MLD often coincide because sound speed increases with depth down to the MLD, where (typically) a decrease in temperature occurs, resulting in a local maximum sound speed. The depth of this maximum sound speed is the SLD. The SLD and MLD are not always the same because sound speed is substantially more sensitive to temperature than to salinity compared to density. Since MLD is a commonly known and studied parameter, MLD is often used as a proxy for SLD in scientific and operational applications. In the boreal spring when fresh restratification events occur, the SLD is 10 m deeper (shallower) than the MLD in 39% (7%) of the observed profiles. A parabolic equation acoustic transmission model is used to evaluate the relative skill of the SLD and MLD estimates to predict surface acoustic trapping as measured by a simple metric. C1 [Helber, Robert W.; Barron, Charlie N.; Carnes, Michael R.; Zingarelli, Robert A.] USN REs Lab, Stennis Space Ctr, Bay St Louis, MS 39529 USA. RP Helber, RW (reprint author), USN REs Lab, Stennis Space Ctr, Code 7323, Bay St Louis, MS 39529 USA. EM helber@nrlssc.navy.mil RI Barron, Charlie/C-1451-2008 NR 29 TC 8 Z9 8 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 EI 2169-9291 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD JUL 24 PY 2008 VL 113 IS C7 AR C07033 DI 10.1029/2007JC004595 PG 14 WC Oceanography SC Oceanography GA 331GE UT WOS:000257999900003 ER PT J AU Kuris, AM Hechinger, RF Shaw, JC Whitney, KL Aguirre-Macedo, L Boch, CA Dobson, AP Dunham, EJ Fredensborg, BL Huspeni, TC Lorda, J Mababa, L Mancini, FT Mora, AB Pickering, M Talhouk, NL Torchin, ME Lafferty, KD AF Kuris, Armand M. Hechinger, Ryan F. Shaw, Jenny C. Whitney, Kathleen L. Aguirre-Macedo, Leopoldina Boch, Charlie A. Dobson, Andrew P. Dunham, Eleca J. Fredensborg, Brian L. Huspeni, Todd C. Lorda, Julio Mababa, Luzviminda Mancini, Frank T. Mora, Adrienne B. Pickering, Maria Talhouk, Nadia L. Torchin, Mark E. Lafferty, Kevin D. TI Ecosystem energetic implications of parasite and free-living biomass in three estuaries SO NATURE LA English DT Article ID FOOD-WEB; REPRODUCTIVE EFFORT; BODY-SIZE; DYNAMICS; PATTERNS; ECOLOGY AB Parasites can have strong impacts but are thought to contribute little biomass to ecosystems(1-3). We quantified the biomass of free-living and parasitic species in three estuaries on the Pacific coast of California and Baja California. Here we show that parasites have substantial biomass in these ecosystems. We found that parasite biomass exceeded that of top predators. The biomass of trematodes was particularly high, being comparable to that of the abundant birds, fishes, burrowing shrimps and polychaetes. Trophically transmitted parasites and parasitic castrators subsumed more biomass than did other parasitic functional groups. The extended phenotype biomass controlled by parasitic castrators sometimes exceeded that of their uninfected hosts. The annual production of free-swimming trematode transmission stages was greater than the combined biomass of all quantified parasites and was also greater than bird biomass. This biomass and productivity of parasites implies a profound role for infectious processes in these estuaries. C1 [Kuris, Armand M.; Hechinger, Ryan F.; Shaw, Jenny C.; Whitney, Kathleen L.; Boch, Charlie A.; Lorda, Julio; Mababa, Luzviminda; Talhouk, Nadia L.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. [Aguirre-Macedo, Leopoldina] IPN, Ctr Invest & Estud Avanzados, Merida 97310, Mexico. [Dobson, Andrew P.] Princeton Univ, Princeton, NJ 08544 USA. [Dunham, Eleca J.] Penn State Univ, Ctr Infect Dis Dynam, Dept Biol, University Pk, PA 16802 USA. [Fredensborg, Brian L.] Univ Texas Pan Amer, Dept Biol, Edinburg, TX 78539 USA. [Huspeni, Todd C.] Univ Wisconsin, Dept Biol, Stevens Point, WI 54481 USA. [Mancini, Frank T.] NOAA, Natl Marine Fisheries Serv, Pacific Isl Fisheries Res Ctr, Honolulu, HI 96822 USA. [Mora, Adrienne B.] Univ Calif Riverside, Dept Biol, Riverside, CA 92521 USA. [Pickering, Maria] Univ Connecticut, Unit 3043, Storrs, CT 06269 USA. [Torchin, Mark E.] Smithsonian Trop Res Inst, Balboa 03092, Panama. [Lafferty, Kevin D.] Univ Calif Santa Barbara, Western Ecol Res Ctr, US Geol Survey, Inst Marine Sci, Santa Barbara, CA 93106 USA. RP Kuris, AM (reprint author), Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. EM kuris@lifesci.ucsb.edu RI Aguirre-Macedo, Ma Leopoldina/A-2511-2008; Lorda, Julio/A-3951-2009; Lafferty, Kevin/B-3888-2009; Hechinger, Ryan/F-6754-2010; Fredensborg, Brian/A-5632-2010; Fredensborg, Brian Lund/G-1548-2014 OI Aguirre-Macedo, Ma Leopoldina/0000-0002-3910-8305; Lorda, Julio/0000-0002-4293-7518; Lafferty, Kevin/0000-0001-7583-4593; Fredensborg, Brian Lund/0000-0002-4837-5974 NR 30 TC 213 Z9 224 U1 12 U2 136 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD JUL 24 PY 2008 VL 454 IS 7203 BP 515 EP 518 DI 10.1038/nature06970 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 329IC UT WOS:000257860300051 PM 18650923 ER PT J AU Beig, G Scheer, J Mlynczak, MG Keckhut, P AF Beig, G. Scheer, J. Mlynczak, M. G. Keckhut, P. TI Overview of the temperature response in the mesosphere and lower thermosphere to solar activity SO REVIEWS OF GEOPHYSICS LA English DT Review ID HALOGEN OCCULTATION EXPERIMENT; MIDDLE ATMOSPHERE RESPONSE; GENERAL-CIRCULATION MODEL; MESOPAUSE REGION AIRGLOW; LONG-TERM BEHAVIOR; PROTON EVENTS; UPPER-STRATOSPHERE; INTERANNUAL VARIABILITY; IRRADIANCE VARIATIONS; 3-DIMENSIONAL MODEL AB The natural variability in the terrestrial mesosphere needs to be known to correctly quantify global change. The response of the thermal structure to solar activity variations is an important factor. Some of the earlier studies highly overestimated the mesospheric solar response. Modeling of the mesospheric temperature response to solar activity has evolved in recent years, and measurement techniques as well as the amount of data have improved. Recent investigations revealed much smaller solar signatures and in some cases revealed no significant solar signal at all. However, not much effort has been made to synthesize the results available so far. This article presents an overview of the energy budget of the mesosphere and lower thermosphere and an up-to-date status of solar response in temperature structure based on recently available observational data. An objective evaluation of the data sets is attempted, and important factors of uncertainty are discussed. C1 [Beig, G.] Indian Inst Trop Meteorol, Pune 411008, Maharashtra, India. [Keckhut, P.] Univ Versailles St Quentin Yvelines, Inst Pierre Simon Laplace, Serv Aeron, F-91371 Verrieres Le Buisson, France. [Mlynczak, M. G.] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA. [Scheer, J.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. RP Beig, G (reprint author), Indian Inst Trop Meteorol, Pune 411008, Maharashtra, India. EM beig@tropmet.res.in RI Mlynczak, Martin/K-3396-2012; OI Beig, Gufran/0000-0002-5564-7210 NR 120 TC 24 Z9 24 U1 1 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 8755-1209 J9 REV GEOPHYS JI Rev. Geophys. PD JUL 24 PY 2008 VL 46 IS 3 AR RG3002 DI 10.1029/2007RG000236 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 331HC UT WOS:000258002300001 ER PT J AU Lallart, P Kahn, R Tanre, D AF Lallart, Pierre Kahn, Ralph Tanre, Didier TI POLDER2/ADEOSII, MISR, and MODIS/Terra reflectance comparisons SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID CALIBRATION; RETRIEVAL AB Reflectance differences among Multiangle Imaging Spectroradiometer (MISR), Moderate Resolution Imaging Spectroradiometer (MODIS)/Terra and Polarization and Directionality of the Earth's Reflectances (POLDER2) are characterized, as functions of observation geometry and spectral bands. For observations having similar geometry, corresponding normalized reflectances from MISR and MODIS fall within 3% for all bands except the MISR red band, which is higher than MODIS and POLDER2 by about 3.5%. POLDER2 and MODIS are within less than about 1% in the blue and red, 4% in the near-infrared, and 5% in the green. Generally, MISR reflectances are at the high end of the reflectance envelope, whereas POLDER2 tends to be at the low end, yielding a spread of about 5% in the red, 5% in the near-infrared, and over 7% in the green. Reflectance differences were not quantitatively corrected for instrument-to-instrument spectral band pass differences because of the uncertainties associated with such calculations. However, these uncertainties are assessed, and the envelopes can be used to bound calibration contributions to derived geophysical quantity uncertainties, including aerosol amount and type. This is of particular importance when data from the three instruments are used together in geophysical applications. C1 [Kahn, Ralph] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lallart, Pierre; Tanre, Didier] Univ Sci & Technol Lille, Opt Atmospher Lab, F-59655 Villeneuve Dascq, France. [Lallart, Pierre] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Lallart, P (reprint author), Univ Sci & Technol Lille, Opt Atmospher Lab, F-59655 Villeneuve Dascq, France. EM ralph.kahn@nasa.gov RI Kahn, Ralph/D-5371-2012 OI Kahn, Ralph/0000-0002-5234-6359 NR 12 TC 9 Z9 9 U1 0 U2 0 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 2008 VL 113 IS D14 AR D14S02 DI 10.1029/2007JD009656 PG 8 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 331FA UT WOS:000257996900007 ER PT J AU Matsui, T Beltran-Przekurat, A Niyogi, D Pielke, RA Coughenour, M AF Matsui, Toshihisa Beltran-Przekurat, Adriana Niyogi, Dev Pielke, Roger A., Sr. Coughenour, Michael TI Aerosol light scattering effect on terrestrial plant productivity and energy fluxes over the eastern United States SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SYSTEM NLDAS PROJECT; STOMATAL CONDUCTANCE; DIFFUSE-RADIATION; CARBON-DIOXIDE; WATER-VAPOR; PHOTOSYNTHESIS; MODEL; CLOUDS; TRANSPIRATION; VEGETATION AB This study reports the first regional-scale assessment of aerosol effects on plant productivity and surface energy fluxes over the eastern United States. Analysis is conducted using an established modeling framework, which is composed of a regional land surface model, regional daily aerosol optical depth (AOD) estimates, and meteorological forcings. The sensitivity experiments were conducted from May to September in 2000 and 2001 over the eastern United States with and without the aerosol light scattering effect. Results show that the aerosol light scattering effect results in enhanced productivity for high-LAI and optimum temperature environments under cloudless-sky conditions around noon, while it results in least productive for low-LAI, low-temperature environments under cloud-sky conditions in early morning or late afternoon. As a result, domain-aver aged plant productivities, measured as net primarily production, are changed by -0.71 g C m(-2) (-0.09%) in 2000 and +5.00 g C m(-2) (+0.5%) in 2001. These responses of plant productivity and photosynthesis to the aerosol light scattering effect uniquely modulate the surface flux as follows. The aerosol light scattering effect reduces the surface downwelling solar radiation (14.9 W m(-2) in 2000 and 16.0 W m(-2) in 2001) and net radiation in vegetation canopy, but simultaneously increases the photosynthesis and stomatal conductance. Consequently, surface latent heat flux ( transpiration and evaporation) is reduced by a small amount particularly over the forests, while aerosol loading often results in larger reduction in the sensible heat flux. For the whole domain, latent heat flux is changed by -3.10 W m(-2) (-2.1%) in 2000 and -3.12 W m(-2) (-2.1%) in 2001, sensible heat flux is changed by -7.57 W m(-2) (-12.9%) in 2000 and -8.36 W m(-2) (-11.3%) in 2001, and surface skin temperature is changed by -0.25 K (-0.1%) in 2000 and -0.27 K (-0.1%) in 2001. C1 [Matsui, Toshihisa] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Beltran-Przekurat, Adriana] Univ Colorado, Cooperat Inst Res Environm Sci, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA. [Coughenour, Michael] Colorado State Univ, Nat Resource & Environm Lab, Ft Collins, CO 80523 USA. [Niyogi, Dev] Purdue Univ, Dept Agron, W Lafayette, IN 47906 USA. RP Matsui, T (reprint author), NASA, Goddard Space Flight Ctr, Code 663-1, Greenbelt, MD 20771 USA. EM matsui@agnes.gsfc.nasa.gov RI Pielke, Roger/A-5015-2009 NR 47 TC 19 Z9 19 U1 0 U2 16 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 22 PY 2008 VL 113 IS D14 AR D14S14 DI 10.1029/2007JD009658 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 331FA UT WOS:000257996900009 ER PT J AU Dietrich, DE Tseng, YH Medina, R Piacsek, SA Liste, M Olabarrieta, M Bowman, MJ Mehra, A AF Dietrich, David E. Tseng, Yu-Heng Medina, Raul Piacsek, Steve A. Liste, Maria Olabarrieta, Maitane Bowman, Malcolm J. Mehra, Avichal TI Mediterranean Overflow Water (MOW) simulation using a coupled multiple-grid Mediterranean Sea/North Atlantic Ocean model SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID NORTH-ATLANTIC; ALBORAN-SEA; CIRCULATION; ENTRAINMENT; COORDINATE; 1/10-DEGREES; CLIMATOLOGY; TOPOGRAPHY; DYNAMICS; OUTFLOW AB [1] A z- level, 4th- order- accurate ocean model is applied in six two- way- coupled grids spanning the Mediterranean Sea and North Atlantic Ocean ( MEDiNA). Resolutions vary from 1/4 degrees in central North Atlantic to 1/24 degrees in Strait of Gibraltar region. This allows the MEDiNA model to efficiently resolve small features ( e. g., Strait of Gibraltar) in a multibasin, multiscale model. Such small features affect all scales because of nonlinearity and low dissipation. The grid coupling using one coarse grid overlap is nearly seamless without intergrid sponge layers. No instant convective adjustment or other highly diffusive process is used. The deep water in the 1/ 8 Mediterranean Sea grid is formed by the resolved flows that emulate subgrid- scale processes directly. Downslope migration of Mediterranean Overflow Water ( MOW) water involves dense water flowing away from the bottom laterally over bottom stairsteps in the z- level model, thus flowing over less dense underlying water. Without excessively water mass- diluting process, the advection dominates the downslope migration of thin, dense MOW in the simulation. The model results show realisticMOWmigration to the observed equilibrium depth, followed by lateral spreading near that depth. The results are also consistent with the climatology along 43 degrees N, where the MOW hugs a steep shelfslope centered at similar to 1 km depth and then spreads westward, with the salinity core ( S > 35.7) reaching 18 degrees W. This study clearly restores z- level models to a competitive status doing density current simulations. C1 [Dietrich, David E.] AcuSea Inc, La Jolla, CA USA. [Bowman, Malcolm J.] SUNY Stony Brook, Marine Sci Res Ctr, Stony Brook, NY USA. [Medina, Raul; Liste, Maria; Olabarrieta, Maitane] Univ Cantabria, Ocean & Coastal Res Grp, E-39005 Santander, Spain. [Mehra, Avichal] NOAA, NCEP NWS, Environm Modeling Ctr, Camp Springs, MD USA. [Piacsek, Steve A.] USN, Res Lab, Div Oceanog, Stennis Space Ctr, Stennis Space Ctr, MS USA. [Tseng, Yu-Heng] Natl Taiwan Univ, Dept Atmospher Sci, Taipei 10617, Taiwan. RP Dietrich, DE (reprint author), AcuSea Inc, 8450-101 Via Sonoma, La Jolla, CA USA. RI Medina, Raul/L-2456-2014; OI Medina, Raul/0000-0002-0126-2710; Tseng, Yu-heng/0000-0002-4816-4974 NR 45 TC 14 Z9 14 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-OCEANS JI J. Geophys. Res.-Oceans PD JUL 22 PY 2008 VL 113 IS C7 AR C07027 DI 10.1029/2006JC003914 PG 14 WC Oceanography SC Oceanography GA 331GD UT WOS:000257999800001 ER PT J AU Carnell, LS Siochi, EJ Holloway, NM Stephens, RM Rhim, C Niklason, LE Clark, RL AF Carnell, Lisa S. Siochi, Emilie J. Holloway, Nancy M. Stephens, Ralph M. Rhim, Caroline Niklason, Laura E. Clark, Robert L. TI Aligned mats from electrospun single fibers SO MACROMOLECULES LA English DT Article ID POLYMER NANOFIBERS; FABRICATION; ORIENTATION; ALIGNMENT; SCAFFOLD; JET AB Highly aligned electrospun micro- and nanoscale fibers and pseudowoven mats were produced via electrospinning by incorporating an auxiliary counter electrode to create an electric field of controlled geometry and magnitude. Two polymers were examined using this technique: a polyimide (CP2) and a biodegradable polymer, poly(glycolic acid) (PGA). Highly aligned electrospun CP2 fibers were on the order of 10 mu m in diameter, and fiber spacing in the Spun mats ranged between 25 and 30 mu m. Electrospun PGA aligned fibers were on the order of 500 run in diameter with spacing between fibers ranging from 7 to 10 mu m in the spun mats. High-speed videography illustrated the influence of the auxiliary electrode on the elimination of jet whipping and bending instability commonly associated with the electrospinning process. The data presented here demonstrate the direct influence of an opposing electric field on the degree of fiber alignment and control of fiber placement. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. Duke Univ, Dept Biomed Engn, Durham, NC 27708 USA. Yale Univ, Dept Biomed Engn, New Haven, CT 06520 USA. Duke Univ, Dept Mech Engn & Mat Sci, Durham, NC 27708 USA. RP Carnell, LS (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM lisa.a.scottcarnell@nasa.gov NR 29 TC 70 Z9 72 U1 2 U2 52 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0024-9297 J9 MACROMOLECULES JI Macromolecules PD JUL 22 PY 2008 VL 41 IS 14 BP 5345 EP 5349 DI 10.1021/ma8000143 PG 5 WC Polymer Science SC Polymer Science GA 326NJ UT WOS:000257665900037 ER PT J AU Booth-Morrison, C Mao, ZG Noebe, RD Seidman, DN AF Booth-Morrison, Christopher Mao, Zugang Noebe, Ronald D. Seidman, David N. TI Chromium and tantalum site substitution patterns in Ni(3)Al (L1(2)) gamma '-precipitates SO APPLIED PHYSICS LETTERS LA English DT Article ID TOTAL-ENERGY CALCULATIONS; AL-CR SUPERALLOY; WAVE BASIS-SET; TERNARY ADDITIONS; ALLOYING BEHAVIOR; ATOM-PROBE; PREFERENCE; ELEMENTS; PHASE; MODEL AB The site substitution behavior of Cr and Ta in the Ni(3)Al (L1(2))-type gamma(')-precipitates of a Ni-Al-Cr-Ta alloy is investigated by atom-probe tomography (APT) and first-principles calculations. Measurements of the gamma(')-phase composition by APT suggest that Al, Cr, and Ta share the Al sublattice sites of the gamma(')-precipitates. The calculated substitutional energies of the solute atoms at the Ni and Al sublattice sites indicate that Ta has a strong preference for the Al sites, while Cr has a weak Al site preference. Furthermore, Ta is shown to replace Cr at the Al sublattice sites of the gamma(')-precipitates, altering the elemental phase partitioning behavior of the Ni-Al-Cr-Ta alloy. (C) 2008 American Institute of Physics. C1 [Booth-Morrison, Christopher; Mao, Zugang; Seidman, David N.] Northwestern Univ, Dept Mat Sci & Engn, Evanston, IL 60208 USA. [Noebe, Ronald D.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Seidman, David N.] Northwestern Univ, Ctr Atom Probe Tomog, Evanston, IL 60208 USA. RP Booth-Morrison, C (reprint author), Northwestern Univ, Dept Mat Sci & Engn, 2220 Campus Dr, Evanston, IL 60208 USA. EM c-booth@northwestern.edu; z-mao2@northwestern.edu; d-seidman@northwestern.edu RI Seidman, David/B-6697-2009 NR 35 TC 28 Z9 28 U1 2 U2 18 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD JUL 21 PY 2008 VL 93 IS 3 AR 033103 DI 10.1063/1.2956398 PG 3 WC Physics, Applied SC Physics GA 330UQ UT WOS:000257968700064 ER PT J AU Mohanchandra, KP Karnani, S Emmons, MC Richards, WL Carman, GP AF Mohanchandra, K. P. Karnani, S. Emmons, M. C. Richards, W. L. Carman, G. P. TI Thin film NiTi coatings on optical fiber Bragg sensors SO APPLIED PHYSICS LETTERS LA English DT Article ID TEMPERATURE-DEPENDENCE; GRATINGS; TARGET AB This paper describes the sputter deposition and characterization of nickel titanium (NiTi) thin film shape memory alloy onto the surface of an optical fiber Bragg grating. The NiTi coating uniformity, crystallinity, and transformation temperatures are measured using scanning electron microscope, x-ray diffraction, and differential scanning calorimeter, respectively. The strain in the optical fiber is measured using centroid calculation of wavelength shifts. Results show distinct and abrupt changes in the optical fiber signal with the four related transformation temperatures represented by the austenite-martensite forward and reverse phase transformations. These tests demonstrate a coupling present between optical energy and thermal energy, i.e., a modified multiferroic material. C1 [Mohanchandra, K. P.; Karnani, S.; Emmons, M. C.; Carman, G. P.] Univ Calif Los Angeles, Dept Aerosp Engn & Mech, Los Angeles, CA 90095 USA. [Richards, W. L.] NASA Dryden Flight Res Ctr, Edwards AFB, CA 93523 USA. RP Mohanchandra, KP (reprint author), Univ Calif Los Angeles, Dept Aerosp Engn & Mech, Los Angeles, CA 90095 USA. EM carman@seas.ucla.edu NR 13 TC 3 Z9 3 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 0003-6951 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD JUL 21 PY 2008 VL 93 IS 3 AR 031914 DI 10.1063/1.2961002 PG 3 WC Physics, Applied SC Physics GA 330UQ UT WOS:000257968700031 ER PT J AU George, MR Fabian, AC Baumgartner, WH Mushotzky, RF Tueller, J AF George, M. R. Fabian, A. C. Baumgartner, W. H. Mushotzky, R. F. Tueller, J. TI On active galactic nuclei as sources of ultra-high energy cosmic rays SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE cosmic rays; galaxies : active; galaxies : nuclei ID ARRIVAL DIRECTIONS; ANISOTROPY; SPECTRUM; SEARCH AB We measure the correlation between sky coordinates of the Swift Burst Alert Telescope (BAT) catalogue of active galactic nuclei (AGN) with the arrival directions of the highest energy cosmic rays detected by the Auger Observatory. The statistically complete, hard X-ray catalogue helps to distinguish between AGN and other source candidates that follow the distribution of local large-scale structure. The positions of the full catalogue are marginally uncorrelated with the cosmic ray arrival directions, but when weighted by their hard X-ray flux, AGN within 100 Mpc are correlated at a significance level of 98 per cent. This correlation sharply decreases for sources beyond similar to 100 Mpc, suggestive of a GZK suppression. We discuss the implications for determining the mechanism that accelerates particles to these extreme energies in excess of 10(19) eV. C1 [George, M. R.; Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Baumgartner, W. H.; Mushotzky, R. F.; Tueller, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Baumgartner, W. H.] Univ Maryland, Baltimore, MD 21250 USA. RP George, MR (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM mrg@ast.cam.ac.uk RI Tueller, Jack/D-5334-2012 NR 39 TC 32 Z9 32 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 21 PY 2008 VL 388 IS 1 BP L59 EP L63 DI 10.1111/j.1745-3933.2008.00499.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 327CD UT WOS:000257706300013 ER PT J AU Okazaki, AT Owocki, SP Russell, CMP Corcoran, ME AF Okazaki, A. T. Owocki, S. P. Russell, C. M. P. Corcoran, M. E. TI Modelling the RXTE light curve of eta Carinae from a 3D SPH simulation of its binary wind collision SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries : general; stars : early-type; stars : individual : eta Carinae; stars : winds, outflows; X-rays : stars ID X-RAY-EMISSION; VARIABILITY; STARS AB The very massive star system eta Carinae exhibits regular 5.54 yr (2024 d) period disruptive events in wavebands ranging from the radio to X-ray. There is a growing consensus that these events likely stem from periastron passage of an (as yet) unseen companion in a highly eccentric (e similar to 0.9) orbit. This Letter presents 3D smoothed particle hydrodynamics (SPH) simulations of the orbital variation of the binary wind-wind collision, and applies these to modelling the X-ray light curve observed by the Rossi X-ray Timing Explorer (RXTE). By providing a global 3D model of the phase variation of the density of the interacting winds, the simulations allow computation of the associated variation in X-ray absorption, presumed here to originate from near the apex of the wind-wind interaction cone. We find that the observed RXTE light curve can be readily fitted if the observer's line of sight is within this cone along the general direction of apastron. Specifically, the data are well fitted by an assumed inclination i = 45 degrees for the orbit's polar axis, which is thus consistent with orbital angular momentum being along the inferred polar axis of the Homunculus nebula. The fits also constrain the position angle phi that an orbital-plane projection makes with the apastron side of the semimajor axis, strongly excluding positions phi < 9 degrees along or to the retrograde side of the axis, with the best-fitting position given by phi = 27 degrees. Overall the results demonstrate the utility of a fully 3D dynamical model for constraining the geometric and physical properties of this complex colliding wind binary system. C1 [Okazaki, A. T.] Hokkai Gakuen Univ, Fac Engn, Toyohira Ku, Sapporo, Hokkaido 0628605, Japan. [Owocki, S. P.; Russell, C. M. P.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Corcoran, M. E.] NASA GSFC, CRESST & Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Corcoran, M. E.] Univ Space Res Assoc, Columbia, MD 21044 USA. RP Okazaki, AT (reprint author), Hokkai Gakuen Univ, Fac Engn, Toyohira Ku, Sapporo, Hokkaido 0628605, Japan. EM okazaki@elsa.hokkai-s-u.ac.jp; owocki@bartol.udel.edu; crussell@udel.edu; michael.f.corcoran@nasa.gov NR 19 TC 65 Z9 65 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 21 PY 2008 VL 388 IS 1 BP L39 EP L43 DI 10.1111/j.1745-3933.2008.00496.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 327CD UT WOS:000257706300009 ER PT J AU Prialnik, D A'Hearn, MF Meech, KJ AF Prialnik, D. A'Hearn, M. F. Meech, K. J. TI A mechanism for short-lived cometary outbursts at sunrise as observed by Deep Impact on 9P/Tempel 1 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE comets : general; comets : individual : 9P/Tempel 1 ID NUCLEUS; COMET-9P/TEMPEL-1; EVOLUTION; SURFACE AB We explore a possible mechanism that may explain the outbursts observed by the Deep Impact mission on comet 9P/Tempel 1 that appear to occur near sunrise on a particular area. Assuming that the area is covered by a porous, poorly conducting dust layer, the heat wave generated by solar radiation at local noon propagates through the dust layer towards the ice-rich layer underneath it. The heated ice sublimates and the vapour flows towards the surface. However, by the time the heat wave reaches the ice, the spot has moved out of sunlight and its temperature has started dropping. As the vapour flows outwards, the surface has become so cold that it refreezes. Thus, at night some ice accumulates in the dust layer, very close to the surface. At sunrise, it immediately evaporates, producing a short-lived surge of activity. Numerical simulations of this mechanism provide the duration and water production of such outbursts, which are compatible with the 9P/Tempel 1 observations of small outbursts. C1 [Prialnik, D.] Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Meech, K. J.] Univ Hawaii, NASA, Astrobiol Inst, Honolulu, HI 96822 USA. RP Prialnik, D (reprint author), Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel. EM dina@planet.tau.ac.il NR 17 TC 8 Z9 8 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 JUL 21 PY 2008 VL 388 IS 1 BP L20 EP L23 DI 10.1111/j.1745-3933.2008.00491.x PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 327CD UT WOS:000257706300005 ER PT J AU Peters, RD Lay, OP Jeganathan, M AF Peters, Robert D. Lay, Oliver. P. Jeganathan, Muthu TI Broadband phase and intensity compensation with a deformable mirror for an interferometric nuller SO APPLIED OPTICS LA English DT Article AB Nulling interferometry has been proposed for the direct detection of Earth-like planets. Deep stable nulls require careful control of the relative intensity and phase of the beams that are being combined. We present a novel compensator, the Adaptive Nuller, that corrects the intensity and phase as a function of wavelength from 8 to 12 mu m using a deformable mirror. This compensator has been used to produce rejection ratios of 82000: lover a bandwidth of 3.2 mu m centered around 10 mu m. (C) 2008 Optical Society of America. C1 [Peters, Robert D.; Lay, Oliver. P.; Jeganathan, Muthu] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Peters, RD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Robert.D.Peters@jpl.nasa.gov FU National Aeronautics and Space Administration FX The authors gratefully acknowledge the assistance Peter Lawson in the preparation of this paper. The work described in this paper was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 9 TC 11 Z9 11 U1 0 U2 1 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 JUL 20 PY 2008 VL 47 IS 21 BP 3920 EP 3926 DI 10.1364/AO.47.003920 PG 7 WC Optics SC Optics GA 337EW UT WOS:000258419300030 PM 18641762 ER PT J AU Melendez, M Kraemer, SB Armentrout, BK Deo, RP Crenshaw, DM Schmitt, HR Mushotzky, RF Tueller, J Markwardt, CB Winter, L AF Melendez, M. Kraemer, S. B. Armentrout, B. K. Deo, R. P. Crenshaw, D. M. Schmitt, H. R. Mushotzky, R. F. Tueller, J. Markwardt, C. B. Winter, L. TI New indicators for agn power: The correlation between [O IV] 25.89 mu m and hard X-ray luminosity for nearby seyfert galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : Seyfert; infrared : galaxies; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; NARROW-LINE REGION; SPITZER-SPACE-TELESCOPE; INFRARED-SELECTED SAMPLE; XMM-NEWTON OBSERVATIONS; EMISSION-LINE; PHYSICAL CONDITIONS; RADIO-SOURCES; RESOLVED SPECTROSCOPY; INTRINSIC ABSORPTION AB We have studied the relationship between the [O iv] 25.89 mu m emission- line luminosities, obtained from Spitzer spectra, the X- ray continua in the 2Y10 keV band, primarily from ASCA, and the 14Y195 keV band obtained with the SWIFT Burst Alert Telescope ( BAT), for a sample of nearby ( z < 0: 08) Seyfert galaxies. For comparison, we have examined the relationship between the [ O iii] k5007, the 2Y10 keV, and the 14Y195 keV luminosities for the same set of objects. We find that both the [ O iv] and [ O iii] luminosities are well correlated with the BAT luminosities. When comparing [ O iv] and [ O iii] luminosities for the different types of galaxies, we find that the Seyfert 2s have significantly lower [ O iii] to [ Oiv] ratios than the Seyfert 1s. We suggest that this is due to more reddening of the narrowline region ( NLR) of the Seyfert 2s, since the [ O iv] 25.89 mu m emission line is much less affected by extinction. The combined effects of reddening and the X- ray absorption is the probable reason why the [ O iii] versus 2Y10 keV correlation is better than the [ O iv] versus 2Y10 kev correlation. Based on photoionization models, we find that the [ O iv] comes from higher ionization states and lower density regions than previous studies had determined for [ O iii]. Overall, we find the [ O iv] to be an accurate indicator of the power of the AGN. C1 [Melendez, M.; Kraemer, S. B.; Armentrout, B. K.] Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Deo, R. P.; Crenshaw, D. M.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA. [Schmitt, H. R.] Interferometr Inc, Herndon, VA 20151 USA. [Schmitt, H. R.] USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA. [Mushotzky, R. F.; Tueller, J.; Markwardt, C. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Winter, L.] Univ Maryland, College Pk, MD 20742 USA. RP Melendez, M (reprint author), Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. EM 07melendez@cua.edu RI Tueller, Jack/D-5334-2012 NR 90 TC 84 Z9 84 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 2008 VL 682 IS 1 BP 94 EP 103 DI 10.1086/588807 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 328YL UT WOS:000257834000008 ER PT J AU Brown, TM Smith, E Ferguson, HC Sweigart, AV Kimble, RA Bowers, CW AF Brown, Thomas M. Smith, Ed Ferguson, Henry C. Sweigart, Allen V. Kimble, Randy A. Bowers, Charles W. TI The dearth of UV-bright stars in M32: Implications for stellar evolution theory SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : evolution; galaxies : individual (M32); galaxies : stellar content; stars : evolution; stars : horizontal-branch ID TELESCOPE IMAGING SPECTROGRAPH; ULTRAVIOLET-UPTURN PHENOMENON; GALACTIC GLOBULAR-CLUSTERS; ASYMPTOTIC GIANT BRANCH; BACK TIME EVOLUTION; ELLIPTIC GALAXIES; PLANETARY-NEBULAE; POPULATIONS; PHOTOMETRY; RADIATION AB Using the Space Telescope Imaging Spectrograph on the Hubble Space Telescope, we have obtained deep, far-ultraviolet images of the compact elliptical galaxy M32. When combined with earlier near- ultraviolet images of the same field, these data enable the construction of an ultraviolet color- magnitude diagram of the hot horizontal branch ( HB) population and other hot stars in late phases of stellar evolution. We find few post - asymptotic giant branch ( PAGB) stars in the galaxy, implying that these stars either cross the H- R diagram more rapidly than expected, and/ or that they spend a significant fraction of their time enshrouded in circumstellar material. The predicted luminosity gap between the hot HB and its AGB- manque ( AGBM) progeny is less pronounced than expected, especially when compared to evolutionary tracks with enhanced helium abundances, implying that the presence of hot HB stars in this metal- rich population is not due to Delta Y/Delta Z greater than or similar to 4. Only a small fraction ( similar to 2%) of the HB population is hot enough to produce significant UV emission, yet most of the UV emission in this galaxy comes from the hot HB and AGBM stars, implying that PAGB stars are not a significant source of UV emission, even in those elliptical galaxies with a weak UV excess. C1 [Brown, Thomas M.; Smith, Ed; Ferguson, Henry C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Sweigart, Allen V.; Kimble, Randy A.; Bowers, Charles W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Brown, TM (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM tbrown@stsci.edu; edsmith@stsci.edu; ferguson@stsci.edu; allen.v.sweigart@nasa.gov; randy.a.kimble@nasa.gov; charles.w.bowers@nasa.gov RI Kimble, Randy/D-5317-2012; OI Brown, Thomas/0000-0002-1793-9968 NR 44 TC 42 Z9 42 U1 1 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2008 VL 682 IS 1 BP 319 EP 335 DI 10.1086/589611 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 328YL UT WOS:000257834000025 ER PT J AU Yusef-Zadeh, F Wardle, M Heinke, C Dowell, CD Roberts, D Baganoff, FK Cotton, W AF Yusef-Zadeh, F. Wardle, M. Heinke, C. Dowell, C. D. Roberts, D. Baganoff, F. K. Cotton, W. TI Simultaneous Chandra, CSO, and VLA observations of Sgr A*: The nature of flaring activity SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; Galaxy : center ID SUPERMASSIVE BLACK-HOLE; DIFFUSIVE SHOCK ACCELERATION; INEFFICIENT ACCRETION FLOWS; VARIABLE INFRARED-EMISSION; SAGITTARIUS-A; X-RAY; GALACTIC-CENTER; LINEAR-POLARIZATION; ELECTRON ACCELERATION; SPECTRAL INDEX AB Sgr A*,the massive black hole at the center of the Galaxy, varies in radio through X-ray emission on hourly timescales. The flare activity is thought to arise from the innermost region of an accretion flow onto Sgr A*. We present simultaneous light curves of Sgr A* in radio, submillimeter and X-rays that show a possible time delay of 110 +/- 17 minutes between X-ray and 850 mu m suggesting that the submillimeter flare emission is optically thick. At radio wavelengths, we detect time lags of 20.4 +/- 6: 8, 30 +/- 12, and 20 +/- 6 minutes between the flare peaks observed at 13 and 7 mm ( 22 and 43 GHz) in three different epochs using the VLA. Linear polarization of 1% +/- 0.2% and 0.7 +/- 0.1% is detected at 7 and 13 mm, respectively, when averaged over the entire observation on 2006 July 17. A simple model of a bubble of synchrotron-emitting electrons cooling via adiabatic expansion can explain the time delay between various wavelengths, the asymmetric shape of the light curves, and the observed polarization of the flare emission at 43 and 22 GHz. The derived physical quantities that characterize the emission give an expansion speed of v(exp) similar to 0.003-0.1 c, magnetic field of B similar to 10-70 G, and particle spectral index p similar to 1-2. These parameters suggest that the associated plasma cannot escape from Sgr A* unless it has a large bulk motion. C1 [Yusef-Zadeh, F.; Roberts, D.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Wardle, M.] Macquarie Univ, Dept Phys, Sydney, NSW 2109, Australia. [Heinke, C.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Dowell, C. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Baganoff, F. K.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Cotton, W.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. RP Yusef-Zadeh, F (reprint author), Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. EM zadeh@northwestern.edu; wardle@physics.mq.edu.au; coh5z@virginia.edu; cdd@submm.caltech.edu; fkb@space.mit.edu; bcotton@nrao.edu OI Wardle, Mark/0000-0002-1737-0871; Heinke, Craig/0000-0003-3944-6109 NR 55 TC 70 Z9 70 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2008 VL 682 IS 1 BP 361 EP 372 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 328YL UT WOS:000257834000028 ER PT J AU Marrone, DP Baganoff, FK Morris, MR Moran, JM Ghez, AM Hornstein, SD Dowell, CD Munoz, DJ Bautz, MW Ricker, GR Brandt, WN Garmire, GP Lu, JR Matthews, K Zhao, JH Rao, R Bower, GC AF Marrone, D. P. Baganoff, F. K. Morris, M. R. Moran, J. M. Ghez, A. M. Hornstein, S. D. Dowell, C. D. Munoz, D. J. Bautz, M. W. Ricker, G. R. Brandt, W. N. Garmire, G. P. Lu, J. R. Matthews, K. Zhao, J. -H. Rao, R. Bower, G. C. TI An X-ray, infrared, and submillimeter flare of Sagittarius A* SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; Galaxy : center; polarization ID SUPERMASSIVE BLACK-HOLE; SGR-A; GALACTIC-CENTER; LINEAR-POLARIZATION; SPECTRAL INDEX; RADIO OUTBURST; INTRINSIC SIZE; MILKY-WAY; GAMMA-RAY; 3C 273 AB Energetic flares are observed in the Galactic supermassive black hole Sagittarius A* from radio to X-ray wavelengths. On a few occasions, simultaneous flares have been detected in IR and X-ray observations, but clear counterparts at longer wavelengths have not been seen. We present a flare observed over several hours on 2006 July 17 with the Chandra X-Ray Observatory, the Keck II telescope, the Caltech Submillimeter Observatory, and the Submillimeter Array. All telescopes observed strong flare events, but the submillimeter peak is found to occur nearly 100 minutes after the X-ray peak. Submillimeter polarization data show linear polarization in the excess flare emission, increasing from 9% to 17% as the flare passes through its peak, consistent with a transition from optically thick to thin synchrotron emission. The temporal and spectral behavior of the flare require that the energetic electrons responsible for the emission cool faster than expected from their radiative output. This is consistent with adiabatic cooling in an expanding emission region, with X-rays produced through self-Compton scattering, although not consistent with the simplest model of such expansion. We also present a submillimeter flare that followed a bright IR flare on 2005 July 31. Compared to 2006, this event had a larger peak IR flux and similar submillimeter flux, but it lacked measurable X-ray emission. It also showed a shorter delay between the IR and submillimeter peaks. Based on these events we propose a synchrotron and self-Compton model to relate the submillimeter lag and the variable IR/X-ray luminosity ratio. C1 [Marrone, D. P.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Baganoff, F. K.; Bautz, M. W.; Ricker, G. R.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Morris, M. R.; Ghez, A. M.; Lu, J. R.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Moran, J. M.; Munoz, D. J.; Zhao, J. -H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ghez, A. M.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Hornstein, S. D.] Univ Colorado, Dept Astrophys & Planetary Sci, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Dowell, C. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Brandt, W. N.; Garmire, G. P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Matthews, K.] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA. [Rao, R.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Bower, G. C.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Bower, G. C.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. EM dmarrone@uchicago.edu RI Brandt, William/N-2844-2015; OI Brandt, William/0000-0002-0167-2453; Marrone, Daniel/0000-0002-2367-1080; Lu, Jessica/0000-0001-9611-0009; Moran, James/0000-0002-3882-4414 NR 67 TC 96 Z9 96 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 JUL 20 PY 2008 VL 682 IS 1 BP 373 EP 383 DI 10.1086/588806 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 328YL UT WOS:000257834000029 ER PT J AU Arendt, RG Stolovy, SR Ramirez, SV Sellgren, K Cotera, AS Law, CJ Yusef-Zadeh, F Smith, HA Gezari, DY AF Arendt, R. G. Stolovy, S. R. Ramirez, S. V. Sellgren, K. Cotera, A. S. Law, C. J. Yusef-Zadeh, F. Smith, H. A. Gezari, D. Y. TI The mid-infrared colors of the interstellar medium and extended sources at the Galactic center SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; Galaxy : center; infrared : ISM ID SPITZER-SPACE-TELESCOPE; INFRARED ARRAY CAMERA; CENTER MOLECULAR CLOUDS; STAR-FORMATION; CENTER REGION; SUPERNOVA REMNANT; ISO OBSERVATIONS; INNER GALAXY; IONIZED-GAS; EMISSION AB A mid-infrared (3.6-8 mu m) survey of the Galactic center has been carried out with the IRAC instrument on the Spitzer Space Telescope. This survey covers the central 2 degrees x 1.4 degrees (similar to 280 x 200 pc) of the Galaxy. At 3.6 and 4.5 mu m the emission is dominated by stellar sources, the fainter ones merging into an unresolved background. At 5.8 and 8 mu m the stellar sources are fainter, and large-scale diffuse emission from the ISM of the Galaxy's central molecular zone becomes prominent. The survey reveals that the 8-to-5.8 mu m color of the ISM emission is highly uniform across the surveyed region. This uniform color is consistent with a flat extinction law and emission from polycyclic aromatic hydrocarbons (PAHs). Models indicate that this broadband color should not be expected to change if the incident radiation field heating the dust and PAHs is < 10(4) times that of the solar neighborhood. The few regions with unusually red emission are areas where the PAHs are underabundant and the radiation field is locally strong enough to heat large dust grains to produce significant 8 mu m emission. These red regions include compact H II regions, Sgr B1, and wider regions around the Arches and Quintuplet clusters. In these regions the radiation field is greater than or similar to 10(4) times that of the solar neighborhood. Other regions of very red emission indicate cases where thick dust clouds obscure deeply embedded objects or very early stages of star formation. C1 [Arendt, R. G.] NASA, CRESST UMBC, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Stolovy, S. R.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Ramirez, S. V.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Sellgren, K.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Cotera, A. S.] SETI Inst, Mountain View, CA 94043 USA. [Law, C. J.; Yusef-Zadeh, F.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Law, C. J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Smith, H. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Arendt, RG (reprint author), NASA, CRESST UMBC, Goddard Space Flight Ctr, Code 665,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM richard.g.arendt@nasa.gov OI Arendt, Richard/0000-0001-8403-8548 NR 67 TC 15 Z9 15 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 2008 VL 682 IS 1 BP 384 EP 399 DI 10.1086/589635 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 328YL UT WOS:000257834000030 ER PT J AU Williams, SJ Gies, DR Henry, TJ Orosz, JA McSwain, MV Hillwig, TC Penny, LR Sonneborn, G Iping, R van der Hucht, KA Kaper, L AF Williams, S. J. Gies, D. R. Henry, T. J. Orosz, J. A. McSwain, M. V. Hillwig, T. C. Penny, L. R. Sonneborn, G. Iping, R. van der Hucht, K. A. Kaper, L. TI Dynamical masses for the Large Magellanic Cloud massive binary system [L72] LH 54-425 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : spectroscopic; stars : early-type; stars : fundamental parameters; stars : individual ([L72] LH 54-425) ID BLANKETED MODEL ATMOSPHERES; GALACTIC O-STARS; TOMOGRAPHIC SEPARATION; COMPOSITE SPECTRA; UBV PHOTOMETRY; STELLAR; ASSOCIATIONS; EVOLUTION; PARAMETERS; CLUSTER AB We present results from an optical spectroscopic investigation of the massive binary system [L72] LH 54-425 in the LH 54 OB association in the Large Magellanic Cloud. We revise the ephemeris of [L72] LH 54-425 and find an orbital period of 2.24741 +/- 0.00004 days. We find spectral types of O3 V for the primary and O5 V for the secondary. We made a combined solution of the radial velocities and previously published V-band photometry to determine the inclination for two system configurations, i = 52(-3)(+2) degrees for the configuration of the secondary star being more tidally distorted and i = 55 degrees +/- 1 degrees for the primary as the more tidally distorted star. We argue that the latter case is more probable, and this solution yields masses and radii of M-1 = 47 +/- 2 M-circle dot and R-1 = 11.4 +/- 0.1 R-circle dot for the primary, and M-2 = 28 +/- 1 M-circle dot and R-2 = 8.1 +/- 0.1 R-circle dot for the secondary. Our analysis places LH 54-425 among the most massive stars known. Based on the position of the two stars plotted on a theoretical HR diagram, we find the age of the system to be similar to 1.5 Myr. C1 [Williams, S. J.] Georgia State Univ, Ctr High Angular Resolut Astron, Atlanta, GA 30302 USA. Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA. [Orosz, J. A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [McSwain, M. V.] Lehigh Univ, Dept Phys, Bethlehem, PA 18015 USA. [Hillwig, T. C.] Valparaiso Univ, Dept Phys & Astron, Valparaiso, IN 46383 USA. [Penny, L. R.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA. [Sonneborn, G.; Iping, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Iping, R.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [van der Hucht, K. A.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [van der Hucht, K. A.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1097 SJ Amsterdam, Netherlands. [Kaper, L.] Univ Amsterdam, Astron Inst, NL-1098 SJ Amsterdam, Netherlands. RP Williams, SJ (reprint author), Georgia State Univ, Ctr High Angular Resolut Astron, POB 4106, Atlanta, GA 30302 USA. EM swilliams@chara.gsu.edu; gies@chara.gsu.edu; thenry@chara.gsu.edu; orosz@sciences.sdsu.edu; mcswain@lehigh.edu; todd.hillwig@valpo.edu; pennyl@cofc.edu; george.sonneborn@nasa.gov; Rosina.C.Iping@nasa.gov; k.a.van.der.hucht@sron.nl; lexk@science.uva.nl RI Sonneborn, George/D-5255-2012; Williams, Stephen/L-3659-2013; OI Hillwig, Todd/0000-0002-0816-1090 NR 28 TC 15 Z9 15 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2008 VL 682 IS 1 BP 492 EP 498 DI 10.1086/589687 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 328YL UT WOS:000257834000039 ER PT J AU Estrada, PR Cuzzi, JN AF Estrada, P. R. Cuzzi, J. N. TI Solving the coagulation equation by the moments method SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; methods : numerical; radiative transfer; solar system : formation ID PROTOPLANETARY DISKS; SOLAR NEBULA; CIRCUMSTELLAR DISKS; DUST COAGULATION; PLANET FORMATION; GRAIN-GROWTH; ACCRETION; PLANETESIMALS; PARTICLES; GAS AB We demonstrate an approach to solving the coagulation equation that involves using a finite number of moments of the particle size distribution. This approach is particularly useful when only general properties of the distribution, and their time evolution, are needed. The numerical solution to the integrodifferential Smoluchowski coagulation equation at every time step, for every particle size, and at every spatial location is computationally expensive and serves as the primary bottleneck in running evolutionary models over long periods of time. The advantage of using the moments method comes in the computational time savings gained from only tracking the time rate of change of the moments, as opposed to tracking the entire mass histogram which can contain hundreds or thousands of bins depending on the desired accuracy. The collision kernels of the coagulation equation contain all the necessary information about particle relative velocities, cross sections, and sticking coefficients. We show how arbitrary collision kernels may be treated. We discuss particle relative velocities in both turbulent and nonturbulent regimes. We present examples of this approach that utilize different collision kernels and find good agreement between the moment solutions and the moments as calculated from direct integration of the coagulation equation. As practical applications, we demonstrate how the moments method can be used to track the evolving opacity and also indicate how one may incorporate porous particles. C1 [Estrada, P. R.] SETI Inst, Mountain View, CA 94043 USA. [Cuzzi, J. N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Estrada, PR (reprint author), SETI Inst, 515 N Whisman Rd, Mountain View, CA 94043 USA. NR 42 TC 12 Z9 12 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 JUL 20 PY 2008 VL 682 IS 1 BP 515 EP 526 DI 10.1086/589685 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 328YL UT WOS:000257834000042 ER PT J AU Wisniewski, JP Clampin, M Grady, CA Ardila, DR Ford, HC Golimowski, DA Illingworth, GD Krist, JE AF Wisniewski, John P. Clampin, Mark Grady, Carol A. Ardila, David R. Ford, Holland C. Golimowski, David A. Illingworth, Garth D. Krist, John E. TI The HD 163296 circumstellar disk in scattered light: Evidence of time-variable self-shadowing SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems : formation; planetary systems : protoplanetary disks; stars : individual (HD 163296) ID HERBIG AE/BE STARS; TELESCOPE ADVANCED CAMERA; INTERMEDIATE-MASS STARS; TAURI CIRCUMBINARY DISK; HIGH-RESOLUTION; DEBRIS DISK; AE SYSTEMS; PROTOPLANETARY DISKS; ISO SPECTROSCOPY; GRAIN-GROWTH AB We present the first multicolor view of the scattered light disk of the Herbig Ae star HD 163296, based on coronagraphic observations from the Hubble Space Telescope Advanced Camera for Surveys (HSTACS). Radial profile fits of the surface brightness along the disk's semimajor axis indicate that the disk is not continuously flared, and extends to similar to 540 AU. The disk's color (V - I) = 1.1 at a radial distance of 3.5 '' is redder than the observed stellar color (V - I) = 0.15. This red disk color might be indicative of either an evolution in the grain size distribution (i.e., grain growth) and/or composition, both of which would be consistent with the observed nonflared geometry of the outer disk. We also identify a single ansa morphological structure in our F435W ACS data, which is absent from earlier epoch F606W and F814W ACS data, but corresponds to one of the two ansae observed in archival HST Space Telescope Imaging Spectrograph (STIS) coronagraphic data. Following transformation to similar bandpasses, we find that the scattered light disk of HD 163296 is 1 mag arcsec(-2) fainter at 3.5 '' in the STIS data than in the ACS data. Moreover, variations are seen in (1) the visibility of the ansa(e) structures, (2) the relative surface brightness of the ansa(e) structures, and (3) the (known) intrinsic polarization of the system. These results indicate that the scattered light from the HD 163296 disk is variable. We speculate that the inner disk wall, which Sitko et al. suggests has a variable scale height as diagnosed by near-IR SED variability, induces variable self-shadowing of the outer disk. We further speculate that the observed surface brightness variability of the ansa(e) structures may indicate that the inner disk wall is azimuthally asymmetric. C1 [Wisniewski, John P.; Clampin, Mark; Grady, Carol A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Grady, Carol A.] Eureka Sci, Oakland, CA 94602 USA. [Ardila, David R.] Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Ford, Holland C.; Golimowski, David A.] Johns Hopkins Univ, Baltimore, MD 20218 USA. [Illingworth, Garth D.] Univ Calif Santa Cruz, Lick Observ, Santa Cruz, CA 95064 USA. [Krist, John E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Wisniewski, JP (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. EM john.p.wisniewski@gmail.com; mark.clampin@nasa.gov; carol.a.grady@nasa.gov; ardila@ipac.caltech.edu; ford@pha.jhu.edu; dag@pha.jhu.edu; gdi@ucolick.org; john.e.krist@jpl.nasa.gov RI Clampin, mark/D-2738-2012 NR 45 TC 37 Z9 37 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 2008 VL 682 IS 1 BP 548 EP 558 DI 10.1086/589629 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 328YL UT WOS:000257834000045 ER PT J AU Showman, AP Cooper, CS Fortney, JJ Marley, MS AF Showman, Adam P. Cooper, Curtis S. Fortney, Jonathan J. Marley, Mark S. TI Atmospheric circulation of hot Jupiters: Three-dimensional circulation models of HD 209458b and HD 189733b with simplified forcing SO ASTROPHYSICAL JOURNAL LA English DT Article DE atmospheric effects; methods : numerical; planets and satellites : general; planets and satellites : individual (HD 209458b) ID EXTRASOLAR GIANT PLANETS; SHALLOW-WATER TURBULENCE; HD 209458B; GENERAL-CIRCULATION; SECONDARY ECLIPSE; THERMAL STRUCTURE; SPECTRAL MODELS; BROWN DWARFS; LIGHT CURVES; DYNAMICS AB We present global, three-dimensional numerical simulations of the atmospheric circulation on HD 209458b and HD 189733b and calculate the infrared spectra and light curves predicted by these simulations, which we compare with available observations. Radiative heating/cooling is parameterized with a simplified Newtonian relaxation scheme. Our simulations develop day-night temperature contrasts that vary strongly with pressure. At low pressure (< 10 mbar), air flows from the substellar point toward the antistellar point, both along the equator and over the poles. At deeper levels, the flow develops an eastward equatorial jet with speeds of 3-4 km s(-1), with weaker westward flows at high latitudes. This basic flow pattern is robust to variations in model resolution, gravity, radiative time constant, and initial temperature structure. Nightside spectra show deep absorption bands of H2O, CO, and/or CH4, whereas on the dayside these absorption bands flatten out or even flip into emission. This results from the strong effect of dynamics on the vertical temperature-pressure structure; the temperature decreases strongly with altitude on the nightside but becomes almost isothermal on the dayside. In Spitzer bandpasses, our predicted planet-to-star flux ratios vary by a factor of similar to 2-10 with orbital phase, depending on the wavelength and chemistry. For HD 189733b, where a detailed 8 mu m light curve has been obtained, we correctly produce the observed phase offset of the flux maximum, but we do not explain the flux minimum and we overpredict the total flux variation. This discrepancy likely results from the simplifications inherent in the Newtonian relaxation scheme and provides motivation for incorporating realistic radiative transfer in future studies. C1 [Showman, Adam P.; Cooper, Curtis S.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Showman, Adam P.; Cooper, Curtis S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Cooper, Curtis S.] Univ Arizona, NASA, Astrobiol Inst, Tucson, AZ 85721 USA. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Lick Observ, UCO, Santa Cruz, CA 95064 USA. [Fortney, Jonathan J.; Marley, Mark S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Showman, AP (reprint author), Univ Arizona, Dept Planetary Sci, 1629 Univ Blvd, Tucson, AZ 85721 USA. EM showman@lpl.arizona.edu RI Marley, Mark/I-4704-2013; OI Fortney, Jonathan/0000-0002-9843-4354 NR 77 TC 108 Z9 109 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2008 VL 682 IS 1 BP 559 EP 576 DI 10.1086/589325 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 328YL UT WOS:000257834000046 ER PT J AU Brosius, JW Rabin, DM Thomas, RJ AF Brosius, Jeffrey W. Rabin, Douglas M. Thomas, Roger J. TI Rapid cadence EUNIS-06 observations of a HeII transient brightening in the quiet sun SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : corona; Sun : magnetic fields; Sun : transition region; Sun : UV radiation ID CORONAL DIAGNOSTIC SPECTROMETER; EXTREME-ULTRAVIOLET SPECTRUM; SOLAR TRANSITION REGION; LOOP RADIATIVE HYDRODYNAMICS; HIGH TIME RESOLUTION; ACTIVE-REGION; CHROMOSPHERIC EVAPORATION; EXPLOSIVE EVENTS; SOUNDING ROCKET; BLINKERS AB We observed a transient brightening in the quiet Sun at rapid cadence (2.10 s) with the Extreme Ultraviolet Normal Incidence Spectrograph (EUNIS-06) sounding rocket instrument on 2006 April 12. The transient was visible only in He II at 303.78 angstrom ( T approximate to 5 x 10(4) K), and its maximum temperature T was < 4 x 10(5) K. Taking its linear extent along the EUNIS slit to be the diameter of a circular feature, the transient's solar surface area was 7.8 x 10(7) km(2). EUNIS observed the brightening to begin at 18: 12: 52 and peak at 18: 13: 29 UT; coordinated observations with SOHO's EIT confirm that EUNIS observed the onset of the brightening. EUNIS spectra yield maximum and average He II intensity enhancements of 2.09 and 1.46, respectively, relative to the pre- event quiet Sun. He II line profiles from EUNIS reveal that relative upflows were persistent during the transient ( with a maximum speed around 20 km s(-1)) and that the upflow speed and intensity were positively correlated. Variations in the observed He II intensity and relative Doppler velocity were neither abrupt not impulsive, but occurred slowly compared to the EUNIS cadence. The local photospheric longitudinal magnetic field strength measured with SOHO's MDI revealed no significant variability. The transient's measured properties are consistent with its identification as a blinker or an elementary blinker, and its observed behavior suggests a formation mechanism involving gentle chromospheric evaporation. C1 [Brosius, Jeffrey W.] Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. RP Brosius, JW (reprint author), Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Solar Phys Lab, Code 671, Greenbelt, MD 20771 USA. EM jeffrey.w.brosius@nasa.gov; douglas.m.rabin@nasa.gov; roger.j.thomas@nasa.gov NR 32 TC 4 Z9 4 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2008 VL 682 IS 1 BP 630 EP 637 DI 10.1086/589281 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 328YL UT WOS:000257834000052 ER PT J AU Schorghofer, N AF Schorghofer, Norbert TI Lifetime of ice on main belt asteroids SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; comets : general; minor planets; asteroids ID THERMAL-CONDUCTIVITY MEASUREMENTS; ASTROPHYSICAL IMPLICATIONS; PARTICULATE MATERIALS; POROUS MEDIA; WATER ICE; COMET; H2O; SUBLIMATION; INSOLATION; DIFFUSION AB We theoretically estimate the loss rate of buried ice from spherical bodies 2-3.3 AU from the Sun. The loss rate is explored as a function of about a dozen parameters. We introduce the concept of a "buried snow line,'' where the loss of ice is sufficiently slow over the age of the solar system. For a dusty surface layer, ice can persist within the top few meters of the surface over billions of years, if the mean surface temperature is less than about 145 K. Variations in surface layer properties within a plausible range are unlikely to change this threshold temperature by more than 10 K. Longevity of ice in the shallow subsurface of asteroid 7968 Elst-Pizarro is plausible. Parameter regions for ice to survive over the age of the solar system exist for all of the main asteroid belt, but preferentially for large distances from the Sun and slowly rotating bodies with surfaces consisting of small particles, leading to low thermal conductivity and short molecular free paths. Rocky surfaces, in contrast to dusty surfaces, are rarely able to retain ice in the shallow subsurface. C1 [Schorghofer, Norbert] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Schorghofer, Norbert] Univ Hawaii, NASA Astrobiol Inst, Honolulu, HI 96822 USA. RP Schorghofer, N (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. RI Schorghofer, Norbert/A-1194-2007 NR 37 TC 67 Z9 67 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 2008 VL 682 IS 1 BP 697 EP 705 DI 10.1086/588633 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 328YL UT WOS:000257834000059 ER PT J AU Baker, JG Boggs, WD Centrella, J Kelly, BJ McWilliams, ST Miller, MC Van Meter, JR AF Baker, John G. Boggs, William D. Centrella, Joan Kelly, Bernard J. McWilliams, Sean T. Miller, M. Coleman Van Meter, James R. TI Modeling kicks from the merger of generic black hole binaries SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE black hole physics; galaxies : nuclei; gravitational waves; relativity ID GRAVITATIONAL RECOIL; GLOBULAR-CLUSTERS; GALACTIC NUCLEI; STAR-CLUSTERS; GROWTH; SPIN; COALESCENCE; MCG-6-30-15; VELOCITIES; SIGNATURES AB Recent numerical relativistic results demonstrate that the merger of comparable-mass spinning black holes has a maximum "recoil kick" of up to similar to 4000 km s(-1). However, the scaling of these recoil velocities with mass ratio is poorly understood. We present new runs showing that the maximum possible kick perpendicular to the orbital plane does not scale as similar to eta(2) (where eta is the symmetric mass ratio), as previously proposed, but is more consistent with similar to eta(3), at least for systems with low orbital precession. We discuss the effect of this dependence on galactic ejection scenarios and retention of intermediate-mass black holes in globular clusters. C1 [Baker, John G.; Centrella, Joan; Kelly, Bernard J.; Van Meter, James R.] NASA, Goddard Space Flight Ctr, Lab Gravitat Astrophys, Greenbelt, MD 20771 USA. [Miller, M. Coleman] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Boggs, William D.; McWilliams, Sean T.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. RP Baker, JG (reprint author), NASA, Goddard Space Flight Ctr, Lab Gravitat Astrophys, Greenbelt, MD 20771 USA. RI van meter, james/E-7893-2011; Kelly, Bernard/G-7371-2011; OI Kelly, Bernard/0000-0002-3326-4454 NR 51 TC 104 Z9 104 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 20 PY 2008 VL 682 IS 1 BP L29 EP L32 DI 10.1086/590927 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 326MF UT WOS:000257662700008 ER PT J AU Moskovitz, NA Lawrence, S Jedicke, R Willman, M Haghighipour, N Bus, SJ Gaidos, E AF Moskovitz, Nicholas A. Lawrence, Samuel Jedicke, Robert Willman, Mark Haghighipour, Nader Bus, Schelte J. Gaidos, Eric TI A spectroscopically unique main-belt asteroid: 10537 (1991 RY16) SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE minor planets, asteroids; solar system : formation ID MINOR ABSORPTION-BANDS; V-TYPE ASTEROIDS; REFLECTANCE SPECTRA; PARENT BODIES; NEAR-EARTH; SECULAR RESONANCES; CLOSE ENCOUNTERS; SOLAR-SYSTEM; VESTA FAMILY; SPECTROGRAPH AB We present visible and near-infrared reflectance spectra and interpreted surface mineralogy for asteroid 10537 ( 1991 RY16). The spectrum of this object is without precedent among the main-belt asteroids. A unique absorption band centered at 0.63 mu m could be attributed to one of several mineralogies. Pronounced 1 and 2 mu m absorption bands suggest that the composition of 10537 is a mixture of pyroxenes and olivine and that it originated from a parent body that was partially or fully differentiated. The closest available analog is the large main-belt asteroid 349 Dembowska, but 10537 may be an isolated fragment from a completely eroded parent body. C1 [Moskovitz, Nicholas A.; Jedicke, Robert; Willman, Mark] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Lawrence, Samuel] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Haghighipour, Nader; Gaidos, Eric] Univ Hawaii, NASA Astrobiol Inst, Honolulu, HI 96822 USA. [Bus, Schelte J.] Inst Astron, Hilo, HI 96720 USA. [Gaidos, Eric] Univ Hawaii, Dept Geol & Geophys, Honolulu, HI 96822 USA. RP Moskovitz, NA (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM nmosko@ifa.hawaii.edu; sjlawren@asu.edu; jedicke@ifa.hawaii.edu; willman@ifa.hawaii.edu; nader@ifa.hawaii.edu; sjb@ifa.hawaii.edu; gaidos@hawaii.edu NR 65 TC 10 Z9 10 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 20 PY 2008 VL 682 IS 1 BP L57 EP L60 DI 10.1086/591030 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 326MF UT WOS:000257662700015 ER PT J AU Borovsky, JE Hesse, M Birn, J Kuznetsova, MM AF Borovsky, Joseph E. Hesse, Michael Birn, Joachim Kuznetsova, Maria M. TI What determines the reconnection rate at the dayside magnetosphere? SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID INTERPLANETARY MAGNETIC-FIELD; PILE-UP RECONNECTION; MAGNETOPAUSE RECONNECTION; ELECTRIC-FIELD; LARGE SYSTEMS; MHD; COLLISIONLESS; ENVIRONMENT; CHALLENGE; MAGNETOSHEATH AB Reconnection between the magnetosphere and magnetosheath at the dayside magnetopause is studied for southward IMF using high-resolution 3-D MHD simulations. The BATSRUS code is run at CCMC with a resistive spot added on the magnetopause to ensure that fast reconnection occurs and to control the reconnection physics. A large range of Mach numbers (1.9-15) are run. The reconnection rate at the nose of the magnetosphere is measured and compared with local plasma parameters and with upstream-solar wind parameters. It is found that the reconnection rate is controlled by four local plasma parameters: B(s) (the magnetic field strength in the magnetosheath), B(m) (the magnetic field strength in the magnetosphere), rho(s) (the plasma mass density in the magnetosheath), and rho(m) (the plasma mass density in the magnetosphere). The Cassak-Shay formula for fast reconnection was tested and found to successfully describe the reconnection rate on the dayside magnetopause. It was found that reconnection itself does not significantly modify the local plasma parameters that control dayside reconnection and argued that reconnection does not significantly alter the flow pattern of the magnetosheath. This means that dayside reconnection is not "driven'' in the sense that plasma pileup occurs to change the local parameters to adjust the reconnection rate to balance the driving. A "plasmasphere effect'' was observed in the simulations wherein high-density magnetospheric plasma flows into the magnetopause reconnection site and mass loads the reconnection: a spatially localized plume of plasma was observed to locally reduce the reconnection rate by about a factor of 2. C1 [Borovsky, Joseph E.; Birn, Joachim] Los Alamos Natl Lab, Space Sci & Applicat Grp ISR 1, Los Alamos, NM 87545 USA. [Hesse, Michael; Kuznetsova, Maria M.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. RP Borovsky, JE (reprint author), Los Alamos Natl Lab, Space Sci & Applicat Grp ISR 1, Mail Stop D466, Los Alamos, NM 87545 USA. EM jborovsky@lanl.gov RI Hesse, Michael/D-2031-2012; Kuznetsova, Maria/F-6840-2012; NASA MMS, Science Team/J-5393-2013 OI NASA MMS, Science Team/0000-0002-9504-5214 NR 70 TC 63 Z9 64 U1 0 U2 10 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 19 PY 2008 VL 113 IS A7 AR A07210 DI 10.1029/2007JA012645 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 328MD UT WOS:000257801600001 ER PT J AU LeGrande, AN Schmidt, GA AF LeGrande, Allegra N. Schmidt, Gavin A. TI Ensemble, water isotope-enabled, coupled general circulation modeling insights into the 8.2 ka event SO PALEOCEANOGRAPHY LA English DT Article ID ABRUPT CLIMATE-CHANGE; ATLANTIC THERMOHALINE CIRCULATION; GLACIAL LAKE AGASSIZ; ATMOSPHERE-OCEAN MODEL; NORTH-ATLANTIC; COLD EVENT; BP EVENT; CATASTROPHIC DRAINAGE; LAST DEGLACIATION; HOLOCENE CLIMATE AB Freshwater forcing has long been postulated as a catalyst for abrupt climate change because of its potential to interfere with thermohaline circulation (THC). The most recent example may have occurred about 8.2 ka ago with the sudden drainage of glacial lakes Agassiz and Ojibway into the Hudson Bay. We perform an ensemble of simulations for this freshwater release using the fully coupled atmosphere ocean general circulation model, Goddard Institute for Space Studies ModelE-R. In all cases, simulated effects include reduced ocean heat transport and enhanced atmospheric heat transport in the Atlantic, increased surface albedo ( through greater low cloud and sea ice cover), and local cooling of up to 3 degrees C. Our suite of ensemble experiments allows us to examine the importance of the initial ocean state, in particular the presence or absence of Labrador Sea Water, in controlling the magnitude and length of the climate response. Water isotope tracers included in this model provide an improved means for direct comparisons of the modeled tracer response to water isotope-based, climate proxy data. Comparison of model simulations to data implies that there was an abrupt approximate halving of Atlantic THC, hence providing strong support for the hypothesis that the 8.2 ka event was caused by an abrupt release of fresh water into the North Atlantic. C1 [LeGrande, Allegra N.; Schmidt, Gavin A.] NASA Goddard Inst Space Studies, Ctr Climate Syst Res, New York, NY 10025 USA. RP LeGrande, AN (reprint author), NASA Goddard Inst Space Studies, Ctr Climate Syst Res, 2880 Broadway, New York, NY 10025 USA. EM legrande@giss.nasa.gov RI Schmidt, Gavin/D-4427-2012; LeGrande, Allegra/D-8920-2012 OI Schmidt, Gavin/0000-0002-2258-0486; LeGrande, Allegra/0000-0002-5295-0062 NR 59 TC 44 Z9 45 U1 2 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0883-8305 EI 1944-9186 J9 PALEOCEANOGRAPHY JI Paleoceanography PD JUL 19 PY 2008 VL 23 IS 3 AR PA3207 DI 10.1029/2008PA001610 PG 19 WC Geosciences, Multidisciplinary; Oceanography; Paleontology SC Geology; Oceanography; Paleontology GA 328MG UT WOS:000257801900001 ER PT J AU Buker, ML Hitchman, MH Tripoli, GJ Pierce, RB Browell, EV Al-Saadi, JA AF Bueker, M. L. Hitchman, Matthew H. Tripoli, Gregory J. Pierce, R. B. Browell, E. V. Al-Saadi, J. A. TI Long-range convective ozone transport during INTEX SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID STRATOSPHERE-TROPOSPHERE EXCHANGE; ROSSBY-WAVE BREAKING; SUBTROPICAL TROPOPAUSE; TRACE CONSTITUENTS; MODEL; CLIMATOLOGY; SIMULATION; BUDGET; MASS AB Ozone transport across the tropopause near a convective region in the central Pacific is calculated for a 1-day period using a nested grid, high-resolution simulation with the University of Wisconsin Nonhydrostatic Modeling System (UWNMS). This ozone is then tracked into the region where DC-8 lidar ozone observations on 6 July 2004 were taken over the United States during the Intercontinental Chemical Transport Experiment-North America (INTEX-NA). On 2 July a convective complex developed north of the Midway Islands and intensified as it propagated eastward. Satellite observations captured this event well, and the UWNMS simulation placed the convection just east of an upper level trough along the subtropical jet. The proximity of the strong convection to the lowered tropopause resulted in significant stratospheric ozone contribution (SOC) to the troposphere. During the 24 h period starting at 1200 UTC 2 July, total net ozone flux into the troposphere was calculated to be about 0.2 Tg across the nested grid domain. Because the convective outflow was feeding the subtropical jet, the SOC was quickly transported across the eastern Pacific and into the INTEX-NA region. Using an "SOC tracer" we show that a small but significant percentage of observed ozone on the DC8 flight can be attributed to SOC from this one convective event. This supports the idea that the stratosphere over the Pacific is an important source of ozone for air entering North America from the west. C1 [Bueker, M. L.; Hitchman, Matthew H.; Tripoli, Gregory J.] Univ Wisconsin, Dept Atmospher & Ocean Sci, Madison, WI 53706 USA. [Pierce, R. B.; Browell, E. V.; Al-Saadi, J. A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Buker, ML (reprint author), Univ Wisconsin, Dept Atmospher & Ocean Sci, 1225 W Dayton, Madison, WI 53706 USA. EM bukerm@uwosh.edu; matt@aos.wisc.edu; tripoli@aos.wisc.edu; r.b.pierce@larc.nasa.gov; e.v.browell@larc.nasa.gov; jaal-saadi@larc.nasa.gov RI Pierce, Robert Bradley/F-5609-2010 OI Pierce, Robert Bradley/0000-0002-2767-1643 NR 36 TC 5 Z9 5 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 18 PY 2008 VL 113 IS D14 AR D14S90 DI 10.1029/2007JD009345 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 328KW UT WOS:000257798300003 ER PT J AU Jiang, JH Su, H Schoeberl, MR Massie, ST Colarco, P Platnick, S Livesey, NJ AF Jiang, Jonathan H. Su, Hui Schoeberl, Mark R. Massie, Steven T. Colarco, Peter Platnick, Steven Livesey, Nathaniel J. TI Clean and polluted clouds: Relationships among pollution, ice clouds, and precipitation in South America SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID AEROSOLS; VALIDATION; PARAMETERS; RESOLUTION; CLIMATE; ALBEDO; IMPACT; SMOKE AB We analyze nearly-simultaneous measurements of ice clouds and pollutants along satellite tracks. We use Aura MLS CO and ice water content measurements at 215 hPa to classify ice clouds as "clean'' or "polluted''. We then examine Aqua MODIS ice particle effective radius (re) and aerosol optical thickness (AOT) along with TRMM precipitation to investigate how pollution changes ice particle size and precipitation. We find suppressed precipitation and reduced re associated with polluted clouds during the dry season in South America when there is a strong positive correlation between the CO and AOT. In contrast, during the wet season, we find little difference in ice particle size and precipitation between the polluted clouds and the clean clouds, as indicated by the CO levels, when the AOT is significantly lower than that in the dry season. C1 [Jiang, Jonathan H.; Su, Hui; Livesey, Nathaniel J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Schoeberl, Mark R.; Colarco, Peter; Platnick, Steven] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Massie, Steven T.] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA. RP Jiang, JH (reprint author), CALTECH, Jet Prop Lab, Mail Stop 183-701,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM jonathan.h.jiang@jpl.nasa.gov RI Colarco, Peter/D-8637-2012; Platnick, Steven/J-9982-2014 OI Colarco, Peter/0000-0003-3525-1662; Platnick, Steven/0000-0003-3964-3567 NR 30 TC 29 Z9 31 U1 0 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 17 PY 2008 VL 35 IS 14 AR L14804 DI 10.1029/2008GL034631 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 328KJ UT WOS:000257797000005 ER PT J AU Gao, RS Hall, SR Swartz, WH Schwarz, JP Spackman, JR Watts, LA Fahey, DW Aikin, KC Shetter, RE Bui, TP AF Gao, R. S. Hall, S. R. Swartz, W. H. Schwarz, J. P. Spackman, J. R. Watts, L. A. Fahey, D. W. Aikin, K. C. Shetter, R. E. Bui, T. P. TI Calculations of solar shortwave heating rates due to black carbon and ozone absorption using in situ measurements SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID LOWER STRATOSPHERE; LIGHT-SCATTERING; SOOT; PHOTOCHEMISTRY; PHOTOMETER; PARTICLES; AEROSOLS; POLARIS; CLIMATE; CLOUD AB Results for the solar heating rates in ambient air due to absorption by black-carbon (BC) containing particles and ozone are presented as calculated from airborne observations made in the tropical tropopause layer (TTL) in January -February 2006. The method uses airborne in situ observations of BC particles, ozone and actinic flux. Total BC mass is obtained along the flight track by summing the masses of individually detected BC particles in the range 90 to 600-nm volume-equivalent diameter, which includes most of the BC mass. Ozone mixing ratios and upwelling and partial downwelling solar actinic fluxes were measured concurrently with BC mass. Two estimates used for the BC wavelength-dependent absorption cross section yielded similar heating rates. For mean altitudes of 16.5, 17.5, and 18.5 km (+/- 0.5 km) in the tropics, average BC heating rates were near 0.0002 K d(-1). Observed BC coatings on individual particles approximately double derived BC heating rates. Ozone heating rates exceeded BC heating rates by approximately a factor of 100 on average and at least a factor of 4, suggesting that BC heating rates in this region are negligible in comparison. C1 [Gao, R. S.; Schwarz, J. P.; Spackman, J. R.; Watts, L. A.; Fahey, D. W.; Aikin, K. C.] NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO 80305 USA. [Bui, T. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Hall, S. R.; Shetter, R. E.] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80305 USA. [Swartz, W. H.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Schwarz, J. P.; Spackman, J. R.; Watts, L. A.; Fahey, D. W.; Aikin, K. C.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. RP Gao, RS (reprint author), NOAA, Div Chem Sci, Earth Syst Res Lab, 325 Broadway R-CSD 6, Boulder, CO 80305 USA. EM rushan.gao@noaa.gov RI Swartz, William/A-1965-2010; schwarz, joshua/G-4556-2013; Gao, Ru-Shan/H-7455-2013; Aikin, Kenneth/I-1973-2013; Watts, Laurel/G-4532-2013; Fahey, David/G-4499-2013; Manager, CSD Publications/B-2789-2015 OI Swartz, William/0000-0002-9172-7189; schwarz, joshua/0000-0002-9123-2223; Watts, Laurel/0000-0002-0834-3329; Fahey, David/0000-0003-1720-0634; NR 34 TC 15 Z9 16 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 17 PY 2008 VL 113 IS D14 AR D14203 DI 10.1029/2007JD009358 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 328KV UT WOS:000257798200002 ER PT J AU Li, T Leblanc, T McDermid, IS AF Li, Tao Leblanc, Thierry McDermid, I. Stuart TI Interannual variations of middle atmospheric temperature as measured by the JPL lidar at Mauna Loa Observatory, Hawaii (19.5 degrees N, 155.6 degrees W) SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID QUASI-BIENNIAL OSCILLATION; 11-YEAR SOLAR-CYCLE; UPPER-STRATOSPHERE; TOTAL OZONE; ENSO; SIMULATIONS; TRENDS; MODEL; QBO; MESOSPHERE AB The Jet Propulsion Laboratory Rayleigh-Raman lidar at Mauna Loa Observatory (MLO), Hawaii (19.5 degrees N, 155.6 degrees W) has been measuring atmospheric temperature vertical profiles routinely since 1993. Linear regression analysis was applied to the 13.5-yearlong (January 1994 to June 2007) deseasonalized monthly mean lidar temperature time series for each 1-km altitude bin between 15 and 85 km. The regression analysis included components representing the Quasi-Biennial Oscillation (QBO), El Nino-Southern Oscillation (ENSO), and the 11-year solar cycle. Where overlapping was possible, the results were compared to those obtained from the twice-daily National Weather Service (NWS) radiosonde profiles at Hilo (5 -30 km) located 60 km east-north-east of the lidar site, and the four-times-daily temperature analysis of the European Centre for Medium Range Weather Forecast (ECMWF). The analysis revealed the dominance of the QBO (1 -3 K) in the stratosphere and mesosphere, and a strong winter signature of ENSO in the troposphere and lowermost stratosphere (similar to 1.5 K/MEI). Additionally, and for the first time, a statistically significant signature of ENSO was observed in the mesosphere, consistent with the findings of recent model simulations. The annual mean response to the solar cycle shows two statistically significant maxima of similar to 1.3 K/100 F10.7 units at 35 and 55 km. The temperature responses to QBO, ENSO, and solar cycle are all maximized in winter. Comparisons with the global ECMWF temperature analysis clearly showed that the middle atmosphere above MLO is under a subtropical/ extratropical regime, i. e., generally out-of-phase with that in the equatorial regions, and synchronized to the northern hemisphere winter/spring. C1 [Leblanc, Thierry; McDermid, I. Stuart] CALTECH, Jet Prop Lab, Table Mt Facil, Wrightwood, CA 92397 USA. RP Li, T (reprint author), Univ Sci & Technol China, Sch Earth & Space Sci, 96 Jinzhai Rd, Hefei 230026, Anhui, Peoples R China. EM litao@ustc.edu.cn RI Li, Tao/J-8950-2014 OI Li, Tao/0000-0002-5100-4429 NR 38 TC 27 Z9 28 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 JUL 17 PY 2008 VL 113 IS D14 AR D14109 DI 10.1029/2007JD009764 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 328KV UT WOS:000257798200007 ER PT J AU Liang, Q Stolarski, RS Douglass, AR Newman, PA Nielsen, JE AF Liang, Qing Stolarski, Richard S. Douglass, Anne R. Newman, Paul A. Nielsen, J. Eric TI Evaluation of emissions and transport of CFCs using surface observations and their seasonal cycles and the GEOS CCM simulation with emissions-based forcing SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID CARBON-MONOXIDE; AIR-POLLUTION; MACE HEAD; OZONE; PACIFIC; TROPOSPHERE; EXCHANGE; STRATOSPHERE; TROPOPAUSE; ATMOSPHERE AB Levels of ozone depleting substances (ODSs) in our atmosphere are determined by production, emission, and loss processes. However, atmospheric models are forced by the specified mixing ratios of these ODSs rather than the more fundamental emissions-based forcing. To more accurately represent the physics and chemistry of climate change on atmospheric circulation and ODSs, and therefore future ozone recovery, it is desirable to switch from the current highly constrained mixing-ratio-based forcing to emissions-based forcing in general circulation models (GCMs). As a first step of this model transition, we have conducted a 45-year (1960-2005) emissions-based simulation of the three primary chlorofluorocarbons (CFC-11,-12,-113) using the GEOS coupled chemistry-climate model (CCM). The simulated CFC concentrations and their seasonal cycles are compared with AGAGE and NOAA-GMD observations to evaluate emissions and atmospheric transport. The simulated CFC-12 agrees well with the observations, indicating a good estimate of emission and atmospheric loss. The simulated CFC-11 and CFC-113 shows high biases due to overestimate of emissions. Using tagged CFC tracers to track recent surface emissions and aged air masses transported downward from the stratosphere separately, we quantify the relative contribution of stratosphere-troposphere exchange (STE) and tropospheric transport to the seasonal cycles of CFCs in the lower troposphere. The seasonal cycles of CFCs in the lower troposphere are dominated by tropospheric transport of recent emissions during 1985-1994. The 1995-1999 period marks the transition period when variations due to fresh emissions and STE become equally important. Seasonal cycles of CFCs at most surface sites in the 2000-2004 period are dominated by STE. Seasonal cycles of CFCs due to STE show a late winter/early spring maximum and a summer/fall minimum. Seasonality of the tropospheric transport component at individual stations is governed by seasonal transport variations of fresh emissions from the polluted regions. C1 [Liang, Qing; Stolarski, Richard S.; Douglass, Anne R.; Newman, Paul A.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Greenbelt, MD 20771 USA. [Liang, Qing] Oak Ridge Associated Univ, NASA, Postdoctoral Program, Oak Ridge, TN 37831 USA. [Nielsen, J. Eric] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Nielsen, J. Eric] Sci Syst & Applicat Inc, Lanham, MD USA. RP Liang, Q (reprint author), NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Code 613-3, Greenbelt, MD 20771 USA. EM qing.liang-1@nasa.gov; richard.s.stolarski@nasa.gov; anne.r.douglass@nasa.gov; paul.a.newman@nasa.gov; nielsen@gmao.gsfc.nasa.gov RI Liang, Qing/B-1276-2011; Newman, Paul/D-6208-2012; Douglass, Anne/D-4655-2012; Stolarski, Richard/B-8499-2013 OI Newman, Paul/0000-0003-1139-2508; Stolarski, Richard/0000-0001-8722-4012 NR 46 TC 15 Z9 15 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 17 PY 2008 VL 113 IS D14 AR D14302 DI 10.1029/2007JD009617 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 328KV UT WOS:000257798200006 ER PT J AU Salstein, DA Ponte, RM Cady-Pereira, K AF Salstein, David A. Ponte, Rui M. Cady-Pereira, Karen TI Uncertainties in atmospheric surface pressure fields from global analyses SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID VARIABILITY; GRACE; MASS; SYSTEM; OCEAN AB Operational analyses from the U. S. National Centers for Environmental Prediction (NCEP) and the European Centre for Medium-Range Weather Forecasts (ECMWF) provide, among other quantities, atmospheric surface pressure. This field is especially useful for data processing and interpretation of altimeter and gravity satellite missions like Jason-1 and GRACE (Gravity Recovery and Climate Experiment). Quantitative use of this pressure field, however, requires knowledge of its uncertainties. To assess these uncertainties, we compare NCEP and ECMWF analyses of surface pressure to an extensive set of surface barometric observations for the period 2001-2005, both land-and ocean-based, as well as to each other. Differences between each analysis and the observations are quite similar, indicating that both analyses generally fit the station observations equally well. Such differences, including both bias and variance about the bias, are largest over parts of the Southern Ocean, and over Asia, central Africa, and Antarctica. These bias and variance differences between the NCEP and ECMWF surface pressure fields change only slightly over the period of study. More importantly, though, such differences are substantially smaller than those found by previous studies for an earlier period (1993-1995), suggesting recent improvements in both analyses. The largest differences are found over high latitudes, particularly over Antarctica, and in the respective winter hemisphere. Much of the differences occur on rapid timescales, though with a significant portion at timescales longer than 1-2 months. The potential impact of such uncertainties on de-aliasing and interpreting sea level and gravity data from altimeter and GRACE missions is discussed. C1 [Salstein, David A.; Ponte, Rui M.; Cady-Pereira, Karen] Atmospher & Environm Res Inc, Lexington, MA 02421 USA. [Salstein, David A.] Univ Maryland Baltimore Campus, GEST Program, NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Salstein, DA (reprint author), Atmospher & Environm Res Inc, 131 Hartwell Ave, Lexington, MA 02421 USA. EM salstein@aer.com OI Ponte, Rui/0000-0001-7206-6461 NR 16 TC 22 Z9 22 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 17 PY 2008 VL 113 IS D14 AR D14107 DI 10.1029/2007JD009531 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 328KV UT WOS:000257798200004 ER PT J AU Cho, HG Kushto, GP Andrews, L Bauschlicher, CW AF Cho, Han-Gook Kushto, Gary P. Andrews, Lester Bauschlicher, Charles W., Jr. TI Infrared spectra of HC C-MH and M-eta(2)-(C(2)H(2)) from reactions of laser-ablated group-4 transition-metal atoms with acetylene SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID ELECTRON-SPIN-RESONANCE; DENSITY-FUNCTIONAL CALCULATIONS; MATRIX-ISOLATION; ETHYLENE COMPLEXES; SOLID ARGON; GAS-PHASE; MOLECULES; HYDROGEN; VINYLIDENE; CHEMISTRY AB Reactions of laser-ablated group 4 transition-metal atoms with acetylene have been carried out. The ethynyl metal hydrides (HC C-MH) and corresponding pi complexes (M-eta(2)-(C(2)H(2))) are identified in the matrix infrared spectra. The observed M-H and C-M stretching absorptions show that oxidative C-H insertion readily occurs during codeposition and photolysis afterward. The absorptions frorn the pi complex, on the other hand, are relatively weak in the original deposition spectrum but increase dramatically in the process of annealing. The vinylidene complex, another plausible product, is not identified in this study. The observed spectra and DFT calculations both show that the back-donations from the group 4 metals to the antibonding pi* orbital Of C(2)H(2) are extensive such that the group 4 metals form unusually strong n complexes. Thus, it is the formation of two Ti-C bonds in the group 4 systems than leads to the stronger bonding than that in the group 8 systems. While bonds form, the Ti atom is weakly bound to C(2)H(2), and we still refer to it as a pi complex. Evidence of relativistic effects is also observed in frequency trends for the Ti, Zr, and Hf products. C1 [Andrews, Lester] Univ Incheon, Dept Chem, Inchon 402749, South Korea. Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA. NASA, Ames Res Ctr, Space Technol Div, Moffett Field, CA 94035 USA. RP Andrews, L (reprint author), Univ Incheon, Dept Chem, 177 Dohwa Dong, Inchon 402749, South Korea. EM lsa@virginia.edu NR 39 TC 30 Z9 30 U1 0 U2 8 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 17 PY 2008 VL 112 IS 28 BP 6295 EP 6304 DI 10.1021/jp801336d PG 10 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 324TN UT WOS:000257542400010 PM 18616219 ER PT J AU Mustard, JF Murchie, SL Pelkey, SM Ehlmann, BL Milliken, RE Grant, JA Bibring, JP Poulet, F Bishop, J Dobrea, EN Roach, L Seelos, F Arvidson, RE Wiseman, S Green, R Hash, C Humm, D Malaret, E McGovern, JA Seelos, K Clancy, T Clark, R Des Marais, D Izenberg, N Knudson, A Langevin, Y Martin, T McGuire, P Morris, R Robinson, M Roush, T Smith, M Swayze, G Taylor, H Titus, T Wolff, M AF Mustard, John F. Murchie, S. L. Pelkey, S. M. Ehlmann, B. L. Milliken, R. E. Grant, J. A. Bibring, J. -P. Poulet, F. Bishop, J. Dobrea, E. Noe Roach, L. Seelos, F. Arvidson, R. E. Wiseman, S. Green, R. Hash, C. Humm, D. Malaret, E. McGovern, J. A. Seelos, K. Clancy, T. Clark, R. Des Marais, D. Izenberg, N. Knudson, A. Langevin, Y. Martin, T. McGuire, P. Morris, R. Robinson, M. Roush, T. Smith, M. Swayze, G. Taylor, H. Titus, T. Wolff, M. TI Hydrated silicate minerals on mars observed by the Mars reconnaissance orbiter CRISM instrument SO NATURE LA English DT Article ID OLIVINE; DIVERSITY; REGION AB Phyllosilicates, a class of hydrous mineral first definitively identified on Mars by the OMEGA ( Observatoire pour la Mineralogie, L'Eau, les Glaces et l'Activitie') instrument(1,2), preserve a record of the interaction of water with rocks on Mars. Global mapping showed that phyllosilicates are widespread but are apparently restricted to ancient terrains and a relatively narrow range of mineralogy ( Fe/ Mg and Al smectite clays). This was interpreted to indicate that phyllosilicate formation occurred during the Noachian ( the earliest geological era of Mars), and that the conditions necessary for phyllosilicate formation ( moderate to high pH and high water activity(3)) were specific to surface environments during the earliest era of Mars's history(4). Here we report results from the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM)(5) of phyllosilicate- rich regions. We expand the diversity of phyllosilicate mineralogy with the identification of kaolinite, chlorite and illite or muscovite, and a new class of hydrated silicate ( hydrated silica). We observe diverse Fe/ Mg-OH phyllosilicates and find that smectites such as nontronite and saponite are the most common, but chlorites are also present in some locations. Stratigraphic relationships in the Nili Fossae region show olivine- rich materials overlying phyllosilicate- bearing units, indicating the cessation of aqueous alteration before emplacement of the olivine- bearing unit. Hundreds of detections of Fe/ Mg phyllosilicate in rims, ejecta and central peaks of craters in the southern highland Noachian cratered terrain indicate excavation of altered crust from depth. We also find phyllosilicate in sedimentary deposits clearly laid by water. These results point to a rich diversity of Noachian environments conducive to habitability. C1 [Mustard, John F.; Pelkey, S. M.; Ehlmann, B. L.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Murchie, S. L.; Seelos, F.; Humm, D.; McGovern, J. A.; Seelos, K.; Izenberg, N.; Taylor, H.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Milliken, R. E.; Dobrea, E. Noe; Green, R.; Martin, T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Grant, J. A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, Washington, DC 20560 USA. [Bibring, J. -P.; Poulet, F.; Langevin, Y.] Ctr Univ Paris Sud, Inst Astrophys Spatiale, F-91405 Orsay, France. [Bishop, J.; Des Marais, D.; Roush, T.] Ames Res Ctr, Natl Aeronaut & Space Adm, Mountain View, CA 94043 USA. [Arvidson, R. E.; Wiseman, S.; Knudson, A.; McGuire, P.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Hash, C.; Malaret, E.] Appl Coherent Technol, Herndon, VA 22070 USA. [Clancy, T.; Swayze, G.; Wolff, M.] Space Sci Inst, Boulder, CO 80301 USA. [Clark, R.] US Geol Survey, Denver Fed Ctr, Denver, CO 80225 USA. [Morris, R.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Robinson, M.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Smith, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Titus, T.] US Geol Survey, Flagstaff, AZ 86001 USA. RP Mustard, JF (reprint author), Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. EM john_mustard@brown.edu RI Smith, Michael/C-8875-2012; McGuire, Patrick/D-2962-2013; Murchie, Scott/E-8030-2015; Izenberg, Noam/F-3952-2015; Seelos, Kimberly/F-4647-2015; Humm, David/B-8825-2016; Seelos, Frank/C-7875-2016 OI McGuire, Patrick/0000-0001-6592-4966; Murchie, Scott/0000-0002-1616-8751; Izenberg, Noam/0000-0003-1629-6478; Seelos, Kimberly/0000-0001-7236-0580; Humm, David/0000-0003-1520-261X; Seelos, Frank/0000-0001-9721-941X NR 31 TC 356 Z9 359 U1 14 U2 85 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD JUL 17 PY 2008 VL 454 IS 7202 BP 305 EP 309 DI 10.1038/nature07097 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 326ND UT WOS:000257665300032 PM 18633411 ER PT J AU Engebretson, MJ Posch, JL Westerman, AM Otto, NJ Slavin, JA Le, G Strangeway, RJ Lessard, MR AF Engebretson, M. J. Posch, J. L. Westerman, A. M. Otto, N. J. Slavin, J. A. Le, G. Strangeway, R. J. Lessard, M. R. TI Temporal and spatial characteristics of Pc1 waves observed by ST5 SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ION-CYCLOTRON WAVES; HYDROMAGNETIC EMISSIONS; MAGNETIC PULSATIONS; GEOMAGNETIC STORMS; DUCT PROPAGATION; UPPER IONOSPHERE; HIGH-LATITUDES; MAGNETOSPHERE; DISTRIBUTIONS; REGION AB We present the results of a study of Pc1 waves (0.2-5 Hz) recorded by the three spacecraft of NASA's Space Technology 5 (ST5) mission, which operated in a dawn-dusk, 300 x 4500 km Sun-synchronous orbit in a "string-of-pearls'' configuration from 26 March through 23 June 2006. Regions with Pc1 wave activity are not only localized to rather narrow L shells but can appear and disappear on the time scales of similar to 10 s to 10 min as examined by ST5. Only half of the 48 identified events were observed by all three spacecraft, and five events were observed by only one spacecraft. Only seven events were observed below L = 4, and only one was observed below L = 3.6, consistent with the relatively quiet geomagnetic conditions during this interval. The temporal occurrence distribution of Pc1 events was similar to that recorded at Halley, Antarctica (L = 4.56), during this same interval in that the number and intensity of events increased during magnetospheric compressions and during the recovery phase of magnetic storms, but they were reduced or absent during main phase and early recovery phase. This agreement suggests that if Pc1 events occur during main phase, their nearly universal absence in ground records cannot be ascribed to ionospheric screening effects or obscuration by irregular ULF noise generated in the ionosphere. These findings also suggest that although electromagnetic ion cyclotron waves might theoretically cause rapid depletion of radiation belt electrons during the main phase of storms, such waves cannot be assumed to occur during the main phase of all storms. C1 [Engebretson, M. J.; Posch, J. L.; Westerman, A. M.; Otto, N. J.] Augsburg Coll, Dept Phys, Minneapolis, MN 55454 USA. [Le, G.] NASA, Space Weather Lab, Heliophys Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lessard, M. R.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Lessard, M. R.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [Slavin, J. A.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Strangeway, R. J.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. RP Engebretson, MJ (reprint author), Augsburg Coll, Dept Phys, 2211 Riverside Ave, Minneapolis, MN 55454 USA. EM engebret@augsburg.edu RI Le, Guan/C-9524-2012; Slavin, James/H-3170-2012 OI Le, Guan/0000-0002-9504-5214; Slavin, James/0000-0002-9206-724X NR 27 TC 24 Z9 24 U1 0 U2 4 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 16 PY 2008 VL 113 IS A7 AR A07206 DI 10.1029/2008JA013145 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 328MA UT WOS:000257801300003 ER PT J AU Matsumoto, K Hanada, H Namiki, N Iwata, T Goossens, S Tsuruta, S Kawano, N Rowlands, DD AF Matsumoto, Koji Hanada, Hideo Namiki, Noriyuki Iwata, Takahiro Goossens, Sander Tsuruta, Seiitsu Kawano, Nobuyuki Rowlands, David D. TI A simulation study for anticipated accuracy of lunar gravity field model by SELENE tracking data SO ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 9th ILEWG Conference on the Exploration and Utilisation of the Moon (ICEUM9) CY JUL 23-27, 2006 CL Sorrento, ITALY SP Int Lunar Explorat WG DE lunar gravity field recovery; SELENE; 4-way Doppler measurement; differential VLBI ID PROSPECTOR; VLBI AB Results of numerical simulations are presented to examine the global gravity field recovery capability of the Japanese lunar exploration project SELENE (SELenological and ENgineering Explorer) which will be launched in 2007. New characteristics of the SELENE lunar gravimetry include 4-way satellite-to-satellite Doppler tracking of main orbiter and differential VLBI tracking of two small free-flier satellites. It is shown that the proposed satellite constellation will provide the first truly global satellite tracking data coverage. The expected results from these data are; (1) drastic reduction in far-side gravity error, (2) estimation of many gravity coefficients by the observation, not by a priori information, and (3) one order of magnitude improvement over existing gravity models for low-degree field. (C) 2007 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Matsumoto, Koji; Hanada, Hideo; Goossens, Sander; Tsuruta, Seiitsu; Kawano, Nobuyuki] Natl Astron Observ Japan, RISE Project Off, Mizusawa, Oshu 0230861, Japan. [Iwata, Takahiro] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Kanagawa 2298510, Japan. [Namiki, Noriyuki] Kyushu Univ, Fukuoka 8128581, Japan. [Rowlands, David D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Matsumoto, K (reprint author), Natl Astron Observ Japan, RISE Project Off, 2-12 Hoshigaoka, Mizusawa, Oshu 0230861, Japan. EM matumoto@miz.nao.ac.jp RI Rowlands, David/D-2751-2012; Goossens, Sander/K-2526-2015 OI Goossens, Sander/0000-0002-7707-1128 NR 15 TC 14 Z9 16 U1 0 U2 1 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PD JUL 15 PY 2008 VL 42 IS 2 BP 331 EP 336 DI 10.1016/j.asr.2007.03.066 PG 6 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 324NZ UT WOS:000257526600020 ER PT J AU Kaneko, H Bey, KS Lenbury, Y Toghaw, P AF Kaneko, Hideaki Bey, Kim S. Lenbury, Yongwimon Toghaw, Puntip TI Numerical experiments using hierarchical finite element method for nonlinear heat conduction in plates SO APPLIED MATHEMATICS AND COMPUTATION LA English DT Article DE discontinuous Galerkin method; nonlinear parabolic equations ID DIMENSIONAL REDUCTION METHOD; BOUNDARY-VALUE-PROBLEMS; PARABOLIC PROBLEMS AB In this paper, we consider a nonlinear hierarchical finite element method for heat conduction problems over two-or three- dimensional plates. Problems considered are nonlinear because the heat conductivity parameter depends upon the temperature itself. This paper explores a new technique recently proposed by the first author which transforms a nonlinear parabolic problem to a linear problem at the discrete level. We present several numerical examples which demonstrate the efficiency of the current technique. (c) 2008 Published by Elsevier Inc. C1 [Kaneko, Hideaki] Old Dominion Univ, Dept Math & Stat, Norfolk, VA 23529 USA. [Bey, Kim S.] NASA, Langley Res Ctr, Thermal Struct Branch, Struct Div, Hampton, VA 23681 USA. [Lenbury, Yongwimon; Toghaw, Puntip] Mahidol Univ, Dept Math, Bangkok 10700, Thailand. RP Kaneko, H (reprint author), Old Dominion Univ, Dept Math & Stat, Norfolk, VA 23529 USA. EM hkaneko@odu.edu NR 16 TC 1 Z9 1 U1 0 U2 0 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0096-3003 J9 APPL MATH COMPUT JI Appl. Math. Comput. PD JUL 15 PY 2008 VL 201 IS 1-2 BP 414 EP 430 DI 10.1016/j.amc.2007.12.062 PG 17 WC Mathematics, Applied SC Mathematics GA 312HQ UT WOS:000256660400040 ER PT J AU Lohrenz, SE Redalje, DG Cai, WJ Acker, J Dagg, M AF Lohrenz, Steven E. Redalje, Donald G. Cai, Wei-Jun Acker, James Dagg, Michael TI A retrospective analysis of nutrients and phytoplankton productivity in the Mississippi River plume SO CONTINENTAL SHELF RESEARCH LA English DT Article; Proceedings Paper CT Symposium on Coastal Ecosystem Responses to Changing Nutrient Inputs from Large Temperate and Sub-Tropical Rivers CY MAY 29-JUN 01, 2005 CL Xiamen Univ China, Fujian, PEOPLES R CHINA HO Xiamen Univ China DE Mississippi River; nutrients Gulf of Mexico; primary production; nutrient limitation; SeaWiFS; chlorophyll ID GULF-OF-MEXICO; CONTINENTAL-SHELF; COASTAL WATERS; LOUISIANA SHELF; SURFACE WATERS; ORGANIC-CARBON; WIND STRESS; HYPOXIA; NITROGEN; BASIN AB Long-term patterns in riverine nutrient flux in the lower Mississippi River were examined in relationship to spatial and temporal patterns in surface nutrient concentrations, chlorophyll, and primary productivity in the outflow region in the northern Gulf of Mexico. A retrospective analysis of dissolved inorganic nutrient fluxes based on USGS water quality data and US Army Corps of Engineers discharge data from the 1950s to mid-2004 showed an increase in river-borne dissolved inorganic nitrogen (DIN) flux after 1967. Flux of DIN peaked in the early 1980s and has since fluctuated and shown a general decreasing trend since the early 1990s. Records for total phosphorus (total P) fluxes beginning in mid-1974 exhibited a variable but slight increasing trend up to 2004. The increase in fluxes during the 1970s and into the 1980s can be attributed to increases in both nutrient concentrations and river discharge. DIN concentrations since the 1980s have shown a decreasing trend. Total P concentrations exhibited large fluctuations, with no consistent long-term trend. Dissolved organic nitrogen (DON) concentrations and orthophosphate (Ortho P) peaked in the 1980s, declined relative to DIN and remained relatively low. DIN:Ortho P ratios were consistently well above the Redfield N:P ratio of 16:1. DIN:Total P ratios were variable and lower, fluctuating around the Redfield 16:1 value. Both DIN:Ortho P and DIN:Total P ratios were weakly, but significantly, correlated with river discharge and fluctuations were largely a reflection of higher DIN concentrations during high-discharge events. DIN:Ortho P ratios in surface waters of the outflow region adjacent to the birdfoot delta were higher in spring, consistent with seasonal variation in riverine DIN:Ortho P ratios. The seasonal signal diminished with increasing distance to the west of the delta, indicating a selective removal of DIN or source of Ortho P along the shelf. DIN fluxes and SeaWiFS satellite-derived chlorophyll showed seasonally elevated values during the first half of the year followed by generally lower values in late summer and fall. This seasonal signal diminished from east to west. The observed relationship between DIN flux and chlorophyll was consistent with ship-based observations of a linkage between riverine nutrient inputs and productivity. Long-term trends in river discharge were correlated with the Multivariate ENSO (El Nino Southern Oscillation) Index (MEI) (r = -0.281, p < 0.0001), evidence that river discharge was influenced by global climatic trends. C 2008 Elsevier Ltd. All rights reserved. C1 [Lohrenz, Steven E.; Redalje, Donald G.] Univ So Mississippi, Dept Marine Sci, Stennis Space Ctr, MS 39529 USA. [Cai, Wei-Jun] Univ Georgia, Dept Marine Sci, Athens, GA 30602 USA. [Acker, James] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dagg, Michael] Louisiana Univ Marine Consortium, Chauvin, LA 70344 USA. RP Lohrenz, SE (reprint author), Univ So Mississippi, Dept Marine Sci, Stennis Space Ctr, MS 39529 USA. EM Steven.Lohrenz@usm.edu; wcai@uga.edu; jim.acker@gsfc.nasa.gov; mdagg@lumcon.edu RI Cai, Wei-Jun/C-1361-2013; OI Cai, Wei-Jun/0000-0003-3606-8325; Lohrenz, Steven/0000-0003-3811-2975 NR 62 TC 53 Z9 54 U1 5 U2 24 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 JUL 15 PY 2008 VL 28 IS 12 BP 1466 EP 1475 DI 10.1016/j.csr.2007.06.019 PG 10 WC Oceanography SC Oceanography GA 325WU UT WOS:000257620200008 ER PT J AU D'Antoni, HL Rothschild, LJ Skiles, JW AF D'Antoni, Hector L. Rothschild, Lynn J. Skiles, J. W. TI Reply to comment by Stephan D. Flint et al. on "Extreme environments in the forests of Ushuaia, Argentina'' SO GEOPHYSICAL RESEARCH LETTERS LA English DT Editorial Material C1 [D'Antoni, Hector L.; Rothschild, Lynn J.; Skiles, J. W.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP D'Antoni, HL (reprint author), NASA, Ames Res Ctr, MS 239-20, Moffett Field, CA 94035 USA. EM hector.l.dantoni@nasa.gov; lynn.j.rothschild@nasa.gov; joseph.w.skiles@nasa.gov NR 5 TC 0 Z9 0 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 15 PY 2008 VL 35 IS 13 AR L13711 DI 10.1029/2008GL033836 PG 3 WC Geosciences, Multidisciplinary SC Geology GA 328JW UT WOS:000257795700002 ER PT J AU Hulley, GC Hook, SJ Baldridge, AM AF Hulley, G. C. Hook, S. J. Baldridge, A. M. TI ASTER land surface emissivity database of California and Nevada SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB Land surface temperature and emissivity (LST&E) are essential parameters for a wide range of studies undertaken at a variety of spatial scales. LST&E products are generated by a number of spaceborne sensors such as ASTER, MODIS, and AIRS at varying spatial, spectral and temporal resolutions. We have developed an approach for producing gridded, mean, seasonal ASTER LST&E Datasets at a spatial resolution of 100 m at nadir. This paper shows a mean wintertime and summertime emissivity dataset for California and Nevada, USA using all available data since mission launch ( 2000). Comparison of the two seasonal datasets indicates the greatest variability occurs in areas affected by snow such as the Sierra Nevada Mountains, and in agricultural regions. Comparisons of the new emissivity dataset with laboratory measurements of geologic samples show emissivity differences of less than 0.5%, while 1-3% differences were found for water and vegetation using spectra from the MODIS UCSB library. C1 [Hulley, G. C.; Hook, S. J.; Baldridge, A. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Hulley, GC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM glynn.hulley@jpl.nasa.gov NR 10 TC 25 Z9 25 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 JUL 15 PY 2008 VL 35 IS 13 AR L13401 DI 10.1029/2008GL034507 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 328JW UT WOS:000257795700006 ER PT J AU Smith, WL Minnis, P Finney, H Palikonda, R Khaiyer, MM AF Smith, William L., Jr. Minnis, Patrick Finney, Heather Palikonda, Rabindra Khaiyer, Mandana M. TI An evaluation of operational GOES-derived single-layer cloud top heights with ARSCL data over the ARM Southern Great Plains Site SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID GOES SOUNDER DATA; LIDAR DATA; SATELLITE; RADAR; FIRE; RADIATION; SHEBA; CYCLE AB Cloud top heights retrieved from Geostationary Operational Environmental Satellite (GOES) data are evaluated using comparisons to 5 years of surface-based cloud radar and lidar data taken at the Atmospheric Radiation Measurement (ARM) program's site near Lamont, Oklahoma. Separate daytime and nighttime algorithms developed at NASA Langley Research Center (LaRC) applied to GOES imager data and an operational CO(2)-slicing technique applied to GOES sounder data are tested. Comparisons between the daytime, nighttime and CO(2)-slicing cloud top heights and the surface retrievals yield mean differences of -0.84 +/- 1.48 km, -0.56 +/- 1.31 km, and -1.30 +/- 2.30 km, respectively, for all clouds. The errors generally increase with increasing cloud altitude and decreasing optical thickness. These results, which highlight some of the challenges associated with passive satellite cloud height retrievals, are being used to guide development of a blended LaRC/CO(2)-slicing cloud top height product with accuracies suitable for assimilation into weather forecast models. C1 [Smith, William L., Jr.; Minnis, Patrick] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. [Finney, Heather] Hastings Coll Law, Dept Phys, Hastings, NE 68901 USA. [Palikonda, Rabindra; Khaiyer, Mandana M.] SSAI, Hampton, VA 23666 USA. RP Smith, WL (reprint author), NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. EM william.l.smith@nasa.gov RI Minnis, Patrick/G-1902-2010 OI Minnis, Patrick/0000-0002-4733-6148 NR 24 TC 18 Z9 18 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 15 PY 2008 VL 35 IS 13 AR L13820 DI 10.1029/2008GL034275 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 328JW UT WOS:000257795700004 ER PT J AU Akturk, A Goldsman, N Aslam, S Sigwarth, J Herrero, F AF Akturk, Akin Goldsman, Neil Aslam, Shahid Sigwarth, John Herrero, Fred TI Comparison of 4H-SiC impact ionization models using experiments and self-consistent simulations SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID UV AVALANCHE PHOTODIODES; 4H AB We report comparisons of measured photocurrent versus voltage curves of avalanche photodiodes (APDs) with those calculated using different 4H-SiC hole and electron impact ionization coefficients. As the published impact ionization coefficients result in ionization rates that differ greatly in magnitude, the predicted breakdown voltages using these models vary by many volts. To this end, we investigate the breakdown voltage prediction capability of three prevailing impact ionization models in conjunction with several experiments. To obtain APD performance numerically, we developed a device simulator, which shows that the inclusion of proper electric field-dependent impact ionization rates can accurately predict a variety of measured current-voltage curves, breakdown voltages, and current multiplication rates. (c) 2008 American Institute of Physics. C1 [Akturk, Akin; Goldsman, Neil] Univ Maryland, College Pk, MD 20742 USA. [Akturk, Akin; Goldsman, Neil] CoolCAD Elect, Takoma Pk, MD 20912 USA. [Aslam, Shahid; Sigwarth, John; Herrero, Fred] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Akturk, A (reprint author), Univ Maryland, College Pk, MD 20742 USA. EM akturka@umd.edu RI Aslam, Shahid/D-1099-2012 NR 14 TC 5 Z9 5 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 0021-8979 J9 J APPL PHYS JI J. Appl. Phys. PD JUL 15 PY 2008 VL 104 IS 2 AR 026101 DI 10.1063/1.2958320 PG 3 WC Physics, Applied SC Physics GA 333TH UT WOS:000258174800140 ER PT J AU Golombek, MP Huertas, A Marlow, J McGrane, B Klein, C Martinez, M Arvidson, RE Heet, T Barry, L Seelos, K Adams, D Li, W Matijevic, JR Parker, T Sizemore, HG Mellon, M McEwen, AS Tamppari, LK Cheng, Y AF Golombek, M. P. Huertas, A. Marlow, J. McGrane, B. Klein, C. Martinez, M. Arvidson, R. E. Heet, T. Barry, L. Seelos, K. Adams, D. Li, W. Matijevic, J. R. Parker, T. Sizemore, H. G. Mellon, M. McEwen, A. S. Tamppari, L. K. Cheng, Y. TI Size-frequency distributions of rocks on the northern plains of Mars with special reference to Phoenix landing surfaces SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID SITE PREDICTIONS; BRITTLE SOLIDS; FRAGMENT SIZE; WIND EROSION; FRACTURE AB The size-frequency distributions of rocks > 1.5 m diameter fully resolvable in High Resolution Imaging Science Experiment (HiRISE) images of the northern plains follow exponential models developed from lander measurements of smaller rocks and are continuous with rock distributions measured at the landing sites. Dark pixels at the resolution limit of Mars Orbiter Camera thought to be boulders are shown to be mostly dark shadows of clustered smaller rocks in HiRISE images. An automated rock detector algorithm that fits ellipses to shadows and cylinders to the rocks, accurately measured (within 1-2 pixels) rock diameter and height (by comparison to spacecraft of known size) of similar to 10 million rocks over > 1500 km(2) of the northern plains. Rock distributions in these counts parallel models for cumulative fractional area covered by 30-90% rocks in dense rock fields around craters, 10-30% rock coverage in less dense rock fields, and 0-10% rock coverage in background terrain away from craters. Above similar to 1.5 m diameter, HiRISE resolves the same population of rocks seen in lander images, and thus size- frequency distributions can be extrapolated along model curves to estimate the number of rocks at smaller diameters. Extrapolating sparse rock distributions in the Phoenix landing ellipse indicate < 1% chance of encountering a potentially hazardous rock during landing or that could impede the opening of the solar arrays. Extrapolations further suggest rocks large enough to depress the ground ice table and small enough to be picked up or pushed by the robotic arm should be present within reach for study after landing. C1 [Golombek, M. P.; Huertas, A.; Martinez, M.; Adams, D.; Parker, T.; Tamppari, L. K.; Cheng, Y.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Marlow, J.; Arvidson, R. E.; Heet, T.; Barry, L.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Klein, C.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Li, W.] CALTECH, Dept Computat & Neural Syst, Pasadena, CA 91125 USA. [Martinez, M.] Univ Washington, Dept Aeronaut & Astronaut, Seattle, WA 98195 USA. [McEwen, A. S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [McGrane, B.] Occidental Coll, Dept Geol, Los Angeles, CA 90041 USA. [Sizemore, H. G.; Mellon, M.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. [Seelos, K.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Golombek, MP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mgolombek@jpl.nasa.gov RI Seelos, Kimberly/F-4647-2015; Mellon, Michael/C-3456-2016 OI Seelos, Kimberly/0000-0001-7236-0580; NR 53 TC 30 Z9 30 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUL 15 PY 2008 VL 113 AR E00A09 DI 10.1029/2007JE003065 PG 32 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 328LT UT WOS:000257800600003 ER PT J AU Hall, FG Hilker, T Coops, NC Lyapustin, A Huemmrich, KF Middleton, E Margolis, H Drolet, G Black, TA AF Hall, Forrest G. Hilker, Thomas Coops, Nicholas C. Lyapustin, Alexei Huemmrich, Karl F. Middleton, Elizabeth Margolis, Hank Drolet, Guillaume Black, T. Andrew TI Multi-angle remote sensing of forest light use efficiency by observing PRI variation with canopy shadow fraction SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE remote sensing; photochemical reflectance index; light use efficiency; forest; PRI; LUE; multi-angle; shadow fraction ID PHOTOCHEMICAL REFLECTANCE INDEX; RADIATION-USE-EFFICIENCY; CARBON-DIOXIDE FLUXES; LEAF PIGMENT CONTENT; DOUGLAS-FIR FOREST; BIDIRECTIONAL REFLECTANCE; SPECTRAL REFLECTANCE; BOREAL FOREST; CHLOROPHYLL FLUORESCENCE; SUNFLOWER LEAVES AB We show that observed co-variations at sub-hourly time scales between the photochemical reflectance index (PRI) and canopy light use efficiency (LUE) over a Douglas-fir forest result directly from sub-hourly leaf reflectance changes in a 531 mm spectral window roughly 50 nm wide. We conclude then, that over a forest stand we are observing the direct effects of photosynthetic down-regulation on leaf-level reflectance at 531 nm. Key to our conclusion is our ability to simultaneously measure the LUE and reflectance of the Douglas-fir stand as a function of shadow fraction from the "hot spot" to the "dark spot" and a new finding herein, based on radiative transfer theory, that the magnitude of a normalized reflectance difference index (NDRI) such as PRI can vary with shadow fraction only in case the reflectance of the shaded and sunlit leaves differ in at least one of the NDRI bands. Our spectrometer measurements over a nearly 6 month period show that at a forest stand scale, only two NDRIs (both containing a band near 570 nm) vary with shadow fraction and are correlated with LUE: an NDRI with a band centered at 531 nm roughly 50 nm wide, and another near 705 nm. Therefore, we are able to conclude that only these two bands' reflectance differ between the sunlit and the shaded elements of the canopy. Their reflectance changes on time scales of a few minutes or less. Our observations also show that the reflectance changes at 531 nm are more highly correlated with variations in canopy light use efficiency when only sunlit canopy elements are viewed (the hot spot), than when only shaded elements (the dark spot) are viewed. Taken together then, these results demonstrate that the observed sub-hourly changes in foliage reflectance at 531 nm and 705 turn can only result from corresponding variations in photosynthetic rates. The importance of our results are as follows: (1) We show that variations in PRI with LUE are a direct result of rapid changes in foliage reflectance at 531 nm resulting from photosynthetic down-regulation, and can be observed at forest scales. (2) Our findings also suggest a new sensor and methodology for the direct retrieval from space of changes in forest LUE by measuring PRI as a function of shadow fraction using a multi-angle spectrometer simultaneously retrieving both shadow fraction and PRI. (c) 2008 Elsevier Inc. All rights reserved. C1 [Hall, Forrest G.; Huemmrich, Karl F.] Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore Cty Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hilker, Thomas; Coops, Nicholas C.] Univ British Columbia, Fac Forest Resource Management, Vancouver, BC V6T 1Z4, Canada. [Lyapustin, Alexei] GSFC, Goddard Earth Sci & Technol, Greenbelt, MD 20771 USA. [Middleton, Elizabeth] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Margolis, Hank; Drolet, Guillaume] Univ Laval, Fac Foresterie & Geomat, Ste Foy, PQ G1K 7P4, Canada. [Black, T. Andrew] Univ British Columbia, Fac Land & Food Syst, Vancouver, BC V6T 1Z4, Canada. RP Hall, FG (reprint author), Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore Cty Goddard Space Flight Ctr, Code 614-4, Greenbelt, MD 20771 USA. EM fghall@ltpmail.gsfc.nasa.gov RI 黄, 建荣/B-8070-2011; Coops, Nicholas/J-1543-2012; Lyapustin, Alexei/H-9924-2014 OI Coops, Nicholas/0000-0002-0151-9037; Lyapustin, Alexei/0000-0003-1105-5739 NR 66 TC 95 Z9 98 U1 5 U2 36 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 15 PY 2008 VL 112 IS 7 BP 3201 EP 3211 DI 10.1016/j.rse.2008.03.015 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 325PJ UT WOS:000257600500001 ER PT J AU de Asis, ED Li, Y Ohta, R Austin, A Leung, J Nguyen, CV AF de Asis, Edward D., Jr. Li, You Ohta, Riichiro Austin, Alex Leung, Joseph Nguyen, Cattien V. TI Length dependent behavior of a carbon nanotube interacting at liquid-air interface SO APPLIED PHYSICS LETTERS LA English DT Article ID SCANNING PROBE; BIOLOGICAL-SYSTEMS; FORCE MICROSCOPY; RESOLUTION; TIPS AB We report the irreversible structural failure of individual multiwalled carbon nanotube (MWNT) tips after water submersion. We used 11 individual MWNTs with varying geometries and showed length dependent MWNT failure with scanning electron microscopy. Shorter MWNTs are more likely to survive penetration of the water-air interface. We observed the bending of MWNT probes on the water surface using optical microscopy. Surface tension force acting on MWNTs at the water-air interface was calculated. Compared to shorter MWNTs, the calculations suggest that longer MWNTs exert a smaller bending restoring force with respect to surface tension force, leading to MWNT bending until failure. (C) 2008 American Institute of Physics. C1 [de Asis, Edward D., Jr.; Li, You; Nguyen, Cattien V.] NASA, Ames Res Ctr, ELORET Corp, Moffett Field, CA 94035 USA. [de Asis, Edward D., Jr.] Santa Clara Univ, Dept Elect Engn, Santa Clara, CA 95053 USA. [Li, You; Austin, Alex] Stanford Univ, Stanford, CA 94305 USA. [Ohta, Riichiro] Univ Calif Santa Cruz, Univ Affiliated Res Ctr, Santa Cruz, CA 95064 USA. RP de Asis, ED (reprint author), NASA, Ames Res Ctr, ELORET Corp, M-S 229-1, Moffett Field, CA 94035 USA. EM cattien.v.nguyen@nasa.gov NR 21 TC 4 Z9 4 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 0003-6951 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD JUL 14 PY 2008 VL 93 IS 2 AR 023129 DI 10.1063/1.2953688 PG 3 WC Physics, Applied SC Physics GA 328KA UT WOS:000257796100106 ER PT J AU Liu, J Angelopoulos, V Sibeck, D Phan, T Pu, ZY McFadden, J Glassmeier, KH Auster, HU AF Liu, J. Angelopoulos, V. Sibeck, D. Phan, T. Pu, Z. Y. McFadden, J. Glassmeier, K. H. Auster, H. U. TI THEMIS observations of the dayside traveling compression region and flows surrounding flux transfer events SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID KELVIN-HELMHOLTZ INSTABILITY; CLUSTER OBSERVATIONS; SOLAR-WIND; MAGNETOPAUSE; MAGNETOSPHERE; RECONNECTION; WAVES; FIELD AB [1] We present multipoint observations of Flux Transfer Events (FTEs) by the THEMIS spacecraft in a string- ofpearls configuration, at the near- equatorial magnetopause. Common characteristics from a number of cases, examined at various local times, are exemplified here by a case study of FTE trains observed in the pre- noon sector, on Aug. 18, 2007. We show that the magneto- pause- normal flow velocity is consistently towards and away from the magnetopause on the inbound and outbound transit of the FTE, on all spacecraft sufficiently away from the magnetopause. The velocity just outside the FTE at the time of closest proximity to the FTE core is opposite to the FTE direction of motion even when the FTE moves in the same direction as the adjacent sheath. The total pressure inside and just outside the FTE is consistently larger than expected from pressure balance at a nominal ( unperturbed) magnetopause and therefore the result of local compression by the passing FTE. The multi- spacecraft observation enables the reconstruction of the Dayside Traveling Compression Region ( DTCR), whose result is consistent with previous theoretical results. Semi- periodic compressional velocity oscillations were observed and are likely driven by nearby occurrences of FTE trains, implying recurrent reconnection with a similar periodicity. Citation: Liu, J., V. Angelopoulos, D. Sibeck, T. Phan, Z. Y. Pu, J. McFadden, K. H. Glassmeier, and H. U. Auster ( 2008), THEMIS observations of the dayside traveling compression region and flows surrounding flux transfer events. C1 [Liu, J.; Angelopoulos, V.] Univ Calif Los Angeles, IGPP, ESS, Los Angeles, CA 90095 USA. [Phan, T.; McFadden, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Sibeck, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Pu, Z. Y.] Peking Univ, SESS, Beijing 100871, Peoples R China. [Glassmeier, K. H.; Auster, H. U.] TUBS, Inst Geophys & Extraterrestr Phys, D-38106 Braunschweig, Germany. RP Liu, J (reprint author), Univ Calif Los Angeles, IGPP, ESS, Los Angeles, CA 90095 USA. EM jliu@igpp.ucla.edu RI Sibeck, David/D-4424-2012; Liu, Jiang/B-3015-2014 OI Liu, Jiang/0000-0002-7489-9384 NR 28 TC 13 Z9 14 U1 2 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 12 PY 2008 VL 35 IS 17 AR L17S07 DI 10.1029/2008GL033673 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 327OW UT WOS:000257739400001 ER PT J AU Hilker, T Coops, NC Hall, FG Black, TA Chen, B Krishnan, P Wulder, MA Sellers, PJ Middleton, EM Huemmrich, KF AF Hilker, Thomas Coops, Nicholas C. Hall, Forrest G. Black, T. Andrew Chen, Baozhang Krishnan, Praveena Wulder, Michael A. Sellers, Piers J. Middleton, Elizabeth M. Huemmrich, Karl F. TI A modeling approach for upscaling gross ecosystem production to the landscape scale using remote sensing data SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article ID LIGHT-USE EFFICIENCY; PHOTOSYNTHETICALLY ACTIVE RADIATION; AIRBORNE LASER SCANNER; DOUGLAS-FIR FOREST; LEAF-AREA INDEX; PHOTOCHEMICAL REFLECTANCE INDEX; SURFACE PARAMETERIZATION SIB2; LAND-SURFACE; SOLAR-RADIATION; BIDIRECTIONAL REFLECTANCE AB Gross ecosystem production (GEP) can be estimated at the global scale and in a spatially continuous mode using models driven by remote sensing. Multiple studies have demonstrated the capability of high resolution optical remote sensing to accurately measure GEP at the leaf and stand level, but upscaling this relationship using satellite data remains challenging. Canopy structure is one of the complicating factors as it not only alters the strength of a measured signal depending on integrated leaf-angle-distribution and sun-observer geometry, but also drives the photosynthetic output and light-use-efficiency (e) of individual leaves. This study introduces a new approach for upscaling multiangular canopy level reflectance measurements to satellite scales which takes account of canopy structure effects by using Light Detection and Ranging (LiDAR). A tower-based spectro-radiometer was used to observe canopy reflectances over an annual period under different look and solar angles. This information was then used to extract sunlit and shaded spectral end-members corresponding to minimum and maximum values of canopy-epsilon over 8-d intervals using a bidirectional reflectance distribution model. Using three-dimensional information of the canopy structure obtained from LiDAR, the canopy light regime and leaf area was modeled over a 12 km(2) area and was combined with spectral end-members to derive high resolution maps of GEP. Comparison with eddy covariance data collected at the site shows that the spectrally driven model is able to accurately predict GEP (r(2) between 0.75 and 0.91, p < 0.05). C1 [Hilker, Thomas; Coops, Nicholas C.] Univ British Columbia, Fac Forest Resources Management, Vancouver, BC V6T 1Z4, Canada. [Black, T. Andrew; Chen, Baozhang] Univ British Columbia, Fac Land & Food Syst, Vancouver, BC V6T 1Z4, Canada. [Hall, Forrest G.] Univ Maryland, Joint Ctr Earth Syst Technol, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Huemmrich, Karl F.] Univ Maryland, Joint Ctr Earth Syst Technol, Catonsville, MD 21228 USA. [Krishnan, Praveena] Natl Ocean & Atmospher Adm, Atmospher Turbulence & Diffus Div, Oak Ridge, TN 37830 USA. [Middleton, Elizabeth M.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. [Sellers, Piers J.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Wulder, Michael A.] Nat Resources Canada, Canadian Forest Serv, Pacific Forestry Ctr, Victoria, BC V8Z 1M5, Canada. RP Hilker, T (reprint author), Univ British Columbia, Fac Forest Resources Management, 2424 Main Mall, Vancouver, BC V6T 1Z4, Canada. EM thilker@interchange.ubc.ca RI Krishnan, Praveena/F-8169-2010; Coops, Nicholas/J-1543-2012; Wulder, Michael/J-5597-2016 OI Coops, Nicholas/0000-0002-0151-9037; Wulder, Michael/0000-0002-6942-1896 NR 82 TC 25 Z9 25 U1 2 U2 24 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD JUL 12 PY 2008 VL 113 IS G3 AR G03006 DI 10.1029/2007JG000666 PG 15 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 327QQ UT WOS:000257744000002 ER PT J AU Ribeiro, NS Saatchi, SS Shugart, HH Washington-Allen, RA AF Ribeiro, Natasha S. Saatchi, Sassan S. Shugart, Herman H. Washington-Allen, Robert A. TI Aboveground biomass and Leaf Area Index (LAI) mapping for Niassa Reserve, northern Mozambique SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article ID WILDLIFE RESEARCH AREA; SAVANNA-WOODLANDS; AFRICAN SAVANNAS; MARA WOODLANDS; FOREST BIOMASS; FIRE; ELEPHANTS; ZIMBABWE; PRODUCTIVITY; VEGETATION AB Estimations of biomass are critical in miombo woodlands because they represent the primary source of goods and services for over 80% of the population in southern Africa. This study was carried out in Niassa Reserve, northern Mozambique. The main objectives were first to estimate woody biomass and Leaf Area Index (LAI) using remotely sensed data [RADARSAT (Cband, lambda = 5.7cm)] and Landsat ETM+ derived Normalized Difference Vegetation Index (NDVI) and Simple Ratio (SR) calibrated by field measurements and, second to determine, at both landscape and plot scales, the environmental controls (precipitation, woody cover density, fire and elephants) of biomass and LAI. A landcover map (72% overall accuracy) was derived from the June 2004 ETM+ mosaic. Field biomass and LAI were correlated with RADARSAT backscatter (r(biomass) = 0.65, r(LAI) = 0.57, p < 0.0001) from July 2004, NDVI (r(biomass) = 0.30, r(LAI) = 0.35; p < 0.0001) and SR (r(biomass) = 0.36, r(LAI) = 0.40, p < 0.0001). A jackknife stepwise regression technique was used to develop the best predictive models for biomass (biomass = -5.19 + 0.074 * radarsat + 1.56 * SR, r(2) = 0.55) and LAI (LAI = -0.66 + 0.01 * radarsat + 0.22 * SR, r(2) = 0.45). Biomass and LAI maps were produced with an estimated peak of 18 kg m(-2) and 2.80 m(2) m(-2), respectively. On the landscapescale, both biomass and LAI were strongly determined by mean annual precipitation (F = 13.91, p = 0.0002). On the plot spatial scale, woody biomass was significantly determined by fire frequency, and LAI by vegetation type. C1 [Ribeiro, Natasha S.; Shugart, Herman H.; Washington-Allen, Robert A.] Univ Virginia, Dept Environm Sci, Ctr Reg & Environm Studies, Charlottesville, VA 22904 USA. [Ribeiro, Natasha S.] Univ Eduardo Mondlane, Fac Agron & Engn Florestal, Maputo 258, Mozambique. [Saatchi, Sassan S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ribeiro, NS (reprint author), Univ Virginia, Dept Environm Sci, Ctr Reg & Environm Studies, Charlottesville, VA 22904 USA. EM joluci2000@yahoo.com RI Mitchard, Edward/C-6346-2009; Shugart, Herman/C-5156-2009 NR 55 TC 10 Z9 12 U1 1 U2 18 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD JUL 12 PY 2008 VL 113 IS G2 AR G02S02 DI 10.1029/2007JG000550 PG 12 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 327QN UT WOS:000257743700001 ER PT J AU Buzulukova, N Fok, MC Moore, TE Ober, DM AF Buzulukova, N. Fok, M. -C. Moore, T. E. Ober, D. M. TI Generation of plasmaspheric undulations SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID EVENT; MODEL AB We have modeled the plasmaspheric plume region using the Comprehensive Ring Current model (CRCM) and the Dynamical Global Core Plasma model (DGCPM), for an event that exhibited substantial undulations or ripples as observed by the IMAGE EUV imager during 17 April 2002. We drove the simulated electric field using the Weimer cross polar cap potential. We specified the magnetic field to vary in response to solar wind conditions according to the T96 model. As a control, we performed a run with a fixed magnetic field and a run with a low ring current pressure. The results show that particle injections into the inner magnetosphere and ring current-ionosphere-plasmasphere interaction are an essential part of the undulation response. We also conclude that the undulations are stronger in the case of magnetic field variations because associated induction electric field causes more pronounced injections. C1 [Buzulukova, N.; Fok, M. -C.; Moore, T. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Buzulukova, N.] Space Res Inst IKI, Moscow, Russia. [Ober, D. M.] USAF, Res Lab, Hanscom AFB, MA USA. RP Buzulukova, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM nbuzulukova@gmail.com RI Moore, Thomas/D-4675-2012; Fok, Mei-Ching/D-1626-2012 OI Moore, Thomas/0000-0002-3150-1137; NR 15 TC 5 Z9 5 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 11 PY 2008 VL 35 IS 13 AR L13105 DI 10.1029/2008GL034164 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 327OS UT WOS:000257739000004 ER PT J AU Fischer, AM Shindell, DT Winter, B Bourqui, MS Faluvegi, G Rozanov, E Schraner, M Bronnimann, S AF Fischer, A. M. Shindell, D. T. Winter, B. Bourqui, M. S. Faluvegi, G. Rozanov, E. Schraner, M. Broennimann, S. TI Stratospheric winter climate response to ENSO in three chemistry-climate models SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID EL-NINO; NORTHERN-HEMISPHERE; TEMPERATURE; SIMULATIONS AB Three different chemistry-climate models are compared with respect to their simulation of the stratospheric response to extreme cases of ENSO. Ensemble simulations of an unusually warm ENSO event (1940-1941) compared to a very cold event (1975-1976) reveal a weaker and warmer polar vortex in the Northern Hemisphere winter. This follows from anomalously propagating waves decelerating the zonal flow and strengthening the residual mean circulation. Models are in good agreement in simulating the observed (statistically reconstructed for the case 1941) flow in the lower stratosphere over the Pacific North American region, but less so over the North Atlantic European sector with insufficient reproduction of the wave structure. Modeled column ozone is reduced in the Tropics and increased on average in the northern extra tropics in accord with the general pattern seen in observations and in line with an intensification of the Brewer-Dobson circulation. C1 [Fischer, A. M.; Rozanov, E.; Schraner, M.; Broennimann, S.] ETH, Inst Atmospher & Climate Sci, CH-8092 Zurich, Switzerland. [Winter, B.; Bourqui, M. S.] McGill Univ, Dept Atmospher & Ocean Sci, Montreal, PQ H3A 2K6, Canada. [Shindell, D. T.; Faluvegi, G.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Fischer, AM (reprint author), ETH, Inst Atmospher & Climate Sci, CH-8092 Zurich, Switzerland. EM andreas.fischer@env.ethz.ch RI Bronnimann, Stefan/A-5737-2008; Rozanov, Eugene/A-9857-2012; Shindell, Drew/D-4636-2012; OI Rozanov, Eugene/0000-0003-0479-4488; Bronnimann, Stefan/0000-0001-9502-7991 NR 20 TC 15 Z9 16 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 11 PY 2008 VL 35 IS 13 AR L13819 DI 10.1029/2008GL034289 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 327OS UT WOS:000257739000006 ER PT J AU Antoine, D d'Ortenzio, F Hooker, SB Becu, G Gentili, B Tailliez, D Scott, AJ AF Antoine, David d'Ortenzio, Fabrizio Hooker, Stanford B. Becu, Guislain Gentili, Bernard Tailliez, Dominique Scott, Alec J. TI Assessment of uncertainty in the ocean reflectance determined by three satellite ocean color sensors (MERIS, SeaWiFS and MODIS-A) at an offshore site in the Mediterranean Sea (BOUSSOLE project) SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID ABOVE-WATER RADIOMETRY; IN-ORBIT CALIBRATION; ATMOSPHERIC CORRECTION; CASE-1 WATERS; MULTISENSOR APPROACH; VALIDATION; INSTRUMENT; IMAGERY; CHLOROPHYLL; MODEL AB The match-up of satellite-derived reflectances with in situ observations is crucial to evaluate their quality and temporal stability. To contribute to this effort, a project has been set up to collect a data set of in situ radiometric and bio-optical quantities, in support to satellite ocean color calibration and validation. The project has been named "BOUSSOLE'', and one of its key elements is a deep-sea optics mooring collecting data on a near-continuous basis since September 2003. This buoy is deployed in the deep clear waters of the northwestern Mediterranean Sea, and is visited on a monthly basis for servicing and acquisition of complementary data. The characteristics of the work area establish the site as a satisfactory location for validating satellite ocean color observations. A description of the data processing protocols is provided, followed by an analysis of the uncertainty of the buoy radiometry measurements. The results of a match-up analysis of the marine reflectances, diffuse attenuation coefficients, and chlorophyll concentrations for three major missions, i.e., MERIS, SeaWiFS, and MODIS-A, are then analyzed. They show poor performances for the bluest band (412 nm) of the three sensors, and performances within requirements at 443 and 490 nm for SeaWiFS and MODIS-A. These results suggest that a vicarious calibration should be introduced for the MERIS sensor. This analysis also demonstrates that a major effort is still required to improve atmospheric correction procedures whatever the mission. C1 [Antoine, David] CNRS, Lab Oceanog Villefranche, UMR 7093, F-06238 Villefranche Sur Mer, France. [Antoine, David; d'Ortenzio, Fabrizio; Gentili, Bernard; Tailliez, Dominique] Univ Paris, UPMC, Villefranche Sur Mer, France. [Hooker, Stanford B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Becu, Guislain] ACRI St SAS, Sophia Antipolis, France. RP Antoine, D (reprint author), CNRS, Lab Oceanog Villefranche, UMR 7093, BP 8, F-06238 Villefranche Sur Mer, France. EM antoine@obs-vlfr.fr RI Hooker, Stanford/E-2162-2012; Antoine, David/C-3817-2013 OI Antoine, David/0000-0002-9082-2395 NR 71 TC 100 Z9 101 U1 3 U2 21 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 11 PY 2008 VL 113 IS C7 AR C07013 DI 10.1029/2007JC004472 PG 22 WC Oceanography SC Oceanography GA 327RK UT WOS:000257746000001 ER PT J AU Coe, D Fuselier, E Benitez, N Broadhurst, T Frye, B Ford, H AF Coe, D. Fuselier, E. Benitez, N. Broadhurst, T. Frye, B. Ford, H. TI Lensperfect: Gravitational lens mass map reconstructions yielding exact reproduction of all multiple images SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies : clusters : general; gravitational lensing; methods : data analysis ID DARK-MATTER SUBSTRUCTURE; ADVANCED CAMERA; NONPARAMETRIC RECONSTRUCTION; ABELL-1689; GALAXIES; MODELS; HALOES; WEAK; DEGENERACIES; INVERSION AB We present a new approach to gravitational lens mass map reconstruction. Our mass map solutions perfectly reproduce the positions, fluxes, and shears of all multiple images, and each mass map accurately recovers the under-lying mass distribution to a resolution limited by the number of multiple images detected. We demonstrate our technique given a mock galaxy cluster similar to Abell 1689, which gravitationally lenses 19 mock background galaxies to produce 93 multiple images. We also explore cases in which as few as four multiple images are observed. Mass map solutions are never unique, and our method makes it possible to explore an extremely flexible range of physical ( and unphysical) solutions, all of which perfectly reproduce the data given. Each reconfiguration of the source galaxies produces a new mass map solution. An optimization routine is provided to find those source positions ( and redshifts, within uncertainties) that produce the "most physical'' mass map solution, according to a new figure of merit developed here. Our method imposes no assumptions about the slope of the radial profile or mass following light. However, unlike "nonparametric'' grid-based methods, the number of free parameters that we solve for is only as many as the number of observable constraints ( or slightly greater if fluxes are constrained). For each set of source positions and redshifts, mass map solutions are obtained "instantly'' via direct matrix inversion by smoothly interpolating the deflection field using a recently developed mathematical technique. Our LensPerfect software is straightforward and easy to use, and is publicly available on our Web site. C1 [Coe, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Coe, D.; Ford, H.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Coe, D.; Benitez, N.] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. [Fuselier, E.] US Mil Acad, Dept Math Sci, West Point, NY 10996 USA. [Benitez, N.] CSIC, Inst Matemat & Fis Fundamental, E-28006 Madrid, Spain. [Broadhurst, T.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Frye, B.] Dublin City Univ, Dept Phys Sci, Dublin 9, Ireland. RP Coe, D (reprint author), CALTECH, Jet Prop Lab, MS 169-327, Pasadena, CA 91109 USA. EM coe@caltech.edu OI Benitez, Narciso/0000-0002-0403-7455 NR 56 TC 32 Z9 32 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 JUL 10 PY 2008 VL 681 IS 2 BP 814 EP 830 DI 10.1086/588250 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 324JX UT WOS:000257516000007 ER PT J AU Markoff, S Nowak, M Young, A Marshall, HL Canizares, CR Peck, A Krips, M Petitpas, G Schodel, R Bower, GC Chandra, P Ray, A Muno, M Gallagher, S Hornstein, S Cheung, CC AF Markoff, Sera Nowak, Michael Young, Andrew Marshall, Herman L. Canizares, Claude R. Peck, Alison Krips, Melanie Petitpas, Glen Schoedel, Rainer Bower, Geoffrey C. Chandra, Poonam Ray, Alak Muno, Michael Gallagher, Sarah Hornstein, Seth Cheung, Chi C. TI Results from an extensive simultaneous broadband campaign on the underluminous active nucleus M81*: Further evidence for mass-scaling accretion in black holes SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies : active; galaxies : individual (M81); radiation mechanisms : nonthermal ID SAGITTARIUS-A-ASTERISK; ADVECTION-DOMINATED ACCRETION; X-RAY BINARIES; LONG-TERM VARIABILITY; LOW-LUMINOSITY AGN; SGR-A; CIRCULAR-POLARIZATION; GALACTIC NUCLEUS; LINEAR-POLARIZATION; FUNDAMENTAL PLANE AB We present the results of a broadband simultaneous campaign on the nearby low-luminosity active galactic nucleus M81*. From 2005 February through August, we observed M81* five times using the Chandra X-Ray Observatory with the HETGS, complemented by ground-based observations with the Giant Meterwave Radio Telescope, the Very Large Array and Very Large Baseline Array, the Plateau de Bure Interferometer at IRAM, the Submillimeter Array, and Lick Observatory. We discuss how the resulting spectra vary over short and longer timescales compared to previous results, especially in the X-rays where this is the first ever longer term campaign at spatial resolution high enough to nearly isolate the nucleus (17 pc). We compare the spectrum to our Galactic center weakly active nucleus Sgr A*, which has undergone similar campaigns, as well as to weakly accreting X-ray binaries in the context of outflow-dominated models. In agreement with recent results suggesting that the physics of weakly accreting black holes scales predictably with mass, we find that the exact same model that successfully describes hard-state X-ray binaries applies to M81*, with very similar physical parameters. C1 [Markoff, Sera] Univ Amsterdam, Sterrekundig Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Nowak, Michael; Young, Andrew; Marshall, Herman L.; Canizares, Claude R.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Peck, Alison; Krips, Melanie; Petitpas, Glen] Harvard Smithsonian Ctr Astrophys, Submillimeter Array Project, Hilo, HI 96720 USA. [Schoedel, Rainer] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. [Bower, Geoffrey C.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Chandra, Poonam] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Chandra, Poonam] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Ray, Alak] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. [Muno, Michael; Gallagher, Sarah; Hornstein, Seth] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. [Cheung, Chi C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Markoff, S (reprint author), Univ Amsterdam, Sterrekundig Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. EM sera@science.uva.nl; mnowak@space.mit.edu; ayoung@space.mit.edu; apeck@alma.cl; mkrips@cfa.harvard.edu; gpetitpas@cfa.harvard.edu; rainer@iaa.es; gbower@astro.berkeley.edu; pchandra@virginia.edu; akr@tifr.rcs.in; mmuno@astro.ucla.edu; sgall@astro.ucla.edu; seth@astro.ucla.edu; chi.c.cheung@nasa.gov RI Schoedel, Rainer/D-4751-2014 OI Schoedel, Rainer/0000-0001-5404-797X NR 79 TC 59 Z9 59 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2008 VL 681 IS 2 BP 905 EP 924 DI 10.1086/588718 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 324JX UT WOS:000257516000012 ER PT J AU Lehmer, BD Brandt, WN Alexander, DM Bell, EF Hornschemeier, AE McIntosh, DH Bauer, FE Gilli, R Mainieri, V Schneider, DP Silverman, JD Steffen, AT Tozzi, P Wolf, C AF Lehmer, B. D. Brandt, W. N. Alexander, D. M. Bell, E. F. Hornschemeier, A. E. McIntosh, D. H. Bauer, F. E. Gilli, R. Mainieri, V. Schneider, D. P. Silverman, J. D. Steffen, A. T. Tozzi, P. Wolf, C. TI Tracing the mass-dependent star formation history of late-type galaxies using X-ray emission: Results from the Chandra Deep Fields SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmology : observations; galaxies : active; galaxies : general; galaxies : spiral; stars : formation; surveys; X-rays : galaxies; X-rays : general ID LYMAN-BREAK GALAXIES; ACTIVE GALACTIC NUCLEI; GOODS-SOUTH FIELD; ULTRAVIOLET LUMINOSITY DENSITY; POINT-SOURCE CATALOGS; MULTIVARIATE STATISTICAL-ANALYSIS; COLOR-MAGNITUDE DISTRIBUTION; FORMATION RATE INDICATOR; XMM-NEWTON OBSERVATIONS; FRANCE REDSHIFT SURVEY AB We report on the X-ray evolution over the last approximate to 9 Gyr of cosmic history (i.e., since z = 1.4) of late-type galaxy populations in the Chandra Deep Field-North and Extended Chandra Deep Field-South (CDF-N and E-CDF-S, respectively; jointly CDFs) survey fields. Our late-type galaxy sample consists of 2568 galaxies, which were identified using rest-frame optical colors and HST morphologies. We utilized X-ray stacking analyses to investigate the X-ray emission from these galaxies, emphasizing the contributions from normal galaxies that are not dominated by active galactic nuclei (AGNs). Over this redshift range, we find significant increases (factors of approximate to 5-10) in the X-ray-to-optical mean luminosity ratio (L(X)/L(B)) and the X-ray-to-stellar mass mean ratio (L(X)/M(star)) for galaxy populations selected by L(B) and M(star), respectively. When analyzing galaxy samples selected via SFR, we find that the mean X-ray-to-SFR ratio (L(X)/SFR) is consistent with being constant over the entire redshift range for galaxies with SFR = 1-100 M(circle dot) yr(-1), thus demonstrating that X-ray emission can be used as a robust indicator of star formation activity out to z approximate to 1.4. We find that the star formation activity (as traced by X-ray luminosity) per unit stellar mass in a given redshift bin increases with decreasing stellar mass over the redshift range z = 0.2-1, which is consistent with previous studies of how star formation activity depends on stellar mass. Finally, we extend our X-ray analyses to Lyman break galaxies at z similar to 3 and estimate that L(X)/L(B) at z similar to 3 is similar to its value at z = 1.4. C1 [Lehmer, B. D.; Brandt, W. N.; Schneider, D. P.; Steffen, A. T.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Lehmer, B. D.; Alexander, D. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Bell, E. F.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Hornschemeier, A. E.] NASA, Lab Xray Astrophys, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [McIntosh, D. H.] Univ Massachusetts, Dept Astron, Amherst, MA 01007 USA. [Bauer, F. E.] Columbia Univ, Pupin Lab, Columbia Astrophys Lab, New York, NY 10027 USA. [Gilli, R.; Tozzi, P.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Mainieri, V.] European So Observ, D-85748 Garching, Germany. [Mainieri, V.; Silverman, J. D.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Silverman, J. D.] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland. [Wolf, C.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. RP Lehmer, BD (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. RI Brandt, William/N-2844-2015; OI Brandt, William/0000-0002-0167-2453; Alexander, David/0000-0002-5896-6313; Bell, Eric/0000-0002-5564-9873 NR 165 TC 61 Z9 61 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2008 VL 681 IS 2 BP 1163 EP 1182 DI 10.1086/588459 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 324JX UT WOS:000257516000032 ER PT J AU Abbott, B Abbott, R Adhikari, R Agresti, J Ajith, P Allen, B Amin, R Anderson, SB Anderson, WG Arain, M Araya, M Armandula, H Ashley, M Aston, S Aufmuth, P Aulbert, C Babak, S Ballmer, S Bantilan, H Barish, BC Barker, C Barker, D Barr, B Barriga, P Barton, MA Bayer, K Betzwieser, J Beyersdorf, PT Bhawal, B Bilenko, IA Billingsley, G Biswas, R Black, E Blackburn, K Blackburn, L Blair, D Bland, B Bogenstahl, J Bogue, L Bork, R Boschi, V Bose, S Brady, PR Braginsky, VB Brau, JE Brinkmann, M Brooks, A Brown, DA Bullington, A Bunkowski, A Buonanno, A Burmeister, O Busby, D Byer, RL Cadonati, L Cagnoli, G Camp, JB Cannizzo, J Cannon, K Cantley, CA Cao, J Cardenas, L Castaldi, G Cepeda, C Chalkley, E Charlton, P Chatterji, S Chelkowski, S Chen, Y Chiadini, F Christensen, N Clark, J Cochrane, P Cokelaer, T Coldwell, R Conte, R Cook, D Corbitt, T Coyne, D Creighton, JDE Croce, RP Crooks, DRM Cruise, AM Cumming, A Dalrymple, J D'Ambrosio, E Danzmann, K Davies, G Debra, D Degallaix, J Degree, M Demma, T Dergachev, V Desai, S DeSalvo, R Dhurandhar, S Diaz, M Dickson, J Di Credico, A Diederichs, G Dietz, A Doomes, EE Drever, RWP Dumas, JC Dupuis, RJ Dwyer, JG Ehrens, P Espinoza, E Etzel, T Evans, M Evans, T Fairhurst, S Fan, Y Fazi, D Fejer, MM Finn, LS Fiumara, V Fotopoulos, N Franzen, A Franzen, KY Freise, A Frey, R Fricke, T Fritschel, P Frolov, VV Fyffe, M Galdi, V Garofoli, J Gholami, I Giaime, JA Giampanis, S Giardina, KD Goda, K Goetz, E Goggin, LM Gonzalez, G Gossler, S Grant, A Gras, S Gray, C Gray, M Greeniialgii, J Gretarsson, AM Grosso, R Grote, H Grunewald, S Guenther, M Gustafson, R Hage, B Hammer, D Hanna, C Hanson, J Harms, J Harry, G Harstad, E Hayler, T Heefner, J Heng, IS Heptonstall, A Heurs, M Hewitson, M Hild, S Hirose, E Hoak, D Hosken, D Hough, J Hoyland, D Huttner, SH Ingram, D Innerhofer, E Ito, M Itoh, Y Ivanov, A Johnson, B Johnson, WW Jones, DI Jones, G Jones, R Ju, L Kalmus, P Kalogera, V Kasprzyk, D Katsavounidis, E Kawabe, K Kawamura, S Kawazoe, F Kells, W Keppel, DG Khalili, FY Kim, C King, P Kissel, JS Klimenko, S Kokeyama, K Kondrashov, V Kopparapu, RK Kozak, D Krishnan, B Kwee, P Lam, PK Landry, M Lantz, B Lazzarini, A Lei, M Leiner, J Leonhardt, V Leonor, I Libbrecht, K Lindquist, P Lockerbie, NA Longo, M Lormand, M Lubinski, M Luck, H Machenschalk, B MacInnis, M Mageswaran, M Mailand, K Malec, M Mandic, V Marano, S Marka, S Markowitz, J Maros, E Martin, I Marx, JN Mason, K Matone, L Matta, V Mavalvala, N McCarthy, R McClelland, DE McGuire, SC McHugh, M McKenzie, K McWilliams, S Meier, T Melissinos, A Mendell, G Mercer, RA Meshkov, S Messenger, CJ Meyers, D Mikhailov, E Mitra, S Mitrofanov, VP Mitselmakher, G Mittleman, R Miyakawa, O Mohanty, S Moreno, G Mossavi, K MowLowry, C Moylan, A Mudge, D Mueller, G Mukherjee, S Muller-Ebhardt, H Munch, J Murray, P Myers, E Myers, J Nash, T Newton, G Nishizawa, A Numata, K O'Reilly, B O'Shaughnessy, R Ottaway, DJ Overmier, H Owen, BJ Pan, Y Papa, MA Parameshwaraiah, V Patel, P Pedraza, M Penn, S Pierro, V Pinto, IM Pitkin, M Pletsch, H Plissi, MV Postiglione, F Prix, R Quetschke, V Raab, F Rabeling, D Radkins, H Rahkola, R Rainer, N Rakhmanov, M Ramsunder, M Ray-Majumder, S Re, V Rehbein, H Reid, S Reitze, DH Ribichini, L Riesen, R Riles, K Rivera, B Robertson, NA Robinson, C Robinson, EL Roddy, S Rodriguez, A Rogan, AM Rollins, J Romano, JD Romie, J Route, R Rowan, S Rudiger, A Ruet, L Russell, P Ryan, K Sakata, S Samidi, M de la Jordana, LS Sandberg, V Sannibale, V Saraf, S Sarin, P Sathyaprakash, BS Sato, S Saulson, PR Savage, R Savov, P Schediwy, S Schilling, R Schnabel, R Schofield, R Schutz, BF Schwinberg, P Scott, SM Searle, AC Sears, B Seifert, F Sellers, D Sengupta, AS Shawhan, P Shoemaker, DH Sibley, A Siemens, X Sigg, D Sinha, S Sintes, AM Slagmolen, BJJ Slutsky, J Smith, JR Smith, MR Somiya, K Strain, KA Strom, DM Stuver, A Summerscales, TZ Sun, KX Sung, M Sutton, PJ Takahashi, H Tanner, DB Taylor, R Taylor, R Thacker, J Thorne, KA Thorne, KS Thuring, A Tokmakov, KV Torres, C Torrie, C Traylor, G Trias, M Tyler, W Ugolini, D Urbanek, K Vahlbruch, H Vallisneri, M Van Den Broeck, C Varvella, M Vass, S Vecchio, A Veitch, J Veitch, P Villar, A Vorvick, C Vyachanin, SP Waldman, SJ Wallace, L Ward, H Ward, R Watts, K Weidner, A Weinert, M Weinstein, A Weiss, R Wen, S Wette, K Whelan, JT Whitcomb, SE Whiting, BF Wilkinson, C Willems, PA Williams, L Willke, B Wilmut, I Winkler, W Wipf, CC Wise, S Wiseman, AG Woan, G Woods, D Wooley, R Worden, J Wu, W Yakushin, I Yamamoto, H Yan, Z Yoshida, S Yunes, N Zanolin, M Zhang, J Zhang, L Zhao, C Zotov, N Zucker, M Muhlen, HZ Zweizig, J Hurley, KC AF Abbott, B. Abbott, R. Adhikari, R. Agresti, J. Ajith, P. Allen, B. Amin, R. Anderson, S. B. Anderson, W. G. Arain, M. Araya, M. Armandula, H. Ashley, M. Aston, S. Aufmuth, P. Aulbert, C. Babak, S. Ballmer, S. Bantilan, H. Barish, B. C. Barker, C. Barker, D. Barr, B. Barriga, P. Barton, M. A. Bayer, K. Betzwieser, J. Beyersdorf, P. T. Bhawal, B. Bilenko, I. A. Billingsley, G. Biswas, R. Black, E. Blackburn, K. Blackburn, L. Blair, D. Bland, B. Bogenstahl, J. Bogue, L. Bork, R. Boschi, V. Bose, S. Brady, P. R. Braginsky, V. B. Brau, J. E. Brinkmann, M. Brooks, A. Brown, D. A. Bullington, A. Bunkowski, A. Buonanno, A. Burmeister, O. Busby, D. Byer, R. L. Cadonati, L. Cagnoli, G. Camp, J. B. Cannizzo, J. Cannon, K. Cantley, C. A. Cao, J. Cardenas, L. Castaldi, G. Cepeda, C. Chalkley, E. Charlton, P. Chatterji, S. Chelkowski, S. Chen, Y. Chiadini, F. Christensen, N. Clark, J. Cochrane, P. Cokelaer, T. Coldwell, R. Conte, R. Cook, D. Corbitt, T. Coyne, D. Creighton, J. D. E. Croce, R. P. Crooks, D. R. M. Cruise, A. M. Cumming, A. Dalrymple, J. D'Ambrosio, E. Danzmann, K. Davies, G. Debra, D. Degallaix, J. Degree, M. Demma, T. Dergachev, V. Desai, S. DeSalvo, R. Dhurandhar, S. Diaz, M. Dickson, J. Di Credico, A. Diederichs, G. Dietz, A. Doomes, E. E. Drever, R. W. P. Dumas, J. -C. Dupuis, R. J. Dwyer, J. G. Ehrens, P. Espinoza, E. Etzel, T. Evans, M. Evans, T. Fairhurst, S. Fan, Y. Fazi, D. Fejer, M. M. Finn, L. S. Fiumara, V. Fotopoulos, N. Franzen, A. Franzen, K. Y. Freise, A. Frey, R. Fricke, T. Fritschel, P. Frolov, V. V. Fyffe, M. Galdi, V. Garofoli, J. Gholami, I. Giaime, J. A. Giampanis, S. Giardina, K. D. Goda, K. Goetz, E. Goggin, L. M. Gonzalez, G. Gossler, S. Grant, A. Gras, S. Gray, C. Gray, M. Greeniialgii, J. Gretarsson, A. M. Grosso, R. Grote, H. Grunewald, S. Guenther, M. Gustafson, R. Hage, B. Hammer, D. Hanna, C. Hanson, J. Harms, J. Harry, G. Harstad, E. Hayler, T. Heefner, J. Heng, I. S. Heptonstall, A. Heurs, M. Hewitson, M. Hild, S. Hirose, E. Hoak, D. Hosken, D. Hough, J. Hoyland, D. Huttner, S. H. Ingram, D. Innerhofer, E. Ito, M. Itoh, Y. Ivanov, A. Johnson, B. Johnson, W. W. Jones, D. I. Jones, G. Jones, R. Ju, L. Kalmus, P. Kalogera, V. Kasprzyk, D. Katsavounidis, E. Kawabe, K. Kawamura, S. Kawazoe, F. Kells, W. Keppel, D. G. Khalili, F. Ya. Kim, C. King, P. Kissel, J. S. Klimenko, S. Kokeyama, K. Kondrashov, V. Kopparapu, R. K. Kozak, D. Krishnan, B. Kwee, P. Lam, P. K. Landry, M. Lantz, B. Lazzarini, A. Lei, M. Leiner, J. Leonhardt, V. Leonor, I. Libbrecht, K. Lindquist, P. Lockerbie, N. A. Longo, M. Lormand, M. Lubinski, M. Lueck, H. Machenschalk, B. MacInnis, M. Mageswaran, M. Mailand, K. Malec, M. Mandic, V. Marano, S. Marka, S. Markowitz, J. Maros, E. Martin, I. Marx, J. N. Mason, K. Matone, L. Matta, V. Mavalvala, N. McCarthy, R. McClelland, D. E. McGuire, S. C. McHugh, M. McKenzie, K. McWilliams, S. Meier, T. Melissinos, A. Mendell, G. Mercer, R. A. Meshkov, S. Messenger, C. J. Meyers, D. Mikhailov, E. Mitra, S. Mitrofanov, V. P. Mitselmakher, G. Mittleman, R. Miyakawa, O. Mohanty, S. Moreno, G. Mossavi, K. MowLowry, C. Moylan, A. Mudge, D. Mueller, G. Mukherjee, S. Mueller-Ebhardt, H. Munch, J. Murray, P. Myers, E. Myers, J. Nash, T. Newton, G. Nishizawa, A. Numata, K. O'Reilly, B. O'Shaughnessy, R. Ottaway, D. J. Overmier, H. Owen, B. J. Pan, Y. Papa, M. A. Parameshwaraiah, V. Patel, P. Pedraza, M. Penn, S. Pierro, V. Pinto, I. M. Pitkin, M. Pletsch, H. Plissi, M. V. Postiglione, F. Prix, R. Quetschke, V. Raab, F. Rabeling, D. Radkins, H. Rahkola, R. Rainer, N. Rakhmanov, M. Ramsunder, M. Ray-Majumder, S. Re, V. Rehbein, H. Reid, S. Reitze, D. H. Ribichini, L. Riesen, R. Riles, K. Rivera, B. Robertson, N. A. Robinson, C. Robinson, E. L. Roddy, S. Rodriguez, A. Rogan, A. M. Rollins, J. Romano, J. D. Romie, J. Route, R. Rowan, S. Ruediger, A. Ruet, L. Russell, P. Ryan, K. Sakata, S. Samidi, M. de la Jordana, L. Sancho Sandberg, V. Sannibale, V. Saraf, S. Sarin, P. Sathyaprakash, B. S. Sato, S. Saulson, P. R. Savage, R. Savov, P. Schediwy, S. Schilling, R. Schnabel, R. Schofield, R. Schutz, B. F. Schwinberg, P. Scott, S. M. Searle, A. C. Sears, B. Seifert, F. Sellers, D. Sengupta, A. S. Shawhan, P. Shoemaker, D. H. Sibley, A. Siemens, X. Sigg, D. Sinha, S. Sintes, A. M. Slagmolen, B. J. J. Slutsky, J. Smith, J. R. Smith, M. R. Somiya, K. Strain, K. A. Strom, D. M. Stuver, A. Summerscales, T. Z. Sun, K. -X. Sung, M. Sutton, P. J. Takahashi, H. Tanner, D. B. Taylor, R. Taylor, R. Thacker, J. Thorne, K. A. Thorne, K. S. Thuering, A. Tokmakov, K. V. Torres, C. Torrie, C. Traylor, G. Trias, M. Tyler, W. Ugolini, D. Urbanek, K. Vahlbruch, H. Vallisneri, M. Van Den Broeck, C. Varvella, M. Vass, S. Vecchio, A. Veitch, J. Veitch, P. Villar, A. Vorvick, C. Vyachanin, S. P. Waldman, S. J. Wallace, L. Ward, H. Ward, R. Watts, K. Weidner, A. Weinert, M. Weinstein, A. Weiss, R. Wen, S. Wette, K. Whelan, J. T. Whitcomb, S. E. Whiting, B. F. Wilkinson, C. Willems, P. A. Williams, L. Willke, B. Wilmut, I. Winkler, W. Wipf, C. C. Wise, S. Wiseman, A. G. Woan, G. Woods, D. Wooley, R. Worden, J. Wu, W. Yakushin, I. Yamamoto, H. Yan, Z. Yoshida, S. Yunes, N. Zanolin, M. Zhang, J. Zhang, L. Zhao, C. Zotov, N. Zucker, M. Muehlen, H. Zur Zweizig, J. Hurley, K. C. CA LIGO Sci Collaboration TI Implications for the origin of GRB 070201 from LIGO observations SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts; gravitational waves; methods : data analysis ID GAMMA-RAY BURSTS; GRAVITATIONAL-WAVE BURSTS; BLACK-HOLE; HOST GALAXY; JET BREAKS; SUPERNOVA; AFTERGLOW; SPECTRUM; FLARE; ASSOCIATION AB We analyzed the available LIGO data coincident with GRB 070201, a short-duration, hard-spectrum gamma-ray burst (GRB) whose electromagnetically determined sky position is coincident with the spiral arms of the Andromeda galaxy (M31). Possible progenitors of such short, hard GRBs include mergers of neutron stars or a neutron star and a black hole, or soft gamma-ray repeater (SGR) flares. These events can be accompanied by gravitational-wave emission. No plausible gravitational-wave candidates were found within a 180 s long window around the time of GRB 070201. This result implies that a compact binary progenitor of GRB 070201, with masses in the range 1 M-circle dot < m(1) < 3 M-circle dot and 1 M-circle dot < m(2) < 40 M-circle dot, located in M31 is excluded at > 99% confidence. If the GRB 070201 progenitor was not in M31, then we can exclude a binary neutron star merger progenitor with distance D < 3.5 Mpc, assuming random inclination, at 90% confidence. The result also implies that an unmodeled gravitational-wave burst from GRB 070201 most probably emitted less than 4.4; 10(-4) M(circle dot)c(2) (7.9 x 10(50) ergs) in any 100 ms long period within the signal region if the source was in M31 and radiated isotropically at the same frequency as LIGO's peak sensitivity (f approximate to 150 Hz). This upper limit does not exclude current models of SGRs at the M31 distance. C1 [Abbott, B.; Abbott, R.; Adhikari, R.; Agresti, J.; Anderson, S. B.; Araya, M.; Armandula, H.; Ballmer, S.; Barish, B. C.; Bhawal, B.; Billingsley, G.; Black, E.; Blackburn, K.; Bork, R.; Boschi, V.; Brown, D. A.; Busby, D.; Cardenas, L.; Cepeda, C.; Chatterji, S.; Coyne, D.; D'Ambrosio, E.; DeSalvo, R.; Dupuis, R. J.; Ehrens, P.; Espinoza, E.; Etzel, T.; Evans, M.; Fairhurst, S.; Fazi, D.; Goggin, L. M.; Heefner, J.; Ivanov, A.; Kells, W.; Keppel, D. G.; King, P.; Kondrashov, V.; Kozak, D.; Lazzarini, A.; Lei, M.; Libbrecht, K.; Lindquist, P.; Mageswaran, M.; Mailand, K.; Mandic, V.; Maros, E.; Marx, J. N.; Meshkov, S.; Meyers, D.; Miyakawa, O.; Nash, T.; Patel, P.; Pedraza, M.; Robertson, N. A.; Russell, P.; Samidi, M.; Sannibale, V.; Sears, B.; Siemens, X.; Smith, M. R.; Sutton, P. J.; Taylor, R.; Tyler, W.; Varvella, M.; Vass, S.; Villar, A.; Waldman, S. J.; Wallace, L.; Ward, R.; Weinstein, A.; Whitcomb, S. E.; Willems, P. A.; Yamamoto, H.; Zhang, L.; Zweizig, J.] LIGO Calif Inst Technol, Pasadena, CA 91125 USA. [Ajith, P.; Allen, B.; Brinkmann, M.; Bunkowski, A.; Burmeister, O.; Chelkowski, S.; Cochrane, P.; Danzmann, K.; Grote, H.; Harms, J.; Heurs, M.; Hewitson, M.; Lueck, H.; Mossavi, K.; Mueller-Ebhardt, H.; Pletsch, H.; Rainer, N.; Rehbein, H.; Ribichini, L.; Ruediger, A.; Schnabel, R.; Seifert, F.; Smith, J. R.; Somiya, K.; Weidner, A.; Weinert, M.; Willke, B.; Winkler, W.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany. [Allen, B.; Anderson, W. G.; Biswas, R.; Brady, P. R.; Cannon, K.; Creighton, J. D. E.; Fotopoulos, N.; Hammer, D.; Itoh, Y.; Wiseman, A. G.; Woods, D.] Univ Wisconsin, Milwaukee, WI 53201 USA. [Amin, R.; Giaime, J. A.; Gonzalez, G.; Hanna, C.; Johnson, W. W.; Kissel, J. S.; Rodriguez, A.; Sung, M.; Wen, S.] Louisiana State Univ, Baton Rouge, LA 70803 USA. [Arain, M.; Klimenko, S.; Mercer, R. A.; Mitselmakher, G.; Mueller, G.; Quetschke, V.; Reitze, D. H.; Whiting, B. F.; Wise, S.; Wu, W.] Univ Florida, Gainesville, FL 32611 USA. [Ashley, M.; Dickson, J.; Gossler, S.; Gray, M.; Lam, P. K.; McKenzie, K.; MowLowry, C.; Moylan, A.; Rabeling, D.; Scott, S. M.; Slagmolen, B. J. J.; Wette, K.] Australian Natl Univ, Canberra, ACT 0200, Australia. [Aston, S.; Cruise, A. M.; Hoyland, D.; Kasprzyk, D.; Re, V.; Robinson, E. L.] Univ Birmingham, Birmingham B15 2TT, England. [Aufmuth, P.; Danzmann, K.; Diederichs, G.; Franzen, A.; Hage, B.; Hild, S.; Kwee, P.; Lueck, H.; Malec, M.; Meier, T.; Thuering, A.; Willke, B.; Muehlen, H. Zur] Leibniz Univ Hannover, D-30167 Hannover, Germany. [Aulbert, C.; Babak, S.; Chen, Y.; Grunewald, S.; Krishnan, B.; Papa, M. A.; Prix, R.; Schutz, B. F.; Sintes, A. M.; Somiya, K.; Takahashi, H.; Whelan, J. T.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany. [Bantilan, H.; Cepeda, C.] Carleton Coll, Northfield, MN 55057 USA. [Barker, C.; Barker, D.; Bland, B.; Cook, D.; Garofoli, J.; Gray, C.; Ingram, D.; Johnson, B.; Kawabe, K.; Landry, M.; Lubinski, M.; McCarthy, R.; Mendell, G.; Moreno, G.; Myers, E.; Myers, J.; Parameshwaraiah, V.; Raab, F.; Radkins, H.; Rivera, B.; Ryan, K.; Sandberg, V.; Savage, R.; Schwinberg, P.; Sigg, D.; Vorvick, C.; Wilkinson, C.; Worden, J.] LIGO Hanford Observ, Richland, WA 99352 USA. [Barr, B.; Barton, M. A.; Bogenstahl, J.; Cagnoli, G.; Cantley, C. A.; Chalkley, E.; Clark, J.; Crooks, D. R. M.; Cumming, A.; Grant, A.; Heng, I. S.; Heptonstall, A.; Hough, J.; Huttner, S. H.; Jones, R.; Martin, I.; Messenger, C. J.; Murray, P.; Newton, G.; Pitkin, M.; Plissi, M. V.; Reid, S.; Robertson, N. A.; Rowan, S.; Taylor, R.; Tokmakov, K. V.; Torrie, C.; Veitch, J.; Ward, H.; Woan, G.] Univ Glasgow, Glasgow G12 8QQ, Lanark, Scotland. [Barriga, P.; Blair, D.; Degallaix, J.; Dumas, J. -C.; Fan, Y.; Gras, S.; Ju, L.; Schediwy, S.] Univ Western Australia, Crawley, WA 6009, Australia. [Bayer, K.; Betzwieser, J.; Blackburn, L.; Cadonati, L.; Cao, J.; Corbitt, T.; Fritschel, P.; Goda, K.; Harry, G.; Innerhofer, E.; Katsavounidis, E.; MacInnis, M.; Markowitz, J.; Mason, K.; Mavalvala, N.; Mikhailov, E.; Ottaway, D. J.; Ruet, L.; Sarin, P.; Shoemaker, D. H.; Weiss, R.; Wipf, C. C.; Zanolin, M.; Zucker, M.] LIGO Massachusetts Inst Technol, Cambridge, MA 02139 USA. [Beyersdorf, P. T.] San Jose State Univ, San Jose, CA 95192 USA. [Bilenko, I. A.; Braginsky, V. B.; Dickson, J.; Gossler, S.; Lam, P. K.; McClelland, D. E.; McKenzie, K.; Vyachanin, S. P.] Moscow MV Lomonosov State Univ, Moscow 119992, Russia. [Bogue, L.; Frolov, V. V.; Fyffe, M.; Giaime, J. A.; Giardina, K. D.; Hoak, D.; Lormand, M.; Riesen, R.; Roddy, S.; Romie, J.; Sellers, D.; Sibley, A.; Thacker, J.; Traylor, G.; Watts, K.; Wooley, R.; Yakushin, I.] LIGO Livingston Observ, Livingston, LA 70754 USA. [Bose, S.; Leiner, J.; Rogan, A. M.] Washington State Univ, Pullman, WA 99164 USA. [Brau, J. E.; Frey, R.; Harstad, E.; Ito, M.; Schofield, R.] Univ Oregon, Eugene, OR 97403 USA. [Brooks, A.; Hosken, D.; Mudge, D.; Munch, J.; Veitch, P.] Univ Adelaide, Adelaide, SA 5005, Australia. [Brown, D. A.; Savov, P.; Siemens, X.; Thorne, K. S.; Vallisneri, M.] CALTECH, CaRT, Pasadena, CA USA. [Bullington, A.; Byer, R. L.; Debra, D.; Degree, M.; Fejer, M. M.; Urbanek, K.] Stanford Univ, Stanford, CA 94305 USA. [Buonanno, A.; Pan, Y.; Shawhan, P.] Univ Maryland, College Pk, MD 20742 USA. [Buonanno, A.; Pan, Y.; Shawhan, P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Castaldi, G.; Croce, R. P.; Demma, T.; Galdi, V.; Pierro, V.] Univ Sannio Benevento, I-82100 Benevento, Italy. [Charlton, P.] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia. [Conte, R.; Longo, M.; Marano, S.; Matta, V.; Postiglione, F.] Univ Salerno, I-84084 Fisciano, Salerno, Italy. [Cokelaer, T.; Davies, G.; Dietz, A.; Fairhurst, S.; Jones, G.; Robinson, C.; Romano, J. D.; Sathyaprakash, B. S.; Schutz, B. F.; Sengupta, A. S.; Van Den Broeck, C.] Cardiff Univ, Cardiff CF24 3AA, England. [Dalrymple, J.; Di Credico, A.; Hirose, E.; Saulson, P. R.] Syracuse Univ, Syracuse, NY 13244 USA. [Dergachev, V.; Goetz, E.; Gustafson, R.; Riles, K.] Univ Michigan, Ann Arbor, MI 48109 USA. [Desai, S.; Finn, L. S.; Kopparapu, R. K.; Owen, B. J.; Rakhmanov, M.; Ramsunder, M.; Stuver, A.; Thorne, K. A.] Penn State Univ, University Pk, PA 16802 USA. [Dhurandhar, S.; Mitra, S.] Inter Univ Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. [Diaz, M.; Mohanty, S.; Mukherjee, S.] Univ Texas Brownsville, Brownsville, TX 78520 USA. Univ Texas Brownsville & Texas Southmost Coll, Brownsville, TX 78520 USA. [Doomes, E. E.] So Univ, Baton Rouge, LA 70813 USA. A&M Coll, Baton Rouge, LA 70813 USA. [Dwyer, J. G.; Kalmus, P.; Marka, S.; Matone, L.] Columbia Univ, New York, NY 10027 USA. [Giampanis, S.; Melissinos, A.] Univ Rochester, Rochester, NY 14627 USA. [Greeniialgii, J.; Hayler, T.; Wilmut, I.] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Gretarsson, A. M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA. [Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England. [Kalogera, V.; Kim, C.; O'Shaughnessy, R.] NW Univ, Evanston, IL 60208 USA. [Kawamura, S.; Kawazoe, F.; Kokeyama, K.; Leonhardt, V.; Sakata, S.; Sato, S.] Natl Astron Observ Japan, Tokyo 1818588, Japan. [Lockerbie, N. A.] Univ Strathclyde, Glasgow G1 1XQ, Lanark, Scotland. [McHugh, M.] Loyola Univ, New Orleans, LA 70118 USA. [Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA. [de la Jordana, L. Sancho; Sintes, A. M.; Trias, M.] Univ Illes Balears, E-07122 Palma de Mallorca, Spain. [Saraf, S.] Rochester Inst Technol, Rochester, NY 14623 USA. [Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA. [Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA. [Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA. [Zotov, N.] Louisiana Tech Univ, Ruston, LA 71272 USA. [Hurley, K. C.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Abbott, B (reprint author), LIGO Calif Inst Technol, Pasadena, CA 91125 USA. RI Ward, Robert/I-8032-2014; Vecchio, Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Ottaway, David/J-5908-2015; Postiglione, Fabio/O-4744-2015; Biswas, Rahul/H-7474-2016; Sigg, Daniel/I-4308-2015; Pinto, Innocenzo/L-3520-2016; Harms, Jan/J-4359-2012; Frey, Raymond/E-2830-2016; Mitrofanov, Valery/D-8501-2012; Bilenko, Igor/D-5172-2012; Allen, Bruce/K-2327-2012; Chen, Yanbei/A-2604-2013; Barker, David/A-5671-2013; Fricke, Thomas/B-6885-2013; Zhao, Chunnong/C-2403-2013; Ju, Li/C-2623-2013; Re, Virginia /F-6403-2013; Pitkin, Matthew/I-3802-2013; Vyatchanin, Sergey/J-2238-2012; Khalili, Farit/D-8113-2012; Chiadini, Francesco/E-1812-2015; Lam, Ping Koy/A-5276-2008; Galdi, Vincenzo/B-1670-2008; McClelland, David/E-6765-2010; Martin, Iain/A-2445-2010; Hild, Stefan/A-3864-2010; Rowan, Sheila/E-3032-2010; Strain, Kenneth/D-5236-2011; Raab, Frederick/E-2222-2011; Lueck, Harald/F-7100-2011; Kawazoe, Fumiko/F-7700-2011; Freise, Andreas/F-8892-2011; Kawabe, Keita/G-9840-2011; Finn, Lee Samuel/A-3452-2009; Agresti, Juri/G-8168-2012 OI Freise, Andreas/0000-0001-6586-9901; MATTA, VINCENZO/0000-0002-2046-4027; MARANO, Stefano/0000-0002-5307-0980; Whiting, Bernard F/0000-0002-8501-8669; Ward, Robert/0000-0001-5503-5241; Whelan, John/0000-0001-5710-6576; Fairhurst, Stephen/0000-0001-8480-1961; Boschi, Valerio/0000-0001-8665-2293; Pinto, Innocenzo M./0000-0002-2679-4457; Nishizawa, Atsushi/0000-0003-3562-0990; Zweizig, John/0000-0002-1521-3397; O'Shaughnessy, Richard/0000-0001-5832-8517; Vecchio, Alberto/0000-0002-6254-1617; Postiglione, Fabio/0000-0003-0628-3796; Biswas, Rahul/0000-0002-0774-8906; Sigg, Daniel/0000-0003-4606-6526; Frey, Raymond/0000-0003-0341-2636; LONGO, Maurizio/0000-0001-8325-4003; Pierro, Vincenzo/0000-0002-6020-5521; Allen, Bruce/0000-0003-4285-6256; Zhao, Chunnong/0000-0001-5825-2401; Pitkin, Matthew/0000-0003-4548-526X; Chiadini, Francesco/0000-0002-9339-8622; Lam, Ping Koy/0000-0002-4421-601X; Galdi, Vincenzo/0000-0002-4796-3600; McClelland, David/0000-0001-6210-5842; Strain, Kenneth/0000-0002-2066-5355; Lueck, Harald/0000-0001-9350-4846; Finn, Lee Samuel/0000-0002-3937-0688; Agresti, Juri/0000-0001-6119-2470 NR 64 TC 115 Z9 115 U1 3 U2 22 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 10 PY 2008 VL 681 IS 2 BP 1419 EP 1430 DI 10.1086/587954 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 324JX UT WOS:000257516000052 ER PT J AU Rebull, LM Stapelfeldt, KR Werner, MW Mannings, VG Chen, C Stauffer, JR Smith, PS Song, I Hines, D Low, FJ AF Rebull, L. M. Stapelfeldt, K. R. Werner, M. W. Mannings, V. G. Chen, C. Stauffer, J. R. Smith, P. S. Song, I. Hines, D. Low, F. J. TI Spitzer MIPS observations of stars in the beta Pictoris moving group SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; stars : individual (beta Pictoris moving group) ID MULTIBAND IMAGING PHOTOMETER; STANDARD STELLAR LIBRARY; MICROSCOPII DEBRIS DISK; TW HYDRAE ASSOCIATION; SUN-LIKE STARS; SPACE-TELESCOPE; MU-M; YOUNG STARS; ABSOLUTE CALIBRATION; INTERSTELLAR CLOUDS AB We present Multiband Imaging Photometer for Spitzer (MIPS) observations at 24 and 70 mu m for 30 stars, and at 160 mu m for a subset of 12 stars, in the nearby (similar to 30 pc), young (similar to 12 Myr) beta Pictoris moving group (BPMG). In several cases, the new MIPS measurements resolve source confusion and background contamination issues in the IRAS data for this sample. We find that 7 members have 24 mu m excesses, implying a debris disk fraction of 23%, and that at least 11 have 70 mu m excesses (disk fraction of >= 37%). Five disks are detected at 160 mu m(out of a biased sample of 12 stars observed), with a range of 160/70 flux ratios. The disk fraction at 24 and 70 mu m, and the size of the excesses measured at each wavelength, are both consistent with an "inside-out'' infrared excess decrease with time, wherein the shorter wavelength excesses disappear before longer wavelength excesses, and consistent with the overall decrease of infrared excess frequency with stellar age, as seen in Spitzer studies of other young stellar groups. Assuming that the infrared excesses are entirely due to circumstellar disks, we characterize the disk properties using simple models and fractional infrared luminosities. Optically thick disks, seen in the younger TW Hya and eta Cha associations, are entirely absent in the BPMG. Additional flux density measurements at 24 and 70 mu m are reported for nine Tucana-Horologium association member stars. Since this is < 20% of the association membership, limited analysis on the complete disk fraction of this association is possible. C1 [Rebull, L. M.; Mannings, V. G.; Stauffer, J. R.; Song, I.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Stapelfeldt, K. R.; Werner, M. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Chen, C.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Smith, P. S.; Low, F. J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Rebull, LM (reprint author), CALTECH, Spitzer Sci Ctr, Mail Stop 220-6,1200 E Calif Blvd, Pasadena, CA 91125 USA. EM luisa.rebull@jpl.nasa.gov RI Stapelfeldt, Karl/D-2721-2012; OI Rebull, Luisa/0000-0001-6381-515X NR 70 TC 75 Z9 75 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 10 PY 2008 VL 681 IS 2 BP 1484 EP 1504 DI 10.1086/588182 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 324JX UT WOS:000257516000058 ER PT J AU Jennings, DE Nixon, CA Jolly, A Bezard, B Coustenis, A Vinatier, S Irwin, PGJ Teanby, NA Romani, PN Achterberg, RK Flasar, FM AF Jennings, D. E. Nixon, C. A. Jolly, A. Bezard, B. Coustenis, A. Vinatier, S. Irwin, P. G. J. Teanby, N. A. Romani, P. N. Achterberg, R. K. Flasar, F. M. TI Isotopic ratios in Titan's atmosphere from Cassini CIRS limb sounding: HC3N in the north SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE infrared : solar system; planets and satellites : formation; planets and satellites : individual ( Titan); radiative transfer ID LATITUDINAL VARIATIONS; BAND INTENSITIES; HCN; C-12/C-13; HYDROCARBONS; STRATOSPHERE; SPECTRA; TEMPERATURE; RETRIEVAL; N-14/N-15 AB This Letter reports the first detection of the three C-13 isotopologues of HC3N on Titan, from Cassini Composite nfrared Spectrometer (CIRS) infrared spectra. The data are limb spectra taken at latitudes N54 degrees-N69 degrees in 2006 and 2007 when HC3N was enhanced in the north. Using a new line list for the nu(5) bands of all isotopologues, we have modeled the isolated emission of (HCCCN)-C-13 at 658.7 cm(-1) and both (HCCCN)-C-13 and (HCCCN)-C-13 at 663.0 cm(-1), which are blended with the Q-branch of HC3N at 663.3 cm(-1) at the resolution of CIRS (0.5 cm(-1)) and detectable as an increase in the intensity of the low-frequency wing. Using the resolved pair (HCCCN)-C-13 /HC3N we find C-12/C-13 = 79 +/- 17, in line with other measurements on Titan from Cassini and Huygens. C1 [Jennings, D. E.; Nixon, C. A.; Romani, P. N.; Achterberg, R. K.; Flasar, F. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Nixon, C. A.; Achterberg, R. K.] Univ Maryland, College Pk, MD 20742 USA. [Jolly, A.] Univ Paris 12, CNRS, LISA, F-94010 Creteil, France. [Bezard, B.; Coustenis, A.; Vinatier, S.] Observ Paris, LESIA, F-92195 Meudon, France. [Irwin, P. G. J.; Teanby, N. A.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England. RP Jennings, DE (reprint author), NASA, Goddard Space Flight Ctr, Code 693, Greenbelt, MD 20771 USA. EM conor.a.nixon@nasa.gov RI JOLLY, antoine/D-3238-2009; Nixon, Conor/A-8531-2009; Flasar, F Michael/C-8509-2012; Romani, Paul/D-2729-2012; Jennings, Donald/D-7978-2012 OI Nixon, Conor/0000-0001-9540-9121; NR 24 TC 17 Z9 17 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 10 PY 2008 VL 681 IS 2 BP L109 EP L111 DI 10.1086/590534 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 326LY UT WOS:000257661900015 ER PT J AU Monnier, JD Tannirkulam, A Tuthill, PG Ireland, M Cohen, R Danchi, WC Baron, F AF Monnier, J. D. Tannirkulam, A. Tuthill, P. G. Ireland, M. Cohen, R. Danchi, W. C. Baron, F. TI Discovery of a circumbinary disk around Herbig Ae/Be system V892 tauri SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries : close; infrared : stars; stars : individual (V892 Tauri); stars : pre-main-sequence; techniques : interferometric ID INTERMEDIATE-MASS STARS; MAIN-SEQUENCE EVOLUTION; AURIGA MOLECULAR CLOUD; CIRCUMSTELLAR DISKS; PROTOPLANETARY DISK; TAURUS; INTERFEROMETRY; ELIAS-1; TELESCOPE; HALO AB We report the discovery of a circumbinary disk around the Herbig Ae/Be system V892 Tau. Our detailed mid-infrared images were made using segment-tilting interferometry on the Keck I telescope and reveal an asymmetric disk inclined at similar to 60 degrees with an inner hole diameter of 250 mas (35 AU), approximately 5 times larger than the apparent separation of the binary components. In addition, we report a new measurement along the binary orbit using near-infrared Keck aperture masking, allowing a crude estimate of orbital parameters and the system mass for the first time. The size of the inner hole appears to be consistent with the minimum size prediction from tidal truncation theory, bearing a resemblance to the recently unmasked binary CoKu Tau/4. Our results have motivated a reanalysis of the system spectral energy distribution, concluding the luminosity of this system has been severely underestimated. With further study and monitoring, V892 Tau should prove a powerful testing ground for both predictions of dynamical models for disk-star interactions in young systems with gas-rich disks and for calibrations of pre-main-sequence tracks for intermediate-mass stars. C1 [Monnier, J. D.; Tannirkulam, A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Tuthill, P. G.; Ireland, M.] Univ Sydney, Sydney, NSW 2006, Australia. [Danchi, W. C.] NASA, Goddard Space Flight Ctr, Washington, DC 20546 USA. [Baron, F.] Univ Cambridge, Cambridge CB2 1TN, England. RP Monnier, JD (reprint author), Univ Michigan, Dept Astron, 941 Dennison Bldg, Ann Arbor, MI 48109 USA. EM monnier@umich.edu NR 31 TC 18 Z9 18 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 10 PY 2008 VL 681 IS 2 BP L97 EP L100 DI 10.1086/590532 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 326LY UT WOS:000257661900012 ER PT J AU Nakagawa, YE Sakamoto, T Sato, G Gehrels, N Hurley, K Palmer, DM AF Nakagawa, Y. E. Sakamoto, T. Sato, G. Gehrels, N. Hurley, K. Palmer, D. M. TI The swift discovery of X-ray afterglows accompanying short bursts from SGR 1900+14 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE pulsars : individual (SGR 1900+14); stars : neutron ID SGR 1900+14; GIANT FLARE; EMISSION; SGR-1806-20; GALAXY; GRB-050709; TELESCOPE; MAGNETARS; OUTBURST; MISSION AB The discovery of X-ray afterglows accompanying two short bursts from SGR 1900+ 14 is presented. The afterglow luminosities at the end of each observation are lower by 30%-50% than their initial luminosities, and decay with power-law indices p similar to 0.2-0.4. Their initial bolometric luminosities are L similar to 10(34)-10(35) erg s(-1). We discuss analogies and differences between the X-ray afterglows of SGR short bursts and short gamma-ray bursts. C1 [Nakagawa, Y. E.] Aoyama Gakuin Univ, Grad Sch Sci & Engn, Kanagawa 2298558, Japan. [Nakagawa, Y. E.] RIKEN, Inst Phys & Chem Res, Wako, Saitama 3510198, Japan. [Sakamoto, T.; Sato, G.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sakamoto, T.] Univ Maryland, Baltimore, MD 21250 USA. [Hurley, K.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Palmer, D. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RP Nakagawa, YE (reprint author), Aoyama Gakuin Univ, Grad Sch Sci & Engn, Kanagawa 2298558, Japan. RI Gehrels, Neil/D-2971-2012 NR 37 TC 2 Z9 2 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 10 PY 2008 VL 681 IS 2 BP L89 EP L92 DI 10.1086/590428 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 326LY UT WOS:000257661900010 ER PT J AU Nixon, CA Jennings, DE Bezard, B Teanby, NA Achterberg, RK Coustenis, A Vinatier, S Irwin, PGJ Romani, PN Hewagama, T Flasar, FM AF Nixon, C. A. Jennings, D. E. Bezard, B. Teanby, N. A. Achterberg, R. K. Coustenis, A. Vinatier, S. Irwin, P. G. J. Romani, P. N. Hewagama, T. Flasar, F. M. TI Isotopic ratios in Titan's atmosphere from Cassini CIRS limb sounding: CO2 at low and midlatitudes SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE infrared : solar system; planets and satellites : formation; planets and satellites : individual (Titan); radiative transfer ID SPECTROSCOPIC DATABASE; STRATOSPHERE; JUPITER; SPECTRA; SATURN AB This Letter reports on a search for infrared emissions of isotopologues of CO2 in the atmosphere of Titan using spectral data recorded by the Cassini Composite Infrared Spectrometer (CIRS). We have made a successful 6.5 sigma detection of (CO2)-C-13 at a fraction CO2/(CO2)-C-13 = 84 +/- 17, consistent with measurements of C-12/C-13 in other species, and also the terrestrial value (89). We also find a probable 3.5 sigma detection of (COO)-O-16-O-18 at a fraction CO2/(COO)-O-16-O-18 = 173 +/- 55, slightly lower than the terrestrial value (253) and consistent with the twofold enhancement in O-18 reported previously in CO, or with an intermediate value as suggested by chemistry. These isotopic ratios provide important constraints on models of the formation, evolution, and current processes in Titan's atmosphere. C1 [Nixon, C. A.; Achterberg, R. K.; Hewagama, T.] Univ Maryland, College Pk, MD 20742 USA. [Jennings, D. E.; Achterberg, R. K.; Romani, P. N.; Hewagama, T.; Flasar, F. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bezard, B.; Coustenis, A.; Vinatier, S.] Observ Paris, LESIA, F-92195 Meudon, France. [Teanby, N. A.; Irwin, P. G. J.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England. RP Nixon, CA (reprint author), Univ Maryland, College Pk, MD 20742 USA. EM conor.a.nixon@nasa.gov RI Nixon, Conor/A-8531-2009; Hewagama, T/C-8488-2012; Flasar, F Michael/C-8509-2012; Romani, Paul/D-2729-2012; Jennings, Donald/D-7978-2012; OI Nixon, Conor/0000-0001-9540-9121; Teanby, Nicholas/0000-0003-3108-5775; Irwin, Patrick/0000-0002-6772-384X NR 24 TC 17 Z9 17 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 10 PY 2008 VL 681 IS 2 BP L101 EP L103 DI 10.1086/590553 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 326LY UT WOS:000257661900013 ER PT J AU Straus, T Fleck, B Jefferies, SM Cauzzi, G McIntosh, SW Reardon, K Severino, G Steffen, M AF Straus, Thomas Fleck, Bernhard Jefferies, Stuart M. Cauzzi, Gianna McIntosh, Scott W. Reardon, Kevin Severino, Giuseppe Steffen, Matthias TI The energy flux of internal gravity waves in the lower solar atmosphere SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE hydrodynamics; Sun : atmospheric motions; Sun : chromosphere; Sun : photosphere; waves ID FREQUENCY ACOUSTIC-WAVES; MODEL ATMOSPHERES; ELECTRIC-CURRENTS; CHROMOSPHERE; DYNAMICS; PHOTOSPHERE; STARS; OSCILLATIONS; SIMULATIONS; PROPAGATION AB Stably stratified fluids, such as stellar and planetary atmospheres, can support and propagate gravity waves. On Earth these waves, which can transport energy and momentum over large distances and can trigger convection, contribute to the formation of our weather and global climate. Gravity waves also play a pivotal role in planetary sciences and modern stellar physics. They have also been proposed as an agent for the heating of stellar atmospheres and coronae, the exact mechanism behind which is one of the outstanding puzzles in solar and stellar physics. Using a combination of high-quality observations and 3D numerical simulations we have the first unambiguous detection of propagating gravity waves in the Sun's (and hence a stellar) atmosphere. Moreover, we are able to determine the height dependence of their energy flux and find that at the base of the Sun's chromosphere it is around 5 kW m(-2). This amount of energy is comparable to the radiative losses of the entire chromosphere and points to internal gravity waves as a key mediator of energy into the solar atmosphere. C1 [Straus, Thomas; Severino, Giuseppe] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Fleck, Bernhard] NASA, Goddard Space Flight Ctr, ESA Sci Operat Dept, Greenbelt, MD 20771 USA. [Jefferies, Stuart M.] Univ Hawaii, Inst Astron, Pukulani, HI 96768 USA. [Cauzzi, Gianna; Reardon, Kevin] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [McIntosh, Scott W.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Steffen, Matthias] Inst Astrophys, D-14482 Potsdam, Germany. RP Straus, T (reprint author), Osserv Astron Capodimonte, INAF, Via Moiariello 16, I-80131 Naples, Italy. EM straus@oacn.inaf.it; bfleck@esa.nascom.nasa.gov; stuartj@ifa.hawaii.edu; gcauzzi@arcetri.astro.it; mscott@ucar.edu; kreardon@arcetri.astro.it; severino@oacn.inaf.it; msteffen@aip.de RI Fleck, Bernhard/C-9520-2012; OI Straus, Thomas/0000-0002-6280-806X; Cauzzi, Gianna/0000-0002-6116-7301 NR 40 TC 44 Z9 45 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 10 PY 2008 VL 681 IS 2 BP L125 EP L128 DI 10.1086/590495 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 326LY UT WOS:000257661900019 ER PT J AU Frey, H AF Frey, Herbert TI Ages of very large impact basins on Mars: Implications for the late heavy bombardment in the inner solar system SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB A sharp peak in both relative crater retention ages and inferred model absolute ages for the largest impact basins on Mars may be a Martian equivalent of a late heavy bombardment (LHB) terminal lunar cataclysm (TLC). If so, it supports a NICE-type LHB, provides an important temporal connection between lunar and Martian chronologies, and suggests the current Martian chronology overestimates the age of large basins and perhaps other events in early Martian history. C1 NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. RP Frey, H (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Mail Code 698, Greenbelt, MD 20771 USA. EM herbert.v.frey@nasa.gov NR 18 TC 56 Z9 57 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 10 PY 2008 VL 35 IS 13 AR L13203 DI 10.1029/2008GL033515 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 327OQ UT WOS:000257738800002 ER PT J AU Sanchez-Lavega, A Hueso, R Piccioni, G Drossart, P Peralta, J Perez-Hoyos, S Wilson, CF Taylor, FW Baines, KH Luz, D Erard, S Lebonnois, S AF Sanchez-Lavega, A. Hueso, R. Piccioni, G. Drossart, P. Peralta, J. Perez-Hoyos, S. Wilson, C. F. Taylor, F. W. Baines, K. H. Luz, D. Erard, S. Lebonnois, S. TI Variable winds on Venus mapped in three dimensions SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID GALILEO; IMAGES; DYNAMICS; TRACKING; MISSION; EXPRESS AB We present zonal and meridional wind measurements at three altitude levels within the cloud layers of Venus from cloud tracking using images taken with the VIRTIS instrument on board Venus Express. At low latitudes, zonal winds in the Southern hemisphere are nearly constant with latitude with westward velocities of 105 ms(-1) at cloud-tops (altitude similar to 66 km) and 60-70 ms(-1) at the cloud-base (altitude similar to 47 km). At high latitudes, zonal wind speeds decrease linearly with latitude with no detectable vertical wind shear (values lower than 15 ms(-1)), indicating the possibility of a vertically coherent vortex structure. Meridional winds at the cloud-tops are poleward with peak speed of 10 ms(-1) at 55 degrees S but below the cloud tops and averaged over the South hemisphere are found to be smaller than 5 ms(-1). We also report the detection at subpolar latitudes of wind variability due to the solar tide. C1 [Sanchez-Lavega, A.; Hueso, R.; Peralta, J.; Perez-Hoyos, S.] Univ Basque Country, Dept Fis Aplicada 1, Escuela Super Ingn, E-48013 Bilbao, Spain. [Piccioni, G.] Ist Nazl Astrofis, I-00133 Rome, Italy. [Piccioni, G.] Ist Astrofis Spaziale & Fisica Cosmica, I-00133 Rome, Italy. [Drossart, P.; Luz, D.; Erard, S.] Univ Paris Diderot, Lab Etud Spatiales & Instrumentat Astrophys Obser, CNRS, UPMC,Observ Paris, F-92195 Meudon, France. [Wilson, C. F.; Taylor, F. W.] Univ Oxford, Dept Phys, Oxford OX1 3PU, England. [Baines, K. H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Luz, D.] Univ Lisbon, Astron Observ, Ctr Astron & Astrofis, P-1699 Lisbon, Portugal. [Lebonnois, S.] UPMC, Meteorol Dynam Lab, IPSL, CNRS, F-75252 Paris, France. RP Sanchez-Lavega, A (reprint author), Univ Basque Country, Dept Fis Aplicada 1, Escuela Super Ingn, Alameda Urquijo S-N, E-48013 Bilbao, Spain. EM agustin.sanchez@ehu.es RI Luz, David/J-4588-2013; Perez-Hoyos, Santiago/L-7543-2014; OI Piccioni, Giuseppe/0000-0002-7893-6808; Luz, David/0000-0002-9473-8035; Perez-Hoyos, Santiago/0000-0002-2587-4682; Sanchez-Lavega, Agustin/0000-0001-7355-1522; Hueso, Ricardo/0000-0003-0169-123X; Peralta, Javier/0000-0002-6823-1695; LEBONNOIS, SEBASTIEN/0000-0002-2390-8164 NR 18 TC 68 Z9 68 U1 2 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 10 PY 2008 VL 35 IS 13 AR L13204 DI 10.1029/2008GL033817 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 327OQ UT WOS:000257738800004 ER PT J AU Wenig, MO Cede, AM Bucsela, EJ Celarier, EA Boersma, KF Veefkind, JP Brinksma, EJ Gleason, JF Herman, JR AF Wenig, M. O. Cede, A. M. Bucsela, E. J. Celarier, E. A. Boersma, K. F. Veefkind, J. P. Brinksma, E. J. Gleason, J. F. Herman, J. R. TI Validation of OMI tropospheric NO2 column densities using direct-Sun mode Brewer measurements at NASA Goddard Space Flight Center SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID ROTATIONAL RAMAN-SCATTERING; NITROGEN-DIOXIDE; ABSORPTION-MEASUREMENTS; SURFACE REFLECTIVITY; STRATOSPHERIC NO2; GOME; NM; ATMOSPHERE; CLIMATOLOGY; RETRIEVAL AB [1] This paper presents a comparison of NO2 data measured with the Ozone Monitoring Instrument (OMI) on board the EOS-AURA satellite with ground-based direct-Sun Brewer measurement data. Since its deployment in July 2004, OMI has provided more than 2 years of daily high-resolution (similar to 13 x 24 km 2 at nadir) NO2 vertical column density maps. We describe the retrieval, which includes an estimation of the stratospheric and tropospheric fraction of total NO2 columns, the air mass factor (AMF) correction based on detected tropospheric NO2 enhancements, and the generation of the gridded data product. We present a validation study of the gridded NO2 data set using data from a Brewer MK3 double monochromator in direct-Sun mode located at NASA Goddard Space Flight Center in Greenbelt, Maryland, USA. Monthly averages of coinciding measurements correlate well (r = 0.9) but OMI data are about 25% lower than the Brewer measurement data ( slope 0.75, intercept -0.38 x 10(15) molecules/cm(2)). We present a detailed uncertainty analysis for both ground and satellite data and discuss the possible reasons for the observed differences. C1 [Wenig, M. O.] City Univ Hong Kong, Dept Phys & Mat Sci, Kowloon, Hong Kong, Peoples R China. [Wenig, M. O.; Brinksma, E. J.] Univ Maryland, NASA GSFC, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21250 USA. [Cede, A. M.] Univ Maryland, NASA GSFC, Earth System Sci Interdisciplinary Ctr, College Pk, MD 20740 USA. [Celarier, E. A.] SGT Inc, NASA GSFC, College Pk, MD 20770 USA. [Boersma, K. F.] Harvard Univ, Dept Atmospher Chem, Cambridge, MA 02138 USA. [Veefkind, J. P.; Brinksma, E. J.] Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Wenig, MO (reprint author), City Univ Hong Kong, Dept Phys & Mat Sci, Kowloon, Hong Kong, Peoples R China. EM mark.wenig@cityu.edu.hk RI Gleason, James/E-1421-2012; Boersma, Klaas/H-4559-2012; Wenig, Mark/K-7279-2012 OI Boersma, Klaas/0000-0002-4591-7635; NR 36 TC 41 Z9 43 U1 2 U2 13 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 9 PY 2008 VL 113 IS D16 AR D16S45 DI 10.1029/2007JD008988 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 327QK UT WOS:000257743400001 ER PT J AU Mannucci, AJ Tsurutani, BT Abdu, MA Gonzalez, WD Komjathy, A Echer, E Iijima, BA Crowley, G Anderson, D AF Mannucci, A. J. Tsurutani, B. T. Abdu, M. A. Gonzalez, W. D. Komjathy, A. Echer, E. Iijima, B. A. Crowley, G. Anderson, D. TI Superposed epoch analysis of the dayside ionospheric response to four intense geomagnetic storms SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID TOTAL ELECTRON-CONTENT; MAGNETIC STORMS; SOLAR; FIELD; ELECTRODYNAMICS; SYSTEM; MODEL AB Prompt daytime ionospheric responses are presented for the following four intense geomagnetic storms: 29 October 2003, 30 October 2003, 20 November 2003, and 7 November 2004. We perform a superposed epoch analysis of the storms by defining the start time of the epoch when the Kan-Lee interplanetary electric field (proportional to the reconnection electric field) first reaches 10 mV/m during a period of continuously southward B-z. Measurements from the GPS receiver onboard the CHAMP satellite at 400 km altitude indicate significant low- to middle-latitude daytime total electron content (TEC) increases above the satellite within 1 - 2 h of the defined start time for three of the storms (similar to 1400 local solar time). The 20 November 2003 data follow a different pattern: the largest TEC increases appear several hours (similar to 5 - 7) following the interplanetary magnetic field Bz event onset. TEC data obtained from ground-based GPS receivers for the November 2003 storm tend to confirm a "late'' TEC increase for this storm at similar to 1400 LT. Estimates of vertical plasma uplift near the equator at Jicamarca longitudes (similar to 281 E) using the dual-magnetometer technique suggest that variability of the timing of the TEC response is associated with variability in the prompt penetration of electric fields to low latitudes. It is also found that for the November 2003 magnetic storm the cross-correlation function between the SYM-H index and the interplanetary electric field reached maximum correlation with a lag time of 4 h. Such a large lag time has never been noted before. The long delays of both the ionosphere and magnetosphere responses need to be better understood. C1 [Mannucci, A. J.; Tsurutani, B. T.; Komjathy, A.; Iijima, B. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Abdu, M. A.; Gonzalez, W. D.; Echer, E.] Natl Inst Space Res, BR-12201970 Sao Jose Dos Campos, SP, Brazil. [Anderson, D.] Univ Colorado, Space Environm Ctr, Cooperat Inst Res Environm Sci, Boulder, CO 80305 USA. [Crowley, G.] Atmospher & Space Technol Res Associates, San Antonio, TX 78249 USA. RP Mannucci, AJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 138-308, Pasadena, CA 91109 USA. EM tony.mannucci@jpl.nasa.gov NR 44 TC 42 Z9 42 U1 2 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUL 9 PY 2008 VL 113 AR A00A02 DI 10.1029/2007JA012732 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 327SB UT WOS:000257747700001 ER PT J AU Liu, WT Tang, WQ Xie, XS AF Liu, W. Timothy Tang, Wenqing Xie, Xiaosu TI Wind power distribution over the ocean SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SEA; CLIMATOLOGY; QUIKSCAT; SPEED; WATER AB Probability distribution and power density of wind speed over global oceans are computed from eight years of QuikSCAT measurements. They describe the variation and higher moments of wind speed that are critical in relating the non-linear effects of wind on electric power generation capability, shipping hazard, and air-sea exchanges in heat, water, and greenhouse gases. The power density distribution confirms our general knowledge of atmospheric circulation related to mid-latitude storm tracks, trade winds, and monsoons. It also reveals regions of high wind power associated with flow distortion by land, wind channeled by land topography, and buoyancy effect on turbulent stress driven by ocean fronts. C1 [Liu, W. Timothy; Tang, Wenqing; Xie, Xiaosu] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Liu, WT (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM w.timothy.liu@jpl.nasa.gov NR 21 TC 42 Z9 43 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 JUL 8 PY 2008 VL 35 IS 13 AR L13808 DI 10.1029/2008GL034172 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 327ON UT WOS:000257738500004 ER PT J AU Siskind, DE Marsh, DR Mlynczak, MG Martin-Torres, FJ Russell, JM AF Siskind, David E. Marsh, Daniel R. Mlynczak, Martin G. Martin-Torres, F. Javier Russell, James M., III TI Decreases in atomic hydrogen over the summer pole: Evidence for dehydration from polar mesospheric clouds? SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID WATER-VAPOR; DENSITIES; RATES AB Observations from the Sounding of the Atmosphere with Broadband Emission Radiometry (SABER) instrument on the NASA/Thermospheric Ionosphere Mesosphere Energetics and Dynamics satellite show a surprising decrease in the inferred atomic hydrogen (H) over the polar regions in the lowermost thermosphere during the summer. This contrasts with predictions by global models that H should peak in this region at this time. We suggest the decrease is a consequence of the sequestering of the water vapor by the formation of polar mesospheric clouds (PMCs) that redistributes the H2O thus reducing the chemical source of H. This decrease is more pronounced in the Northern rather than the Southern summer which is roughly consistent with the known morphology of PMCs. A model calculation which includes a PMC parameterization gives good qualitative agreement with the data suggesting that this process should be considered in global models of the coupling between the middle and upper atmosphere. C1 [Siskind, David E.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Marsh, Daniel R.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Mlynczak, Martin G.] NASA Langley Res, Hampton, VA 23681 USA. [Martin-Torres, F. Javier] AS&M Inc, Hampton, VA 23681 USA. [Russell, James M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. RP Siskind, DE (reprint author), USN, Res Lab, Div Space Sci, 4555 Overlook Ave SW, Washington, DC 20375 USA. EM david.siskind@nrl.navy.mil RI Marsh, Daniel/A-8406-2008; Mlynczak, Martin/K-3396-2012; Martin-Torres, Francisco Javier/G-6329-2015 OI Marsh, Daniel/0000-0001-6699-494X; Martin-Torres, Francisco Javier/0000-0001-6479-2236 NR 18 TC 4 Z9 4 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 8 PY 2008 VL 35 IS 13 AR L13809 DI 10.1029/2008GL033742 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 327ON UT WOS:000257738500001 ER PT J AU Sun, W Zhou, XY Du, A AF Sun, W. Zhou, X. -Y. Du, A. TI Quantitative separation of the directly-driven and unloading components of the ionospheric electric field SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MAGNETOSPHERIC SUBSTORMS AB It is well known that the ionospheric electric field turns to southward in the auroral zone midnight sector at a substorm expansion phase onset. This letter reports a study of quantitatively separating the southward electric field (Es) from the total electric field by using the Natural Orthogonal Components (NOC) algorithm. The Es will be regarded as an unloading component of substorms. The westward component of the electric filed (Ew) in the midnight sector, which is associated with two-cell convection, is identified as a directly driven component of substorms. Separated results for the event on April 18, 2002 are shown in the present study, which are characterized as a sawtooth event. It is found that the Es increased significantly to 30 40 mV/m during substorm expansion phases. Substorms may not develop if Es/Ew < 1 and Es < similar to 30 mV/m during the sawtooth event. C1 [Sun, W.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA. [Zhou, X. -Y.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Du, A.] Chinese Acad Sci, Inst Geol & Geophys, Beijing 100029, Peoples R China. RP Sun, W (reprint author), Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA. EM xiaoyan.zhou@jpl.nasa.gov NR 15 TC 6 Z9 6 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 8 PY 2008 VL 35 IS 13 AR L13104 DI 10.1029/2008GL033931 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 327ON UT WOS:000257738500003 ER PT J AU Suzuki, S Taguchi, S Hosokawa, K Collier, MR Moore, TE Frey, HU Mende, SB AF Suzuki, S. Taguchi, S. Hosokawa, K. Collier, M. R. Moore, T. E. Frey, H. U. Mende, S. B. TI Conjugate observations of ENA signals in the high-altitude cusp and proton auroral spot in the low-altitude cusp with IMAGE spacecraft SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MAGNETIC-FIELD; MAGNETOPAUSE; RECONNECTION; DYNAMICS; IMF AB On 28 April 2001, significant enhancements of neutral atom signals were detected in the direction of a high-altitude cusp by the Low-Energy Neutral Atom (LENA) imager onboard the Imager for Magnetopause-to-Aurora Global Exploration (IMAGE). Simultaneously, proton auroral emission was observed in the low-altitude cusp by the Far-Ultraviolet Instrument (FUV) on the IMAGE spacecraft. The temporal variations of their intensities showed a good correlation, suggesting they had a common source. During a brief period, the proton auroral spot moved antisunward and dawnward in conjunction with the motion of the ionospheric footprint of the LENA cusp signal. The Tsyganenko-96 model shows that the possible source location of the LENA cusp signals maps to the FUV spot. Considering the solar wind variations, we have attributed this "moving proton auroral spot'' to a moving flux tube that was created by transient reconnection on the dayside magnetopause and contained relatively high proton densities. C1 [Suzuki, S.] Univ Electrocommun, Sugadaira Space Radio Observ, Tokyo 1828585, Japan. [Taguchi, S.; Hosokawa, K.] Univ Electrocommun, Dept Informat & Commun Engn, Tokyo 1828585, Japan. [Collier, M. R.; Moore, T. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Frey, H. U.; Mende, S. B.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Suzuki, S (reprint author), Univ Electrocommun, Sugadaira Space Radio Observ, Tokyo 1828585, Japan. EM shin.s@ice.uec.ac.jp RI Moore, Thomas/D-4675-2012; Collier, Michael/I-4864-2013; OI Moore, Thomas/0000-0002-3150-1137; Collier, Michael/0000-0001-9658-6605; Frey, Harald/0000-0001-8955-3282 NR 17 TC 6 Z9 6 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 8 PY 2008 VL 35 IS 13 AR L13103 DI 10.1029/2008GL034543 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 327ON UT WOS:000257738500007 ER PT J AU Stubi, R Levrat, G Hoegger, B Viatte, P Staehelin, J Schmidlin, FJ AF Stuebi, Rene Levrat, Gilbert Hoegger, Bruno Viatte, Pierre Staehelin, Johannes Schmidlin, F. J. TI In-flight comparison of Brewer-Mast and electrochemical concentration cell ozonesondes SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID GROUND-BASED LIDAR; OZONE PROFILES; INTERCOMPARISON CAMPAIGN; STOIC 1989; TROPOSPHERIC OZONE; CATHODE SOLUTIONS; TRENDS; ECC; PHOTOMETER; PROGRAM AB The analysis of 140 dual flights between two types of ozonesondes, namely, the Brewer-Mast (BM) and the electrochemical concentration cell (ECC), is presented in this study. These dual flights were performed before the transition from BM to ECC as the operational ozonesonde for the Payerne Aerological Station, Switzerland. The different factors of the ozonesonde data processing are considered and their influences on the profile of the difference are evaluated. The analysis of the ozone difference between the BM and the ECC ozonesonde data shows good agreement between the two sonde types. The profile of the ozone difference is limited to +/- 5% (+/- 0.3 mPa) from the ground to 32 km. The analysis confirms the appropriateness of the standard BM data processing method and the usefulness of the normalization of the ozonesonde data. The conclusions of the extended dual flight campaigns are corroborated by the analysis of the time series of the Payerne soundings for the periods of 5 years before and after the change from BM to ECC which occurred in September 2002. No significant discontinuity can be identified in 2002 attributable to the change of sonde. C1 [Stuebi, Rene; Levrat, Gilbert; Hoegger, Bruno; Viatte, Pierre] MeteoSwiss, Payerne Aerol Stn, CH-1530 Payerne, Switzerland. [Schmidlin, F. J.] NASA, Goddard Space Flight Ctr, Wallops Isl, VA 23337 USA. [Staehelin, Johannes] ETH, Inst Atmospher & Climate Sci, CH-8092 Zurich, Switzerland. RP Stubi, R (reprint author), MeteoSwiss, Payerne Aerol Stn, CH-1530 Payerne, Switzerland. EM rene.stubi@meteoswiss.ch NR 52 TC 19 Z9 20 U1 2 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 8 PY 2008 VL 113 IS D13 AR D13302 DI 10.1029/2007JD009091 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 327PB UT WOS:000257739900001 ER PT J AU Lei, SL Palazzolo, A AF Lei, Shuliang Palazzolo, Alan TI Control of flexible rotor systems with active magnetic bearings SO JOURNAL OF SOUND AND VIBRATION LA English DT Article AB An approach is presented for the analysis and design of magnetic suspension systems with large flexible rotordynamics models including dynamics, control, and simulation. The objective is to formulate and synthesize a large-order, flexible shaft rotordynamics model for a flywheel supported with magnetic bearings. A finite element model of the rotor system is assembled and then employed to develop a magnetic suspension compensator to provide good reliability and disturbance rejection. Stable operation over the complete speed range and optimization of the closed-loop rotordynamic properties are obtained via synthesis of eigenvalue analysis, Campbell plots, waterfall plots, and mode shapes. The large order of the rotor model and high spin speed of the rotor present a challenge for magnetic suspension control. A flywheel system is studied as an example for realizing a physical controller that provides stable rotor suspension and good disturbance rejection in all operating states. The baseline flywheel system control is determined from extensive rotordynamics synthesis and analysis for rotor critical speeds, mode shapes, frequency responses, and time responses. (C) 2007 Elsevier Ltd. All rights reserved. C1 [Lei, Shuliang] Texas A&M Univ, NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Palazzolo, Alan] Texas A&M Univ, Dept Mech Engn, College Stn, TX 77843 USA. RP Lei, SL (reprint author), Texas A&M Univ, NASA, Glenn Res Ctr, MS 301-5, Cleveland, OH 44135 USA. EM slei26@gmail.com NR 13 TC 34 Z9 35 U1 3 U2 21 PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0022-460X J9 J SOUND VIB JI J. Sound Vibr. PD JUL 8 PY 2008 VL 314 IS 1-2 BP 19 EP 38 DI 10.1016/j.jsv.2007.12.028 PG 20 WC Acoustics; Engineering, Mechanical; Mechanics SC Acoustics; Engineering; Mechanics GA 305RI UT WOS:000256195100003 ER PT J AU Swartzlander, GA Ford, EL Abdul-Malik, RS Close, LM Peters, MA Palacios, DM Wilson, DW AF Swartzlander, Grover A., Jr. Ford, Erin L. Abdul-Malik, Rukiah S. Close, Laird M. Peters, Mary Anne Palacios, David M. Wilson, Daniel W. TI Astronomical demonstration of an optical vortex coronagraph SO OPTICS EXPRESS LA English DT Article ID ELECTRON-BEAM LITHOGRAPHY; PHASE-MASK CORONAGRAPH; LABORATORY DEMONSTRATION; PLANET; FILTER AB Using an optical vortex coronagraph and simple adaptive optics techniques, we have made the first convincing demonstration of an optical vortex coronagraph that is coupled to a star gazing telescope. We suppressed by 97% the primary star of a resolvable binary system, Cor Caroli. The stars had an angular separation of 1.9 lambda/D at our imaging camera. The secondary star suffered no suppression from the vortex lens. (C) 2008 Optical Society of America. C1 [Swartzlander, Grover A., Jr.; Ford, Erin L.; Abdul-Malik, Rukiah S.] Univ Arizona, Coll Opt Sci, Tucson, AZ 85721 USA. [Close, Laird M.; Peters, Mary Anne] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Palacios, David M.; Wilson, Daniel W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Swartzlander, GA (reprint author), Univ Arizona, Coll Opt Sci, Tucson, AZ 85721 USA. EM grover.swartzlander@gmail.com OI Swartzlander, Grover/0000-0003-3513-2225 NR 30 TC 57 Z9 58 U1 2 U2 9 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD JUL 7 PY 2008 VL 16 IS 14 BP 10200 EP 10207 DI 10.1364/OE.16.010200 PG 8 WC Optics SC Optics GA 325BV UT WOS:000257564100020 PM 18607427 ER PT J AU Garriques, S Shabanov, NV Swanson, K Morisette, JT Baret, F Myneni, RB AF Garriques, S. Shabanov, N. V. Swanson, K. Morisette, J. T. Baret, F. Myneni, R. B. TI Intercomparison and sensitivity analysis of Leaf Area Index retrievals from LAI-2000, AccuPAR, and digital hemispherical photography over croplands SO AGRICULTURAL AND FOREST METEOROLOGY LA English DT Article DE Effective Plant Area Index; gap fraction; optical techniques; LAI-2000; AccuPAR; Digital Hemispherical Photograph; LAI validation ID CLUMPED CANOPIES; BOREAL FORESTS; LAI; RADIATION; VEGETATION; PRODUCTS; TRANSMITTANCE; INSTRUMENTS; VALIDATION; ECOSYSTEMS AB Validation of Leaf Area Index (LAI) derived from moderate resolution remote sensing observations generally involves optical technique to measure ground LAI. As the current validation datasets are derived using multiple optical retrieval techniques, assessment of the consistency between these techniques is required. in this study the effective Plant Area Index (PAI(eff)) retrievals by three major optical instruments, LAI-2000, AccuPAR, and Digital Hemispherical Photographs (DHPs), were analyzed over 10 crops (soybean, com, alfalfa, sorghum, peanut and pasture) at Manfredi site in Cordoba province, Argentina. The focus of research was on quantifying PAI(eff) sensitivity to the type of instrument, retrieval parameters and gap fraction inversion methods as well as environmental conditions (canopy heterogeneity, senescent vegetation, illumination conditions). Results indicate that sensitivity of DHP method to illumination conditions is low (14% compared to 28% and 86% for LAI-2000 and AccuPAR, respectively). The intercomparison of PAI(eff) retrievals indicates large discrepancies between optical techniques for short canopy over which downward-pointing DHP technique performs better than LAI-2000 and AccuPAR. Better agreement was found for tall canopy without senescent vegetation and low spatial heterogeneity. Overall, discrepancies in PAI(eff) between instruments are mainly explained by differences in spatial sampling of transmittance between instruments (over short and heterogeneous canopies) caused by variations in instrument footprint, azimuthal range, and zenith angle spatial resolution (coarser for LAI-2000 than DHP). Our results indicate that DHP is the most robust technique in terms of low sensitivity to illumination conditions, accurate spatial sampling of transmittance, ability to capture gap fraction over short canopy using downward-looking photographs, independence from canopy optical ancillary information, and potential to derive clumping index. It can thus be applied to a large range of canopy structures, and environmental conditions as required by validation protocols. (C) 2008 Elsevier B.V. All rights reserved. C1 [Garriques, S.; Morisette, J. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Garriques, S.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Shabanov, N. V.; Swanson, K.; Myneni, R. B.] Boston Univ, Dept Geog, Boston, MA 02215 USA. [Baret, F.] EMMAH, UMR1114, INRA, F-84914 Avignon, France. RP Garriques, S (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 614-4, Greenbelt, MD 20771 USA. EM Sebastien.garrigues@gsfc.nasa.gov RI Myneni, Ranga/F-5129-2012; Baret, Fred/C-4135-2011 OI Baret, Fred/0000-0002-7655-8997 NR 44 TC 71 Z9 81 U1 6 U2 41 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-1923 EI 1873-2240 J9 AGR FOREST METEOROL JI Agric. For. Meteorol. PD JUL 4 PY 2008 VL 148 IS 8-9 BP 1193 EP 1209 DI 10.1016/j.agrformet.2008.02.014 PG 17 WC Agronomy; Forestry; Meteorology & Atmospheric Sciences SC Agriculture; Forestry; Meteorology & Atmospheric Sciences GA 333BW UT WOS:000258128000001 ER PT J AU Wang, Z Stephens, G Deshler, T Trepte, C Parish, T Vane, D Winker, D Liu, D Adhikari, L AF Wang, Zhien Stephens, Graeme Deshler, Terry Trepte, Charles Parish, Thomas Vane, Deborah Winker, Dave Liu, Dong Adhikari, Loknath TI Association of Antarctic polar stratospheric cloud formation on tropospheric cloud systems SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID OZONE DEPLETION; PARTICLES; AEROSOL; WAVES; LIDAR AB The formation of polar stratospheric clouds (PSCs) is critical to the development of polar ozone loss. However, the mechanisms of PSC formation remain poorly understood, which affects ozone loss models. Here, based on observations by the NASA A-train satellites, we show that 66% +/- 16% and 52% +/- 17% of PSCs over west and east Antarctica during the period June-October 2006 were associated with deep tropospheric cloud systems, with maximum depths exceeding 7 km. The development of such deep tropospheric cloud systems should cool the lower stratosphere through adiabatic and radiative processes, favoring PSC development. These deep systems also transport lower tropospheric air into the upper troposphere and lower stratosphere. These new findings suggest that Antarctic PSC formation is closely connected to tropospheric meteorology and thus governed by synoptic scale dynamics, local topography, and large-scale circulation. More dedicated studies are still needed to better understand Antarctic PSC formation. C1 [Wang, Zhien; Deshler, Terry; Parish, Thomas; Liu, Dong; Adhikari, Loknath] Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82072 USA. [Stephens, Graeme] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Trepte, Charles; Winker, Dave] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Vane, Deborah] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Wang, Z (reprint author), Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82072 USA. EM zwang@uwyo.edu RI Wang, Zhien/F-4857-2011 NR 21 TC 21 Z9 21 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 4 PY 2008 VL 35 IS 13 AR L13806 DI 10.1029/2008GL034209 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 323FO UT WOS:000257431000004 ER PT J AU Schaefer, M Baker, DJ Gibbons, JH Groat, CG Kennedy, D Kennel, CF Rejeski, D AF Schaefer, Mark Baker, D. James Gibbons, John H. Groat, Charles G. Kennedy, Donald Kennel, Charles F. Rejeski, David TI Science and government - An Earth Systems Science Agency SO SCIENCE LA English DT Editorial Material C1 [Schaefer, Mark; Groat, Charles G.] US Geol Survey, Reston, VA 20192 USA. [Baker, D. James] NOAA, Washington, DC USA. [Gibbons, John H.] White House Off Sci & Technol Policy, Washington, DC USA. [Kennedy, Donald] US FDA, Rockville, MD 20857 USA. [Kennel, Charles F.] NASA, Mission Planet Earth, Washington, DC 20546 USA. RP Schaefer, M (reprint author), US Geol Survey, Reston, VA 20192 USA. EM markschaefer24@msn.com; djamesbaker@comcast.net; jackgibbons@hughes.net; cgroat@mail.utexas.edu; kennedyd@stanford.edu; ckennel@ucsd.edu; david.rejeski@wilsoncenter.org RI Wright, Dawn/A-4518-2011 OI Wright, Dawn/0000-0002-2997-7611 NR 2 TC 3 Z9 3 U1 0 U2 2 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JUL 4 PY 2008 VL 321 IS 5885 BP 44 EP 45 DI 10.1126/science.1160192 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 321QE UT WOS:000257320800024 PM 18599760 ER PT J AU Solomon, SC McNutt, RL Watters, TR Lawrence, DJ Feldman, WC Head, JW Krimigis, SM Murchie, SL Phillips, RJ Slavin, JA Zuber, MT AF Solomon, Sean C. McNutt, Ralph L., Jr. Watters, Thomas R. Lawrence, David J. Feldman, William C. Head, James W. Krimigis, Stamatios M. Murchie, Scott L. Phillips, Roger J. Slavin, James A. Zuber, Maria T. TI Return to Mercury: A global perspective on MESSENGER's first mercury flyby SO SCIENCE LA English DT Article ID MAGNETIC-FIELD; SHELL; SPECTROMETER; SPACECRAFT; CORE AB In January 2008, the MErcury Surface, Space ENvironment, GEochemistry, and Ranging ( MESSENGER) spacecraft became the first probe to fly past the planet Mercury in 33 years. The encounter revealed that Mercury is a dynamic system; its liquid iron- rich outer core is coupled through a dominantly dipolar magnetic field to the surface, exosphere, and magnetosphere, all of which interact with the solar wind. MESSENGER images confirm that lobate scarps are the dominant tectonic landform and record global contraction associated with cooling of the planet. The history of contraction can be related to the history of volcanism and cratering, and the total contractional strain is at least one- third greater than inferred from Mariner 10 images. On the basis of measurements of thermal neutrons made during the flyby, the average abundance of iron in Mercury's surface material is less than 6% by weight. C1 [Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. [McNutt, Ralph L., Jr.; Lawrence, David J.; Krimigis, Stamatios M.; Murchie, Scott L.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Laurel, MD 20723 USA. [Watters, Thomas R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Feldman, William C.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Head, James W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Krimigis, Stamatios M.] Acad Athens, Athens 11527, Greece. [Phillips, Roger J.] SW Res Inst, Boulder, CO 80302 USA. [Slavin, James A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. RP Solomon, SC (reprint author), Carnegie Inst Washington, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. EM scs@dtm.ciw.edu RI McNutt, Ralph/E-8006-2010; Slavin, James/H-3170-2012; Murchie, Scott/E-8030-2015; Lawrence, David/E-7463-2015 OI McNutt, Ralph/0000-0002-4722-9166; Slavin, James/0000-0002-9206-724X; Murchie, Scott/0000-0002-1616-8751; Lawrence, David/0000-0002-7696-6667 NR 37 TC 102 Z9 103 U1 1 U2 13 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JUL 4 PY 2008 VL 321 IS 5885 BP 59 EP 62 DI 10.1126/science.1159706 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 321QE UT WOS:000257320800032 PM 18599768 ER PT J AU Zuber, MT Smith, DE Solomon, SC Phillips, RJ Peale, SJ Head, JW Hauck, SA McNutt, RL Oberst, J Neumann, GA Lemoine, FG Sun, XL Barnouin-Jha, O Harmon, JK AF Zuber, Maria T. Smith, David E. Solomon, Sean C. Phillips, Roger J. Peale, Stanton J. Head, James W., III Hauck, Steven A., II McNutt, Ralph L., Jr. Oberst, Juergen Neumann, Gregory A. Lemoine, Frank G. Sun, Xiaoli Barnouin-Jha, Olivier Harmon, John K. TI Laser altimeter observations from MESSENGER's first Mercury flyby SO SCIENCE LA English DT Article ID CORE AB A 3200- kilometers- long profile of Mercury by the Mercury Laser Altimeter on the MESSENGER spacecraft spans similar to 20% of the near- equatorial region of the planet. Topography along the profile is characterized by a 5.2- kilometer dynamic range and 930- meter root- mean- square roughness. At long wavelengths, topography slopes eastward by 0.02 degrees, implying a variation of equatorial shape that is at least partially compensated. Sampled craters on Mercury are shallower than their counterparts on the Moon, at least in part the result of Mercury's higher gravity. Crater floors vary in roughness and slope, implying complex modification over a range of length scales. C1 [Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Smith, David E.; Neumann, Gregory A.; Lemoine, Frank G.; Sun, Xiaoli] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. [Phillips, Roger J.] SW Res Inst, Boulder, CO 80302 USA. [Peale, Stanton J.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Head, James W., III] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Hauck, Steven A., II] Case Western Reserve Univ, Dept Geol Sci, Cleveland, OH 44106 USA. [McNutt, Ralph L., Jr.; Barnouin-Jha, Olivier] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Oberst, Juergen] DLR, Inst Planetary Res, D-12489 Berlin, Germany. [Harmon, John K.] Natl Astron & Ionosphere Ctr, Arecibo Observ, Arecibo, PR 00612 USA. RP Zuber, MT (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. EM zuber@mit.edu RI Hauck, Steven/A-7865-2008; Sun, Xiaoli/B-5120-2013; Lemoine, Frank/D-1215-2013; Neumann, Gregory/I-5591-2013; McNutt, Ralph/E-8006-2010; Barnouin, Olivier/I-7475-2015 OI Hauck, Steven/0000-0001-8245-146X; Neumann, Gregory/0000-0003-0644-9944; McNutt, Ralph/0000-0002-4722-9166; Barnouin, Olivier/0000-0002-3578-7750 NR 14 TC 33 Z9 33 U1 1 U2 6 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JUL 4 PY 2008 VL 321 IS 5885 BP 77 EP 79 DI 10.1126/science.1159086 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 321QE UT WOS:000257320800037 PM 18599773 ER PT J AU Anderson, BJ Acuna, MH Korth, H Purucker, ME Johnson, CL Slavin, JA Solomon, SC McNutt, RL AF Anderson, Brian J. Acuna, Mario H. Korth, Haje Purucker, Michael E. Johnson, Catherine L. Slavin, James A. Solomon, Sean C. McNutt, Ralph L., Jr. TI The structure of Mercury's magnetic field from MESSENGER's first flyby SO SCIENCE LA English DT Article ID ORIGIN AB During its first flyby of Mercury, the MESSENGER spacecraft measured the planet's near- equatorial magnetic field. The field strength is consistent to within an estimated uncertainty of 10% with that observed near the equator by Mariner 10. Centered dipole solutions yield a southward planetary moment of 230 to 290 nanotesla R-M(3) ( where R-M is Mercury's mean radius) tilted between 5 and 12 from the rotation axis. Multipole solutions yield non- dipolar contributions of 22% to 52% of the dipole field magnitude. Magnetopause and tail currents account for part of the high- order field, and plasma pressure effects may explain the remainder, so that a pure centered dipole cannot be ruled out. C1 [Anderson, Brian J.; Korth, Haje; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Acuna, Mario H.; Purucker, Michael E.] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Johnson, Catherine L.] Univ British Columbia, Dept Earth & Ocean Sci, Vancouver, BC V6T 1Z4, Canada. [Slavin, James A.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. RP Anderson, BJ (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM brian.anderson@jhuapl.edu RI Anderson, Brian/I-8615-2012; Slavin, James/H-3170-2012; McNutt, Ralph/E-8006-2010 OI Slavin, James/0000-0002-9206-724X; McNutt, Ralph/0000-0002-4722-9166 NR 22 TC 112 Z9 112 U1 0 U2 6 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 JUL 4 PY 2008 VL 321 IS 5885 BP 82 EP 85 DI 10.1126/science.1159081 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 321QE UT WOS:000257320800039 PM 18599775 ER PT J AU Slavin, JA Acuna, MH Anderson, BJ Baker, DN Benna, M Gloeckler, G Gold, RE Ho, GC Killen, RM Korth, H Krimigis, SM McNutt, RL Nittler, LR Raines, JM Schriver, D Solomon, SC Starr, RD Travnicek, P Zurbuchen, TH AF Slavin, James A. Acuna, Mario H. Anderson, Brian J. Baker, Daniel N. Benna, Mehdi Gloeckler, George Gold, Robert E. Ho, George C. Killen, Rosemary M. Korth, Haje Krimigis, Stamatios M. McNutt, Ralph L., Jr. Nittler, Larry R. Raines, Jim M. Schriver, David Solomon, Sean C. Starr, Richard D. Travnicek, Pavel Zurbuchen, Thomas H. TI Mercury's magnetosphere after MESSENGER's first flyby SO SCIENCE LA English DT Article ID SOLAR-WIND; GEOTAIL OBSERVATIONS; ULF WAVES; MAGNETOTAIL; SPECTROMETER; INSTRUMENT; SPACECRAFT; EARTH; MODEL; IONS AB Observations by MESSENGER show that Mercury's magnetosphere is immersed in a comet- like cloud of planetary ions. The most abundant, Na+, is broadly distributed but exhibits flux maxima in the magnetosheath, where the local plasma flow speed is high, and near the spacecraft's closest approach, where atmospheric density should peak. The magnetic field showed reconnection signatures in the form of flux transfer events, azimuthal rotations consistent with Kelvin- Helmholtz waves along the magnetopause, and extensive ultralow- frequency wave activity. Two outbound current sheet boundaries were observed, across which the magnetic field decreased in a manner suggestive of a double magnetopause. The separation of these current layers, comparable to the gyro- radius of a Na+ pickup ion entering the magnetosphere after being accelerated in the magnetosheath, may indicate a planetary ion boundary layer. C1 [Slavin, James A.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Acuna, Mario H.; Benna, Mehdi] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Anderson, Brian J.; Gold, Robert E.; Ho, George C.; Korth, Haje; Krimigis, Stamatios M.; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Baker, Daniel N.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA. [Gloeckler, George; Raines, Jim M.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Gloeckler, George; Killen, Rosemary M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Krimigis, Stamatios M.] Acad Athens, Athens 11527, Greece. [Nittler, Larry R.; Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Schriver, David] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [Starr, Richard D.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Travnicek, Pavel] Acad Sci Czech Republic, Inst Astron, CR-12023 Prague, Czech Republic. RP Slavin, JA (reprint author), NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM james.a.slavin@nasa.gov RI McNutt, Ralph/E-8006-2010; Anderson, Brian/I-8615-2012; Slavin, James/H-3170-2012; Travnicek, Pavel/G-8608-2014; Ho, George/G-3650-2015; Benna, Mehdi/F-3489-2012 OI McNutt, Ralph/0000-0002-4722-9166; Slavin, James/0000-0002-9206-724X; Ho, George/0000-0003-1093-2066; NR 28 TC 95 Z9 95 U1 1 U2 11 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 JUL 4 PY 2008 VL 321 IS 5885 BP 85 EP 89 DI 10.1126/science.1159040 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 321QE UT WOS:000257320800040 PM 18599776 ER PT J AU Zurbuchen, TH Raines, JM Gloeckler, G Krimigis, SM Slavin, JA Koehn, PL Killen, RM Sprague, AL McNutt, RL Solomon, SC AF Zurbuchen, Thomas H. Raines, Jim M. Gloeckler, George Krimigis, Stamatios M. Slavin, James A. Koehn, Patrick L. Killen, Rosemary M. Sprague, Ann L. McNutt, Ralph L., Jr. Solomon, Sean C. TI MESSENGER observations of the composition of Mercury's ionized exosphere and plasma environment SO SCIENCE LA English DT Article ID SOLAR-WIND; MAGNETOSPHERE; SPECTROMETER; MODEL AB The region around Mercury is filled with ions that originate from interactions of the solar wind with Mercury's space environment and through ionization of its exosphere. The MESSENGER spacecraft's observations of Mercury's ionized exosphere during its first flyby yielded Na(+), O(+), and K(+) abundances, consistent with expectations from observations of neutral species. There are increases in ions at a mass per charge (m/q) = 32 to 35, which we interpret to be S(+) and H(2)S(+), with ( S(+) + H(2)S(+))/( Na(+) + Mg(+)) = 0.67 +/- 0.06, and from water- group ions around m/ q = 18, at an abundance of 0.20 +/- 0.03 relative to Na(+) plus Mg(+). The fluxes of Na(+), O(+), and heavier ions are largest near the planet, but these Mercury- derived ions fill the magnetosphere. Doubly ionized ions originating from Mercury imply that electrons with energies less than 1 kiloelectron volt are substantially energized in Mercury's magnetosphere. C1 [Zurbuchen, Thomas H.; Raines, Jim M.; Gloeckler, George] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Krimigis, Stamatios M.; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Krimigis, Stamatios M.] Acad Athens, Astron & Appl Math Res Ctr, Athens 11527, Greece. [Slavin, James A.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Koehn, Patrick L.] Eastern Michigan Univ, Dept Phys & Astron, Ypsilanti, MI 48197 USA. [Killen, Rosemary M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Sprague, Ann L.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. RP Zurbuchen, TH (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, 2455 Hayward St, Ann Arbor, MI 48109 USA. EM thomasz@umich.edu RI Slavin, James/H-3170-2012; McNutt, Ralph/E-8006-2010 OI Slavin, James/0000-0002-9206-724X; McNutt, Ralph/0000-0002-4722-9166 NR 16 TC 80 Z9 80 U1 0 U2 2 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JUL 4 PY 2008 VL 321 IS 5885 BP 90 EP 92 DI 10.1126/science.1159314 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 321QE UT WOS:000257320800041 PM 18599777 ER PT J AU Pulkkinen, A Pirjola, R Viljanen, A AF Pulkkinen, A. Pirjola, R. Viljanen, A. TI Statistics of extreme geomagnetically induced current events SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID NATURAL-GAS PIPELINE; AURORAL ELECTROJET; SOLAR-WIND; FIELD; STORMS; EARTH; PROBABILITY; SYSTEMS; SURFACE AB [1] In this work, space weather events associated with extreme geoelectric field and geomagnetically induced current (GIC) magnitudes are investigated. The geoelectric field and consequent GIC are computed using geomagnetic field recordings over an extended time period and ground conductivity and technological system configurations favorable for large GIC. The statistics are derived for both overall occurrence of the geoelectric field and geoelectric field occurrence conditioned by the state of the magnetosphere and the solar wind. It is shown that in high-latitude areas having resistive ground conductivity structures and in systems having characteristics favorable for large GIC, GIC amplitudes of about 200 A can be expected to occur 10(2)-10(3) times (in 10-s values) per year while GIC of about 2000 A occur only 10-100 times in 100 years. On the basis of the Dst index and the solar wind electric field values derived by Siscoe et al. (2006) and Tsurutani et al. (2003), it is estimated by means of derived conditional probability distributions that although magnitudes of about 10 V/km are possible, the most probable value for the maximum magnitude of the geoelectric field during the Carrington event of 1-2 September 1859 is about 4 V/km. The usage of derived conditional probabilities in space weather applications is also discussed. C1 [Pulkkinen, A.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Pulkkinen, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Pirjola, R.; Viljanen, A.] Finnish Meteorol Inst, Geophys Res Div, FIN-00101 Helsinki, Finland. RP Pulkkinen, A (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. EM antti.a.pulkkinen@nasa.gov; risto.pirjola@fmi.fi; ari.viljanen@fmi.fi NR 43 TC 22 Z9 23 U1 0 U2 4 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 4 PY 2008 VL 6 IS 7 AR S07001 DI 10.1029/2008SW000388 PG 10 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 323GO UT WOS:000257434700001 ER PT J AU Chand, D Anderson, TL Wood, R Charlson, RJ Hu, Y Liu, Z Vaughan, M AF Chand, D. Anderson, T. L. Wood, R. Charlson, R. J. Hu, Y. Liu, Z. Vaughan, M. TI Quantifying above-cloud aerosol using spaceborne lidar for improved understanding of cloudy-sky direct climate forcing SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID WATER CLOUDS; ANTHROPOGENIC SULFATE; OPTICAL DEPTH; SAFARI 2000; BACKSCATTER; CAMPAIGN; MODEL; DEPOLARIZATION; EXTINCTION; SCATTERING AB [1] Estimates of global mean direct climate forcing by absorbing aerosols located above boundary layer clouds are large, uncertain, and almost entirely unconstrained by observations. Spaceborne lidar offers a new opportunity for global constraints. Here we examine techniques for using liquid water clouds as lidar targets, allowing aerosol optical depth and Angstrom exponent to be deduced directly from aerosol effects on light transmission. Two such techniques are examined using data from the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO). The first is a previously reported method based on measurements of cloud depolarization ratio (DR) at 532-nm wavelength. The second is a new method using measurements of cloud color ratio (CR), which is the ratio of the signal from the cloud at 1064 nm to that at 532 nm. Optical depth retrievals from these two methods compare favorably over the eastern tropical Atlantic Ocean during August 2006, when biomass burning aerosols are frequently advected over marine stratiform clouds. The CR technique is mainly sensitive to fine-mode aerosols and essentially insensitive to clouds and coarse-mode dust. Because anthropogenic aerosol is predominantly found in the fine mode, the CR technique can be used to help identify situations where anthropogenic cloudy-sky direct radiative forcing is occurring. We demonstrate this capability using 6 months data over the eastern tropical Atlantic Ocean. C1 [Chand, D.; Anderson, T. L.; Wood, R.; Charlson, R. J.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. [Hu, Y.; Vaughan, M.] NASA Langley Res Ctr, Hampton, VA 23681 USA. [Liu, Z.] Natl Inst Aerosp, Hampton, VA 23666 USA. RP Chand, D (reprint author), Univ Washington, Dept Atmospher Sci, Box 351640, Seattle, WA 98195 USA. EM duli@u.washington.edu; tadand@u.washington.edu; robwood2@u.washington.edu; bobwhan@comcast.net; yongxiang.hu-1@nasa.gov; zhaoyan.liu-1@nasa.gov; mark.a.vaughan@nasa.gov RI Liu, Zhaoyan/A-9604-2009; Liu, Zhaoyan/B-1783-2010; Wood, Robert/A-2989-2008; Hu, Yongxiang/K-4426-2012 OI Liu, Zhaoyan/0000-0003-4996-5738; Wood, Robert/0000-0002-1401-3828; NR 39 TC 45 Z9 46 U1 1 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 3 PY 2008 VL 113 IS D13 AR D13206 DI 10.1029/2007JD009433 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 323FU UT WOS:000257431800005 ER PT J AU Kinnison, DE Gille, J Barnett, J Randall, C Harvey, VL Lambert, A Khosravi, R Alexander, MJ Bernath, PF Boone, CD Cavanaugh, C Coffey, M Craig, C Dean, VC Eden, T Ellis, D Fahey, DW Francis, G Halvorson, C Hannigan, J Hartsough, C Hepplewhite, C Krinsky, C Lee, H Mankin, B Marcy, TP Massie, S Nardi, B Packman, D Popp, PJ Santee, ML Yudin, V Walker, KA AF Kinnison, D. E. Gille, J. Barnett, J. Randall, C. Harvey, V. L. Lambert, A. Khosravi, R. Alexander, M. J. Bernath, P. F. Boone, C. D. Cavanaugh, C. Coffey, M. Craig, C. Dean, V. C. Eden, T. Ellis, D. Fahey, D. W. Francis, G. Halvorson, C. Hannigan, J. Hartsough, C. Hepplewhite, C. Krinsky, C. Lee, H. Mankin, B. Marcy, T. P. Massie, S. Nardi, B. Packman, D. Popp, P. J. Santee, M. L. Yudin, V. Walker, K. A. TI Global observations of HNO3 from the High Resolution Dynamics Limb Sounder (HIRDLS): First results SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID POLAR STRATOSPHERIC CLOUDS; NITRIC-ACID; MASS-SPECTROMETER; OZONE DESTRUCTION; INFRARED MONITOR; UARS; AEROSOL; MLS; PARTICLES; DEPLETION AB We present the first evaluation of the HNO3 data product (version 2.04.09) from the High Resolution Dynamics Limb Sounder (HIRDLS) on the Earth Observing System (EOS) Aura satellite. The HIRDLS instrument obtains between 5000 and 7000 HNO3 profiles per day. HIRDLS HNO3 data are generally good over the latitude range of 64 degrees S to 80 degrees N and pressure range 100 to 10 hPa, with some profiles, depending on latitude, having useful information between 100 to 161 hPa. The individual profile "measured'' precision is between 10 and 15%, but can be much larger if the HNO3 abundance is low or outside the 100 hPa to 10 hPa range. Global results are compared with the HNO3 observations from version 2.2 of the EOS Aura Microwave Limb Sounder (MLS), and it is found that large-scale features are consistent between the two instruments. HIRDLS HNO3 is biased 0-20% low relative to Aura MLS in the mid-to-high latitudes and biased high in the tropical stratosphere. HIRDLS HNO3 is also compared with Atmospheric Chemistry Experiment Fourier Transform Spectrometer (ACE-FTS). In these mostly high-latitude comparisons the HIRDLS HNO3 data are biased 10-30% low, depending on altitude. Finally, the HIRDLS HNO3 is compared to in situ data taken by the NOAA Chemical Ionization Mass Spectrometer (CIMS) instrument flown during the 2005 NASA Houston Aura Validation Experiment (AVE) and the ability of HIRDLS to measure HNO3 in the UTLS region is examined. C1 [Kinnison, D. E.; Gille, J.; Khosravi, R.; Cavanaugh, C.; Coffey, M.; Craig, C.; Eden, T.; Francis, G.; Halvorson, C.; Hannigan, J.; Hartsough, C.; Mankin, B.; Massie, S.; Nardi, B.; Packman, D.; Yudin, V.] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80301 USA. [Gille, J.; Randall, C.; Dean, V. C.; Ellis, D.; Krinsky, C.] Univ Colorado, Boulder, CO 80309 USA. [Barnett, J.; Hepplewhite, C.] Univ Oxford, Ocean & Planetary Phys Dept, Oxford OX1 3PU, England. [Randall, C.; Harvey, V. L.] Atmospher & Space Phys Lab, Boulder, CO 80303 USA. [Lambert, A.; Santee, M. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Alexander, M. J.] NW Res Associates Inc, Boulder, CO 80301 USA. [Bernath, P. F.; Boone, C. D.; Walker, K. A.] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. [Bernath, P. F.] Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. [Fahey, D. W.; Marcy, T. P.; Popp, P. J.] Natl Ocean & Atmospher Adm, Earth Syst Res Lab, Div Chem Sci, Boulder, CO 80305 USA. [Marcy, T. P.; Popp, P. J.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Walker, K. A.] Univ Toronto, Dept Phys, Toronto, ON, Canada. RP Kinnison, DE (reprint author), Natl Ctr Atmospher Res, Div Atmospher Chem, 3450 Mitchell Lane, Boulder, CO 80301 USA. EM dkin@ucar.edu RI Bernath, Peter/B-6567-2012; Hartsough, Craig/K-5706-2015; Fahey, David/G-4499-2013; Randall, Cora/L-8760-2014; Manager, CSD Publications/B-2789-2015 OI Bernath, Peter/0000-0002-1255-396X; Fahey, David/0000-0003-1720-0634; Randall, Cora/0000-0002-4313-4397; NR 62 TC 13 Z9 13 U1 2 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 3 PY 2008 VL 113 IS D16 AR D16S44 DI 10.1029/2007JD008814 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 323FW UT WOS:000257432100001 ER PT J AU Rudich, Y Kaufman, YJ Dayan, U Yu, H Kleidman, RG AF Rudich, Y. Kaufman, Y. J. Dayan, U. Yu, Hongbin Kleidman, R. G. TI Estimation of transboundary transport of pollution aerosols by remote sensing in the eastern Mediterranean SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID ATMOSPHERIC SULFUR; GOCART MODEL; SATELLITE MEASUREMENTS; VERTICAL-DISTRIBUTION; OPTICAL-THICKNESS; SYNOPTIC ANALYSIS; AIR-POLLUTION; SAHARAN DUST; ISRAEL; MODIS AB [1] Quantifying transboundary transport of pollution is important for understanding the global distribution of pollution and pollutant burdens in regional and global scales. Using observations from the Moderate resolution Imaging Spectroradiometer ( MODIS) on board the Terra and Aqua satellites, the transport of pollution sulfate aerosol was estimated in the eastern Mediterranean. Over a 150 km line west of the Israeli coast, the estimated annual sulfate flux is in a range of 0.025 to 0.062 Tg S a(-1). These estimates are consistent with airborne measurements which estimated an annual flux of sulfate of 0.024-0.054 TgS a(-1). The MODIS-based estimates are also in good agreement with estimates of seasonal and annual fluxes from the GOCART model. This case study demonstrates a feasible way to estimate transboundary transport of pollution aerosol by remote sensing means. C1 [Rudich, Y.] Weizmann Inst Sci, Dept Environm Sci, IL-76100 Rehovot, Israel. [Dayan, U.] Hebrew Univ Jerusalem, Dept Geog, IL-91905 Jerusalem, Israel. [Kleidman, R. G.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Yu, Hongbin] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Kaufman, Y. J.; Yu, Hongbin; Kleidman, R. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Rudich, Y (reprint author), Weizmann Inst Sci, Dept Environm Sci, IL-76100 Rehovot, Israel. EM yinon@wisemail.weizmann.ac.il RI Yu, Hongbin/C-6485-2008; Rudich, Yinon/K-1498-2012; Dayan, Uri/D-4855-2014; OI Yu, Hongbin/0000-0003-4706-1575; Dayan, Uri/0000-0002-1336-1441; Rudich, Yinon/0000-0003-3149-0201 NR 51 TC 14 Z9 14 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 3 PY 2008 VL 113 IS D14 AR D14S13 DI 10.1029/2007JD009601 PG 8 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 323FV UT WOS:000257431900001 ER PT J AU Zahnle, K AF Zahnle, Kevin TI Atmospheric chemistry - Her dark materials SO NATURE LA English DT Editorial Material ID MULTIPLE SULFUR ISOTOPES; SEDIMENTS; SULFATE; OXYGEN C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Zahnle, K (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM kevin.j.zahnle@nasa.gov NR 11 TC 2 Z9 2 U1 0 U2 0 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JUL 3 PY 2008 VL 454 IS 7200 BP 41 EP 42 DI 10.1038/454041a PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 321MC UT WOS:000257308300029 PM 18596795 ER PT J AU Stone, EC Cummings, AC McDonald, FB Heikkila, BC Lal, N Webber, WR AF Stone, Edward C. Cummings, Alan C. McDonald, Frank B. Heikkila, Bryant C. Lal, Nand Webber, William R. TI An asymmetric solar wind termination shock SO NATURE LA English DT Article ID INTERSTELLAR MAGNETIC-FIELD; ENERGETIC PARTICLES; VOYAGER-1; ACCELERATION; HELIOSHEATH; HELIOSPHERE; ANISOTROPIES; INTENSITIES; SPACECRAFT; UPSTREAM AB Voyager 2 crossed the solar wind termination shock at 83.7 AU in the southern hemisphere, 10 AU closer to the Sun than found by Voyager 1 in the north(1-4). This asymmetry could indicate an asymmetric pressure from an interstellar magnetic field(5,6), from transient-induced shock motion(7), or from the solar wind dynamic pressure. Here we report that the intensity of 4 - 5 MeV protons accelerated by the shock near Voyager 2 was three times that observed concurrently by Voyager 1, indicating differences in the shock at the two locations. ( Companion papers report on the plasma(8), magnetic field(9), plasma- wave(10) and lower energy particle(11) observations at the shock.) Voyager 2 did not find the source of anomalous cosmic rays at the shock, suggesting that the source is elsewhere on the shock(12-14) or in the heliosheath(15-19). The small intensity gradient of Galactic cosmic ray helium indicates that either the gradient is further out in the heliosheath(20) or the local interstellar Galactic cosmic ray intensity is lower than expected(21). C1 [Stone, Edward C.; Cummings, Alan C.] CALTECH, Pasadena, CA 91125 USA. [McDonald, Frank B.] Univ Maryland, Inst Phys Sci & Technol, College Pk, MD 20742 USA. [Heikkila, Bryant C.; Lal, Nand] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Webber, William R.] 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 26 TC 233 Z9 233 U1 0 U2 4 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD JUL 3 PY 2008 VL 454 IS 7200 BP 71 EP 74 DI 10.1038/nature07022 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 321MC UT WOS:000257308300037 PM 18596802 ER PT J AU Burlaga, LF Ness, NF Acuna, MH Lepping, RP Connerney, JEP Richardson, JD AF Burlaga, L. F. Ness, N. F. Acuna, M. H. Lepping, R. P. Connerney, J. E. P. Richardson, J. D. TI Magnetic fields at the solar wind termination shock SO NATURE LA English DT Article ID COLLISIONLESS-SHOCK; PERPENDICULAR SHOCKS; VOYAGER-1; PLASMA; HELIOSHEATH; WAVES; IONS AB A transition between the supersonic solar wind and the subsonic heliosheath was observed by Voyager 1, but the expected termination shock was not seen owing to a gap in the telemetry(1-4). Here we report observations of the magnetic field structure and dynamics of the termination shock, made by Voyager 2 on 31 August - 1 September 2007 at a distance of 83.7 AU from the Sun ( 1 AU is the Earth - Sun distance). A single crossing of the shock was expected, with a boundary that was stable on a timescale of several days. But the data reveal a complex, rippled, quasi- perpendicular supercritical magnetohydrodynamic shock of moderate strength undergoing reformation on a scale of a few hours. The observed structure suggests the importance of ionized interstellar atoms shock. C1 [Burlaga, L. F.; Acuna, M. H.; Lepping, R. P.; Connerney, J. E. P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ness, N. F.] Catholic Univ Amer, Washington, DC 20064 USA. [Richardson, J. D.] MIT, Cambridge, MA 02139 USA. RP Burlaga, LF (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Leonard.F.Burlaga@nasa.gov RI connerney, john/I-5127-2013; OI connerney, jack/0000-0001-7478-6462 NR 23 TC 135 Z9 135 U1 0 U2 3 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JUL 3 PY 2008 VL 454 IS 7200 BP 75 EP 77 DI 10.1038/nature07029 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 321MC UT WOS:000257308300038 PM 18596803 ER PT J AU Huang, D Liu, YG Wiscombe, W AF Huang, Dong Liu, Yangang Wiscombe, Warren TI Determination of cloud liquid water distribution using 3D cloud tomography SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID LIMITED ANGLE TOMOGRAPHY; ILL-POSED PROBLEMS; COMPUTED-TOMOGRAPHY; MICROWAVE RADIOMETER; TEMPERATURE; INVERSION; RETRIEVAL; SYSTEM; VAPOR; MODEL AB The cloud microwave tomography method for remotely retrieving 3D distributions of cloud Liquid Water Content (LWC) was originally proposed by Warner et al. in the 1980s but has lain dormant since then. This paper revisits and extends the cloud tomography method by rigorously examining the nature of the resultant mathematical problem and its close relationship to the physical configuration of microwave radiometers. The singular value decomposition (SVD) analysis reveals that the retrieval of cloud LWC fields from microwave emission is highly ill-posed, and requires special techniques to solve it. The truncated SVD approach along with the L-curve method for choosing the optimal truncating point is used to obtain a better retrieval of cloud LWC. A group of sensitivity studies show that the retrieval accuracy is determined by several factors, including the number of radiometers, the spatial resolution of output, the number of scanning angles, the radiometer characteristics (e. g., noise level, beam width), the physical arrangement of radiometers, and the uncertainty in the ancillary temperature and water vapor mixing ratio data. When more radiometers and/or more scanning angles are used, and/or the radiometer beam width is reduced, and/or when a coarser output resolution is acceptable, the retrieval problem becomes less ill-posed, and a better retrieval can be obtained. Moreover, the observation system simulations demonstrate that the cloud tomography method is able to retrieve the cloud structures generated by cloud resolving models with a good accuracy. For a setup consisting of four microwave radiometers of typical noise level 0.3 K, the tomography method is capable of retrieving the LWC to within 5% of the maximum LWC in the simulated stratocumulus and broken cumulus cases, with a spatial resolution of a few hundred meters. C1 [Huang, Dong; Liu, Yangang; Wiscombe, Warren] Brookhaven Natl Lab, Dept Environm Sci, Upton, NY 11973 USA. [Wiscombe, Warren] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Huang, D (reprint author), Brookhaven Natl Lab, Dept Environm Sci, 75 Rutherford Dr, Upton, NY 11973 USA. EM dhuang@bnl.gov RI Liu, Yangang/H-6154-2011; Wiscombe, Warren/D-4665-2012; Huang, Dong/H-7318-2014 OI Wiscombe, Warren/0000-0001-6844-9849; Huang, Dong/0000-0001-9715-6922 NR 29 TC 14 Z9 16 U1 1 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 2 PY 2008 VL 113 IS D13 AR D13201 DI 10.1029/2007JD009133 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 323FS UT WOS:000257431600001 ER PT J AU Jules, K AF Jules, Kenol TI Summary of the science performed onboard the International Space Station during increments 12 and 13 SO ACTA ASTRONAUTICA LA English DT Article; Proceedings Paper CT 58th International Astronautical Congress CY SEP 24-28, 2007 CL Hyderabad, INDIA AB The objectives of this paper are four-fold: (1) to briefly review the science conducted on the International Space Station during the previous 15 increments; (2) to compare the original science complement plan for increments 12 and 13 with the on-orbit science accomplishment to illustrate the challenges of performing daily science activity on a space platform that is being built and continuously staffed; (3) to discuss the investigations that were conducted on the station during increments 12 and 13 (the discussion will focus mainly on the primary objectives of each investigation and their associated hypotheses that were investigated during these two increments. Also, some preliminary science results will be discussed for each of the investigations as science results availability permit); (4) to briefly discuss the science research complements that are being planned for increments 16 and 17. Published by Elsevier Ltd. C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Jules, K (reprint author), NASA, Lyndon B Johnson Space Ctr, Mail Code OZ-4,2101 NASA Pkwy, Houston, TX 77058 USA. EM Kenol.jules-1@nasa.gov NR 20 TC 4 Z9 4 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JUL-AUG PY 2008 VL 63 IS 1-4 BP 38 EP 52 DI 10.1016/j.actaastro.2007.12.063 PG 15 WC Engineering, Aerospace SC Engineering GA 325KO UT WOS:000257588000007 ER PT J AU Mitchell, RT AF Mitchell, Robert T. TI The Cassini Mission exploring Saturn SO ACTA ASTRONAUTICA LA English DT Article; Proceedings Paper CT 58th International Astronautical Congress CY SEP 24-28, 2007 CL Hyderabad, INDIA AB The Cassini Mission, an international collaborative effort between the United States and Europe to conduct an in-depth exploration of the Saturnian system, is now entering the fourth and final year of its prime mission in orbit at Saturn. The performance of the spacecraft and its 12 scientific instruments continues to be excellent, and new scientific discoveries continue to be made. This paper summarizes the activities and significant new science results of the mission over the past year. Based on the performance of the mission and resources remaining on the spacecraft, NASA and Europe are considering a two-year extension of the mission with the same rate of satellite encounters and science data acquisition as in the prime mission. A description of the plans and new science data collection opportunities for a proposed two-year mission extension is included in this paper. (C) 2008 Published by Elsevier Ltd. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Mitchell, RT (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM robert.t.mitchell@jpl.nasa.gov NR 1 TC 1 Z9 1 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JUL-AUG PY 2008 VL 63 IS 1-4 BP 61 EP 67 DI 10.1016/j.actaastro.2007.12.064 PG 7 WC Engineering, Aerospace SC Engineering GA 325KO UT WOS:000257588000009 ER PT J AU Johnson, NL Stansbery, E Liou, JC Horstman, M Stokely, C Whitlock, D AF Johnson, Nicholas L. Stansbery, E. Liou, J. -C. Horstman, M. Stokely, C. Whitlock, D. TI The characteristics and consequences of the break-up of the Fengyun-1C spacecraft SO ACTA ASTRONAUTICA LA English DT Article; Proceedings Paper CT 58th International Astronautical Congress CY SEP 24-28, 2007 CL Hyderabad, INDIA AB The intentional break-up of the Fengyun-1C spacecraft on 11 January 2007 via a hypervelocity collision with a ballistic object created the most severe artificial debris cloud in Earth orbit since the beginning of space exploration. More than 2000 debris of the order of 10cm or greater in size have been identified by the US Space Surveillance Network. The majority of these debris reside in long-lived orbits. The NASA Orbital Debris Program Office has conducted a thorough examination of the nature of the Fengyun-1C debris cloud, using Space Surveillance Network (SSN) data for larger debris and special Haystack radar observations for smaller debris. These data have been compared with the NASA standard satellite break-up model for collisions, and the results are presented in this paper. The orbital longevity of the debris have also been evaluated for both small and large debris. The consequent long-term spatial density effects on the low Earth orbit regime and the potential effect of the debris cloud on the growth of the near-Earth satellite population have been addressed. Published by Elsevier Ltd. C1 [Johnson, Nicholas L.; Stansbery, E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Liou, J. -C.; Horstman, M.] ERC, ESCG, Houston, TX USA. [Stokely, C.] Barrios Technol, ESCG, Houston, TX USA. [Whitlock, D.] Hamilton Sundstrand, ESCG, Houston, TX USA. RP Johnson, NL (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM nicholas.l.johnson@nasa.gov; eugene.g.stansbery@nasa.gov; jer-chyi.liou-1@nasa.gov; matt.horstman-1@nasa.gov; christopher.1.stokely@nasa.gov; david.o.whitlock@nasa.gov NR 8 TC 10 Z9 10 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JUL-AUG PY 2008 VL 63 IS 1-4 BP 128 EP 135 DI 10.1016/j.actaastro.2007.12.044 PG 8 WC Engineering, Aerospace SC Engineering GA 325KO UT WOS:000257588000016 ER PT J AU Stone, D Lindenmoyer, A French, G Musk, E Gump, D Kathuria, C Miller, C Sirangelo, M Pickens, T AF Stone, Dennis Lindenmoyer, Alan French, George Musk, Elon Gump, David Kathuria, Chirinjeev Miller, Charles Sirangelo, Mark Pickens, Tom TI NASA's approach to commercial cargo and crew transportation SO ACTA ASTRONAUTICA LA English DT Article; Proceedings Paper CT 58th International Astronautical Congress CY SEP 24-28, 2007 CL Hyderabad, INDIA AB To stimulate the commercial space industry and potentially serve the logistics needs of the International Space Station (ISS) in the post-Space Shuttle era, the National Aeronautics and Space Administration (NASA) in 2006 began the Commercial Orbital Transportation Services (COTS) initiative. NASA entered into agreements with two U.S. firms, Rocketplane Kistler and Space Exploration Technologies to share up to 485,000,000 USD to demonstrate cargo transportation services to and from Low Earth orbit (LEO), with an option for additional funds to demonstrate human transportation services. Subsequently, NASA also entered into unfunded agreements with five companies to develop innovative space transportation capabilities. This paper reviews this unique initiative, describes the concepts of these seven companies, and discusses the potential of this emerging industry to make LEO more accessible. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Stone, Dennis; Lindenmoyer, Alan] NASA, Commercial Crew & Cargo Program Off, Washington, DC 20546 USA. RP Stone, D (reprint author), NASA, Commercial Crew & Cargo Program Off, Washington, DC 20546 USA. EM dennis.a.stone@nasa.gov; alan.j.lindenmoyer@nasa.gov; gfrench28@aol.com; elon@spacex.com; david.gump@transformspace.com; drkathuria@yahoo.com; cmiller@constellationservices.com; mark.sirangelo@spacedev.com; TPickens@spacehab.com NR 1 TC 7 Z9 7 U1 1 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JUL-AUG PY 2008 VL 63 IS 1-4 BP 192 EP 197 DI 10.1016/j.actaastro.2007.12.004 PG 6 WC Engineering, Aerospace SC Engineering GA 325KO UT WOS:000257588000023 ER PT J AU Korsmeyer, DJ Landis, RR Abell, PA AF Korsmeyer, David J. Landis, Rob R. Abell, Paul A. TI Into the beyond: A crewed mission to a near-Earth object SO ACTA ASTRONAUTICA LA English DT Article; Proceedings Paper CT 58th International Astronautical Congress CY SEP 24-28, 2007 CL Hyderabad, INDIA AB Aside from the exploration of Mars, the objects that most capture our interest for a new human visit are the near-Earth objects (NEOs). These objects are ideal candidates for deep-space operations and explorations as we extend the human presence out into the solar system. The notion of a crewed mission to a NEO was first discussed in the Apollo era. The most recent assessment has been undertaken by the Advanced Projects Office within NASA's Constellation Program. This particular study examined the feasibility of sending NASA's new Orion spacecraft (also referred to as the crew exploration vehicle, or CEV) to a NEO. Depending on the specifications of spacecraft and integrated components, a mission profile would include two or three astronauts on a 90- to 180-day spaceflight; including a 7- to 14-day stay at the NEO itself. These missions to NEOs provide exploration with an excellent suite of benefits: operational experience beyond cislunar space, risk reduction for space hardware, confidence building for future mission scenarios, in situ resource utilization evaluation, as well as a rich scientific return. This incremental step along the way towards Mars would mark humanity's first foray beyond the Earth-Moon system. (C) 2008 Published by Elsevier Ltd. C1 [Korsmeyer, David J.] NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA. [Landis, Rob R.] NASA, Lyndon B Johnson Space Ctr, Mission Operat Directorate, Houston, TX 77058 USA. [Abell, Paul A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Korsmeyer, DJ (reprint author), NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA. EM David.J.Korsmeyer@nasa.gov; Rob.R.Landis@nasa.gov; Paul.A.Abell@nasa.gov NR 9 TC 9 Z9 10 U1 1 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JUL-AUG PY 2008 VL 63 IS 1-4 BP 213 EP 220 DI 10.1016/j.actaastro.2007.12.014 PG 8 WC Engineering, Aerospace SC Engineering GA 325KO UT WOS:000257588000026 ER PT J AU Balint, TS Kolawa, EA Cutts, JA Peterson, CE AF Balint, Tibor S. Kolawa, Elizabeth A. Cutts, James A. Peterson, Craig E. TI Extreme environment technologies for NASA's robotic planetary exploration SO ACTA ASTRONAUTICA LA English DT Article; Proceedings Paper CT 58th International Astronautical Congress CY SEP 24-28, 2007 CL Hyderabad, INDIA AB NASA's 2006 Solar System Exploration Roadmap recommended a set of robotic exploration missions for the next 30 years, in small, medium and large mission classes. These proposed missions are expected to target planets, moons and small bodies in the Solar System, while encountering diverse extreme environmental conditions through their mission phases. These extreme environments (EE) include high and low temperatures and pressures, and high radiation environments at various planetary destinations. EE conditions are often coupled, including high temperatures and pressures near the surface of Venus or low temperatures and radiation at the Jovian System, for instance near Europa. Extreme environments due to mission operations are also a consideration, for example aeroshell thermal heating during planetary entry. While some of the technologies for EE mitigation are currently available, development of numerous new technologies are also required to enable missions and thus NASA's exploration plans. In response, a comprehensive assessment was performed to identify the state of practice for EE technologies. Furthermore, recommendations were given for future technology developments. In this paper we outline the findings of the EE Technologies Study Team, including discussions on the state of practice of EE technologies; mission impacts; and emerging technology capabilities to enable mission architectures. Under emerging technologies we describe protection systems; component hardening for electronics, mechanisms and energy storage under high and low temperature conditions; and mobility operations. It is expected that the recommendations from the EE report would assist NASA with technology program planning and would help identifying priorities for near term technology investments. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Balint, Tibor S.; Kolawa, Elizabeth A.; Cutts, James A.; Peterson, Craig E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Balint, TS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 301-170U, Pasadena, CA 91109 USA. EM tibor.balint@jpl.nasa.gov NR 4 TC 6 Z9 6 U1 1 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JUL-AUG PY 2008 VL 63 IS 1-4 BP 285 EP 298 DI 10.1016/j.actaastro.2007.12.009 PG 14 WC Engineering, Aerospace SC Engineering GA 325KO UT WOS:000257588000033 ER PT J AU Krishen, K AF Krishen, Kumar TI New technology innovations with potential for space applications SO ACTA ASTRONAUTICA LA English DT Article; Proceedings Paper CT 58th International Astronautical Congress CY SEP 24-28, 2007 CL Hyderabad, INDIA ID ARTIFICIAL MUSCLES; BIOMIMETIC SENSORS; RESOLUTION; ACTUATORS AB Human exploration and development of space is being pursued by spacefaring nations to explore, use, and enable the development of space and expand the human experience there. The goals include: increasing human knowledge of nature's processes using the space environment; exploring and settling the solar system; achieving routine space travel; and enriching life on Earth through living and working in space. A crucial aspect of future space missions is the development of infrastructure to optimize safety, productivity, and costs. A major component of mission execution is operations management. NASA's International Space Station is providing extensive experience in both infrastructure and operations. In view of this, a vigorously organized approach is needed to implement successful space-, planet-, and ground-based research and operations that entails wise and efficient use of technical and human resources. Many revolutionary technologies being pursued by researchers and technologists may be vital in making space missions safe, reliable, cost-effective, and productive. These include: ionic polymer-metal composite technology; solid-state lasers; time-domain sensors and communication systems; high-temperature superconductivity; nanotechnology; variable specific impulse magneto plasma rocket; fuzzy logic; wavelet technology; and neural networks. An overview of some of these will be presented, along with their application to space missions. (C) 2008 Elsevier Ltd. All rights reserved. C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Krishen, K (reprint author), NASA, Lyndon B Johnson Space Ctr, 2102 Nasa Pkwy, Houston, TX 77058 USA. EM kumar.krishen-1@nasa.gov RI Yin, Yimei/G-7749-2012 NR 32 TC 7 Z9 8 U1 1 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JUL-AUG PY 2008 VL 63 IS 1-4 BP 324 EP 333 DI 10.1016/j.actaastro.2007.12.047 PG 10 WC Engineering, Aerospace SC Engineering GA 325KO UT WOS:000257588000036 ER PT J AU Greenblatt, D Washburn, AE AF Greenblatt, David Washburn, Anthony E. TI Influence of finite span and sweep on active flow control efficacy SO AIAA JOURNAL LA English DT Article; Proceedings Paper CT AIAA 25th Applied Aerodynamics Conference CY JUN 25-28, 2007 CL Miami, FL SP Amer Inst Aeronaut & Astronaut ID DYNAMIC STALL CONTROL; PERIODIC EXCITATION; SEPARATION CONTROL; PART 2; VORTICES; VORTEX AB Active flow control efficacy was investigated by means of leading-edge and flap-shoulder zero mass-flux blowing slots on a semispan wing model that was tested in unswept (standard) and swept configurations. On the standard configuration, the stall commenced inboard; with sweep, the wing stalled initially near the tip. On both configurations, the leading-edge perturbations increased the C-L,C-max and the poststall lift, both with and without deflected flaps. Without sweep, the effect of control was approximately uniform across the wing span, but remained effective to high angles of attack near the tip; when sweep was introduced, a significant effect was noted inboard, but this effect degraded along the span and produced virtually no meaningful lift enhancement near the tip, irrespective of the tip configuration. In the former case, control strengthened the wing tip vortex; in the latter case, a simple semi-empirical model, based on the trajectory or streamline of the evolving perturbation, served to explain the observations. In the absence of sweep, control on finite-span flaps did not differ significantly from their nominally two-dimensional counterpart. Control from the flap produced the expected lift enhancement and C-L,C-max improvements in the absence of sweep, but these improvements degraded with the introduction of sweep. C1 [Greenblatt, David] Technion Israel Inst Technol, Fac Mech Engn, IL-32000 Haifa, Israel. [Washburn, Anthony E.] NASA, Langley Res Ctr, Flow Phys & Control Branch, Hampton, VA 23681 USA. RP Greenblatt, D (reprint author), Technion Israel Inst Technol, Fac Mech Engn, IL-32000 Haifa, Israel. EM davidg@technion.ac.il; Washburn@nasa.gov NR 39 TC 11 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 0001-1452 J9 AIAA J JI AIAA J. PD JUL PY 2008 VL 46 IS 7 BP 1675 EP 1694 DI 10.2514/1.33809 PG 20 WC Engineering, Aerospace SC Engineering GA 321VO UT WOS:000257334800011 ER PT J AU Kota, AK Murphy, L Strohmer, T Bigio, DI Bruck, HA Powell, D AF Kota, Arun K. Murphy, Larry Strohmer, Timo Bigio, David I. Bruck, Hugh A. Powell, Dan TI Combinatorial development of polymer nanocomposites using transient processing conditions in twin screw extrusion SO AICHE JOURNAL LA English DT Article DE composite materials; polymer processing; mathematical modeling; nanotechnology; polymer properties ID RESIDENCE-TIME DISTRIBUTION; MATERIALS SCIENCE; MATERIALS DISCOVERY; CARBON NANOTUBES; EXTRUDERS; DISTRIBUTIONS; FABRICATION; COMPOSITES AB A new approach is presented for combinatorial development of polymer nanocomposites with compositional gradients (CGs). The CGs were developed using transient processing conditions in twin screw extrusion with small quantities of expensive nanoscale fillers. Convolution of step input with normalized residence volume distributions (RVDs) was used to establish the processing-structure relationship for the CGs. The normalized RVD was established as a process characteristic independent of processing conditions and measured in situ using an optical probe. The CG determined nondestructively using the new combinatorial approach was validated through comparison with more time-consuming and destructive thermogravimetric analysis. The CG could also be established with relatively inexpensive microscale fillers using the normalized RVD obtained with nanoscale fillers, suggesting that transient effects of the mixing process are independent of the size of the filler. Finally, structure-property relationship of combinatorially developed polymer nanocomposites was established by characterizing their dynamic mechanical behavior (storage modulus, G', and loss modulus, G ''). The dynamic mechanical behavior of the combinatorially developed composites correlated well with the batch-processed ones, indicating that the transient mixing conditions in extrusion do not affect the material properties. (C) 2008 American Institute of Chemical Engineers. C1 [Kota, Arun K.; Murphy, Larry; Strohmer, Timo; Bigio, David I.; Bruck, Hugh A.] Univ Maryland, Dept Mech Engn, College Pk, MD 20742 USA. [Powell, Dan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Bruck, HA (reprint author), Univ Maryland, Dept Mech Engn, College Pk, MD 20742 USA. EM bruck@umd.edu NR 33 TC 3 Z9 3 U1 0 U2 5 PU JOHN WILEY & SONS INC PI HOBOKEN PA 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0001-1541 J9 AICHE J JI AICHE J. PD JUL PY 2008 VL 54 IS 7 BP 1895 EP 1900 DI 10.1002/aic.11505 PG 6 WC Engineering, Chemical SC Engineering GA 317SO UT WOS:000257040300018 ER PT J AU Whitney, BA Sewilo, M Indebetouw, R Robitaille, TP Meixner, M Gordon, K Meade, MR Babler, BL Harris, J Hora, JL Bracker, S Povich, MS Churchwell, EB Engelbracht, CW For, BQ Block, M Misselt, K Vijh, U Leitherer, C Kawamura, A Blum, RD Cohen, M Fukui, Y Mizuno, A Mizuno, N Srinivasan, S Tielens, AGGM Volk, K Bernard, JP Boulanger, F Frogel, JA Gallagher, J Gorjian, V Kelly, D Latter, WB Madden, S Kemper, F Mould, JR Nota, A Oey, MS Olsen, KA Onishi, T Paladini, R Panagia, N Perez-Gonzalez, P Reach, W Shibai, H Sato, S Smith, LJ Staveley-Smith, L Ueta, T Van Dyk, S Werner, M Wolff, M Zaritsky, D AF Whitney, B. A. Sewilo, M. Indebetouw, R. Robitaille, T. P. Meixner, M. Gordon, K. Meade, M. R. Babler, B. L. Harris, J. Hora, J. L. Bracker, S. Povich, M. S. Churchwell, E. B. Engelbracht, C. W. For, B-Q Block, M. Misselt, K. Vijh, U. Leitherer, C. Kawamura, A. Blum, R. D. Cohen, M. Fukui, Y. Mizuno, A. Mizuno, N. Srinivasan, S. Tielens, A. G. G. M. Volk, K. Bernard, J-P. Boulanger, F. Frogel, J. A. Gallagher, J. Gorjian, V. Kelly, D. Latter, W. B. Madden, S. Kemper, F. Mould, J. R. Nota, A. Oey, M. S. Olsen, K. A. Onishi, T. Paladini, R. Panagia, N. Perez-Gonzalez, P. Reach, W. Shibai, H. Sato, S. Smith, L. J. Staveley-Smith, L. Ueta, T. Van Dyk, S. Werner, M. Wolff, M. Zaritsky, D. TI Spitzer SAGE survey of the Large Magellanic Cloud. III. Star formation and similar to 1000 new candidate Young Stellar Objects SO ASTRONOMICAL JOURNAL LA English DT Review DE circumstellar matter; galaxies : dwarf; infrared : stars; Magellanic Clouds; stars : formation; stars : pre-main sequence ID MAIN-SEQUENCE STARS; 2-DIMENSIONAL RADIATIVE-TRANSFER; SPECTRAL ENERGY-DISTRIBUTIONS; MULTIBAND IMAGING PHOTOMETER; COLOR-MAGNITUDE DIAGRAMS; SPACE-TELESCOPE; MOLECULAR CLOUDS; PLANETARY-NEBULAE; FORMATION HISTORY; CO SURVEY AB We present similar to 1000 new candidate Young Stellar Objects (YSOs) in the Large Magellanic Cloud selected from Spitzer Space Telescope data, as part of the Surveying the Agents of a Galaxy's Evolution (SAGE) Legacy program. The YSOs, detected by their excess infrared (IR) emission, represent early stages of evolution, still surrounded by disks and/or infalling envelopes. Previously, fewer than 20 such YSOs were known. The candidate YSOs were selected from the SAGE Point Source Catalog from regions of color-magnitude space least confused with other IR-bright populations. The YSOs are biased toward intermediate-to high-mass and young evolutionary stages, because these overlap less with galaxies and evolved stars in color-magnitude space. The YSOs are highly correlated spatially with atomic and molecular gas, and are preferentially located in the shells and bubbles created by massive stars inside. They are more clustered than generic point sources, as expected if star formation occurs in filamentary clouds or shells. We applied a more stringent color-magnitude selection to produce a subset of " high-probability" YSO candidates. We fitted the spectral-energy distributions (SEDs) of this subset and derived physical properties for those that were well fitted. The total mass of these well-fitted YSOs is similar to 2900 M(circle dot) and the total luminosity is similar to 2.1 x 10(6)L(circle dot). By extrapolating the mass function with a standard initial mass function and integrating, we calculate a current star-formation rate of similar to 0.06M(circle dot) yr(-1), which is at the low end of estimates based on total ultraviolet and IR flux from the galaxy (similar to 0.05-0.25M(circle dot) yr(-1)), consistent with the expectation that our current YSO list is incomplete. Follow-up spectroscopy and further data mining will better separate the different IR-bright populations and likely increase the estimated number of YSOs. The full YSO list is available as electronic tables, and the SEDs are available as an electronic figure for further use by the scientific community. C1 Space Sci Inst, Boulder, CO 80301 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. Univ Arizona, Steward Observ, Tucson, AZ 85719 USA. Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. Natl Opt Astron Observ, Tucson, AZ 85726 USA. Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. SOFIA Off, NASA Ames Res Ctr, Moffett Field, CA 94035 USA. Gemini Observ, Hilo, HI 96720 USA. CNRS, UPR 341, IAP, F-31028 Toulouse, France. AURA Inc, Washington, DC 20005 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA. CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Cerro Tololo Interamer Observ, La Serena, Chile. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. UCL, Dept Phys & Astron, London WC1E 6BT, England. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. RP Whitney, BA (reprint author), Space Sci Inst, 4750 Walnut St Suite 205, Boulder, CO 80301 USA. EM bwhitney@spacescience.org; sewilo@stsci.edu; remy@virginia.edu; tr9@st-andrews.ac.uk; meixner@stsci.edu; kgordon@as.arizona.edu; meade@sal.wisc.edu; jharris@as.arizona.edu; s_bracker@hotmail.com; povich@astro.wisc.edu; ebc@astro.wisc.edu; cengelbracht@as.arizona.edu; biqing@email.arizona.edu; kmisselt@as.arizona.edu; vijh@stsci.edu; leitherer@stsci.edu; kawamura@a.phys.nagoya-u.ac.jp; rblum@noao.edu; mcohen@astro.berkeley.edu; fukui@a.phys.nagoya-u.ac.jp; mizuno@a.phys.nagoya-u.ac.jp; sundar@pha.jhu.edu; atielens@arc.nasa.gov; kvolk@gemini.edu; Jean-Philippe.Bernard@cesr.fr; Francois.Boulanger@ias.u-psud.fr; jfrogel@aura-astronomy.org; varoujan.gorjian@jpl.nasa.gov; dkelly@as.arizona.edu; latter@ipac.caltech.edu; smadden@cea.fr; f.kemper@manchester.ac.uk; jmould@noao.edu; nota@stsci.edu; msoey@umich.edu; kolsen@ctio.noao.edu; ohnishi@a.phys.nagoya-u.ac.jp; panagia@stsci.edu; pgperez@as.arizona.edu; shibai@nagoya-u.jp; ssato@z.phys.nagoya-u.ac.jp; lsmith@stsci.edu; Lister.Staveley-Smith@csiro.au; tueta@du.edu; vandyk@ipac.caltech.edu; mwerner@sirtfweb.jpl.nasa.gov; wolff@spacescience.org RI Staveley-Smith, Lister/A-1683-2011; Kemper, Francisca/D-8688-2011; Perez-Gonzalez, Pablo/J-2871-2016; OI Staveley-Smith, Lister/0000-0002-8057-0294; Kemper, Francisca/0000-0003-2743-8240; Perez-Gonzalez, Pablo/0000-0003-4528-5639; Babler, Brian/0000-0002-6984-5752; Hora, Joseph/0000-0002-5599-4650; Reach, William/0000-0001-8362-4094; Robitaille, Thomas/0000-0002-8642-1329; Van Dyk, Schuyler/0000-0001-9038-9950 NR 119 TC 128 Z9 128 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 2008 VL 136 IS 1 BP 18 EP 43 DI 10.1088/0004-6256/136/1/18 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 321FN UT WOS:000257290200002 ER PT J AU Velusamy, T Marsh, KA Beichman, CA Backus, CR Thompson, TJ AF Velusamy, T. Marsh, K. A. Beichman, C. A. Backus, C. R. Thompson, T. J. TI HiRes deconvolution of Spitzer infrared images SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared : general; techniques : high angular resolution ID TELESCOPE NICMOS IMAGES; SPACE-TELESCOPE; SUPERNOVA-REMNANT; 1ST-LOOK SURVEY; PROTOSTARS; OUTFLOWS; SYSTEM; HH-46/47; GALAXIES; CLUSTER AB Spitzer provides unprecedented sensitivity in the infrared (IR), but the spatial resolution is limited by a relatively small aperture (0.85 m) of the primary mirror. In order to maximize the scientific return it is desirable to use processing techniques which make the optimal use of the spatial information in the observations. We have developed a deconvolution technique for Spitzer images. The algorithm, "HiRes" and its implementation has been discussed by Backus et al. in 2005. Here we present examples of Spitzer IR images from the Infrared Array Camera (IRAC) and MIPS, reprocessed using this technique. Examples of HiRes processing include a variety of objects from point sources to complex extended regions. The examples include comparison of Spitzer deconvolved images with high-resolution Keck and Hubble Space Telescope images. HiRes deconvolution improves the visualization of spatial morphology by enhancing resolution (to sub-arcsecond levels in the IRAC bands) and removing the contaminating sidelobes from bright sources. The results thereby represent a significant improvement over previously-published Spitzer images. The benefits of HiRes include (a) sub-arcsec resolution (similar to 0 ''.6-0 ''.8 for IRAC channels); (b) the ability to detect sources below the diffraction-limited confusion level; (c) the ability to separate blended sources, and thereby provide guidance to point-source extraction procedures; (d) an improved ability to show the spatial morphology of resolved sources. We suggest that it is a useful technique to identify features which are interesting enough for follow-up deeper analysis. C1 [Velusamy, T.; Marsh, K. A.; Beichman, C. A.; Backus, C. R.; Thompson, T. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Marsh, K. A.] CALTECH, IPAC, Pasadena, CA 91125 USA. [Beichman, C. A.] CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. RP Velusamy, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM velusamy@jpl.nasa.gov; kam@ipac.caltech.edu; chas@mail.jpl.nasa.gov; Charles.R.Backus@jpl.nasa.gov; Timothy.J.Thompson@jpl.nasa.gov NR 38 TC 16 Z9 16 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 2008 VL 136 IS 1 BP 197 EP 211 DI 10.1088/0004-6256/136/1/197 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 321FN UT WOS:000257290200014 ER PT J AU Rosado, M Ghosh, KK Fuentes-Carrera, I AF Rosado, Margarita Ghosh, Kajal K. Fuentes-Carrera, Isaura TI Detection of X-ray elongated emission from an ultraluminous X-ray source in the interacting pair of galaxies NGC 5953/5954 SO ASTRONOMICAL JOURNAL LA English DT Review DE galaxies : individual (NGC 5953, NGC 5954); galaxies : interactions; X-rays : galaxies; X-rays : individual (CXOU J153434.9+151149) ID MASS BLACK-HOLES; XMM-NEWTON OBSERVATIONS; MEDIUM-SENSITIVITY SURVEY; HIGH-RESOLUTION IMAGER; RADIAL-VELOCITY FIELD; RING-SHAPED NEBULAE; ACCRETION DISKS; NEARBY GALAXIES; EXTERNAL GALAXIES; SOURCE POPULATION AB We present radio through X-ray observations of a bright (> 10(40) erg s(-1) in the 0.5-8.0 keV band) ultraluminous X-ray source (ULX), CXOU J153434.9+151149, in the starburst, interacting pair of galaxies NGC 5953/5954. A Chandra image of this ULX shows that it is elongated. From HST/WFPC2/F606W data we have detected a counterpart of the ULX system with M-F606W similar to-7.1 +/- 0.7 mag. This optical counterpart may be either an O-type supergiant star or a young star cluster. From our Fabry-Perot interferometric observations, we have detected Ha and [N II] (6584 angstrom) diffuse emission, with velocity gradients up to 60 km s(-1) at the astrometric corrected Chandra position of the ULX. Different scenarios have been invoked as to explain the possible nature of CXOU J153434.9+151149. Based on the observed X-ray morphology of the ULX, we estimate that the inclination between the line of sight to the observer and the direction of a possibly beamed outflow is similar to 53 degrees. Beaming with this geometry from a stellar-mass black hole system will be inadequate to explain the observed X-ray luminosity of this ULX. Finally, we suggest that mild-beaming from a binary black hole with mass more than 50 M-circle dot associated with a young star cluster, is the most favorable scenario that describes the multiwavelength properties of this ULX. Future observations are definitely needed to determine the nature of this rare object. C1 [Rosado, Margarita] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Ghosh, Kajal K.] NASA, Univ Space Res Assoc, Marshall Space Flight Ctr, Huntsville, AL USA. [Fuentes-Carrera, Isaura] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfericas, Dept Astron, BR-05508900 Sao Paulo, Brazil. [Ghosh, Kajal K.] Univ Paris Diderot, CNRS, Observ Paris, GEPI, F-92190 Meudon, France. RP Rosado, M (reprint author), Univ Nacl Autonoma Mexico, Inst Astron, Apartado Postal 70-264, Mexico City 04510, DF, Mexico. NR 127 TC 2 Z9 2 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 JUL PY 2008 VL 136 IS 1 BP 212 EP 220 DI 10.1088/0004-6256/136/1/212 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 321FN UT WOS:000257290200015 ER PT J AU Pandian, JD Momjian, E Goldsmith, PF AF Pandian, J. D. Momjian, E. Goldsmith, P. F. TI Resolving distance ambiguities towards 6.7 GHz methanol masers SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Galaxy : kinematics and dynamics; Galaxy : structure; HII regions ID ULTRACOMPACT HII-REGIONS; STAR-FORMATION REGIONS; H-II-REGIONS; GALAXY; ABSORPTION; PLANE; FORMALDEHYDE; RESOLUTION; MILKY; MASS AB Context. Distances to most star forming regions are determined using kinematics, through the assumption that the observed radial velocity arises from the motion of the source with respect to the Sun resulting from the differential rotation of Galaxy. The primary challenge associated with the application of this technique in the inner Galaxy is the kinematic distance ambiguity. Aims. In this work, we aim to resolve the kinematic distance ambiguity towards a sample of 6.7 GHz methanol masers, which are signposts of the early stages of massive star formation. Methods. We measured 21 cm Hi absorption spectra using the Very Large Array in C and CnB configurations. A comparison of the maximum velocity of Hi absorption with the source velocity and tangent point velocity was used to resolve the kinematic distance ambiguity. Results. We resolved the distance ambiguity towards 41 sources. Distance determinations that are in conflict with previous measurements are discussed. The NE2001 spiral arm model is broadly consistent with the locations of the star forming complexes. We find that the use of vertical scale height arguments to resolve the distance ambiguity can lead to erroneous classifications for a significant fraction of sources. C1 [Pandian, J. D.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Momjian, E.] Arecibo Observ, Arecibo, PR 00612 USA. [Goldsmith, P. F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Pandian, JD (reprint author), Max Planck Inst Radioastron, Auf Hugel 69, D-53121 Bonn, Germany. EM jpandian@mpifr-bonn.mpg.de; emomjian@naic.edu; Paul.F.Goldsmith@jpl.nasa.gov RI Goldsmith, Paul/H-3159-2016 NR 29 TC 34 Z9 34 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 JUL PY 2008 VL 486 IS 1 BP 191 EP 208 DI 10.1051/0004-6361:200809799 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 321TE UT WOS:000257328600018 ER PT J AU in 't Zand, JJM Bassa, CG Jonker, PG Keek, L Verbunt, F Mendez, M Markwardt, CB AF in 't Zand, J. J. M. Bassa, C. G. Jonker, P. G. Keek, L. Verbunt, F. Mendez, M. Markwardt, C. B. TI An X-ray and optical study of the ultracompact X-ray binary A 1246-58 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays : binaries; X-rays : individuals : A 1246-58; accretion, accretion disks; stars : neutron ID ADVECTION-DOMINATED ACCRETION; PHOTON IMAGING CAMERA; XMM-NEWTON; TIMING-EXPLORER; SPECTRAL STATES; NEUTRON-STARS; 4U 1820-30; BEPPOSAX; TELESCOPE; 2S-0918-549 AB Results are discussed of an X-ray and optical observation campaign of the low-mass X-ray binary A 1246-58 performed with instruments on Satellite per Astronomia X ("BeppoSAX"), the Rossi X-ray Timing Explorer (RXTE), the X-ray Multi-mirror Mission ("XMM-Newton"), the Swift mission, and the Very Large Telescope. Spectra and flux time histories are studied. The most important results are the lack of hydrogen spectral features in the optical spectrum, supporting the proposition that this is an ultracompact X-ray binary (UCXB), the determination of a 4.3 kpc distance from time-resolved spectroscopy of thermonuclear X-ray bursts, and the detection of intermediately long thermonuclear bursts as seen in a number of other UCXBs. There is evidence for a Ne/O abundance ratio in the line of sight that is higher than solar and variable. This may be due to different changes in the ionization degrees of Ne and O, which may be related to the variable irradiating flux. We discuss the spectral variability and the peculiarities of the long-term light curve. C1 [in 't Zand, J. J. M.; Jonker, P. G.; Keek, L.] SRON, Inst Space Res, NL-3584 CA Utrecht, Netherlands. [in 't Zand, J. J. M.; Jonker, P. G.; Keek, L.; Verbunt, F.] Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands. [Bassa, C. G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mendez, M.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Markwardt, C. B.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Markwardt, C. B.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. RP in 't Zand, JJM (reprint author), SRON, Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM jeanz@sron.nl RI Mendez, Mariano/C-8011-2012 OI Mendez, Mariano/0000-0003-2187-2708 NR 68 TC 12 Z9 12 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2008 VL 485 IS 1 BP 183 EP 194 DI 10.1051/0004-6361:200809361 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 312SH UT WOS:000256690600019 ER PT J AU Senziani, F Skinner, GK Jean, P Hernanz, M AF Senziani, F. Skinner, G. K. Jean, P. Hernanz, M. TI Detectability of gamma-ray emission from classical novae with Swift/BAT SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma rays : observations; nuclear reactions, nucleosynthesis, abundances; stars : novae, cataclysmic variables; stars : white dwarfs ID BURST ALERT TELESCOPE; SPECTROMETER OBSERVATIONS; POSITRON-ANNIHILATION; LINES; ABUNDANCES; OUTBURST; MISSION; MODELS AB Context. Classical novae are expected to emit gamma rays during their explosions. The most important contribution to the early gamma-ray emission comes from the annihilation with electrons of the positrons generated by the decay of (13)N and (18)F. The photons are expected to be down-scattered to a few tens of keV, and the emission is predicted to occur some days before the visual discovery and to last similar to 2 days. Despite a number of attempts, no positive detections of such emission have been made, due to lack of sensitivity and of sky coverage. Aims. Because of its huge field of view, good sensitivity, and well-adapted (14-200 keV) energy band, Swift/BAT offers a new opportunity for such searches. BAT data can be retrospectively used to search for prompt gamma-ray emission from the direction of novae after their optical discovery. Methods. We have estimated the expected success rate for the detection with BAT of gamma rays from classical novae using a Monte Carlo approach. Searches were performed for emission from novae occurring since the launch of Swift. Results. Using the actual observing programme during the first 2.3 years of BAT operations as an example, and sensitivity achieved, we estimate the expected rate of detection of classical novae with BAT as similar to 0.2-0.5 yr(-1), implying that several should be seen within a 10 yr mission. The search for emission in the directions of the 24 classical novae discovered since the Swift launch yielded no positive results, but none of these was known to be close enough for this to be a surprise. Detections of a recurrent nova (RS Oph) and a nearby dwarf nova (V455 And) demonstrate the efficacy of the technique. Conclusions. The absence of detections is consistent with the expectations from the Monte Carlo simulations, but the long-term prospects are encouraging given an anticipated Swift operating lifetime of similar to 10 years. C1 [Senziani, F.] Univ Pavia, Dipartimento Fis Nucl & Teor, I-27100 Pavia, Italy. [Senziani, F.] Ist Univ Super IUSS, I-27100 Pavia, Italy. [Senziani, F.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Senziani, F.; Jean, P.] Univ Toulouse 3, CESR, F-31028 Toulouse, France. [Skinner, G. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Skinner, G. K.] Univ Maryland, CRESST, Dept Astron, College Pk, MD 20742 USA. [Hernanz, M.] CSIC, IEEC, Fac Cienc, Bellaterra 08193, Spain. RP Senziani, F (reprint author), Univ Pavia, Dipartimento Fis Nucl & Teor, Via Agostino Bassi 6, I-27100 Pavia, Italy. EM senziani@iasf-milano.inaf.it RI Hernanz, Margarita/K-1770-2014 OI Hernanz, Margarita/0000-0002-8651-7910 NR 44 TC 9 Z9 9 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2008 VL 485 IS 1 BP 223 EP 231 DI 10.1051/0004-6361:200809863 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 312SH UT WOS:000256690600023 ER PT J AU Beltran, MT Wiseman, J Ho, PTP Estalella, R Fuller, GA Wooten, A AF Beltran, M. T. Wiseman, J. Ho, P. T. P. Estalella, R. Fuller, G. A. Wooten, A. TI Dissection of the protostellar envelope surrounding IRAS 05173-0555 in L1634 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM : jets and outflows; stars : circumstellar matter; stars : formation; radio lines : ISM ID BRIGHT-RIMMED CLOUDS; HARO ENERGY-SOURCES; STAR-FORMATION; YOUNG STARS; MOLECULAR CLOUDS; COLD DUST; OUTFLOW; EVOLUTION; JET; AMMONIA AB Context. The youngest protostars that power energetic outflows are surrounded by infalling and rotating envelopes that contain most of the mass of the system. Aims. We study the properties and kinematics of the protostellar envelope surrounding the embedded source IRAS 05173-0555 in L1634. Methods. We carried out VLA ammonia observations at 1.3 cm with the VLA in the D configuration to map the gas towards the core of L1634. Results. The NH(3) emission towards IRAS 05173-0555 is resolved and shows two components that are clearly distinguishable morphologically: a cross-like structure, roughly elongated in the direction of the HH 240/241 outflow and associated with IRAS 05173-0555, plus an arc-like stream elongated towards the north. The properties and kinematics of the gas suggest that the origin of the cross-like morphology could be the interaction between the outflow and the envelope. A more compact and flattened structure, which could be undergoing rotation about the axis of the outflow, has been detected towards the center of the cross-like envelope. The northern stream, which has properties and velocity that are different from those of the cross-like envelope, is likely part of the original cloud envelope, and could be a quiescent core that may never form stars, or instead be in a prestellar phase. C1 [Beltran, M. T.; Estalella, R.] Univ Barcelona, Dept Astron Meterol, E-08028 Barcelona, Catalunya, Spain. [Wiseman, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ho, P. T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ho, P. T. P.] Acad Sinica, Inst Astrophys, Taipei 106, Taiwan. [Fuller, G. A.] Univ Manchester, Jordell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Wooten, A.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. RP Beltran, MT (reprint author), Univ Barcelona, Dept Astron Meterol, Marti Franques 1, E-08028 Barcelona, Catalunya, Spain. EM mbeltran@am.ub.es OI Beltran Sorolla, Maria Teresa/0000-0003-3315-5626 NR 32 TC 4 Z9 4 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 JUL PY 2008 VL 485 IS 2 BP 517 EP 526 DI 10.1051/0004-6361:20079224 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 315OW UT WOS:000256890300023 ER PT J AU Glauser, AM Menard, F Pinte, C Duchene, G Gudel, M Monin, JL Padgett, DL AF Glauser, A. M. Menard, F. Pinte, C. Duchene, G. Guedel, M. Monin, J. -L. Padgett, D. L. TI Multiwavelength studies of the gas and dust disc of IRAS 04158+2805 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : circumstellar matter; stars : pre-main-sequence; stars : individual : IRAS 04158+2805; stars : formation; stars : planetary systems : protoplanetary discs ID AURIGA MOLECULAR CLOUD; INITIAL MASS FUNCTION; T-TAURI STARS; BROWN DWARFS; INTERSTELLAR DUST; EVOLUTION; PROTOSTARS; L1495E; SOLAR AB We present a study of the circumstellar environment of IRAS 04158+2805 based on multi-wavelength observations and models. Images in the optical and near-infrared, a polarisation map in the optical, and mid-infrared spectra were obtained with VLT-FORS1, CFHT-IR, and Spitzer-IRS. Additionally we used an X-ray spectrum observed with Chandra. We interpret the observations in terms of a central star surrounded by an axisymmetric circumstellar disc, but without an envelope, to test the validity of this simple geometry. We estimate the structural properties of the disc and its gas and dust content. We modelled the dust disc with a 3D continuum radiative transfer code, MCFOST, based on a Monte-Carlo method that provides synthetic scattered light images and polarisation maps, as well as spectral energy distributions. We find that the disc images and spectral energy distribution narrowly constrain many of the disc model parameters, such as a total dust mass of 1.0-1.75 x 10(-4) M(circle dot) and an inclination of 62 degrees-63 degrees. The maximum grain size required to fit all available data is of the order of 1.6-2.8 mu m although the upper end of this range is loosely constrained. The observed optical polarisation map is reproduced well by the same disc model, suggesting that the geometry we find is adequate and the optical properties are representative of the visible dust content. We compare the inferred dust column density to the gas column density derived from the X-ray spectrum and find a gas-to-dust ratio along the line of sight that is consistent with the ISM value. To our knowledge, this measurement is the first to directly compare dust and gas column densities in a protoplanetary disc. C1 [Glauser, A. M.; Guedel, M.] Paul Scherrer Inst, CH-5232 Villigen, Switzerland. [Menard, F.; Duchene, G.; Monin, J. -L.] CNRS, Lab Astrophys Grenoble, UJF UMR 5571, F-38041 Grenoble 9, France. [Duchene, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Pinte, C.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Padgett, D. L.] CALTECH, JPL, IPAC, Pasadena, CA 91125 USA. RP Glauser, AM (reprint author), Paul Scherrer Inst, CH-5232 Villigen, Switzerland. EM glauser@phys.ethz.ch RI Guedel, Manuel/C-8486-2015 OI Guedel, Manuel/0000-0001-9818-0588 NR 27 TC 15 Z9 15 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2008 VL 485 IS 2 BP 531 EP 540 DI 10.1051/0004-6361:20065685 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 315OW UT WOS:000256890300025 ER PT J AU Lacour, S Meimon, S Thiebaut, E Perrin, G Verhoelst, T Pedretti, E Schuller, PA Mugnier, L Monnier, J Berger, JP Haubois, X Poncelet, A Le Besnerais, G Eriksson, K Millan-Gabet, R Ragland, S Lacasse, M Traub, W AF Lacour, S. Meimon, S. Thiebaut, E. Perrin, G. Verhoelst, T. Pedretti, E. Schuller, P. A. Mugnier, L. Monnier, J. Berger, J. P. Haubois, X. Poncelet, A. Le Besnerais, G. Eriksson, K. Millan-Gabet, R. Ragland, S. Lacasse, M. Traub, W. TI The limb-darkened Arcturus: imaging with the IOTA/IONIC interferometer SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques : interferometric; stars : fundamental parameters; infrared : stars; stars : individual : Arcturus ID NEAR-INFRARED INTERFEROMETRY; RADIAL-VELOCITY VARIATIONS; STELLAR ATMOSPHERE MODELS; EFFECTIVE TEMPERATURE; OPTICAL INTERFEROMETER; ANGULAR DIAMETERS; BEAM-COMBINATION; DOUBLE STAR; K-GIANTS; IOTA AB Aims. We undertook an H band interferometric examination of Arcturus, a star frequently used as a spatial and spectral calibrator. Methods. Using the IOTA 3 telescope interferometer, we performed spectro-interferometric observations (R approximate to 35) of Arcturus. Atmospheric models and prescriptions were fitted to the data to derive the brightness distribution of the photosphere. Image reconstruction was performed using two software algorithms: WISARD and MIRA. Results. An achromatic power law proved to be a good model of the brightness distribution, with a limb darkening compatible with the one derived from atmospheric model simulations using our mARCS model. A Rosseland diameter of 21.05 +/- 0.21 was derived, corresponding to an effective temperature of T-eff = 4295 +/- 26 K. No companion was detected from the closure phases, with an upper limit on the brightness ratio of 8 x 10(-4) at 1 AU. The dynamic range at such distance from the photosphere was established as 1.5 x 10(-4) (1 sigma rms). An upper limit of 1.7 x 10(-3) was also derived for the level of brightness asymmetries present in the photosphere. C1 [Lacour, S.; Perrin, G.; Haubois, X.; Poncelet, A.] Observ Paris, LESIA, CNRS, UMR 8109, F-92190 Meudon, France. [Lacour, S.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. [Lacour, S.; Berger, J. P.] CNRS, Lab Astrophys Grenoble, UMR 5571, F-38041 Grenoble, France. [Meimon, S.; Mugnier, L.; Le Besnerais, G.] Off Natl Etud & Rech Aeronaut, DOTA, F-92322 Chatillon, France. [Thiebaut, E.] Ctr Rech Astrophys Lyon, CNRS, UMR 5574, F-69561 St Genis Laval, France. [Verhoelst, T.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Verhoelst, T.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Pedretti, E.] Univ St Andrews, St Andrews KY16 9SS, Fife, Scotland. [Schuller, P. A.; Ragland, S.; Lacasse, M.; Traub, W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schuller, P. A.] Univ Paris 11, Inst Astrophys Spatial, F-91405 Orsay, France. [Monnier, J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Eriksson, K.] Uppsala Univ, Dept Space Phys & Astron, S-75120 Uppsala, Sweden. [Millan-Gabet, R.] CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. [Traub, W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lacour, S (reprint author), Observ Paris, LESIA, CNRS, UMR 8109, F-92190 Meudon, France. EM sylvestre.lacour@obspm.fr RI Mugnier, Laurent/A-7630-2012; Haubois, Xavier/I-7026-2012; OI Mugnier, Laurent/0000-0002-8364-4957 NR 57 TC 35 Z9 35 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 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2008 VL 485 IS 2 BP 561 EP 570 DI 10.1051/0004-6361:200809611 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 315OW UT WOS:000256890300028 ER PT J AU Caro, GMM Dartois, E Nakamura-Messenger, K AF Caro, G. M. Munoz Dartois, E. Nakamura-Messenger, K. TI Characterization of the carbon component in cometary Stardust samples by means of infrared and Raman spectroscopy SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE comets : individual : 81P/Wild 2; methods : analytical; techniques : spectroscopic ID INTERSTELLAR ICE ANALOGS; INTERPLANETARY DUST PARTICLES; AMORPHOUS-CARBON; AMINO-ACIDS; 81P/WILD-2; MATTER; IRRADIATION; EVOLUTION; ORGANICS; SPECTRA AB Aims. We attempt to ellucidate the structure and chemical composition of the carbon bulk detected in cometary Stardust particles. We determine if the carbon material observed spectroscopically is of true cometary origin and whether or not it was formed by direct UV-photoprocessing of icy grain mantles in the local dense cloud and/or the solar nebula. Methods. We acquire infrared spectroscopy of ten Stardust cometary particles from track 35 and the aerogel inside and outside the particle track. Using infrared and Raman spectroscopy, the dominant carbon component in cometary Stardust particles was compared to IDPs and organics made from UV-photoprocessing of interstellar/circumstellar ice analogs in the laboratory. The Raman spectra of Stardust particles used in this comparison are adapted from the literature. Results. As indicated in previous works, it is found that the collecting aerogel medium, processed during particle impact, poses serious problems for the infrared analysis of the Stardust cometary particles reported in this paper. We identify the structure of the carbon bulk of the organic material retrieved from the aerogel with a form of (hydrogenated) amorphous carbon. It is found that this material is not a direct product of ice photoprocessing. C1 [Caro, G. M. Munoz] CSIC INTA, Ctr Astrobiol, Madrid 28850, Spain. [Dartois, E.] Univ Paris 11, Inst Astrophys Spatiale, UMR 8617, F-91405 Orsay, France. [Nakamura-Messenger, K.] NASA, Lyndon B Johnson Space Ctr, Engn Sci Contact Grp, Houston, TX 77058 USA. RP Caro, GMM (reprint author), CSIC INTA, Ctr Astrobiol, Carretera Ajalvir,Km 4, Madrid 28850, Spain. EM munozcg@inta.es RI Appourchaux, Thierry/F-4692-2010; Munoz Caro, Guillermo /L-6370-2014 OI Munoz Caro, Guillermo /0000-0001-7003-7368 NR 41 TC 17 Z9 17 U1 0 U2 16 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 JUL PY 2008 VL 485 IS 3 BP 743 EP 751 DI 10.1051/0004-6361:20078879 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 319DL UT WOS:000257144200014 ER PT J AU Reig, P Belloni, T Israel, GL Campana, S Gehrels, N Homan, J AF Reig, P. Belloni, T. Israel, G. L. Campana, S. Gehrels, N. Homan, J. TI Bright flares from the X-ray pulsar SWIFT J1626.6-5156 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays : binaries; stars : neutron; stars : binaries : close; stars : emission-line, Be ID ACCRETING PULSAR; TIMING-EXPLORER; NEUTRON-STAR; GRO J1744-28; 4U 1907+09; TRANSIENT; BINARIES; DISCOVERY; WINDS AB Aims. We have performed a timing and spectral analysis of the X-ray pulsar SWIFT J1626.6-5156 during a major X-ray outburst in order to unveil its nature and investigate its flaring activity. Methods. Epoch-and pulse-folding techniques were used to derive the spin period. Time-average and pulse-phase spectroscopy were employed to study the spectral variability in the flare and out-of-flare states and energy variations with pulse phase. Power spectra were obtained to investigate the periodic and aperiodic variability. Results. Two large flares, with a duration of similar to 450 s were observed on 24 and 25 December 2005. During the flares, the X-ray intensity increased by a factor of 3.5, while the peak-to-peak pulsed amplitude increased from 45% to 70%. A third, smaller flare of duration similar to 180 s was observed on 27 December 2005. The flares seen in SWIFT J1626.6-5156 constitute the shortest events of this kind ever reported in a high-mass X-ray binary. In addition to the flaring activity, strong X-ray pulsations with P(spin) = 15.3714 +/- 0.0003 s characterise the X-ray emission in SWIFT J1626.6-5156. After the major outburst, the light curve exhibits strong long-term variations modulated with a 45-day period. We relate this modulation to the orbital period of the system or to a harmonic. Power density spectra show, in addition to the harmonic components of the pulsation, strong band-limited noise with an integrated 0.01-100 Hz fractional rms of around 40% that increased to 64% during the flares. A weak QPO (fractional rms 4.7%) with characteristic frequency of 1 Hz was detected in the non-flare emission. Conclusions. The timing (short X-ray pulsations, long orbital period) and spectral (power-law with cut off energy and neutral iron line) properties of SWIFT J1626.6-5156 are characteristic of Be/X-ray binaries. C1 [Reig, P.] Fdn Res & Technol, IESL, Iraklion 71110, Greece. [Reig, P.] Univ Crete, Dept Phys, Iraklion 71003, Greece. [Belloni, T.; Campana, S.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [Israel, G. L.] Osserv Astron Roma, INAF, I-00040 Rome, Italy. [Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Homan, J.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Reig, P (reprint author), Fdn Res & Technol, IESL, Iraklion 71110, Greece. EM pau@physics.uoc.gr; tomaso.belloni@brera.inaf.it; gianluca@mporzio.astro.it; sergio.campana@brera.inaf.it; Neil.Gehrels@gsfc.nasa.gov; jeroen@space.mit.edu RI Gehrels, Neil/D-2971-2012; Reig, Pablo/A-1198-2014; OI Reig, Pablo/0000-0002-6446-3050; Israel, GianLuca/0000-0001-5480-6438 NR 37 TC 14 Z9 14 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 JUL PY 2008 VL 485 IS 3 BP 797 EP 805 DI 10.1051/0004-6361:200809457 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 319DL UT WOS:000257144200020 ER PT J AU Tueller, J Mushotzky, RF Barthelmy, S Cannizzo, JK Gehrels, N Markwardt, CB Skinner, GK Winter, LM AF Tueller, J. Mushotzky, R. F. Barthelmy, S. Cannizzo, J. K. Gehrels, N. Markwardt, C. B. Skinner, G. K. Winter, L. M. TI Swift BAT survey of AGNs SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; gamma rays : observations; surveys ID ACTIVE GALACTIC NUCLEI; HARD-X-RAY; DEEP FIELD-SOUTH; XMM-NEWTON OBSERVATIONS; SEYFERT 2 GALAXIES; ALL-SKY SURVEY; BURST ALERT TELESCOPE; LUMINOSITY FUNCTION; RADIO GALAXY; OPTICAL SPECTROSCOPY AB We present the results of the analysis of the first 9 months of data of the SwiftBAT survey of AGNs in the 14-195 keV band. Using archival X-ray data or follow-up Swift XRT observations, we have identified 129 ( 103 AGNs) of 130 objects detected at vertical bar b vertical bar > 15 degrees and with significance >4.8 sigma. One source remains unidentified. These same X-ray data have allowed measurement of the X-ray properties of the objects. We fit a power law to the log N-log S distribution, and find the slope to be 1.42 +/- 0.14. Characterizing the differential luminosity function data as a broken power law, we find a break luminosity log L-* (erg s(-1)) = 43.85 +/- 0.26, a low-luminosity power law slope a - 0.84(-0.22)(+0.16), and a high-luminosity power law slope b 2.55(-0.30)(+0.43) , similar to the values that have been reported based on INTEGRAL data. We obtain a mean photon index 1.98 in the 14-195 keV band, with an rms spread of 0.27. Integration of our luminosity function gives a local volume density of AGNs above 10(41) erg s(-1) of 2.4 x 10(-3) Mpc(-3), which is about 10% of the total luminous local galaxy density above M-* - -19.75. We have obtained X-ray spectra from the literature and from Swift XRT follow-up observations. These show that the distribution of log n(H) is essentially flat from nH = 10(20) to 10(24) cm(-2), with 50% of the objects having column densities of less than 10(22) cm(-2). BAT Seyfert galaxies have a median redshift of 0.03, a maximum log luminosity of 45.1, and approximately half have log n(H) > 22. C1 [Tueller, J.; Mushotzky, R. F.; Barthelmy, S.; Cannizzo, J. K.; Gehrels, N.; Markwardt, C. B.; Skinner, G. K.; Winter, L. M.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Cannizzo, J. K.] Univ Maryland Baltimore Cty, Joint Ctr Astrophys, CRESST, Baltimore, MD 21250 USA. [Markwardt, C. B.; Skinner, G. K.; Winter, L. M.] Univ Maryland, Dept Astron, CRESST, College Pk, MD 20742 USA. RP Tueller, J (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RI Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; Tueller, Jack/D-5334-2012 NR 91 TC 194 Z9 194 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 JUL 1 PY 2008 VL 681 IS 1 BP 113 EP 127 DI 10.1086/588458 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 321FM UT WOS:000257290100011 ER PT J AU Smith, RK AF Smith, Randall K. TI X-ray dust scattering at small angles: The complete halo around GX13+1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; scattering; X-rays : ISM ID INTERSTELLAR GRAINS; INFRARED COUNTERPART; EXTINCTION; DISCOVERY; GX-13+1; BINARIES AB The exquisite angular resolution available with Chandra should allow precision measurements of faint diffuse emission surrounding bright sources, such as the X-ray scattering halos created by interstellar dust. However, the ACIS CCDs suffer from pileup when observing bright sources, and this creates difficulties when trying to extract the scattered halo near the source. The initial study of the X-ray halo around GX13+1 using only the ACIS-I detector performed by Smith, Edgar, & Shafer suffered from a lack of sensitivity within 5000 of the source, limiting what conclusions could be drawn. To address this problem, observations of GX13+1 were obtained with the Chandra HRC-I and simultaneously with the RXTE PCA. Combined with the existing ACIS-I data, this allowed measurements of the X-ray halo between 2'' and 1000''. After considering a range of dust models, each assumed to be smoothly distributed with or without a dense cloud along the line of sight; the results show that there is no evidence in these data for a dense cloud near the source, as suggested by Xiang et al. Finally, although no model leads to formally acceptable results, the Weingartner & Draine model and nearly all of the composite grain models from Zubko, Dwek, & Arendt give poor fits. C1 [Smith, Randall K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Smith, Randall K.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Smith, RK (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. NR 25 TC 12 Z9 12 U1 1 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 1 PY 2008 VL 681 IS 1 BP 343 EP 349 DI 10.1086/588519 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 321FM UT WOS:000257290100029 ER PT J AU Pascale, E Ade, PAR Bock, JJ Chapin, EL Chung, J Devlin, MJ Dicker, S Griffin, M Gundersen, JO Halpern, M Hargrave, PC Hughes, DH Klein, J MacTavish, CJ Marsden, G Martin, PG Martin, TG Mauskopf, P Netterfield, CB Olmi, L Patanchon, G Rex, M Scott, D Semisch, C Thomas, N Truch, MDP Tucker, C Tucker, GS Viero, MP Wiebe, DV AF Pascale, E. Ade, P. A. R. Bock, J. J. Chapin, E. L. Chung, J. Devlin, M. J. Dicker, S. Griffin, M. Gundersen, J. O. Halpern, M. Hargrave, P. C. Hughes, D. H. Klein, J. MacTavish, C. J. Marsden, G. Martin, P. G. Martin, T. G. Mauskopf, P. Netterfield, C. B. Olmi, L. Patanchon, G. Rex, M. Scott, D. Semisch, C. Thomas, N. Truch, M. D. P. Tucker, C. Tucker, G. S. Viero, M. P. Wiebe, D. V. TI The Balloon-borne Large Aperture Submillimeter Telescope: BLAST SO ASTROPHYSICAL JOURNAL LA English DT Article DE balloons; galaxies : evolution; instrumentation : miscellaneous; stars : formation; submillimeter ID COUPLED BOLOMETER ARRAYS; OPTICAL DESIGNS; SPIRE; OPTIMIZATION; SENSITIVITY; PERFORMANCE AB The Balloon-borne Large Aperture Submillimeter Telescope (BLAST) is a suborbital surveying experiment designed to study the evolutionary history and processes of star formation in local galaxies (including the MilkyWay) and galaxies at cosmological distances. The BLAST continuum camera, which consists of 270 detectors distributed between three arrays, observes simultaneously in broadband (30%) spectral windows at 250, 350, and 500 mu m. The optical design is based on a 2 m diameter telescope, providing a diffraction-limited resolution of 3000 at 250 mu m. The gondola pointing system enables raster mapping of arbitrary geometry, with a repeatable positional accuracy of similar to 30''; postflight pointing reconstruction to less than or similar to 5'' rms is achieved. The onboard telescope control software permits autonomous execution of a preselected set of maps, with the option of manual override. In this paper we describe the primary characteristics and measured in-flight performance of BLAST. BLAST performed a test flight in 2003 and has since made two scientifically productive long-duration balloon flights: a 100 hr flight from ESRANGE (Kiruna), Sweden to Victoria Island, northern Canada in 2005 June; and a 250 hr, circumpolar flight from McMurdo Station, Antarctica, in 2006 December. C1 [Pascale, E.; Chung, J.; MacTavish, C. J.; Martin, T. G.; Netterfield, C. B.; Wiebe, D. V.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Pascale, E.; Ade, P. A. R.; Griffin, M.; Hargrave, P. C.; Mauskopf, P.; Tucker, C.] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Bock, J. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bock, J. J.] CALTECH, Pasadena, CA 91125 USA. [Chapin, E. L.; Chung, J.; Halpern, M.; Marsden, G.; Patanchon, G.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Devlin, M. J.; Dicker, S.; Klein, J.; Rex, M.; Semisch, C.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Gundersen, J. O.] Univ Miami, Dept Phys, Coral Gables, FL 33146 USA. [Hughes, D. H.] INAOE, Puebla 72000, Mexico. [Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Martin, P. G.; Netterfield, C. B.; Viero, M. P.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Olmi, L.] Ist Radioastron, I-50125 Florence, Italy. [Olmi, L.] Univ Puerto Rico, Dept Phys, San Juan, PR 00931 USA. [Patanchon, G.] Lab APC, F-75205 Paris, France. [Truch, M. D. P.; Tucker, G. S.] Brown Univ, Dept Phys, Providence, RI 02912 USA. RP Pascale, E (reprint author), Univ Toronto, Dept Phys, 60 St George St, Toronto, ON M5S 1A7, Canada. EM enzo@physics.utoronto.ca RI Klein, Jeffrey/E-3295-2013; OI Olmi, Luca/0000-0002-1162-7947; Scott, Douglas/0000-0002-6878-9840 NR 25 TC 117 Z9 117 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2008 VL 681 IS 1 BP 400 EP 414 DI 10.1086/588541 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 321FM UT WOS:000257290100035 ER PT J AU Truch, DP Ade, PAR Bock, JJ Chapin, EL Devlin, MJ Dicker, S Griffin, M Gundersen, JO Halpern, M Hargrave, PC Hughes, DH Klein, J Marsden, G Martin, PG Mauskopf, P Netterfield, CB Olmi, L Pascale, E Patanchon, G Rex, M Scott, D Semisch, C Tucker, C Tucker, GS Viero, MP Wiebe, DV AF Truch, D. P. Ade, P. A. R. Bock, J. J. Chapin, E. L. Devlin, M. J. Dicker, S. Griffin, M. Gundersen, J. O. Halpern, M. Hargrave, P. C. Hughes, D. H. Klein, J. Marsden, G. Martin, P. G. Mauskopf, P. Netterfield, C. B. Olmi, L. Pascale, E. Patanchon, G. Rex, M. Scott, D. Semisch, C. Tucker, C. Tucker, G. S. Viero, M. P. Wiebe, D. V. TI The Balloon-borne Large Aperture Submillimeter Telescope (BLAST) 2005: Calibration and targeted sources SO ASTROPHYSICAL JOURNAL LA English DT Article DE balloons; submillimeter; telescopes ID ULTRACOMPACT HII-REGIONS; H-II REGIONS; MASS PROTOSTELLAR CANDIDATES; DEGREE EXTRAGALACTIC SURVEY; FAR-INFRARED OBSERVATIONS; LUMINOUS IRAS SOURCES; STAR-FORMATION; CONTINUUM EMISSION; ENERGY-DISTRIBUTIONS; SCUBA OBSERVATIONS AB The Balloon-borne Large Aperture Submillimeter Telescope (BLAST) operated successfully during a 100 hr flight from northern Sweden in 2005 June (BLAST05). As part of the calibration and pointing procedures, several compact sources were mapped, including solar system, Galactic, and extragalactic targets, specifically Pallas, CRL 2688, LDN 1014, IRAS 20126+4104, IRAS 21078+5211, IRAS 21307+5049, IRAS 22134+5834, IRAS 23011+6126, K3-50, W75N, and Mrk 231. One additional source, Arp 220, was observed and used as our primary calibrator. Details of the overall BLAST05 calibration procedure are discussed here. The BLAST observations of each compact source are described, flux densities and spectral energy distributions are reported, and these are compared with previous measurements at other wavelengths. The 250, 350, and 500 mu m BLAST data can provide useful constraints to the amplitude and slope of the submillimeter continuum, which in turn may be useful for the improved calibration of other submillimeter instruments. C1 [Truch, D. P.; Tucker, G. S.] Brown Univ, Dept Phys, Providence, RI 02912 USA. [Ade, P. A. R.; Griffin, M.; Hargrave, P. C.; Mauskopf, P.; Tucker, C.] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Bock, J. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bock, J. J.] CALTECH, Pasadena, CA 91125 USA. [Chapin, E. L.; Halpern, M.; Marsden, G.; Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Devlin, M. J.; Dicker, S.; Klein, J.; Rex, M.; Semisch, C.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Gundersen, J. O.] Univ Miami, Dept Phys, Coral Gables, FL 33146 USA. [Hughes, D. H.] INAOE, Puebla 72000, Mexico. [Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Martin, P. G.; Netterfield, C. B.; Viero, M. P.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Netterfield, C. B.; Pascale, E.; Wiebe, D. V.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Olmi, L.] Ist Radioastron, I-50125 Florence, Italy. [Olmi, L.] Univ Puerto Rico, Dept Phys, San Juan, PR 00931 USA. [Patanchon, G.] Lab APC, F-75205 Paris, France. RP Truch, DP (reprint author), Brown Univ, Dept Phys, Providence, RI 02912 USA. EM matthew@truch.net RI Klein, Jeffrey/E-3295-2013; OI Olmi, Luca/0000-0002-1162-7947; Scott, Douglas/0000-0002-6878-9840 NR 82 TC 22 Z9 22 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2008 VL 681 IS 1 BP 415 EP 427 DI 10.1086/588542 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 321FM UT WOS:000257290100036 ER PT J AU Chapin, EL Ade, PAR Bock, JJ Brunt, C Devlin, MJ Dicker, S Griffin, M Gundersen, JO Halpern, M Hargrave, PC Hughes, DH Klein, J Marsden, G Martin, PG Mauskopf, P Netterfield, CB Olmi, L Pascale, E Patanchon, G Rex, M Scott, D Semisch, C Truch, MDP Tucker, C Tucker, GS Viero, MP Wiebe, DV AF Chapin, E. L. Ade, P. A. R. Bock, J. J. Brunt, C. Devlin, M. J. Dicker, S. Griffin, M. Gundersen, J. O. Halpern, M. Hargrave, P. C. Hughes, D. H. Klein, J. Marsden, G. Martin, P. G. Mauskopf, P. Netterfield, C. B. Olmi, L. Pascale, E. Patanchon, G. Rex, M. Scott, D. Semisch, C. Truch, M. D. P. Tucker, C. Tucker, G. S. Viero, M. P. Wiebe, D. V. TI The Balloon-borne Large Aperture Submillimeter Telescope (BLAST) 2005: A 4 deg(2) Galactic plane survey in Vulpecula (l=59 degrees) SO ASTROPHYSICAL JOURNAL LA English DT Article DE balloons; ISM : clouds; stars : formation; submillimeter ID MASSIVE STAR-FORMATION; H-II-REGIONS; DUST CONTINUUM EMISSION; C2D LEGACY CLOUDS; ULTRACOMPACT HII-REGIONS; OPEN CLUSTER NGC-6823; 5 GHZ SURVEY; PROTOSTELLAR CANDIDATES; MOLECULAR CLOUDS; BOLOMETER ARRAY AB We present the first results from a new 250, 350, and 500 mu m Galactic plane survey taken with the Balloon-borne Large-Aperture Submillimeter Telescope (BLAST) in 2005. This survey's primary goal is to identify and characterize high-mass protostellar objects (HMPOs). The region studied here covers 4 deg(2) near the open cluster NGC 6823 in the constellation Vulpecula (l = 59 degrees). We find 60 compact sources (< 60'' diameter) detected simultaneously in all three bands. Their SEDs are constrained through BLAST, IRAS, Spitzer MIPS, and MSX photometry, with inferred dust temperatures spanning similar to 12-40 K assuming a dust emissivity index beta = 1.5. The luminosity-to-mass ratio, a distance-independent quantity, spans similar to 0.2-130 L-circle dot M-circle dot(-1). Distances are estimated from coincident (CO)-C-13(1 -> 0) velocities combined with a variety of other velocity and morphological data in the literature. In total, 49 sources are associated with a molecular cloud complex encompassing NGC 6823 (distance similar to 2.3 kpc), 10 objects with the Perseus arm (similar to 8.5 kpc), and one object is probably in the outer Galaxy (similar to 14 kpc). Near NGC 6823, the inferred luminosities and masses of BLASTsources span similar to 40-10(4) L-circle dot and similar to 15-700M(circle dot), respectively. The mass spectrum is compatible with molecular gas masses in other high- mass star- forming regions. Several luminous sources appear to be ultracompact H ii regions powered by early B stars. However, many of the objects are cool, massive gravitationally bound clumps with no obvious internal radiation from a protostar, and hence excellent HMPO candidates. C1 [Chapin, E. L.; Halpern, M.; Marsden, G.; Patanchon, G.; Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Ade, P. A. R.; Griffin, M.; Hargrave, P. C.; Mauskopf, P.; Tucker, C.] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Bock, J. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bock, J. J.] CALTECH, Pasadena, CA 91125 USA. [Brunt, C.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Devlin, M. J.; Dicker, S.; Klein, J.; Rex, M.; Semisch, C.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Gundersen, J. O.] Univ Miami, Dept Phys, Carol Gables, FL 33146 USA. [Hughes, D. H.] INAOE, Puebla 72000, Mexico. [Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Martin, P. G.; Netterfield, C. B.; Viero, M. P.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Netterfield, C. B.; Pascale, E.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Olmi, L.] Ist Radioastron, I-50125 Florence, Italy. [Olmi, L.] Univ Puerto Rico, Dept Phys, San Juan, PR 00931 USA. [Patanchon, G.] Lab APC, F-75205 Paris, France. [Truch, M. D. P.; Tucker, G. S.] Brown Univ, Dept Phys, Providence, RI 02912 USA. RP Chapin, EL (reprint author), Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. EM echapin@phas.ubc.ca RI Klein, Jeffrey/E-3295-2013 NR 76 TC 38 Z9 38 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2008 VL 681 IS 1 BP 428 EP 452 DI 10.1086/588544 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 321FM UT WOS:000257290100037 ER PT J AU Marsh, MS Ireland, J Kucera, T AF Marsh, M. S. Ireland, J. Kucera, T. TI Bayesian analysis of solar oscillations SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods : statistical; stars : oscillations; Sun : helioseismology; Sun : oscillations; sunspots; waves ID SUNSPOT UMBRAL OSCILLATIONS; TRANSITION REGION OSCILLATIONS; VERTICAL MAGNETIC-FIELD; PROPAGATION; PHOTOSPHERE; WAVES; SUN AB A Bayesian probability-based approach is applied to the problem of detecting and parameterizing oscillations in the upper solar atmosphere for the first time. Due to its statistical origin, this method provides a mechanism for determining the number of oscillations present, gives precise estimates of the oscillation parameters with a self-consistent statistical error analysis, and allows the oscillatory model signals to be reconstructed within these errors. A highly desirable feature of the Bayesian approach is the ability to resolve oscillations with extremely small frequency separations. The code is applied to SOHO CDS O v lambda 629 observations and resolves four distinct P-4; P-5; P-6, and P-7 p-modes within the same sunspot transition region. This suggests that a spectrum of photospheric p-modes is able to propagate into the upper atmosphere of the Sun and Sun-like stars, and places precise observational constraints on models of umbral eigenmodes. C1 [Kucera, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM mike.s.marsh@gmail.com RI Kucera, Therese/C-9558-2012; Marsh, Mike/I-3920-2012 OI Marsh, Mike/0000-0003-2765-0874 NR 30 TC 11 Z9 11 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 JUL 1 PY 2008 VL 681 IS 1 BP 672 EP 679 DI 10.1086/588751 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 321FM UT WOS:000257290100058 ER PT J AU Patanchon, G Ade, PAR Bock, JJ Chapin, EL Devlin, MJ Dicker, S Griffin, M Gundersen, JO Halpern, M Hargrave, PC Hughes, DH Klein, J Marsden, G Martin, PG Mauskopf, P Netterfield, CB Olmi, L Pascale, E Rex, M Scott, D Semisch, C Truch, MDP Tucker, C Tucker, GS Viero, MP Wiebe, DV AF Patanchon, G. Ade, P. A. R. Bock, J. J. Chapin, E. L. Devlin, M. J. Dicker, S. Griffin, M. Gundersen, J. O. Halpern, M. Hargrave, P. C. Hughes, D. H. Klein, J. Marsden, G. Martin, P. G. Mauskopf, P. Netterfield, C. B. Olmi, L. Pascale, E. Rex, M. Scott, D. Semisch, C. Truch, M. D. P. Tucker, C. Tucker, G. S. Viero, M. P. Wiebe, D. V. TI SANEPIC: A mapmaking method for time stream data from large arrays SO ASTROPHYSICAL JOURNAL LA English DT Article DE balloons; methods : data analysis; submillimeter; techniques : image processing ID MAP-MAKING ALGORITHM; MICROWAVE BACKGROUND EXPERIMENTS; CMB EXPERIMENTS; PLANCK SURVEYOR; ANISOTROPY; TELESCOPE; ARCHEOPS; NOISE AB We describe a mapmaking method that we have developed for the Balloon-borne Large Aperture Submillimeter Telescope (BLAST) experiment, but which should have general application to data from other submillimeter arrays. Our method uses a maximum likelihood-based approach, with several approximations, which allows images to be constructed using large amounts of data with fairly modest computer memory and processing requirements. This new approach, Signal and Noise Estimation Procedure Including Correlations (SANEPIC), builds on several previous methods but focuses specifically on the regime where there are a large number of detectors sampling the same map of the sky, and explicitly allowing for the possibility of strong correlations between the detector time streams. We provide real and simulated examples of how well this method performs compared with more simplistic mapmakers based on filtering. We discuss two separate implementations of SANEPIC: a brute-force approach, in which the inverse pixel-pixel covariance matrix is computed, and an iterative approach, which is much more efficient for large maps. SANEPIC has been successfully used to produce maps using data from the 2005 BLAST flight. C1 [Patanchon, G.; Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Patanchon, G.] Lab APC, F-75205 Paris, France. [Ade, P. A. R.; Griffin, M.; Hargrave, P. C.; Mauskopf, P.; Tucker, C.] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Bock, J. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bock, J. J.] CALTECH, Observ Cosmol, Pasadena, CA 91125 USA. [Devlin, M. J.; Dicker, S.; Klein, J.; Rex, M.; Semisch, C.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Gundersen, J. O.] Univ Miami, Dept Phys, Carol Gables, FL 33146 USA. [Hughes, D. H.] INAOE, Puebla 72000, Mexico. [Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Netterfield, C. B.; Pascale, E.; Wiebe, D. V.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Olmi, L.] Ist Radioastron, I-50125 Florence, Italy. [Olmi, L.] Univ Puerto Rico, Dept Phys, San Juan, PR 00931 USA. [Truch, M. D. P.; Tucker, G. S.] Brown Univ, Dept Phys, Providence, RI 02912 USA. [Martin, P. G.; Netterfield, C. B.; Viero, M. P.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. RP Patanchon, G (reprint author), Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. EM patanchon@apc.univ-paris7.fr RI Klein, Jeffrey/E-3295-2013; OI Olmi, Luca/0000-0002-1162-7947; Scott, Douglas/0000-0002-6878-9840 NR 32 TC 56 Z9 56 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2008 VL 681 IS 1 BP 708 EP 725 DI 10.1086/588543 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 321FM UT WOS:000257290100061 ER PT J AU Li, Y Lynch, BJ Stenborg, G Luhmann, JG Huttunen, KEJ Welsch, BT Liewer, PC Vourlidas, A AF Li, Y. Lynch, B. J. Stenborg, G. Luhmann, J. G. Huttunen, K. E. J. Welsch, B. T. Liewer, P. C. Vourlidas, A. TI The solar magnetic field and coronal dynamics of the eruption on 2007 May 19 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun : corona; Sun : coronal mass ejections (CMEs); Sun : filaments; Sun : flares; Sun : magnetic fields ID MASS EJECTION; FLUX ROPES; EVOLUTION; FILAMENT; TOPOLOGY; IMAGER; MODEL AB The solar eruption on 2007 May 19, from AR 10956 near solar disk center, consisted of a B9.5 flare ( 12: 48 UT), a filament eruption, an EUV dimming, a coronal wave, and a multifront CME. The eruption was observed by the twin STEREO spacecraft at a separation angle of 8.5 degrees. We report analysis of the source region photospheric magnetic field and its preeruption evolution using MDI magnetograms, the coronal magnetic field topology estimated via PFSS modeling, and the coronal dynamics of the eruption through STEREO EUVI wavelet-enhanced anaglyph movies. Despite its moderate magnitude and size, AR 10956 was a complex and highly nonpotential active region with a multipolar configuration, and hosted frequent flares, multiple filament eruptions, and CMEs. In the 2 days prior to the May 19 eruption, the total unsigned magnetic flux of the region decreased by similar to 17%. We interpret the photospheric magnetic field evolution, the coronal field topology, and the observed coronal dynamics in the context of current models of CME initiation and discuss the prospects for future MHD modeling inspired by these analyses. C1 [Li, Y.; Lynch, B. J.; Luhmann, J. G.; Huttunen, K. E. J.; Welsch, B. T.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Stenborg, G.] Interferometrics Inc, Herndon, VA USA. [Huttunen, K. E. J.] Univ Helsinki, Div Theoret Phys, Dept Phys Sci, FIN-00014 Helsinki, Finland. [Liewer, P. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Vourlidas, A.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. RP Li, Y (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM yanli@ssl.berkeley.edu; blynch@ssl.berkeley.edu; stenborg@kreutz.nascom.nasa.gov; jgluhman@ssl.berkeley.edu; huttunen@ssl.berkeley.edu; welsch@ssl.berkeley.edu; paulett.liewer@jpl.nasa.gov; vourlidas@nrl.navy.mil RI Vourlidas, Angelos/C-8231-2009; Kilpua, Emilia/G-8994-2012; Lynch, Benjamin/B-1300-2013; OI Vourlidas, Angelos/0000-0002-8164-5948; Lynch, Benjamin/0000-0001-6886-855X NR 25 TC 30 Z9 30 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 1 PY 2008 VL 681 IS 1 BP L37 EP L40 DI 10.1086/590340 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 326LO UT WOS:000257660800010 ER PT J AU Mandell, AM Mumma, MJ Blake, GA Bonev, BP Villanueva, GL Salyk, C AF Mandell, Avi M. Mumma, Michael J. Blake, Geoffrey A. Bonev, Boncho P. Villanueva, Geronimo L. Salyk, Colette TI Discovery of OH in circumstellar disks around young intermediate-mass stars SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE circumstellar matter; infrared : stars; molecular processes; planetary systems : formation; planetary systems : protoplanetary disks; stars : pre-main-sequence ID HERBIG AE/BE STARS; CO EMISSION; PROTOPLANETARY DISKS; BAND SYSTEM; INNER DISKS; AE STARS; COMETS; GAS; FLUORESCENCE; ULTRAVIOLET AB We detect emission from multiple low-excitation rovibrational transitions of OH from the two Herbig Ae stars AB Aurigae and MWC 758 in the 3.0-3.7 mu m wavelength range (L band), using the NIRSPEC instrument on Keck II. The inner radius for the emitting region in both stars is close to 1 AU. We compare an optically thin LTE model and a thin-wedge fluorescence model, finding rotational temperatures of 650-800 K and OH abundances of 10(42)-10(45) molecules for the two stars. Comparisons with current chemical models support the fluorescence excitation model for AB Aurigae and possibly MWC 758, but further observations and detailed modeling are necessary to improve constraints on OH emission in different disk environments. C1 [Mandell, Avi M.; Mumma, Michael J.; Bonev, Boncho P.; Villanueva, Geronimo L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Blake, Geoffrey A.; Salyk, Colette] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Bonev, Boncho P.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. RP Mandell, AM (reprint author), NASA, Goddard Space Flight Ctr, Code 693, Greenbelt, MD 20771 USA. EM avi.mandell@nasa.gov RI Mandell, Avi/F-9361-2012; mumma, michael/I-2764-2013 NR 31 TC 33 Z9 33 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 1 PY 2008 VL 681 IS 1 BP L25 EP L28 DI 10.1086/590180 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 326LO UT WOS:000257660800007 ER PT J AU Seymour, N Ogle, P De Breuck, C Fazio, GG Galametz, A Haas, M Lacy, M Sajina, A Stern, D Willner, SP Vernet, J AF Seymour, N. Ogle, P. De Breuck, C. Fazio, G. G. Galametz, A. Haas, M. Lacy, M. Sajina, A. Stern, D. Willner, S. P. Vernet, J. TI Mid-infrared spectra of high-redshift (z > 2) radio galaxies SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies : active; galaxies : evolution; galaxies : individual (4C+23.56, 4C+72.26) ID INFRARED LUMINOUS GALAXIES; STAR-FORMATION; HOST GALAXIES; DUST; QUASARS; Z-SIMILAR-TO-2; SPECTROSCOPY; POPULATION; FEATURES; AGN AB We present the first mid-infrared Spitzer/Infrared Spectrograph (IRS)observations of powerful radio galaxies at z > 2. These radio galaxies, 4C + 23.56 (z = 2.48) and 6C J1908 + 7220 (z = 3.53), both show strong mid- infrared continua, but with 6C J1908 + 7220 also showing strong PAH emission at rest-frame 6.2 and 7.7 mm. In 4C + 23.56 we see no obvious PAH features above the continuum. The PAH emission in 6C J1908 + 7220 is the among the most distant observed to date and implies that there is a large instantaneous star formation rate (SFR). This is consistent with the strong detection of 6C J1908 + 7220 at far-IR and sub-mm wavelengths, indicative of large amounts of cold dust, similar to 10(9) M(circle dot). Powerful radio galaxies at lower redshifts tend to have weak or M, undetectable PAH features and typically have lower far-IR luminosities. In addition, 4C + 23.56 shows moderate silicate absorption as seen in less luminous radio galaxies, indicating tau(9.7 mu m) = 0.3 +/- 0.05. This feature is shifted out of the observed wavelength range for 6C J1908 + 7220. The correlation of strong PAH features with large amounts of cold dust, despite the presence of a powerful AGN, is in agreement with other recent results and implies that star formation at high redshift is, in some cases at least, associated with powerful, obscured AGN. C1 [Seymour, N.; Ogle, P.; Lacy, M.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [De Breuck, C.; Galametz, A.; Vernet, J.] European So Observ, D-85748 Garching, Germany. [Fazio, G. G.; Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Galametz, A.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Haas, M.] Ruhr Univ Bochum, Inst Astron, D-44780 Bochum, Germany. [Sajina, A.] Haverford Coll, Dept Phys & Astron, Marian E Koshland Integrated Nat Sci Ctr, Haverford, PA 19041 USA. RP Seymour, N (reprint author), CALTECH, Spitzer Sci Ctr, 1200 E Calif Blvd, Pasadena, CA 91125 USA. EM seymour@ipac.caltech.edu OI Vernet, Joel/0000-0002-8639-8560; Seymour, Nicholas/0000-0003-3506-5536; De Breuck, Carlos/0000-0002-6637-3315 NR 34 TC 23 Z9 23 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 1 PY 2008 VL 681 IS 1 BP L1 EP L4 DI 10.1086/590081 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 326LO UT WOS:000257660800001 ER PT J AU Galache, JL Corbet, RHD Coe, MJ Laycock, S Schurch, MPE Markwardt, C Marshall, FE Lochner, J AF Galache, J. L. Corbet, R. H. D. Coe, M. J. Laycock, S. Schurch, M. P. E. Markwardt, C. Marshall, F. E. Lochner, J. TI A long look at the Be/X-ray binaries of the Small Magellanic Cloud SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Review DE galaxies : individual (Small Magellanic Cloud); pulsars : general; X-rays : binaries ID PROPORTIONAL COUNTER ARRAY; TRANSIENT RX J0117.6-7330; X-RAY; TIMING-EXPLORER; MULTIPERIODIC VARIABILITY; SPECTRAL-ANALYSIS; ORBITAL PERIOD; TIME-SERIES; SPACED DATA; XMM-NEWTON AB We have monitored 41 Be/X-ray binary systems in the Small Magellanic Cloud over similar to 9 yr using PCA RXTE data from a weekly survey program. The resulting light curves were analyzed in search of orbital modulations with the result that 10 known orbital ephemerides were confirmed and refined, while 10 new ones where determined. A large number of X-ray orbital profiles are presented for the first time, showing similar characteristics over a wide range of orbital periods. Lastly, three pulsars, SXP 46.4, SXP 89.0, and SXP 165, were found to be misidentifications of SXP 46.6, SXP 91.1, and SXP 169, respectively. C1 [Galache, J. L.; Laycock, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Corbet, R. H. D.; Markwardt, C.; Marshall, F. E.; Lochner, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Coe, M. J.; Schurch, M. P. E.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. RP Galache, JL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 107 TC 42 Z9 42 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUL PY 2008 VL 177 IS 1 BP 189 EP 215 DI 10.1086/587743 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 326PV UT WOS:000257672300009 ER PT J AU Turner, NJ Grogan, K Breckinridge, JB AF Turner, N. J. Grogan, K. Breckinridge, J. B. TI Probing interstellar dust with space-based coronagraphs SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE dust, extinction; radiative transfer; scattering; techniques : high angular resolution ID X-RAY HALO; SCATTERING PROPERTIES; SOLAR-SYSTEM; GRAINS; ULTRAVIOLET; NEBULA; CLOUD; HELIOSPHERE; TELESCOPE; MODEL AB We show that space-based telescopes such as the proposed Terrestrial Planet Finder Coronagraph will be able to detect the light scattered by the interstellar grains along lines of sight passing near stars in our Galaxy. The relative flux of the scattered light within 1 '' of a star at 100 pc in a uniform interstellar medium of 0.1 H atoms cm(-3) is about 10(-7). The halo increases in strength with the distance to the star and is unlikely to limit the coronagraphic detection of planets around the nearest stars. Grains passing within 100 AU of Sun-like stars are deflected by radiation, gravity, and magnetic forces, leading to features in the scattered light that can potentially reveal the strength of the stellar wind, the orientation of the stellar magnetic field and the relative motion between the star and the surrounding interstellar medium. C1 [Turner, N. J.; Grogan, K.; Breckinridge, J. B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Turner, NJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM neal.turner@jpl.nasa.gov NR 34 TC 0 Z9 0 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUL PY 2008 VL 177 IS 1 BP 335 EP 340 DI 10.1086/587061 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 326PV UT WOS:000257672300015 ER PT J AU Narayanan, G Heyer, MH Brunt, C Goldsmith, PF Snell, R Li, D AF Narayanan, Gopal Heyer, Mark H. Brunt, Christopher Goldsmith, Paul F. Snell, Ronald Li, Di TI The Five College Radio Astronomy Observatory CO mapping survey of the Taurus molecular cloud SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE ISM : clouds; ISM : general; ISM : kinematics and dynamics; ISM : molecules; surveys ID NARROW SELF-ABSORPTION; LARGE-SCALE STRUCTURE; STAR-FORMATION; DARK CLOUDS; CORES; GAS; HI; COMPLEX; EVOLUTION; GALAXY AB The FCRAO Survey of the Taurus molecular cloud observed the (12)CO and (13)CO J = 1-0 emission from 98 deg(2) of this important, nearby, star-forming region. This set of data with 45 '' resolution comprises the highest spatial dynamic range image of an individual molecular cloud constructed to date and provides valuable insights to the molecular gas distribution, kinematics, and the star formation process. In this contribution, we describe the observations, calibration, data processing, and characteristics of the noise and line emission of the survey. The angular distribution of (12)CO and (13)CO emission over 1 km s(-1) velocity intervals and the full velocity extent of the cloud are presented. These reveal a complex, dynamic medium of cold, molecular gas. C1 [Narayanan, Gopal; Heyer, Mark H.; Brunt, Christopher; Snell, Ronald] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Brunt, Christopher] Univ Exeter, Exeter, Devon, England. [Goldsmith, Paul F.; Li, Di] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Narayanan, G (reprint author), Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. EM gopal@astro.umass.edu RI Goldsmith, Paul/H-3159-2016 NR 24 TC 52 Z9 52 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUL PY 2008 VL 177 IS 1 BP 341 EP 361 DI 10.1086/587786 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 326PV UT WOS:000257672300016 ER PT J AU Aguilar, A Ajello, JM Mangina, RS James, GK Abgrall, H Roueff, E AF Aguilar, Alejandro Ajello, Joseph M. Mangina, Rao S. James, Geoffrey K. Abgrall, Herve Roueff, Evelyne TI The electron-excited mid-ultraviolet to near-infrared spectrum of H-2: Cross sections and transition probabilities SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE infrared : general; line : identification; molecular data; molecular processes; ultraviolet : general ID MOLECULAR-HYDROGEN; IMPACT EXCITATION; BAND SYSTEMS; TELESCOPE OBSERVATIONS; (1,3)DELTA(G) STATES; VACUUM-ULTRAVIOLET; EMISSION-SPECTRUM; TW-HYDRAE; MOMENTS; DISSOCIATION AB At high resolving power (lambda/Delta lambda approximate to 10; 000), we have measured the electron impactYinduced fluorescence spectrum of H-2 from 3300-10000 angstrom at 20 and 100 eV. We have analyzed the visible-optical-near-IR (VOIR) emission spectrum under optically thin, single-scattering experimental conditions. The high-resolution spectrum contains transitions from the gerade Rydberg series of singlet states to the ungerade series of Rydberg states (EF (1)Sigma(+)(g), GK (1)Sigma(+)(g), H (H) over bar (1)Sigma(+)(g), I-1 Pi(g), J(1)Delta(g)...-> B-1 Sigma(+)(u), C-1 Pi(u), B'(1)Sigma(+)(u), D-1 Pi(u)) and the Rydberg series of triplet states dominated by d(3)Pi(u), k(3)Pi(u), j(3)Delta(g) -> a(3)Sigma(g)' band systems. A model VOIR spectrum of H-2 from 7500 to 10000 angstrom, based on newly calculated transition probabilities and line positions including rovibrational coupling for singlet gerade states, is in excellent agreement with the observed intensities. The rotational line emission cross sections for direct excitation of the singlet states at 100 eV and triplet states at 20 eV were measured. The absolute cross section values for excitation to the singlet gerade states at 100 eV was measured to be (4: 58 +/- 1: 37); 10(-18) cm(2); the excitation cross section to the triplet states at 20 eV was found to be (1: 38 +/- 0: 41); 10(-18) cm(2). The singlet gerade emission cross sections are the cascading cross sections to the UV spectrum (including the Lyman and Werner band systems) and the triplet state emission cross sections are the cascade dissociation cross sections of the H-2 (a(3)Sigma(+)(g)-b(3)Sigma(+)(u)) continuum for the production of fast hydrogen atoms. Electrons are also effective in exciting high vibrational levels belonging to ungerade symmetry (B, B', C, D) which subsequently emit toward gerade symmetry states in the VOIR domain. Strong emission from the ungerade-gerade transitions are observed from 7300 to 7400 angstrom. C1 [Aguilar, Alejandro; Ajello, Joseph M.; Mangina, Rao S.; James, Geoffrey K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Observ Paris, CNRS, LUTII, F-92195 Meudon, France. Observ Paris, CNRS, UMR 8102, F-92195 Meudon, France. RP Aguilar, A (reprint author), Lawrence Berkeley Natl Lab, Adv Light Source, Berkeley, CA 94720 USA. NR 66 TC 11 Z9 11 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 JUL PY 2008 VL 177 IS 1 BP 388 EP 407 DI 10.1086/587690 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 326PV UT WOS:000257672300019 ER PT J AU Palmeri, P Quinet, P Mendoza, C Bautista, MA Garcia, J Kallman, TR AF Palmeri, P. Quinet, P. Mendoza, C. Bautista, M. A. Garcia, J. Kallman, T. R. TI Radiative and Auger decay of K-vacancy levels in the Ne, Mg, Si, S, Ar, and Ca isonuclear sequences SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE atomic processes; atomic data; line : formation; X-rays : general ID X-RAY-EMISSION; CHANDRA GRATING SPECTROSCOPY; F-LIKE IONS; ISOELECTRONIC SEQUENCE; LIFETIME MEASUREMENTS; ABSORPTION-LINES; FINE-STRUCTURE; SHELL AUGER; BE-LIKE; STATES AB The HFR and AUTOSTRUCTURE atomic structure codes are used to compute complete data sets of level energies, wavelengths, A-values, and radiative and Auger widths for K-vacancy states of the Ne, Mg, Si, S, Ar, and Ca isonuclear sequences. Ions with electron number N > 9 are treated for the first time. Detailed comparisons with previous measurements and theoretical data for ions with N <= 9 are carried out in order to estimate reliable accuracy ratings. C1 [Palmeri, P.; Quinet, P.] Univ Mons, B-7000 Mons, Belgium. [Mendoza, C.; Bautista, M. A.] IVIC, Ctr Fis, Caracas 1020A, Venezuela. [Garcia, J.; Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Palmeri, P (reprint author), Univ Mons, B-7000 Mons, Belgium. EM patrick.palmeri@umh.ac.be; pascal.quinet@umh.ac.be; claudio@ivic.ve; mbautist@ivic.ve; javier@milkyway.gsfc.nasa.gov; timothy.r.kallman@nasa.gov NR 52 TC 37 Z9 37 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 JUL PY 2008 VL 177 IS 1 BP 408 EP 416 DI 10.1086/587804 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 326PV UT WOS:000257672300020 ER PT J AU Jones, JA Cherian, SF Barr, YR Stocco, A AF Jones, Jeffrey A. Cherian, Sebastian F. Barr, Yael R. Stocco, Amber TI Medullary sponge kidney and urinary calculi: Aeromedical concerns SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE sponge kidney; aerospace medicine; weightlessness; nephrolithiasis ID MANAGEMENT AB Medullary sponge kidney (MSK) is a benign disorder associated with a lifetime risk of renal stones in 60% of patients. Patients frequently have episodic painless hematuria, but are often otherwise asymptomatic unless renal calculi or infections complicate the disease. Nephrolithiasis is a relative, but frequently enforced, contraindication to space or other high-performance flight. Two case reports of asymptomatic NASA flight crew with MSK and three cases of United States Air Force (USAF) military aviators diagnosed with MSK are reviewed. All cases resulted in waiver and return to flight status after treatment and a vigorous followup and prophylaxis protocol. MSK in aviation and spaceflight necessitates case-by-case evaluation and treatment to rule out other potential confounding factors that might also contribute to stone formation and in order to requalify the aviator for flight duties. C1 [Jones, Jeffrey A.] Methodist Hosp, Dept Radiol, St Louis Pk, MN USA. [Barr, Yael R.] Univ Texas Galveston, Med Branch, Galveston, TX 77550 USA. [Jones, Jeffrey A.; Stocco, Amber] Baylor Coll Med, Houston, TX 77030 USA. RP Jones, JA (reprint author), NASA JSC SD2, 2101 NASA Rd 1, Houston, TX 77058 USA. EM jeffery.a.jones@nasa.gov NR 31 TC 1 Z9 1 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 JUL PY 2008 VL 79 IS 7 BP 707 EP 711 DI 10.3357/ASEM.2255.2008 PG 5 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 320XQ UT WOS:000257268900011 PM 18619133 ER PT J AU Potter, C Boriah, S Steinbach, M Kumar, V Klooster, S AF Potter, Christopher Boriah, Shyam Steinbach, Michael Kumar, Vipin Klooster, Steven TI Terrestrial vegetation dynamics and global climate controls SO CLIMATE DYNAMICS LA English DT Article ID LEAF-AREA INDEX; SCALE ECOSYSTEM DISTURBANCES; NINO-SOUTHERN OSCILLATION; EL-NINO; INTERANNUAL VARIATIONS; SATELLITE DATA; RECENT HISTORY; CARBON-CYCLE; PRECIPITATION; CO2 AB Monthly data from the moderate resolution imaging spectroradiometer (MODIS) and its predecessor satellite sensors was used to reconstruct vegetation dynamics in response to climate patterns over the period 1983-2005. Results suggest that plant growth over extensive land areas of southern Africa and Central Asia were the most closely coupled of any major land area to E1 Nino-southern oscillation (ENSO) effects on regional climate. Others land areas strongly tied to recent ENSO climate effects were in northern Canada, Alaska, western US, northern Mexico, northern Argentina, and Australia. Localized variations in precipitation were the most common controllers of monthly values for the fraction absorbed of photosynthetically active radiation (FPAR) over these regions. In addition to the areas cited above, seasonal FPAR values from MODIS were closely coupled to rainfall patterns in grassland and cropland areas of the northern and central US. Historical associations between global vegetation FPAR and atmospheric carbon dioxide (CO2) anomalies suggest that the terrestrial biosphere can contribute major fluxes of CO2 during major drought events, such as those triggered by 1997-1998 E1 Nino event. C1 [Potter, Christopher] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Boriah, Shyam; Steinbach, Michael; Kumar, Vipin] Univ Minnesota, Minneapolis, MN USA. [Klooster, Steven] Calif State Univ Monterey Bay, Seaside, CA USA. RP Potter, C (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM cpotter@mail.arc.nasa.gov NR 53 TC 14 Z9 14 U1 0 U2 12 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0930-7575 EI 1432-0894 J9 CLIM DYNAM JI Clim. Dyn. PD JUL PY 2008 VL 31 IS 1 BP 67 EP 78 DI 10.1007/s00382-007-0339-5 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 301CZ UT WOS:000255875300005 ER PT J AU Cook, BI Bonan, GB Levis, S Epstein, HE AF Cook, Benjamin I. Bonan, Gordon B. Levis, Samuel Epstein, Howard E. TI The thermoinsulation effect of snow cover within a climate model SO CLIMATE DYNAMICS LA English DT Article DE snow cover; snow thermal conductivity; climate model sensitivity; soil/atmosphere exchange; permafrost ID GENERAL-CIRCULATION MODELS; ACTIVE-LAYER THICKNESS; GROUND THERMAL REGIME; COMMUNITY LAND MODEL; VERSION-3 CAM3; ATMOSPHERIC RESPONSE; ALBEDO FEEDBACK; GLOBAL CLIMATE; ARCTIC TUNDRA; SYSTEM MODEL AB We use a state of the art climate model (CAM3-CLM3) to investigate the sensitivity of surface climate and land surface processes to treatments of snow thermal conductivity. In the first set of experiments, the thermal conductivity of snow at each grid cell is set to that of the underlying soil (SC-SOIL), effectively eliminating any insulation effect. This scenario is compared against a control run (CTRL), where snow thermal conductivity is determined as a prognostic function of snow density. In the second set of experiments, high (SC-HI) and low (SC-LO) thermal conductivity values for snow are prescribed, based on upper and lower observed limits. These two scenarios are used to envelop model sensitivity to the range of realistic observed thermal conductivities. In both sets of experiments, the high conductivity/low insulation cases show increased heat exchange, with anomalous heat fluxes from the soil to the atmosphere during the winter and from the atmosphere to the soil during the summer. The increase in surface heat exchange leads to soil cooling of up to 20 K in the winter, anomalies that persist (though damped) into the summer season. The heat exchange also drives an asymmetric seasonal response in near-surface air temperatures, with boreal winter anomalies of +6 K and boreal summer anomalies of -2 K. On an annual basis there is a net loss of heat from the soil and increases in ground ice, leading to reductions in infiltration, evapotranspiration, and photosynthesis. Our results show land surface processes and the surface climate within CAM3-CLM3 are sensitive to the treatment of snow thermal conductivity. C1 [Cook, Benjamin I.] Columbia Univ, Lamont Doherty Geol Observ, Palisades, NY 10964 USA. [Cook, Benjamin I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Bonan, Gordon B.; Levis, Samuel] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Epstein, Howard E.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22903 USA. RP Cook, BI (reprint author), Columbia Univ, Lamont Doherty Geol Observ, 61 Route 9W,POB 1000, Palisades, NY 10964 USA. EM bc9z@ldeo.columbia.edu RI Cook, Benjamin/H-2265-2012 NR 64 TC 14 Z9 14 U1 1 U2 7 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0930-7575 EI 1432-0894 J9 CLIM DYNAM JI Clim. Dyn. PD JUL PY 2008 VL 31 IS 1 BP 107 EP 124 DI 10.1007/s00382-007-0341-y PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 301CZ UT WOS:000255875300007 ER PT J AU Goel, T Dorney, DJ Haftka, RT Shyy, W AF Goel, Tushar Dorney, Daniel J. Haftka, Raphael T. Shyy, Wei TI Improving the hydrodynamic performance of diffuser vanes via shape optimization SO COMPUTERS & FLUIDS LA English DT Article ID RESPONSE-SURFACE APPROXIMATION; DESIGN AB The performance of a diffuser in a pump stage depends on its configuration and placement within the stage. The influence of vane shape on the hydrodynamic performance of a diffuser has been studied. The goal of this effort has been to improve the performance of a pump stage by optimizing the shape of the diffuser vanes. The shape of the vanes was defined using Bezier curves and circular arcs. Surrogate model based tools were used to identify regions of the vane that have a strong influence on its performance. Optimization of the vane shape, in the absence of manufacturing and stress constraints, led to a nearly 8% reduction in the total pressure losses compared to the baseline design by reducing the base separation. (C) 2007 Elsevier Ltd. All rights reserved. C1 [Goel, Tushar; Haftka, Raphael T.] Univ Florida, Dept Mech & Aerosp Engn, Gainesville, FL 32611 USA. [Dorney, Daniel J.] NASA, George C Marshall Space Flight Ctr, ER42, Huntsville, AL 35812 USA. [Shyy, Wei] Univ Michigan, Dept Aerosp Engn, Ann Arbor, MI 48109 USA. RP Goel, T (reprint author), Livermore Software Technol Corp, Livermore, CA USA. EM tusharg@ufl.edu OI Shyy, Wei/0000-0001-6670-5394 NR 35 TC 26 Z9 31 U1 0 U2 11 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 JUL PY 2008 VL 37 IS 6 BP 705 EP 723 DI 10.1016/j.compfluid.2007.10.002 PG 19 WC Computer Science, Interdisciplinary Applications; Mechanics SC Computer Science; Mechanics GA 317XS UT WOS:000257054300005 ER PT J AU Brewer, R AF Brewer, Ron TI Evaluating lighting susceptibility SO EE-EVALUATION ENGINEERING LA English DT Article C1 NASA, Kennedy Space Ctr, Washington, DC 20546 USA. RP Brewer, R (reprint author), NASA, Kennedy Space Ctr, Washington, DC 20546 USA. NR 10 TC 0 Z9 0 U1 0 U2 0 PU NELSON PUBLISHING PI NOKOMIS PA 2500 NORTH TAMIAMI TRAIL, NOKOMIS, FL 34275-3482 USA SN 0149-0370 J9 EE-EVAL ENG JI EE-Eval. Eng. PD JUL PY 2008 VL 47 IS 7 BP 64 EP + PG 6 WC Engineering, Electrical & Electronic SC Engineering GA 323JU UT WOS:000257443200010 ER PT J AU Gensch, IV Bunz, H Baumgardner, DG Christensen, LE Fahey, DW Herman, RL Popp, PJ Smith, JB Troy, RF Webster, CR Weinstock, EM Wilson, JC Peter, T Kramer, M AF Gensch, I. V. Bunz, H. Baumgardner, D. G. Christensen, L. E. Fahey, D. W. Herman, R. L. Popp, P. J. Smith, J. B. Troy, R. F. Webster, C. R. Weinstock, E. M. Wilson, J. C. Peter, T. Kraemer, M. TI Supersaturations, microphysics and nitric acid partitioning in a cold cirrus cloud observed during CR-AVE 2006: an observation-modelling intercomparison study SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE cirrus clouds; supersaturations; nitric acid ID LOWER STRATOSPHERE; ICE NUCLEATION; RELATIVE-HUMIDITY; UPPER TROPOSPHERE; SPECTROMETER; PARTICLES; AEROSOL; HNO3; AIRCRAFT; ER-2 AB Supersaturations, microphysics and nitric acid partitioning in a very cold subvisible tropical cirrus cloud observed on 2 February 2006, during the field campaign CR-AVE, are studied by comparing a simulated set of possible cloud development scenarios with the in situ observations. The scenario that best matches the observations is a cirrus cloud forming by heterogeneous freezing of a small number of ice nuclei with subsequent unimpeded mass accommodation of water on ice. Variation of the freezing process, the accommodation coefficient or the amount of available water leads to simulated clouds that differ microphysically from the observed cloud in important respects. In particular, the simulations suggest that heterogeneous ice nucleation or another freezing mechanism producing only a low number of ice crystals could be an important process for cold cirrus cloud formation, possibly explaining the frequent observations of high supersaturations inside the cirrus cloud in this temperature regime. C1 [Gensch, I. V.; Kraemer, M.] Forschungszentrum Julich, ICG 1, Inst Chem & Dynam Geosphare, Julich, Germany. [Bunz, H.] Forschungszentrum Karlsruhe, Inst Meteorol & Klimaforsch, Karlsruhe, Germany. [Baumgardner, D. G.] Univ Nacl Autonoma Mexico, Mexico City 04510, DF, Mexico. [Christensen, L. E.; Herman, R. L.; Webster, C. R.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Fahey, D. W.; Popp, P. J.] NOAA, Earth Syst Res Lab, Div Chem Sci, Boulder, CO USA. [Smith, J. B.; Weinstock, E. M.] Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA. [Wilson, J. C.] Univ Colorado, Denver, CO 80202 USA. [Peter, T.] ETH, Inst Atmosphare & Klima, Zurich, Switzerland. RP Gensch, IV (reprint author), Forschungszentrum Julich, ICG 1, Inst Chem & Dynam Geosphare, Julich, Germany. EM m.kraemer@fz-juelich.de RI Herman, Robert/H-9389-2012; Kramer, Martina/A-7482-2013; Gensch, Iulia/J-8548-2014; Fahey, David/G-4499-2013; Manager, CSD Publications/B-2789-2015; OI Herman, Robert/0000-0001-7063-6424; Fahey, David/0000-0003-1720-0634; Gensch, Iulia/0000-0001-5235-4925 FU EU [SCOUT-O3]; Swiss National Foundation (SNF) FX We thank the scientific team of CR-AVE for providing the data. ECMWF provided the meteorological operational analyses. We thank the CLaMS-team of ICG-1, and especially Rolf P Muller, Forschungszentrum Julich, for support and useful discussions. We gratefully acknowledge Peter Spichtinger, ETH Zurich, for fruitful discussions and suggestions. This work was partly supported by the EU within SCOUT-O3 and by the Swiss National Foundation (SNF). Work performed at the Jet Propulsion Laboratory, California Institute of Technology, was done under contract with NASA. NR 35 TC 16 Z9 16 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-9326 J9 ENVIRON RES LETT JI Environ. Res. Lett. PD JUL-SEP PY 2008 VL 3 IS 3 AR 035003 DI 10.1088/1748-9326/3/3/035003 PG 9 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 353LN UT WOS:000259569300012 ER PT J AU Heintz, RA Short, JW Rice, SD Carls, MG AF Heintz, Ron A. Short, Jeffrey W. Rice, Stanley D. Carls, Mark G. TI Comment on "toxicity of weathered exxon valdez crude oil to pink salmon embryos" SO ENVIRONMENTAL TOXICOLOGY AND CHEMISTRY LA English DT Letter ID HERRING CLUPEA-PALLASI; ONCORHYNCHUS-GORBUSCHA; JAPANESE MEDAKA; FISH EMBRYOS; SPILL; SENSITIVITY; INDUCTION; MORTALITY; SURVIVAL; EXPOSURE C1 [Heintz, Ron A.; Short, Jeffrey W.; Rice, Stanley D.; Carls, Mark G.] Natl Marine Fisheries Serv, Auke Bay Lab, Juneau, AK 99801 USA. RP Heintz, RA (reprint author), Natl Marine Fisheries Serv, Auke Bay Lab, Juneau, AK 99801 USA. NR 15 TC 4 Z9 4 U1 0 U2 15 PU SOC ENVIRONMENTAL TOXICOLOGY & CHEMISTRY-SETAC PI PENSACOLA PA 1010 N 12TH AVE, PENSACOLA, FL 32501-3367 USA SN 0730-7268 J9 ENVIRON TOXICOL CHEM JI Environ. Toxicol. Chem. PD JUL PY 2008 VL 27 IS 7 BP 1475 EP 1476 DI 10.1897/07-236.1 PG 2 WC Environmental Sciences; Toxicology SC Environmental Sciences & Ecology; Toxicology GA 314JW UT WOS:000256806700002 PM 18260694 ER PT J AU Yen, E Chu, IWM AF Yen, Ester Chu, I-Wen Mike TI Image recognition via Bayesian likelihood analysis of wavelet coefficients SO EXPERT SYSTEMS WITH APPLICATIONS LA English DT Article DE wavelet decomposition; Daubechies family; statistical pattern recognition; multi-resolution representations AB This study experiments with a Bayesian approach in recognition of images utilizing a joint-form likelihood of wavelet coefficients built from decomposition. Images of handwritten numerals are attacked via the Mallet decomposition algorithm with Daubechies wavelets to extract the feature vectors of coefficients. The model assumes the coefficient vectors by multivariate normal distributions and employs a Bayesian approach for classification based on the joint form of distributions. The results demonstrate marked improvement in recognition performance at the second level of decomposition. (c) 2007 Elsevier Ltd. All rights reserved. C1 [Yen, Ester] Univ London Imperial Coll Sci Technol & Med, Dept Math, London, England. [Chu, I-Wen Mike] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Yen, E (reprint author), Univ London Imperial Coll Sci Technol & Med, Dept Math, London, England. EM ester_yen@yahoo.com NR 15 TC 1 Z9 1 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0957-4174 J9 EXPERT SYST APPL JI Expert Syst. Appl. PD JUL-AUG PY 2008 VL 35 IS 1-2 BP 556 EP 560 DI 10.1016/j.eswa.2007.07.005 PG 5 WC Computer Science, Artificial Intelligence; Engineering, Electrical & Electronic; Operations Research & Management Science SC Computer Science; Engineering; Operations Research & Management Science GA 325VR UT WOS:000257617100056 ER PT J AU Ponder, MA Thomashow, MF Tiedje, JM AF Ponder, Monica A. Thomashow, Michael F. Tiedje, James M. TI Metabolic activity of Siberian permafrost isolates, Psychrobacter arcticus and Exiguobacterium sibiricum, at low water activities SO EXTREMOPHILES LA English DT Article DE Psychrobacter; Siberian permafrost; Exiguobacterium; salt tolerance; low temperature; low water activity ID BACTERIAL-ACTIVITY; SP-NOV; MICROORGANISMS; SURVIVAL; ASTROBIOLOGY; POPULATIONS; STRATEGIES; PROTEIN; ICE; AGE AB The Siberian permafrost is an extreme, yet stable environment due to its continuously frozen state. Microbes maintain membrane potential and respiratory activity at average temperatures of -10 to -12 degrees C that concentrate solutes to an a(w) = 0.90 (5 osm), The isolation of viable Psychrobacter arcticus sp. 273-4 and Exiguobacterium sibiricum sp. 255-15 from ancient permafrost suggests that these bacteria have maintained some level of metabolic activity for thousands of years. Permafrost water activity was simulated using 1/2 TSB + 2.79 m NaCl (5 osm) at and cells were held at 22 and 4 degrees C. Many cells reduced cyano-tetrazolium chloride (CTC) indicating functioning electron transport systems. Increased membrane permeability was not responsible for this lack of electron transport, as more cells were determined to be intact by LIVE/DEAD staining than were reducing CTC. Low rates of aerobic respiration were determined by the slope of the reduced resazurin line for P. arcticus, and E. sibiricum. Tritiated leucine was incorporated into new proteins at rates indicating basal level metabolism. The continued membrane potential, electron transport and aerobic respiration, coupled with incorporation of radio-labeled leucine into cell material when incubated in high osmolarity media, show that some of the population is metabolically active under simulated in situ conditions. C1 [Ponder, Monica A.] Virginia Polytech Inst & State Univ, Dept Food Sci & Technol, Blacksburg, VA 24061 USA. [Ponder, Monica A.; Thomashow, Michael F.; Tiedje, James M.] Michigan State Univ, Dept Microbiol & Mol Genet, E Lansing, MI 48824 USA. [Thomashow, Michael F.; Tiedje, James M.] Michigan State Univ, Dept Crop & Soil Sci, E Lansing, MI 48824 USA. [Thomashow, Michael F.] Michigan State Univ, Plant Res Lab, MSU DOE, E Lansing, MI 48824 USA. [Ponder, Monica A.; Thomashow, Michael F.; Tiedje, James M.] Michigan State Univ, NASA, Astrobiol Inst Ctr Genom & Evolutionary Studies M, E Lansing, MI 48824 USA. RP Ponder, MA (reprint author), Virginia Polytech Inst & State Univ, Dept Food Sci & Technol, 101 Food Sci & Technol 0418, Blacksburg, VA 24061 USA. EM mponder@vt.edu NR 26 TC 17 Z9 17 U1 0 U2 12 PU SPRINGER TOKYO PI TOKYO PA 1-11-11 KUDAN-KITA, CHIYODA-KU, TOKYO, 102-0073, JAPAN SN 1431-0651 J9 EXTREMOPHILES JI Extremophiles PD JUL PY 2008 VL 12 IS 4 BP 481 EP 490 DI 10.1007/s00792-008-0151-0 PG 10 WC Biochemistry & Molecular Biology; Microbiology SC Biochemistry & Molecular Biology; Microbiology GA 320HO UT WOS:000257224500001 PM 18335164 ER PT J AU Maloney, NE Sigler, MF AF Maloney, Nancy E. Sigler, Michael F. TI Age-specific movement patterns of sablefish (Anoplopoma fimbria) in Alaska SO FISHERY BULLETIN LA English DT Article ID CANADAS WEST-COAST; TAGGED SABLEFISH; PACIFIC; WATERS; RECOVERIES; MANAGEMENT; HARENGUS; GULF AB Over 34,000 age 0-2 juvenile sablefish (Anoplopoma fimbria) were tagged and released in southeast Alaska waters during 1985-2005. The data set resulting from this tagging study was unusual because of its time span (20 years) and because age could be reliably inferred from release length (i.e., tagged and released fish were of known age); thus, age-specific movement patterns could be examined. The depth- and area-related recovery patterns supported the concepts that sablefish move to deeper water with age and migrate counterclockwise in the Gulf of Alaska. Availability to the fishery increased rapidly for fish of younger ages, peaked at age 5 to 6, and then gradually declined as sablefish moved deeper with age. Decreased availability with age may occur because of lower fishing effort in deep water and could have substantial implications for sablefish stock assessments because "dome-shaped" availability influences the reliability of abundance estimates. The area-related recovery pattern was not affected by year-class strength; i.e., there was no significant density-dependent relationship. C1 [Maloney, Nancy E.; Sigler, Michael F.] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr,Auke Bay Labs, Ted Stevens Marine Res Inst, Juneau, AK 99801 USA. RP Maloney, NE (reprint author), NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr,Auke Bay Labs, Ted Stevens Marine Res Inst, 17109 Point Lena Loop Rd, Juneau, AK 99801 USA. EM Nancy.Maloney@noaa.gov RI Bizzarro, Joseph/A-2988-2012 NR 38 TC 10 Z9 10 U1 0 U2 3 PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE PI SEATTLE PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA SN 0090-0656 J9 FISH B-NOAA JI Fish. Bull. PD JUL PY 2008 VL 106 IS 3 BP 305 EP 316 PG 12 WC Fisheries SC Fisheries GA 328WM UT WOS:000257828900008 ER PT J AU Alpers, CN Majzlan, J Koch, CB Bishop, JL Coleman, ML Dyar, MD McCleskey, RB Myneni, SCB Nordstrom, DK Sobron, P AF Alpers, C. N. Majzlan, J. Koch, C. Bender Bishop, J. L. Coleman, M. L. Dyar, M. D. McCleskey, R. B. Myneni, S. C. B. Nordstrom, D. K. Sobron, P. TI Chemistry and spectroscopy of iron-sulfate minerals from iron mountain, California, USA SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Alpers, C. N.] US Geol Survey, Sacramento, CA 95819 USA. [Majzlan, J.] Univ Freiburg, Freiburg, Germany. [Koch, C. Bender] Univ Copenhagen, Frederiksberg C, Denmark. [Bishop, J. L.] SETI Inst, Mountain View, CA USA. [Coleman, M. L.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Dyar, M. D.] Mt Holyoke Coll, S Hadley, MA 01075 USA. [McCleskey, R. B.; Nordstrom, D. K.] US Geol Survey, Boulder, CO USA. [Myneni, S. C. B.] Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA. [Sobron, P.] Univ Valladolid, Valladolid, Spain. EM cnalpers@usgs.gov; juraj.majzlan@minpet.uni-freiburg.de; cbk@life.ku.dk; jbishop@seti.org; mitx.coleman@jpl.nasa.gov; mddyar@amherst.edu; rbmccles@usgs.gov; smyneni@princeton.edu; dkn@usgs.gov; psobron@iq.uva.es RI Koch, Chr./D-4670-2011; Koch, Christian /C-7070-2013 OI Koch, Christian /0000-0002-7496-297X NR 0 TC 2 Z9 2 U1 1 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A17 EP A17 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301600040 ER PT J AU Beegle, LW Johnson, PV Hoydess, R Mielke, R Orzechowska, GE Sollitt, L Kanik, I AF Beegle, Luther W. Johnson, Paul V. Hoydess, Robert Mielke, Randall Orzechowska, Grazyna E. Sollitt, Luke Kanik, Isik TI Toward the in situ quantification of organic molecules in solid samples: Development of sample handling and processing hardware SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Beegle, Luther W.; Johnson, Paul V.; Hoydess, Robert; Mielke, Randall; Orzechowska, Grazyna E.; Kanik, Isik] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Sollitt, Luke] Northrope Gtrumman Space Technol, Redondo Beach, CA 90278 USA. EM Luther.Beegle@jpl.nasa.gov RI Beegle, Luther/A-6354-2010 NR 3 TC 1 Z9 1 U1 0 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A66 EP A66 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301600139 ER PT J AU Bennett, V Brandon, A Nutman, A Wan, Y Black, L AF Bennett, V. Brandon, A. Nutman, A. Wan, Y. Black, L. TI The search for global variations in Nd-142 isotopic compositions of Eoarchean rocks SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA ID DIFFERENTIATION; EARTH C1 [Bennett, V.] Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT 0200, Australia. [Brandon, A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Nutman, A.; Wan, Y.] Chinese Acad Geol Sci, Beijing, Peoples R China. [Black, L.] Geosci Australia, Canberra, ACT, Australia. EM vickie.bennett@anu.edu.au NR 7 TC 1 Z9 1 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A73 EP A73 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301600152 ER PT J AU Benning, LG Eigenbrode, JL Maule, J Wainwright, N Steele, A Amundsen, HEF AF Benning, L. G. Eigenbrode, J. L. Maule, J. Wainwright, N. Steele, A. Amundsen, H. E. F. CA AMASE 2005 2006 TEAMS TI Organic decontamination of sampling devices for life-detection studies SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Benning, L. G.] Univ Leeds, Sch Earth & Environm, Earth & Biosphere Inst, Leeds LS2 9JT, W Yorkshire, England. [Eigenbrode, J. L.; Maule, J.; Steele, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Eigenbrode, J. L.] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. [Wainwright, N.] Charles River Labs Inc, Charleston, SC USA. [Amundsen, H. E. F.; AMASE 2005 2006 TEAMS] Earth & Planetary Explorat, Oslo, Norway. [Maule, J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM liane@see.leeds.ac.uk RI Eigenbrode, Jennifer/D-4651-2012 NR 0 TC 0 Z9 0 U1 1 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A73 EP A73 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301600153 ER PT J AU Bhartia, R Hug, WF Red, RD Salas, EC Nealson, KH Lane, AL AF Bhartia, R. Hug, W. F. Red, R. D. Salas, E. C. Nealson, K. H. Lane, A. L. TI Deep UV native fluorescence and resonance Raman spectroscopy for life-detection SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Bhartia, R.; Lane, A. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hug, W. F.; Red, R. D.] Photon Syst Inc, Covina, CA 91722 USA. [Salas, E. C.; Nealson, K. H.] Univ So Calif, Los Angeles, CA 90089 USA. EM rbhartia@jpl.nasa.gov; w.hug@photonsystems.com; r.reid@photonsystems.com; everetts@usc.edu; knealson@usc.edu; allane@jpl.nasa.gov NR 7 TC 2 Z9 2 U1 2 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A80 EP A80 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301600167 ER PT J AU Brady, A Slater, GF Laval, B Lim, DSS AF Brady, A. Slater, G. F. Laval, B. Lim, D. S. S. TI Isotopic biosignatures associated with freshwater microbialites and carbonate precipitating microbial mats SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Brady, A.; Slater, G. F.] McMaster Univ, Sch Geog & Earth Sci, Hamilton, ON, Canada. [Laval, B.] Univ British Columbia, Dept Civil Engn, Vancouver, BC, Canada. [Lim, D. S. S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM bradyal@mcmaster.ca; gslater@mcmaster.ca; blaval@civil.ubc.ca; Darlene.S.Lim@nasa.gov RI Laval, Bernard/J-9861-2012; Slater, Greg/B-5163-2013 OI Slater, Greg/0000-0001-7418-7566 NR 0 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A109 EP A109 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301600224 ER PT J AU Brandon, AD AF Brandon, A. D. TI The controversy on the bulk Sm/Nd of the Moon SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Brandon, A. D.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM alan.d.brandon@nasa.gov NR 2 TC 0 Z9 0 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A111 EP A111 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301600228 ER PT J AU Claire, MW Catling, DC Zahnle, KJ AF Claire, M. W. Catling, D. C. Zahnle, K. J. TI The great collapse of methane: Rethinking the rise of Oxygen SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA ID ATMOSPHERIC OXYGEN C1 [Claire, M. W.; Catling, D. C.] Univ Washington, Washington, DC USA. [Catling, D. C.] Univ Bristol, Bristol, Avon, England. [Zahnle, K. J.] NASA, Ames Res Ctr, Washington, DC USA. EM mclaire@astro.washington.edu; David.Catling@bristol.ac.uk; Kevin.J.Zahnle@nasa.gov RI Catling, David/D-2082-2009 NR 8 TC 0 Z9 0 U1 1 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A166 EP A166 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301600339 ER PT J AU Cohen, BA AF Cohen, B. A. TI Compositional and geochronological constraints on the lunar cataclysm SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA ID HISTORY; METEORITES; AGES C1 [Cohen, B. A.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM Barbara.A.Cohen@nasa.gov NR 11 TC 0 Z9 0 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A172 EP A172 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301600350 ER PT J AU Coleman, M Rohrssen, M Mielke, R AF Coleman, M. Rohrssen, M. Mielke, R. TI A potential mineral paleo-humidity measure for Martian hydrated evaporite minerals: First results SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Coleman, M.; Rohrssen, M.; Mielke, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM max.coleman@jpl.nasa.gov NR 2 TC 0 Z9 0 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A173 EP A173 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301600352 ER PT J AU Dalton, HA Lee, CTA Peslier, AH Brandon, AD Lapen, T AF Dalton, H. A. Lee, C. -T. A. Peslier, A. H. Brandon, A. D. Lapen, T. TI Trace element analysis and petrology of Martian meteorite RBT04262 SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Dalton, H. A.; Lee, C. -T. A.] Rice Univ, Dept Earth Sci, Houston, TX 77251 USA. [Peslier, A. H.; Brandon, A. D.] NASA JSC, ARES, Houston, TX 77058 USA. [Peslier, A. H.] ESCG, Jacobs Tech, Houston, TX 77058 USA. [Lapen, T.] Univ Houston, Dept Geosci, Houston, TX 77204 USA. EM heather.a.dalton@rice.edu; ctlee@rice.edu; anne.h.peslier@nasa.gov; alan.d.brandon@nasa.gov; tjlapen@uh.edu RI Peslier, Anne/F-3956-2010 NR 1 TC 0 Z9 0 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A195 EP A195 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301600397 ER PT J AU Debaille, V Brandon, AD Yin, QZ Jacobsen, B AF Debaille, V. Brandon, A. D. Yin, Q. -Z. Jacobsen, B. TI The age, duration, and depth of a turbulent magma ocean in Mars SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Debaille, V.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Brandon, A. D.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Yin, Q. -Z.; Jacobsen, B.] Univ Calif Davis, Davis, CA 95616 USA. EM vinciane.debaille@ulb.ac.be; alan.d.brandon@nasa.gov; yin@geology.ucdavis.edu; jacobsen@geology.ucdavis.edu NR 0 TC 1 Z9 1 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A205 EP A205 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301600416 ER PT J AU Des Marais, DJ AF Des Marais, D. J. TI Exploring for photosynthesis in deep time and space SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Des Marais, D. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A212 EP A212 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301600431 ER PT J AU Fike, DA Gammon, CL Finke, N Hoehler, T Turk, K Orphan, VJ AF Fike, David A. Gammon, Crystal L. Finke, Niko Hoehler, Tori Turk, Kendra Orphan, Victoria J. TI Micron-scale mapping of sulfur cycling across the oxycline of a cyanobacterial mat SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Fike, David A.; Gammon, Crystal L.; Orphan, Victoria J.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Finke, Niko; Hoehler, Tori; Turk, Kendra] NASA Ames Res Ctr, Moffett Field, CA 94035 USA. EM dfike@gps.caltech.edu; gammon@gps.caltech.edu; nfinke@web.de; tori.m.hoehler@nasa.gov; kendra.A.Turk@nasa.gov; vorphan@aps.caltech.edu RI Orphan, Victoria/K-1002-2014 OI Orphan, Victoria/0000-0002-5374-6178 NR 0 TC 2 Z9 2 U1 0 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A268 EP A268 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301600542 ER PT J AU Flynn, GJ Wirick, S Keller, LP Messenger, S Jacobsen, C AF Flynn, G. J. Wirick, S. Keller, L. P. Messenger, S. Jacobsen, C. TI Microscale characterization of the organic matter in extraterrestrial samples SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA ID INTERPLANETARY DUST PARTICLES; MOLECULAR-CLOUD MATERIAL C1 [Flynn, G. J.] SUNY Coll Plattsburgh, Dept Phys, Plattsburgh, NY 12901 USA. [Wirick, S.; Jacobsen, C.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Keller, L. P.; Messenger, S.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM george.flynn@plattsburgh.edu RI Jacobsen, Chris/E-2827-2015 OI Jacobsen, Chris/0000-0001-8562-0353 NR 4 TC 0 Z9 0 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A276 EP A276 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301600558 ER PT J AU Guest, A Smrekar, SE AF Guest, A. Smrekar, S. E. TI New constraints on the thermal and volatile evolution of Mars SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Guest, A.] LMU, D-80333 Munich, Germany. [Smrekar, S. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM alice.guest@iaag.geo.uni-muenchen.de; ssmrekar@jpl.nasa.gov NR 4 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A334 EP A334 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301600674 ER PT J AU Guo, W Daeron, M Niles, P Genty, D Kim, ST Vonhof, H Affek, H Wainer, K Blamart, D Eiler, J AF Guo, W. Daeron, M. Niles, P. Genty, D. Kim, S. -T. Vonhof, H. Affek, H. Wainer, K. Blamart, D. Eiler, J. TI C-13-O-18 bonds in dissolved inorganic carbon: Implications for carbonate clumped isotope thermometry SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Guo, W.; Daeron, M.; Eiler, J.] CALTECH, Pasadena, CA 91125 USA. [Daeron, M.; Genty, D.; Wainer, K.; Blamart, D.] CEA Univ, CNRS, Versailles St Quentin, France. [Niles, P.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Kim, S. -T.] Univ Maryland, College Pk, MD 20742 USA. [Vonhof, H.] Vrije Univ Amsterdam, Amsterdam, Netherlands. [Affek, H.] Yale Univ, New Haven, CT USA. EM wfguo@gps.caltech.edu; eiler@gps.caltech.edu RI Guo, Weifu/E-8876-2010; Kim, Sang-Tae/C-2768-2013 NR 0 TC 10 Z9 10 U1 1 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A336 EP A336 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301600679 ER PT J AU Hausrath, EM Golden, DC Morris, RV Ming, DW AF Hausrath, E. M. Golden, D. C. Morris, R. V. Ming, D. W. TI Phosphate alteration on Mars SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA ID BASALTIC GLASS DISSOLUTION; CONSEQUENCES; MECHANISM; RATES C1 [Hausrath, E. M.; Golden, D. C.; Morris, R. V.; Ming, D. W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM Elisabeth.M.Hausrath@nasa.gov NR 6 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A357 EP A357 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301600721 ER PT J AU Hillion, F Kilburn, MR Hoppe, P Messenger, S Weber, PK AF Hillion, F. Kilburn, M. R. Hoppe, P. Messenger, S. Weber, P. K. TI The effect of QSA on S, C, O and Si isotopic ratio measurements SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Hillion, F.] Cameca SA, Gennevilliers, France. [Kilburn, M. R.] Univ Western Australia, Crawley 6009, Australia. [Hoppe, P.] Max Planck Inst Chem, D-55128 Mainz, Germany. [Messenger, S.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Weber, P. K.] Lawrence Livermore Natl Lab, Livermore, CA USA. RI Kilburn, Matthew/C-4515-2011; Hoppe, Peter/B-3032-2015 OI Kilburn, Matthew/0000-0002-1858-8485; Hoppe, Peter/0000-0003-3681-050X NR 2 TC 8 Z9 8 U1 0 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A377 EP A377 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301601018 ER PT J AU Hoehler, TM Alperin, MJ McCollom, TM Rogers, K AF Hoehler, Tori M. Alperin, Marc J. McCollom, Thomas M. Rogers, Karyn TI Habitability of serpentinizinig systems for methanogenic microorganisms: An energy balance model SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Hoehler, Tori M.] NASA, Ames Res Ctr, Washington, DC USA. [Alperin, Marc J.] Univ N Carolina, Chapel Hill, NC 27515 USA. [McCollom, Thomas M.] Univ Colorado, Boulder, CO 80309 USA. [Rogers, Karyn] Univ Missouri, Columbia, MO 65211 USA. EM tori.m.hochler@nasa.gov; alperin@email.unc.edu; tom.mccollom@lasp.colorado.edu; rogerskl@missouri.edu NR 0 TC 1 Z9 1 U1 0 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A383 EP A383 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301601029 ER PT J AU Hurowitz, JA AF Hurowitz, J. A. TI A similar to 3.5By record of water-limited, acidic weathering on Mars SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Hurowitz, J. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM joel.a.hurowitz@jpl.nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A404 EP A404 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301601071 ER PT J AU Jones, JH AF Jones, J. H. TI Nd isotopic constraints on the relative sizes of Martian reservoirs SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA ID METEORITES C1 [Jones, J. H.] NASA, JSC, KR, Houston, TX 77058 USA. EM john.h.jones@nasa.gov NR 5 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A438 EP A438 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301601139 ER PT J AU Keller, LP Nakamura-Messenger, K Messenger, S AF Keller, L. P. Nakamura-Messenger, K. Messenger, S. TI Mineralogy and chemistry of stardust samples SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Keller, L. P.; Messenger, S.] NASA, Lyndon B Johnson Space Ctr, Code KR, Houston, TX 77058 USA. [Nakamura-Messenger, K.] NASA, Lyndon B Johnson Space Ctr, ESCG, Houston, TX 77058 USA. EM Lindsay.P.Keller@nasa.gov; Keiko.Nakamura@nasa.gov; Scott.R.Messenger@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A459 EP A459 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301601181 ER PT J AU Lapen, TJ Brandon, AD Beard, BL Peslier, AH Lee, CTA Dalton, HA AF Lapen, T. J. Brandon, A. D. Beard, B. L. Peslier, A. H. Lee, C-T. A. Dalton, H. A. TI Age and Lu-Hf isotope systematics of RBT04262 and implications for the sources of enriched shergottites SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Lapen, T. J.] Univ Houston, Dept Geosci, Houston, TX 77204 USA. [Brandon, A. D.; Peslier, A. H.] NASA, JSC, Houston, TX 77058 USA. [Beard, B. L.] UW Madison, Dept Geol & Geophys, Madison, WI 53704 USA. [Peslier, A. H.] Jacobs Tech, ESCG, Houston, TX 77058 USA. [Lee, C-T. A.; Dalton, H. A.] Rice Univ, Houston, TX 77251 USA. EM tjlapen@uh.edu; alan.d.brandon@nasa.gov; beardb@geology.wisc.edu; anne.h.peslier@nasa.gov; ctlee@rice.edu RI Peslier, Anne/F-3956-2010 NR 1 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 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A516 EP A516 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301601296 ER PT J AU Malavergne, V Berthet, S Jones, J AF Malavergne, Valerie Berthet, Sophie Jones, John TI New views about the composition of Mercury's core and its magnetic field origin SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Malavergne, Valerie; Berthet, Sophie] Univ Paris Est, Lab Geomat & Geol Ingn G2I, EA 4119, F-77454 Champs Sur Marne 2, Marne La Vallee, France. [Malavergne, Valerie; Berthet, Sophie] Lunar & Planetary Inst, Houston, TX 77058 USA. [Jones, John] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A588 EP A588 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301601439 ER PT J AU Matrajt, G Messenger, S Ito, M Joswiak, D Brownlee, D AF Matrajt, G. Messenger, S. Ito, M. Joswiak, D. Brownlee, D. TI Study of the C-rich phases of two cometary particles with electron microscopy and nanoSIMS SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Matrajt, G.; Joswiak, D.; Brownlee, D.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Messenger, S.; Ito, M.] Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM matrajt@astro.washington.edu; scott.r.messenger@nasa.gov NR 0 TC 1 Z9 1 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A603 EP A603 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301601469 ER PT J AU Morrill, PL Johnson, OJ Cotton, J Eigenbrode, JL Nealson, KH Lollar, BS Fogel, ML AF Morrill, P. L. Johnson, O. J. Cotton, J. Eigenbrode, J. L. Nealson, K. H. Lollar, B. Sherwood Fogel, M. L. TI Isotopic evidence of microbial methane in ultrabasic reducing waters at a continental site of active serpentinization in N. California SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Morrill, P. L.] McMaster Univ, Hamilton, ON, Canada. [Johnson, O. J.; Nealson, K. H.] Univ So Calif, Los Angeles, CA USA. [Cotton, J.] Johns Hopkins Univ, Baltimore, MD USA. [Eigenbrode, J. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lollar, B. Sherwood] Univ Toronto, Toronto, ON, Canada. [Fogel, M. L.] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. EM morrilp@mcmaster.ca RI Eigenbrode, Jennifer/D-4651-2012 NR 0 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 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A652 EP A652 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301601566 ER PT J AU Nakamura-Messenger, K Messenger, S Keller, LP Clemett, SJ Zolensky, ME AF Nakamura-Messenger, K. Messenger, S. Keller, L. P. Clemett, S. J. Zolensky, M. E. TI Presolar organic globules in astromaterials SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Nakamura-Messenger, K.; Clemett, S. J.] NASA, Lyndon B Johnson Space Ctr, ESCG, Houston, TX 77058 USA. [Messenger, S.; Keller, L. P.] NASA, Lyndon B Johnson Space Ctr, Code KR, Houston, TX 77058 USA. [Zolensky, M. E.] NASA, Lyndon B Johnson Space Ctr, Code KT, Houston, TX 77058 USA. EM keiko.nakamura-1@nasa.gov; scott.r.messenger@nasa.gov; lindsay.p.keller@nasa.gov NR 6 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 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A671 EP A671 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301601604 ER PT J AU Oehler, DZ Robert, F Chaussidon, M Gibson, EK AF Oehler, D. Z. Robert, F. Chaussidon, M. Gibson, E. K. TI Bona fide biosignatures: Insights from combined NanoSIMS-SIMS SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Oehler, D. Z.; Gibson, E. K.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Robert, F.] Museum Natl Hist Nat, Lab Etud Mat Extraterr, F-75005 Paris, France. [Chaussidon, M.] CNRS, CRPG, F-54501 Vandoeuvre Les Nancy, France. EM dorothy.z.oehler@nasa.gov NR 2 TC 0 Z9 0 U1 1 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A698 EP A698 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301601658 ER PT J AU Papineau, D Purohit, R Goldberg, T Pi, D Shields, G Bhu, H Fogel, ML AF Papineau, D. Purohit, R. Goldberg, T. Pi, D. Shields, G. Bhu, H. Fogel, M. L. TI High primary productivity and denitrification after the Paleoproterozoic phosphogenic event in the Aravalli Supergroup, India SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Papineau, D.; Fogel, M. L.] Carnegie Inst Washington, Astrobiol Inst, NASA, Washington, DC 20005 USA. [Papineau, D.; Fogel, M. L.] Carnegie Inst Washington, Geophys Lab, Washington, DC 20005 USA. [Goldberg, T.] Univ Newcastle, Sch Civil Eng & Geosci, Callaghan, NSW 2308, Australia. [Pi, D.] Chinese Acad Sci, State Key Lab, Beijing 100864, Peoples R China. [Shields, G.] U Coll London, Dept Earth Sci, London, England. EM dpapineau@ciw.edu RI Shields, Graham/B-6285-2009 OI Shields, Graham/0000-0002-7828-3966 NR 0 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A722 EP A722 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301601707 ER PT J AU Peslier, A Brandon, A Lapen, T Lee, CT AF Peslier, A. Brandon, A. Lapen, T. Lee, C. -T. TI Petrology of new Martian meteorite LAR06319, an olivine-pheric Basaltic Shergottite SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Peslier, A.] Jacobs Tech, Houston, TX USA. [Peslier, A.; Brandon, A.] NASA, JSC, Houston, TX USA. [Lapen, T.] U Houston, Houston, TX USA. [Lee, C. -T.] Rice Univ, Houston, TX USA. EM anne.h.peslier@nasa.gov; alan.d.brandon@nasa.gov; tjlapen@uh.edu; ctlee@rice.edu RI Peslier, Anne/F-3956-2010 NR 0 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A738 EP A738 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301601739 ER PT J AU Stern, JC Sonke, JE Salters, VJM AF Stern, Jennifer C. Sonke, Jeroen E. Salters, Vincent J. M. TI Thorium complexation by humic acid: Results from ligand competition experiments SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Stern, Jennifer C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sonke, Jeroen E.] CNRS, IRD, LMTG, Toulouse, France. [Salters, Vincent J. M.] NHMFL & FSU, Tallahassee, FL 32310 USA. EM Jennifer.Stern@nasa.gov; sonke@lmtg.obs-mip.fr; salters@magnet.fsu.edu RI Stern, Jennifer/E-3135-2012; Salters, Vincent/F-9792-2014 OI Stern, Jennifer/0000-0002-0162-8807; Salters, Vincent/0000-0002-5669-7869 NR 0 TC 1 Z9 1 U1 0 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A898 EP A898 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301602320 ER PT J AU Stoeser, DB Wilson, SA Fikes, J McLemore, C Rickman, D AF Stoeser, D. B. Wilson, S. A. Fikes, J. McLemore, C. Rickman, D. TI Development of lunar highland regolith simulants, NU-LHT-1M,-2M SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Stoeser, D. B.; Wilson, S. A.] USGS, Denver, CO 80225 USA. [Fikes, J.; McLemore, C.; Rickman, D.] NASA, MSFC, Huntsville, AL 35812 USA. EM dstoeser@usgs.gov; swilson@usgs.gov; john.fikes@nasa.gov; carole.a.mcleinore@nasa.gov; Doug.Rickman@nasa.gov NR 0 TC 2 Z9 2 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A902 EP A902 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301602329 ER PT J AU Tosca, NJ Milliken, RE Wyatt, MB AF Tosca, N. J. Milliken, R. E. Wyatt, M. B. TI An experimental approach to clay mineral formation on Mars SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Tosca, N. J.] Harvard Univ, Dept Organism & Evolutionary Biol, Boston, MA 02138 USA. [Milliken, R. E.] Jet Prop Lab, Pasadena, CA 91001 USA. [Wyatt, M. B.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. EM ntosca@fas.harvard.edu NR 0 TC 0 Z9 0 U1 0 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A952 EP A952 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301602429 ER PT J AU Zahnle, K Arndt, N Cockell, C Halliday, A Nisbet, E Selsis, F Sleep, NH AF Zahnle, Kevin Arndt, Nick Cockell, Charles Halliday, Alex Nisbet, Euan Selsis, Franck Sleep, Norman H. TI Emergence of a habitable planet SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Zahnle, Kevin] NASA, Ames Res Ctr, Washington, DC USA. [Arndt, Nick] LGCA, Grenoble, France. [Halliday, Alex] Univ Oxford, Oxford OX1 2JD, England. [Nisbet, Euan] U London, London, England. [Selsis, Franck] Univ Lyon, Lyon, France. [Sleep, Norman H.] Stanford Univ, Stanford, CA 94305 USA. EM Kevin.J.Zahnle@nasa.gov; arndt@ujf-grenoble.fr; c.s.cockell@open.ac.uk; alex.halliday@earth.ox.ac.uk; e.nisbet@gl.rhul.ac.uk; franck.selsis@ens-lyon.fr; norm@pangea.standford.edu NR 1 TC 0 Z9 0 U1 3 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A1070 EP A1070 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301602664 ER PT J AU Ziegler, K Coleman, ML Young, ED AF Ziegler, K. Coleman, M. L. Young, Edward D. TI Tracing the source of oxygen during pyrite oxidation with Delta O-17(SO4) SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Ziegler, K.; Young, Edward D.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Coleman, M. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Young, Edward D.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. EM kziegler@ess.ucla.edu NR 3 TC 1 Z9 1 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A1106 EP A1106 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301602736 ER PT J AU Zolensky, ME AF Zolensky, M. E. TI Wild 2 olivine, low-Ca pyroxene and sulfides SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 18th Annual V M Goldschmidt Conference CY JUL, 2008 CL Vancouver, CANADA C1 [Zolensky, M. E.] NASA, Lyndon B Johnson Space Ctr, KT, Houston, TX 77058 USA. EM michael.e.zolensky@nasa.gov NR 3 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUL PY 2008 VL 72 IS 12 SU 1 BP A1107 EP A1107 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321JU UT WOS:000257301602738 ER PT J AU Nieves-Chinchilla, T Vinas, AF AF Nieves-Chinchilla, T. Vinas, A. F. TI Kappa-like distribution functions inside magnetic clouds SO GEOFISICA INTERNACIONAL LA English DT Article DE electrons; Kappa-like velocity distribution function; megnatic cloud ID PARAMETERS; WIND AB This work presents a study of the electron suprathermal tails profile and its temperature inside of the magnetic clouds. We have modeled the electron velocity distribution function as a superposition of two populations: core (Maxwellian) and halo (Tsallis or kappa-like). The kappa parameter value, which characterizes the supra-thermal tail of the electron halo component has been estimated. We have found, based upon the events studied here, that there are no significant differences in the values of the kappa parameter, inside and outside magnetic clouds. C1 [Nieves-Chinchilla, T.; Vinas, A. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Nieves-Chinchilla, T (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. EM Teresa.Nieves@nasa.com; adolfo.figueroa-vinas.1@gsfc.nasa.gov RI Nieves-Chinchilla, Teresa/F-3482-2016 OI Nieves-Chinchilla, Teresa/0000-0003-0565-4890 NR 7 TC 6 Z9 6 U1 0 U2 0 PU INST GEOPHYSICS UNAM PI MEXICO PA APDO POSTAL 22-118, DEL TLALPAN, MEXICO, 14000 D F, MEXICO SN 0016-7169 J9 GEOFIS INT JI Geofis. Int. PD JUL-SEP PY 2008 VL 47 IS 3 BP 245 EP 249 PG 5 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326QE UT WOS:000257673200014 ER PT J AU Finnegan, NJ Pritchard, ME Lohman, RB Lundgren, PR AF Finnegan, Noah J. Pritchard, Mathew E. Lohman, Rowena B. Lundgren, Paul R. TI Constraints on surface deformation in the Seattle, WA, urban corridor from satellite radar interferometry time-series analysis SO GEOPHYSICAL JOURNAL INTERNATIONAL LA English DT Article DE time series analysis; radar interferometry; hydrology; intra-plate processes; continental tectonics : compressional; North America ID CASCADIA FORE-ARC; PUGET LOWLAND; SAR INTERFEROGRAMS; WASHINGTON; FAULT; SUBSIDENCE; ALGORITHM; MIGRATION; CALDERA; INSAR AB We apply differential InSAR (DInSAR) time-series techniques to the urban corridor between Tacoma, Seattle and Everett, WA, using 93 interferograms from three satellites (ERS 1, ERS 2 and RADARSAT-1) between 1992 and 2007. Our goal is to study local tectonic, geomorphic and groundwater processes. Consequently, we remove long-wavelength (> 50-100 km) deformation signals from unwrapped interferograms. By comparing surface velocities generated via the time-series technique at more than two million points within the overlapping region between two independent ERS tracks, we estimate the uncertainty of relative surface velocity measurements to be similar to 0.5 mm yr(-1) in the vertical. We estimate the uncertainty of relative displacement measurements to be similar to 5.4 mm, given our comparisons of DInSAR-derived time-series to GPS data, a result that is consistent both with previous DInSAR time-series analysis and with the uncertainty expected from GPS displacements projected onto the radar line-of-sight. Active tectonic deformation at shallow depths on the region's numerous east-west structures is absent over the similar to 11.5 yr of SAR data examined. Assuming that the south-dipping thrust beneath Seattle and Tacoma takes up 3 mm yr(-1) of north-south shortening, our data indicate that the fault must be currently locked to a depth of greater than 10 km. We also document extensive groundwater-related deformation throughout much of the study region. Most notably, we identify sharp, linear deformation gradients near Federal Way, WA, and running between Sumner, WA, and Steilacoom, WA. These features may mark the locations of previously unmapped fault splays that locally control groundwater movement. We find no slow landslide deformation on any of the numerous mapped slide complexes within Seattle, although regions of known active landsliding, such as along Perkins Lane in Seattle, exhibit radar phase de-correlation. These observations are consistent with relatively infrequent and rapid landslide deformation within Seattle. C1 [Finnegan, Noah J.; Pritchard, Mathew E.; Lohman, Rowena B.] Cornell Univ, Dept Earth & Atmospher Sci, Ithaca, NY 14850 USA. [Lundgren, Paul R.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Finnegan, NJ (reprint author), Cornell Univ, Dept Earth & Atmospher Sci, Ithaca, NY 14850 USA. EM njf7@cornell.edu RI Lohman, Rowena/C-2324-2013; Pritchard, Matthew/L-5892-2015 OI Lohman, Rowena/0000-0001-7240-3165; Pritchard, Matthew/0000-0003-3616-3373 NR 45 TC 13 Z9 13 U1 0 U2 9 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0956-540X EI 1365-246X J9 GEOPHYS J INT JI Geophys. J. Int. PD JUL PY 2008 VL 174 IS 1 BP 29 EP 41 DI 10.1111/j.1365-246X.2008.03822.x PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 311QS UT WOS:000256615300004 ER PT J AU Larmat, C Montagner, JP Capdeville, Y Banerdt, WB Lognonne, P Vilotte, JP AF Larmat, C. Montagner, J. P. Capdeville, Y. Banerdt, W. B. Lognonne, P. Vilotte, J. -P. TI Numerical assessment of the effects of topography and crustal thickness on martian seismograms using a coupled modal solution-spectral element method SO ICARUS LA English DT Article DE Geophysics; Mars; surface; Earth ID THERMAL EVOLUTION; PLANETARY SEISMOLOGY; INTERNAL STRUCTURE; MARS; DICHOTOMY; MODELS; MANTLE; WAVES; VENUS; EARTH AB The past 4 decades of Mars exploration have provided much information about the Mars surface, when its interior structure remains relatively poorly constrained. Today available data are compatible with a large range of model parameters. Seismology is able to provide valuable additional data but the number of seismographs will likely be quite limited, specially in the early-stage of future Mars seismic networks. It is thus of importance to be able to correctly isolate effects induced by the crust structure. Mars topography is characterized by spectacular reliefs like the Tharsis bulge or the Hellas basin and by the so-called "Mars dichotomy": the north hemisphere is made up of low-altitude plains above a relatively thin crust when the south hemisphere is characterized by a thick crust sustaining high reliefs. The aim of this paper is to study the effects induced on seismograms by the topography of the surface and crust-mantle discontinuities. Synthetic seismograms were computed using the coupled spectral element-modal solution method, which reduces the numerical cost by limiting the use of the spectral element method to the regions where lateral variations, like the presence of a topography, are considered. Due to numerical cost, this study is limited to long period and thus focuses on surface waves, mainly on long period Rayleigh waves. We show that reliefs like the Tharsis bulge or the Hellas basin can induce an apparent velocity anomaly up to 0.5% when only the surface topography is introduced. Apparent anomalies can raise up to 1.0% when the surface topography is fully compensated by a mirror-image topography of the crust-mantle discontinuity. Travel-time of surface wave are systematically increased for seismometers in the north hemisphere of Mars and decreased in the south hemisphere. When comparing effects on seismograms by the Earth and Mars topography, we found them to be larger for the Earth. It is due to the fact that we work with a seismic velocity model of Mars with a mean crust thickness of 110 km when the crust thickness has a mean value of 50 km for the Earth. When changing the Mars model for a thinner crust with a mean thickness of 50 km, effects by the topography on Mars seismograms becomes of the same order when not larger than what is observed on the Earth. (c) 2008 Elsevier Inc. All rights reserved. C1 [Larmat, C.; Montagner, J. P.; Capdeville, Y.; Vilotte, J. -P.] IPGP Case 89, Lab Sismol Globale, F-75252 Paris 05, France. [Banerdt, W. B.] Jet Prop Lab, Pasadena, CA 91109 USA. [Lognonne, P.] IPGP, Lab Planetol & Etudes Spatiales, F-94107 St Maur Des Fosses, Saint Maur, France. RP Larmat, C (reprint author), IPGP Case 89, Lab Sismol Globale, 4 Pl Jussieu, F-75252 Paris 05, France. EM carene@lanl.gov RI Montagner, Jean-Paul/A-8733-2011; Larmat, Carene/B-4686-2011; Lognonne, Philippe/F-8846-2010; OI Montagner, Jean-Paul/0000-0001-9958-3012; Larmat, Carene S/0000-0002-3607-7558 NR 43 TC 6 Z9 7 U1 1 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD JUL PY 2008 VL 196 IS 1 BP 78 EP 89 DI 10.1016/j.icarus.2007.12.030 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 310NR UT WOS:000256536800006 ER PT J AU McAdam, AC Zolotov, MY Sharp, TG Leshin, LA AF McAdam, Amy C. Zolotov, Mikhail Yu. Sharp, Thomas G. Leshin, Laurie A. TI Preferential low-pH dissolution of pyroxene in plagioclase-pyroxene mixtures: Implications for martian surface materials SO ICARUS LA English DT Article DE Mars; surface; Mineralogy ID THERMAL EMISSION SPECTROMETER; MARS; ROCKS; RATES; CONSTRAINTS; MECHANISM; VOLCANO; CRYSTALLIZATION; TEMPERATURE; DEPOSITION AB Acid weathering of plagioclase-pyroxene mixtures has been investigated with an open system kinetic dissolution model. The modeling reveals that elevated plagioclase/pyroxene ratios observed in some low-albedo martian regions and atmospheric dust could be partially caused by preferential dissolution of pyroxenes at pHs below similar to 3-4. Surface materials with smaller grain sizes, affected by lower pH fluids, and/or exposed to longer durations of acid weathering would be enriched in plagioclase. If preferential dissolution is responsible for the observed mineral ratios, the dissolution process likely occurred on a large scale, such as weathering by acid atmospheric precipitates. If dissolution was continuous, modeled timeframes required to produce a high plagioclase/pyroxene ratio are short on geologic timescales; however, it is likely that acid weathering on Mars was episodic, possibly occurring over a longer period of time. (c) 2008 Elsevier Inc. All rights reserved. C1 [McAdam, Amy C.; Zolotov, Mikhail Yu.; Sharp, Thomas G.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Leshin, Laurie A.] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA. RP McAdam, AC (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Box 871404, Tempe, AZ 85287 USA. EM amcadam@asu.edu RI McAdam, Amy/E-1556-2012 NR 58 TC 19 Z9 19 U1 0 U2 12 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUL PY 2008 VL 196 IS 1 BP 90 EP 96 DI 10.1016/j.icarus.2008.01.008 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 310NR UT WOS:000256536800007 ER PT J AU Mitri, G Showman, AP Lunine, JI Lopes, RMC AF Mitri, Giuseppe Showman, Adam P. Lunine, Jonathan I. Lopes, Rosaly M. C. TI Resurfacing of Titan by ammonia-water cryomagma SO ICARUS LA English DT Article DE Titan; Saturn; volcanism; satellites; surfaces; interiors; ices; geophysics ID FRACTURE-MECHANICS APPROACH; PLANETOLOGICAL APPLICATIONS; INTERNAL STRUCTURE; BOTTOM CREVASSES; SURFACE; EUROPA; FEATURES; ORIGIN; METHANE; LIQUID AB The Cassini Titan Radar Mapper observed on Titan several large features interpreted as cryovolcanic during the October 26, 2004 pass at high northern latitudes [Lopes, R.M.C., and 43 colleagues, 2007. Icarus 186, 395-412]. To date, models of ammonia-water resurfacing have not been tied to specific events or evolutionary stages of Titan. We propose a model of cryovolcanism that involves cracking at the base of the ice shell and formation of ammonia-water pockets in the ice. As these ammonia-water pockets undergo partial freezing in the cold ice shell, the ammonia concentration in the pockets increases, decreasing the negative buoyancy of the ammonia-water mixture. If the ice shell is contaminated by silicates delivered in impacts, the liquid-solid density difference would be even less. While the liquid cannot easily become buoyant relative to the surrounding ice, these concentrated ammonia-water pockets are sufficiently close to the neutral buoyancy point that large-scale tectonic stress patterns (tides, non-synchronous rotation, satellite volume changes, solid state convection, or subsurface pressure gradients associated with topography) would enable the ammonia to erupt effusively onto the surface. Rather than suggesting steady-state volcanism over the history of the Solar System, we favor a scenario where the cryovolcanic features could have been associated with episodic (potentially late) geological activity. (c) 2008 Elsevier Inc. All rights reserved. C1 [Mitri, Giuseppe; Lopes, Rosaly M. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Showman, Adam P.; Lunine, Jonathan I.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Showman, Adam P.; Lunine, Jonathan I.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Lunine, Jonathan I.] INAF IFSI, Rome, Italy. RP Mitri, G (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM giuseppe.mitri@jpl.nasa.gov RI Lopes, Rosaly/D-1608-2016 OI Lopes, Rosaly/0000-0002-7928-3167 NR 43 TC 54 Z9 54 U1 2 U2 17 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUL PY 2008 VL 196 IS 1 BP 216 EP 224 DI 10.1016/j.icarus.2008.02.024 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 310NR UT WOS:000256536800016 ER PT J AU Bonev, BP Mumma, MJ Kawakita, H Kobayashi, H Villanueva, GL AF Bonev, Boncho P. Mumma, Michael J. Kawakita, Hideyo Kobayashi, Hitomi Villanueva, Gerommo L. TI IRCS/Subaru observations of water in the inner coma of Comet 73P-B/Schwassmann-Wachmann 3: Spatially resolved rotational temperatures and ortho-para ratios SO ICARUS LA English DT Article DE comets, coma; comets, origin; Comet 73-B/Schwassmann-Wachmann 3; infrared observations; spectroscopy ID CARBON-MONOXIDE; SPIN TEMPERATURES; SUBARU TELESCOPE; HALLEYS-COMET; FRAGMENT-C; C/1996 B2; HALE-BOPP; EMISSION; P/HALLEY; MODEL AB Comet 73P-B/Schwassmann-Wachmann 3 was observed with IRCS/Subaru at geocentric distance of 0.074 AU on UT 10 May 2006. Multiple H(2)O emission lines were detected in non-resonant fluorescence near 2.9 mu m. No significant variation in total H(2)O production rate was found during the (3 h) duration of our observations. H(2)O rotational temperatures and ortho-to-para abundance ratios were measured for several positions in the coma. The temperatures extracted from two different time intervals show very similar spatial distributions. For both, the rotational temperature decreased from similar to 110 to similar to 90 K as the projected distance from the nucleus increased from similar to 5 to similar to 30 km. We see no evidence for OPR change in the coma. The H(2)O ortho-para ratio is consistent with the statistical equilibrium value (3.0) for all spatially resolved measurements. This implies a nuclear spin temperature higher than similar to 45 K. (c) 2008 Elsevier Inc. All rights reserved. C1 [Bonev, Boncho P.; Mumma, Michael J.; Villanueva, Gerommo L.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Bonev, Boncho P.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Kawakita, Hideyo; Kobayashi, Hitomi] Kyoto Sangyo Univ, Dept Phys, Fac Sci, Kita Ku, Kyoto 6038555, Japan. RP Bonev, BP (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. EM bonev@cua.edu RI mumma, michael/I-2764-2013 NR 45 TC 17 Z9 17 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD JUL PY 2008 VL 196 IS 1 BP 241 EP 248 DI 10.1016/j.icarus.2008.02.023 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 310NR UT WOS:000256536800018 ER PT J AU Bills, BG Nimmo, F AF Bills, Bruce G. Nimmo, Francis TI Forced obliquity and moments of inertia of Titan SO ICARUS LA English DT Article DE Titan; rotational dynamics; tides ID TIDALLY EVOLVING SATELLITES; LONG-TERM EVOLUTION; LUNAR SPIN AXIS; INTERNAL STRUCTURE; INTERIOR STRUCTURE; GRAVITY-FIELD; EARTH; DYNAMICS; MERCURY; VENUS AB The obliquity of Titan is small, but certainly non-zero, and may be used to place constraints on Titan's internal structure. The measured gravity coefficients of Titan imply that it is non-hydrostatic and thus the normal Darwin-Radau approach to determining internal structure cannot be applied. However, if the obliquity is assumed to be tidally damped (that is, in a Cassini state) then combining the obliquity with the measured gravity coefficients allows Titan's moment of inertia to be determined without invoking hydrostatic equilibrium. For polar moment values in the range(0.3 < C/MR2 < 0.4), tidally-damped obliquity values of (0.115 degrees < vertical bar epsilon vertical bar < 0.177 degrees) result. If the inferred moment value exceeds 0.4, this strongly suggests the presence of a near-surface ice shell decoupled from the interior, probably by a subsurface ocean. (c) Published by Elsevier Inc. C1 [Bills, Bruce G.] Univ Calif San Diego, Scripps Inst Oceanog, Inst Geophys & Planetary Phys, La Jolla, CA 92093 USA. [Bills, Bruce G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Nimmo, Francis] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. RP Bills, BG (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Inst Geophys & Planetary Phys, La Jolla, CA 92093 USA. EM bbills@ucsd.edu RI Bills, Bruce/C-1156-2008 NR 53 TC 25 Z9 25 U1 0 U2 8 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD JUL PY 2008 VL 196 IS 1 BP 293 EP 297 DI 10.1016/j.icarus.2008.03.002 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 310NR UT WOS:000256536800023 ER PT J AU Elfes, A Hall, JL Kulczycki, EA Clouse, DS Morfopoulos, AC Montgomery, JF Cameron, JM Ansar, A Machuzak, RJ AF Elfes, Alberto Hall, Jeffery L. Kulczycki, Eric A. Clouse, Daniel S. Morfopoulos, Arin C. Montgomery, James F. Cameron, Jonathan M. Ansar, Adnan Machuzak, Richard J. TI Autonomy architecture for aerobot exploration of Saturnian moon Titan SO IEEE AEROSPACE AND ELECTRONIC SYSTEMS MAGAZINE LA English DT Article AB The Huygens probe arrived at Saturn's moon, Titan, January 14, 2005, unveiling a world that is radically different from any other in the solar system. The data obtained, complemented by continuing observations from the Cassini spacecraft, show methane lakes, river channels and drainage basins, sand dunes, cryovolcanos and sierras. This has led to an enormous scientific interest in a follow-up mission to Titan, using a robotic lighter-than-air vehicle (or aerobot). Aerobots have modest power requirements, can fly missions with extended durations, and have very long distance traverse capabilities. They can execute regional surveys, transport and deploy scientific instruments and in-situ laboratory facilities over vast distances, and also provide surface sampling at strategic science sites. This describes our progress in the development of the autonomy technologies that will be required for exploration of Titan. We provide an overview of the autonomy architecture and some of its key components. We also show results obtained from autonomous flight tests conducted in the Mojave Desert(1,2). C1 [Elfes, Alberto; Hall, Jeffery L.; Kulczycki, Eric A.; Clouse, Daniel S.; Morfopoulos, Arin C.; Montgomery, James F.; Cameron, Jonathan M.; Ansar, Adnan; Machuzak, Richard J.] Jet Prop Lab, Pasadena, CA 91109 USA. RP Elfes, A (reprint author), Jet Prop Lab, Pasadena, CA 91109 USA. RI Elfes, Alberto/E-2463-2011 OI Elfes, Alberto/0000-0003-2433-995X NR 16 TC 5 Z9 5 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0885-8985 J9 IEEE AERO EL SYS MAG JI IEEE Aerosp. Electron. Syst. Mag. PD JUL PY 2008 VL 23 IS 7 BP 16 EP 24 DI 10.1109/MAES.2008.4579287 PG 9 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA 331RS UT WOS:000258030900003 ER PT J AU Woollard, D Mattmann, CA Medvidovic, N Gil, Y AF Woollard, David Mattmann, Chris A. Medvidovic, Nenad Gil, Yolanda TI Scientific software as workflows: From discovery to distribution SO IEEE SOFTWARE LA English DT Article ID SYSTEMS C1 [Woollard, David; Mattmann, Chris A.] NASA, Jet Prop Lab, Washington, DC 20546 USA. [Medvidovic, Nenad; Gil, Yolanda] Univ So Calif, Dept Comp Sci, Los Angeles, CA 90089 USA. [Gil, Yolanda] Univ So Calif, Inst Informat Sci, Intelligent Syst Div, Los Angeles, CA 90089 USA. RP Woollard, D (reprint author), NASA, Jet Prop Lab, Washington, DC 20546 USA. EM woollard@ipl.nasa.gov; mattmann@ipl.nasa.gov; neno@usc.edu; gil@isi.edu NR 14 TC 12 Z9 12 U1 0 U2 1 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA SN 0740-7459 J9 IEEE SOFTWARE JI IEEE Softw. PD JUL-AUG PY 2008 VL 25 IS 4 BP 37 EP 43 DI 10.1109/MS.2008.92 PG 7 WC Computer Science, Software Engineering SC Computer Science GA 316RD UT WOS:000256966500009 ER PT J AU Lee, SC Hook, LR AF Lee, Samuel C. Hook, Loyd R. TI Logic and computer design in nanospace SO IEEE TRANSACTIONS ON COMPUTERS LA English DT Article DE sequential logic; hypercube; nanocomputer; logic design; nanotechnology ID HYPERCUBES; SYSTEMS AB Techniques for the advanced logic design of nanodevices and nanoICs in spatial dimensions are being formulated to incorporate specific topologies that satisfy certain requirements of nanotechnology. One of these topologies, the hypercube, is currently being considered for the design of a network-based combinational logic implementation in the form of a hypercube extension called the N-hypercube. We propose the M-hypercube, using a similar topology to design any sequential logic in spatial dimensions. To reduce the complexity of the M-hypercube design, two methods, a top-down and a bottom-up, are presented. The former uses sequential machine decomposition methods and the latter uses a new hypercube topology, called the MN-cell. The MN-cell, consisting of two closely coupled 2D hypercubes, an M-hypercube and an N-hypercube, is a 3D hypercube. It is shown that MN-cells can implement flip-flops and thus can be used as building blocks for sequential logic design in nanodimensions. The logic design of a basic computer in nanospace using MN-cells and N-hypercubes is also presented using several examples. C1 [Lee, Samuel C.] Univ Oklahoma, Sch Elect & Comp Engn, Norman, OK 73019 USA. [Hook, Loyd R.] NASA, Dryden Flight Res Ctr, Edwards AFB, CA 93523 USA. RP Lee, SC (reprint author), Univ Oklahoma, Sch Elect & Comp Engn, Rm 218 Carson Engn Ctr,202 W Boyd St, Norman, OK 73019 USA. EM samlee@ou.edu; loydhook@hotmail.com NR 27 TC 6 Z9 6 U1 0 U2 2 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA SN 0018-9340 J9 IEEE T COMPUT JI IEEE Trans. Comput. PD JUL PY 2008 VL 57 IS 7 BP 965 EP 977 DI 10.1109/TC.2007.70812 PG 13 WC Computer Science, Hardware & Architecture; Engineering, Electrical & Electronic SC Computer Science; Engineering GA 303KK UT WOS:000256039200009 ER PT J AU Kurtz, NT Markus, T Cavalieri, DJ Krabill, W Sonntag, JG Miller, J AF Kurtz, Nathan T. Markus, Thorsten Cavalieri, Donald J. Krabill, William Sonntag, John G. Miller, Jeffrey TI Comparison of ICESat data with airborne laser altimeter measurements over Arctic sea ice SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Ice, Cloud, and land Elevation Satellite (ICESat); laser altimeter; remote sensing; sea ice ID SNOW DEPTH; THICKNESS; OCEAN; COVER AB Surface elevation and roughness measurements from NASA's Ice, Cloud, and land Elevation Satellite (ICESat) are compared with high-resolution airborne laser altimeter measurements over the Arctic sea ice north of Alaska, which were taken during the March 2006 EOS Aqua Advanced Microwave Scanning Radiometer sea ice validation campaign. The comparison of the elevation measurements shows that they agree quite well with correlations of around 0.9 for individual shots and a bias of less than 2 cm. The differences are found to decrease quite rapidly when applying running means. The comparison of the roughness measurements show that there are significant differences between the two data sets, with ICESat generally having higher values. The roughness values are only moderately correlated on an individual-shot basis, but applying running means to the data significantly improves the correlations to as high as 0.9. For the conversion of the elevation measurements into snow-ice freeboard, ocean surface elevation estimates are made with the high-resolution laser altimeter data, as well as several methods using lower resolution ICESat data. Under optimum conditions, i.e., when leads that are larger than the ICESat footprint are present, the ICESat- and Airborne Topographic Mapper-derived freeboards are found to agree to within 2 cm. For other areas, ICESat tends to underestimate the freeboard by up to 9 cm. C1 [Kurtz, Nathan T.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. [Markus, Thorsten; Cavalieri, Donald J.] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA. [Krabill, William; Sonntag, John G.] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA. [Sonntag, John G.] EG&G Tech Serv Inc, Gaithersburg, MD 20878 USA. [Miller, Jeffrey] RS Informat Syst, Mclean, VA 22102 USA. RP Kurtz, NT (reprint author), Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. RI Markus, Thorsten/D-5365-2012 NR 27 TC 34 Z9 38 U1 1 U2 15 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD JUL PY 2008 VL 46 IS 7 BP 1913 EP 1924 DI 10.1109/TGRS.2008.916639 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 321DP UT WOS:000257285200004 ER PT J AU Yang, P Kattawar, GW Hong, G Minnis, P Hu, YX AF Yang, Ping Kattawar, George W. Hong, Gang Minnis, Patrick Hu, Yongxiang TI Uncertainties associated with the surface texture of ice particles in satellite-based retrieval of cirrus clouds - Part I: Single-scattering properties of ice crystals with surface roughness SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE ice crystals; light scattering; ray-tracing; surface roughness ID LIGHT-SCATTERING; RADIATIVE PROPERTIES; INFRARED RADIANCES; ALGORITHM; INFERENCE; COLUMNS; CLIMATE; PHASE; MODIS AB Surface roughness of ice crystals is a morphological parameter important to the scattering characteristics of these particles. The intent of this paper, reported in two parts (hereafter, Parts I and II), is to investigate the accuracy associated with some simplifications in calculating the single-scattering properties of roughened ice crystals and to quantify the effect of surface roughness on the retrieval of the optical and microphysical properties of ice clouds from satellite observations. In Part I, two ray-tracing schemes, a rigorous algorithm and an approximate algorithm with a simplified treatment of surface roughness, are employed to calculate the single-scattering properties of randomly oriented hexagonal ice crystals with size parameters in the geometric optics regime. With the rigorous approach, it requires substantial computational effort to accurately account for the multiple external reflections between various roughness facets and the reentries of outgoing rays into the particles in the ray-tracing computation. With the simplified ray-tracing scheme, the ray-tracing calculation for roughened particles is similar to that for smooth particles except that, in the former case, the normal of the particle surface is statistically perturbed for each reflection-refraction event. The simplified ray-tracing scheme can account for most the effects of surface roughness on particle single-scattering properties without incurring substantial demand on computational resources and, thus, provides an efficient way to compute the single-scattering properties of roughened particles. The effect of ice-crystal surface roughness on the retrieval of the optical thicknesses and effective particle sizes of cirrus clouds is reported in Part II. C1 [Yang, Ping; Hong, Gang] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. [Kattawar, George W.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. [Minnis, Patrick; Hu, Yongxiang] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA. RP Yang, P (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. EM pyang@ariel.met.tamu.edu RI Minnis, Patrick/G-1902-2010; Yang, Ping/B-4590-2011; Hong, Gang/A-2323-2012; Hu, Yongxiang/K-4426-2012 OI Minnis, Patrick/0000-0002-4733-6148; NR 28 TC 41 Z9 41 U1 1 U2 17 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD JUL PY 2008 VL 46 IS 7 BP 1940 EP 1947 DI 10.1109/TGRS.2008.916471 PG 8 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 321DP UT WOS:000257285200006 ER PT J AU Yang, P Hong, G Kattawar, GW Minnis, P Hu, YX AF Yang, Ping Hong, Gang Kattawar, George W. Minnis, Patrick Hu, Yongxiang TI Uncertainties associated with the surface texture of ice particles in satellite-based retrieval of cirrus clouds: Part II - Effect of particle surface roughness on retrieved cloud optical thickness and effective particle size SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE effective particle size; ice crystals; optical depth; remote sensing; scattering; surface roughness ID BULK SCATTERING PROPERTIES; LIGHT-SCATTERING; MICROPHYSICAL PROPERTIES; INFRARED RADIANCES; MODIS DATA; CRYSTALS; SENSITIVITY; PARAMETERIZATION; MODELS; REFLECTANCE AB The simplified ray-tracing technique reported in Part I of this paper is employed to compute the single-scattering properties of hexagonal columns with maximum dimensions ranging from 2 to 3500 mu m with a size-bin resolution of 2 mu m at wavelengths of 0.86 and 2.13 mu m. For small ice crystals, the current treatment of surface roughness may not be adequate because the applicability of the principles of geometric optics breaks down for small roughness scale. However, for ice crystals smaller than 40 mu m, the aspect ratios of these particles are close to one, and the effect of surface roughness is quite small. In this paper, the diffraction is accounted for in the same way as in the case of smooth particles. It is essentially unfeasible to incorporate the effect of surface roughness into the numerical computation of the diffraction contribution. The scattering properties of individual ice crystals are then averaged over 18 particle size distributions whose effective particle radii (r(e)) range from 5 to 90 mu m. The single-scattering properties of ice clouds are strongly sensitive to surface roughness condition. Lookup tables that are built for the correlation between the bidirectional reflectances at wavelengths of 0.86 and 2.13 mu m with different roughness conditions are used to retrieve ice cloud optical thickness and effective particle size over oceans. Pronounced differences are noticed for the retrieved cirrus cloud optical thickness and effective particle sizes in conjunction with different surface roughness conditions. The values of the retrieved cirrus cloud optical thickness in the case of the rough surface are generally smaller than their counterparts associated with smooth surface conditions. The effect of surface roughness on the retrieved effective particle radii is not pronounced for slight and moderate roughness conditions. However, when the surfaces of ice crystals are substantially rough, the retrieved effective radii associated with roughened particles are larger and smaller than their smooth surface counterparts for large (r(e) > 50 mu m) and small (r(e) < 35 mu m) ice crystals, respectively, whereas the effect of surface roughness on the retrieved effective radii shows a nonmonotonic feature for moderate particle sizes (35 mu m < r(e) < 50 mu m). In general, the dominant effect of surface roughness on cloud property retrievals is to decrease the retrieved optical thickness and to increase the retrieved effective particle size in comparison with their counterparts in the case of smooth ice particles. C1 [Yang, Ping; Hong, Gang] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. [Kattawar, George W.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. [Minnis, Patrick; Hu, Yongxiang] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA. RP Yang, P (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. EM pyang@ariel.met.tamu.edu RI Minnis, Patrick/G-1902-2010; Yang, Ping/B-4590-2011; Hong, Gang/A-2323-2012; Hu, Yongxiang/K-4426-2012 OI Minnis, Patrick/0000-0002-4733-6148; NR 43 TC 43 Z9 43 U1 0 U2 17 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD JUL PY 2008 VL 46 IS 7 BP 1948 EP 1957 DI 10.1109/TGRS.2008.916472 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 321DP UT WOS:000257285200007 ER PT J AU Yu, B Sun, XH Ju, SH Janes, DB Meyyappan, M AF Yu, Bin Sun, Xuhui Ju, Sanghyun Janes, David B. Meyyappan, M. TI Chalcogenide-nanowire-based phase change memory SO IEEE TRANSACTIONS ON NANOTECHNOLOGY LA English DT Article DE chalcogenide; nanoelectronics; nanowires (NWs); phase change random access memory (PRAM) ID GERMANIUM TELLURIDE GLASSES; RANDOM-ACCESS MEMORY; SWITCHING BEHAVIOR; TEMPERATURE; INDIUM; FILM; CELL AB We report fabrication of phase change random access memory (PRAM) using nanowires (NWs) of GeTe and In2Se3. NWs were grown by a vapor-liquid-solid technique and ranged from 40 to 80 run in diameter and several micrometers long. A dynamic switching ratio (ON/OFF ratio) of 2200 and 2 x 105 was realized for GeTe and indium selenide devices, respectively. The programming power for the RESET operation is only tens of microwatts compared to the milliwatt power levels required by the conventional thin-film-based PRAM. C1 [Yu, Bin] NASA, Ames Res Ctr, UARC, Moffett Field, CA 94035 USA. [Ju, Sanghyun; Janes, David B.] Purdue Univ, Sch Elect & Comp Engn, W Lafayette, IN 47907 USA. [Ju, Sanghyun] Samsung SDI Co Ltd, Res Ctr, Seoul, South Korea. RP Yu, B (reprint author), NASA, Ames Res Ctr, UARC, Moffett Field, CA 94035 USA. EM byu@arc.nasa.gov; xsun@arc.nasa.gov; janes@ecn.purdue.edu; m.meyyappan@nasa.gov RI Sun, Xuhui /K-5689-2012 FU National Aeronautics and Space Administration [NCC 2-1363]; University Research Engineering and Technology Institutes (URETI) FX This work was supported by the National Aeronautics and Space Administration under Contract NCC 2-1363 to University-Affiliated Research Center (UARC) and University Research Engineering and Technology Institutes (URETI). The review of this paper was arranged by Associate Editor L. Dong. NR 35 TC 31 Z9 33 U1 0 U2 17 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1536-125X EI 1941-0085 J9 IEEE T NANOTECHNOL JI IEEE Trans. Nanotechnol. PD JUL PY 2008 VL 7 IS 4 BP 496 EP 502 DI 10.1109/TNANO.2008.926374 PG 7 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Science & Technology - Other Topics; Materials Science; Physics GA 342EB UT WOS:000258766300018 ER PT J AU Lee, DU Kim, H Jones, CR Villasenor, JD AF Lee, Dong-U Kim, Hyungjin Jones, Christopher R. Villasenor, John D. TI Pilotless frame synchronization for LDPC-coded transmission systems SO IEEE TRANSACTIONS ON SIGNAL PROCESSING LA English DT Article DE block codes; channel coding; frame synchronization ID AWGN CHANNELS; DECODER; OPTIMUM AB We present a pilotless frame synchronization approach that exploits feedback from a low-density parity-check (LDPC) code decoder. The synchronizer is based on syndrome checks using hard decisions from the channel observations. The bandwidth overhead associated with pilot symbols in conventional receiver architectures is eliminated while providing sufficient synchronization performance. An LDPC decoder coupled with our synchronizer exhibits negligible frame error rate degradation over a system with perfect synchronization. The complexity of the frame synchronizer is kept relatively low due to its XOR-based approach. C1 [Lee, Dong-U; Kim, Hyungjin; Villasenor, John D.] Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90095 USA. [Jones, Christopher R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lee, DU (reprint author), Mojix Inc, Los Angeles, CA 90025 USA. EM dongu@mojix.com; hjkimnov@ee.ucla.edu; christop@jpl.nasa.gov; villa@icsl.ucla.edu NR 20 TC 11 Z9 12 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1053-587X J9 IEEE T SIGNAL PROCES JI IEEE Trans. Signal Process. PD JUL PY 2008 VL 56 IS 7 BP 2865 EP 2874 DI 10.1109/TSP.2008.917348 PN 1 PG 10 WC Engineering, Electrical & Electronic SC Engineering GA 319WN UT WOS:000257195800021 ER PT J AU Newcombe, DA La Duc, MT Vaishampayan, P Venkateswaran, K AF Newcombe, David A. La Duc, Myron T. Vaishampayan, Parag Venkateswaran, Kasthuri TI Impact of assembly, testing and launch operations on the airborne bacterial diversity within a spacecraft assembly facility clean-room SO INTERNATIONAL JOURNAL OF ASTROBIOLOGY LA English DT Article DE airborne; bacteria; diversity; clean rooms; phylogenetic; spacecraft ID ACINETOBACTER-RADIORESISTENS; MICROBIAL CHARACTERIZATION; FUNGAL COLONIZATION; UV-IRRADIATION; AIR FILTERS; CABIN AIR; RADIATION; MARS; MICROORGANISMS; ENVIRONMENTS AB In an effort to minimize the probability of forward contamination of pristine extraterrestrial environments, the National Aeronautics and Space Administration requires that all US robotic spacecraft undergo assembly, testing and launch operations (ATLO) in controlled clean-room environments. This Study examines the impact of ATLO activity on the microbial diversity and overall bioburden contained within the air of the clean-room facility in which the Mars Exploration Rovers (MERs) underwent final preparations for launch. Air samples were collected from several facility locations and traditional culture-based and molecular methodologies were used to measure microbial burden and diversity. Surprisingly, the greatest estimates of airborne bioburden, Lis derived from ATP content and Cultivation assays, were observed prior to the commencement of MER ATLO activities. Furthermore, airborne microbial diversity gradually declined from the initiation of ATLO on through to launch. Proteobacterial sequences were common in 16S rDNA clone libraries. Conspicuously absent were members of the Firmicutes phylum, which includes the genus Bacillus. In previous Studies, species of this genus were repeatedly isolated from the surfaces of spacecraft and clean-room assembly facilities. Increased cleaning and maintenance initiated immediately prior to the start of ATLO activity Could explain the observed declines in both airborne bioburden and microbial diversity. C1 [Newcombe, David A.; La Duc, Myron T.; Vaishampayan, Parag; Venkateswaran, Kasthuri] CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA 91109 USA. [Newcombe, David A.] Univ Idaho Coeur dAlene, Environm Sci Program, Coeur Dalene, ID 83814 USA. RP Newcombe, DA (reprint author), CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM kjvenkat@jpl.nasa.gov FU NASA Research Announcement (NRA) ROSS FX Part of the research described in this publication was carried Out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This research was funded by NASA Research Announcement (NRA) ROSS 2003 awarded to Kasthuri Venkateswaran. We are grateful to members of the Biotechnology and Planetary Protection group for technical assistance. We also appreciate the help rendered by R. Stunner, B. Petsos, S. Pillai and D. Dickinson during sampling. We are thankful to J. Spry, K. Buxbaum, and J. Rummel for valuable advice and encouragement. NR 53 TC 8 Z9 8 U1 2 U2 7 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1473-5504 J9 INT J ASTROBIOL JI Int. J. Astrobiol. PD JUL-OCT PY 2008 VL 7 IS 3-4 BP 223 EP 236 DI 10.1017/S1473550408004254 PG 14 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 541AN UT WOS:000273383100006 ER PT J AU Ogasaka, Y Tamura, K Shibata, R Furuzawa, A Miyazawa, T Shimoda, K Fukaya, Y Iwahara, T Nakamura, T Naitou, M Kanou, Y Sasaki, N Ueno, D Okajima, T Miyata, E Tawa, N Mukai, K Ikegami, K Aono, M Uesugi, K Suzuki, Y Takeuchi, S Furamura, T Takahashi, R Sakashita, M Sakai, C Nonoyama, M Yamada, N Onishi, K Miyauchi, T Maeda, Y Okada, S Serlemitsos, P Soong, Y Chan, KW Rohrbach, S Berendse, F Tueller, J Tsunemi, H Kunieda, H Yamashita, K AF Ogasaka, Yasushi Tamura, Keisuke Shibata, Ryo Furuzawa, Akihiro Miyazawa, Takuya Shimoda, Kenta Fukaya, Yoshihiro Iwahara, Tomonaga Nakamura, Tornokazu Naitou, Masataka Kanou, Yasufumi Sasaki, Naoki Ueno, Daislike Okajima, Takashi Miyata, Emi Tawa, Noriaki Mukai, Kenji Ikegami, Kazuhiro Aono, Michihiko Uesugi, Kentaro Suzuki, Yoshio Takeuchi, Satoshi Furamura, Taku Takahashi, Rika Sakashita, Machiko Sakai, Chiaki Nonoyama, Masayuki Yamada, Nobuaki Onishi, Katsuhiko Miyauchi, Tomofumi Maeda, Yoshitomo Okada, Shunsaku Serlemitsos, Peter Soong, Yang Chan, Kai-Wing Rohrbach, Scott Berendse, Fred Tueller, Jack Tsunemi, Hiroshi Kunieda, Hideyo Yamashita, Koujun TI Characterization of a hard x-ray telescope at synchrotron facility SPring-8 SO JAPANESE JOURNAL OF APPLIED PHYSICS LA English DT Article DE X-ray optics; X-ray telescope; synchrotron radiation; multilayer; measurement technique; space science; astronomy ID S BALLOON EXPERIMENT; SUPERMIRROR; PERFORMANCE; ASTRONOMY; SUZAKU; ASCA AB Space-borne astronomical instruments require extensive characterization on the ground before launch. In the hard X-ray region however, it is difficult for a laboratory-based beamline using a conventional X-ray Source to provide a capability sufficient for pre-flight high-precision calibration. In this paper, we describe an experiment to characterize a hard X-ray telescope at a synchrotron facility, mainly on the basis of experimental setup and examples of measured results. We have developed hard X-ray telescopes consisting of Wolter-I grazing incidence optics and platinum-carbon multilayer supermirror coatings. The telescopes have been characterized at the synchrotron facility SPring-8 beamline BL20B2. The measurements at BL20B2 have great advantages such as extremely high flux, large-sized and less-divergent beam, and monochromatic beam covering the entire hard X-ray region front 8 to over 100keV. The telescope was illuminated by monochromatic hard X-rays, and the focused image was measured by high resolution hard X-ray imagers. The entire telescope aperture was mapped by a small beam, and the effective area and the point spread function were obtained as well as local optical properties for further diagnostics of the characteristics of the telescope. C1 [Ogasaka, Yasushi; Tamura, Keisuke; Shibata, Ryo; Furuzawa, Akihiro; Miyazawa, Takuya; Shimoda, Kenta; Fukaya, Yoshihiro; Iwahara, Tomonaga; Nakamura, Tornokazu; Naitou, Masataka; Kanou, Yasufumi; Sasaki, Naoki; Ueno, Daislike; Takeuchi, Satoshi; Furamura, Taku; Takahashi, Rika; Sakashita, Machiko; Sakai, Chiaki; Nonoyama, Masayuki; Yamada, Nobuaki; Onishi, Katsuhiko; Kunieda, Hideyo; Yamashita, Koujun] Nagoya Univ, Dept Phys, Nagoya, Aichi 4648602, Japan. [Okajima, Takashi; Serlemitsos, Peter; Soong, Yang; Chan, Kai-Wing; Rohrbach, Scott; Tueller, Jack] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Miyata, Emi; Tawa, Noriaki; Mukai, Kenji; Ikegami, Kazuhiro; Aono, Michihiko; Miyauchi, Tomofumi] Osaka Univ, Dept Phys, Osaka 5600043, Japan. [Uesugi, Kentaro; Suzuki, Yoshio] Japan Synchrotron Radiat Res Inst, Sayou, Hyogo 6795198, Japan. [Maeda, Yoshitomo; Okada, Shunsaku] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Berendse, Fred] USN, Res Lab, Washington, DC 20375 USA. RP Ogasaka, Y (reprint author), Nagoya Univ, Dept Phys, Nagoya, Aichi 4648602, Japan. EM ogasaka@u.phys.nagoya-u.ac.jp RI Tueller, Jack/D-5334-2012; XRAY, SUZAKU/A-1808-2009 NR 31 TC 17 Z9 17 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0021-4922 EI 1347-4065 J9 JPN J APPL PHYS JI Jpn. J. Appl. Phys. PD JUL PY 2008 VL 47 IS 7 BP 5743 EP 5754 DI 10.1143/JJAP.47.5743 PN 1 PG 12 WC Physics, Applied SC Physics GA 353FD UT WOS:000259550600093 ER PT J AU Goldberg, RK Roberts, GD Littel, JD Binienda, WK AF Goldberg, Robert K. Roberts, Gary D. Littel, Justin D. Binienda, Wieslaw K. TI Approximation of nonlinear unloading effects in the strain rate dependent deformation analysis of polymer matrix materials utilizing a state variable approach SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Article ID CRACK-TIP FIELDS; SEMICRYSTALLINE POLYMER; PART II; MECHANICAL-BEHAVIOR; UNIAXIAL BEHAVIOR; EPOXY-RESIN; MODEL; COMPOSITES; OVERSTRESS; NECKING AB An experimental and analytical program is carried out to explore key behaviors in the loading and unloading behavior of polymers. Specifically, the effects of strain rate and hydrostatic stresses on the nonlinear portions of the deformation response are examined. Tension, compression, and shear load only and load/unload tests are conducted on a representative polymer across a range of strain rates, and key features of the experimental results are identified. To conduct a preliminary exploration of how the key features of the deformation response could be simulated analytically, a previously developed set of constitutive equations, which were developed to analyze the strain rate dependent, nonlinear deformation of polymers including the effects of hydrostatic stresses, were modified in order to approximate key features of the nonlinear unloading behavior observed in the polymer. The constitutive relations are based on state variable constitutive equations originally developed for metals. The nonlinear unloading observed in the experiments is approximated by reducing the unloading modulus of the material as the effective inelastic strain is increased. The effects of the hydrostatic stress state on the unloading modulus are also simulated analytically. To examine the revised formulation, the loading and load/unload responses of the representative polymer in tension, compression, and shear are examined at several strain rates. Results computed using the developed constitutive equations were found to correlate reasonably well with the experimental data. C1 [Goldberg, Robert K.; Roberts, Gary D.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. [Littel, Justin D.] Univ Akron, Dept Civil Engn, Akron, OH 44325 USA. [Binienda, Wieslaw K.] Univ Akron, Dept Civil Engn, Akron, OH 44325 USA. RP Goldberg, RK (reprint author), NASA Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM robert.k.goldberg@nasa.gov NR 27 TC 3 Z9 3 U1 1 U2 5 PU ASCE-AMER SOC CIVIL ENGINEERS PI RESTON PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA SN 0893-1321 J9 J AEROSPACE ENG JI J. Aerosp. Eng. PD JUL PY 2008 VL 21 IS 3 BP 119 EP 131 DI 10.1061/(ASCE)0893-1321(2008)21:3(119) PG 13 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA 317LZ UT WOS:000257023000002 ER PT J AU Zhu, LF Chattopadhyay, A Goldberg, RK AF Zhu, Linfa Chattopadhyay, Aditi Goldberg, Robert K. TI Failure model for rate-dependent polymer matrix composite laminates under high-velocity impact SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Article ID DEFORMATION; STRESS; GLASS AB A modified Hashin failure model is developed to characterize different failure modes related to high-velocity impact of composite laminates. Hashin's compressive fiber failure mode has been extended to consider the shear stress effect. Several micromechanics-based degradation rules are developed and applied to the stress and material property calculations according to different failure modes after the corresponding failure criterion is satisfied. This model has been implemented into a recently developed micromechanics model. Computational results show that this model is able to address shear failure, delamination, and tearing failure observed in the high-velocity impact of composite laminates. C1 [Zhu, Linfa] Altair Engn Inc, Austin, TX 78757 USA. [Chattopadhyay, Aditi] Arizona State Univ, Dept Mech & Aerosp Engn, Tempe, AZ 85287 USA. [Goldberg, Robert K.] NASA Glenn Res Ctr, Mech & Life Predict Branch, Cleveland, OH 44135 USA. RP Zhu, LF (reprint author), Altair Engn Inc, Austin, TX 78757 USA. NR 18 TC 5 Z9 5 U1 1 U2 6 PU ASCE-AMER SOC CIVIL ENGINEERS PI RESTON PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA SN 0893-1321 J9 J AEROSPACE ENG JI J. Aerosp. Eng. PD JUL PY 2008 VL 21 IS 3 BP 132 EP 139 DI 10.1061/(ASCE)0893-1321(2008)21:3(132) PG 8 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA 317LZ UT WOS:000257023000003 ER PT J AU Zheng, XH Binienda, WK AF Zheng, Xiahua Binienda, Wieslaw K. TI Rate-dependent shell element composite material model implementation in LS-DYNA SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Article ID POLYMER MATRIX COMPOSITES; STRAIN-RATE; MECHANICAL-PROPERTIES; BEHAVIOR; COMPRESSION; STRESS; PRESSURE AB A previously developed constitutive model has been modified in order to incorporate the rate dependence of elastic modulus of the polymer matrix constituent into the nonlinear, strain-rate-dependent deformation analysis of polymer matrix composites. To compute the inelastic strains in the polymer matrix, state-variable-based viscoplastic equations originally developed for metals are modified in order to account for the effects of hydrostatic stresses, which are significant in polymers. The polymer constitutive equations are implemented within the strength of a material-based micromechanics method in order to predict the nonlinear, strain-rate-dependent deformation of the polymer matrix composite. The polymer and the composite models are implemented into a commercially available explicit finite-element code, LS-DYNA, as user defined materials (UMATs). The deformation behaviors of several representative polymers and two polymer matrix composites of various fiber configurations are simulated in LS-DYNA with the UMATs for a wide range of strain rates, and the numerical results agree well with the experimental data. UMAT is applied for simulations of braiding/weaving composites using the modified through-thickness integration points method. C1 [Zheng, Xiahua] NASA Glenn Res Ctr, Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA. [Binienda, Wieslaw K.] Univ Akron, Dept Civil Engn, Akron, OH 44325 USA. RP Zheng, XH (reprint author), NASA Glenn Res Ctr, Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA. NR 26 TC 5 Z9 5 U1 0 U2 6 PU ASCE-AMER SOC CIVIL ENGINEERS PI RESTON PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA SN 0893-1321 J9 J AEROSPACE ENG JI J. Aerosp. Eng. PD JUL PY 2008 VL 21 IS 3 BP 140 EP 151 DI 10.1061/(ASCE)0893-1321(2008)21:3(140) PG 12 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA 317LZ UT WOS:000257023000004 ER PT J AU Littell, JD Ruggeri, CR Goldberg, RK Roberts, GD Arnold, WA Binienda, WK AF Littell, Justin D. Ruggeri, Charles R. Goldberg, Robert K. Roberts, Gary D. Arnold, William A. Binienda, Wieslaw K. TI Measurement of epoxy resin tension, compression, and shear stress-strain curves over a wide range of strain rates using small test specimens SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Article ID DEFORMATION; BEHAVIOR; COMPOSITES AB The next generation aircraft engines are designed to be lighter and stronger than engines currently in use by using carbon fiber composites. In order to certify these engines, ballistic impact tests and computational analyses must be completed, which will simulate a "blade out" event in a catastrophic engine failure In order to computationally simulate the engine failure, properties of the carbon fiber and resin matrix must be known. When conducting computer simulations using a micromechanics approach, experimental tensile, compressive, and shear data are needed for constitutive modeling of the resin matrix material. The material properties of an Epon E862 epoxy resin will be investigated because it is a commercial 176 degrees C (350 degrees F) cure resin currently being used in these aircraft engines. These properties will be measured using optical measurement techniques. The epoxy specimens will be tested in tension, compression and torsional loadings under various strain rates ranging from 10(-5) to 10(-1) s(-1) and temperatures ranging from room temperature to 80 degrees C. To test the specimens at high temperatures, a specialized clear temperature chamber was used. The results show that the test procedure developed can accurately and quickly categorize the material response characteristics of an epoxy resin. In addition, the results display clear strain rate and temperature dependencies in the material response. C1 [Littell, Justin D.; Ruggeri, Charles R.; Arnold, William A.; Binienda, Wieslaw K.] Univ Akron, Dept Civil Engn, Akron, OH 44325 USA. [Goldberg, Robert K.; Roberts, Gary D.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Littell, JD (reprint author), Univ Akron, Dept Civil Engn, Akron, OH 44325 USA. EM justin.d.littell@nasa.gov NR 16 TC 48 Z9 48 U1 1 U2 28 PU ASCE-AMER SOC CIVIL ENGINEERS PI RESTON PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA SN 0893-1321 J9 J AEROSPACE ENG JI J. Aerosp. Eng. PD JUL PY 2008 VL 21 IS 3 BP 162 EP 173 DI 10.1061/(ASCE)0893-1321(2008)21:3(162) PG 12 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA 317LZ UT WOS:000257023000006 ER PT J AU Silva, WA AF Silva, Walter A. TI Simultaneous excitation of multiple-input/multiple-output CFD-based unsteady aerodynamic systems SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT 48th AIAA/ASME/ASCE/AHS/ASC Structures, Structural Dynamics and Materials Conference/3rd AIAA Multidisciplinary Design Optimization Specialist Conference CY APR 23-26, 2007 CL Honolulu, HI SP Amer Inst Aeronaut & Astronaut, ASME, ASCE, AHS, ASC ID AEROELASTIC ANALYSIS; MODEL-REDUCTION; IDENTIFICATION AB A significant improvement to the development of computational-fluid-dynamics-based unsteady aerodynamic reduced-order models is presented. The improvement involves the simultaneous excitation of the structural modes of the computational-fluid-dynamics-based unsteady aerodynamic system. This improvement enables the computation of the unsteady aerodynamic state-space model using a single computational fluid dynamics execution, independent of the number of structural modes. Two new types of input functions are presented that can be used for the simultaneous excitation of the unsteady aerodynamic system via the excitation of the structural modes. Results are presented for a semispan configuration using the CFL3Dv6.4 code. C1 NASA, Langley Res Ctr, Aeroelast Branch, Hampton, VA 23681 USA. RP Silva, WA (reprint author), NASA, Langley Res Ctr, Aeroelast Branch, Hampton, VA 23681 USA. NR 37 TC 19 Z9 25 U1 0 U2 2 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD JUL-AUG PY 2008 VL 45 IS 4 BP 1267 EP 1274 DI 10.2514/1.34328 PG 8 WC Engineering, Aerospace SC Engineering GA 336UF UT WOS:000258389400018 ER PT J AU Li, W Shields, E Le, D AF Li, Wu Shields, Elwood Le, Daniel TI Interactive inverse design optimization of fuselage shape for low-boom supersonic concepts SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT AIAA/ASME/ASCE/AHS/ASC 46th Structures, Structural Dynamics and Materials Conference/1st AIAA Multidisciplinary Design Optimization Specialist Conference CY APR 18-21, 2005 CL Austin, TX SP AIAA, ASME, ASCE, AHS, ASC ID MINIMIZATION; AIRPLANE AB This paper introduces a tool for boom optimization using smoothest shape modifications. This, tool allows interactive inverse design optimization to develop a fuselage shape that yields a low-boom aircraft configuration. A fundamental reason for developing this boom optimization tool is the need to generate feasible low-boom conceptual designs that are appropriate for further refinement using computational-fluid-dynamics-based preliminary design methods. The boom optimization tool was not developed to provide a numerical solution to the inverse design problem. Instead, it was intended to help designers find the right configuration among an infinite number of possible configurations that are equally good using any numerical figure of merit. This boom optimization tool uses the smoothest shape modification strategy for modifying the fuselage radius distribution at 100 or more longitudinal locations to find a smooth fuselage shape, which reduces the discrepancies between the design and target equivalent area distributions over any specified range of effective distance. For any given supersonic concept (with wing, fuselage, nacelles, tails, and/or canards), a designer can examine the differences between the design and target equivalent areas, decide which part of the design equivalent area curve needs to be modified, choose a desirable rate for the reduction of the discrepancies over the specified range, and select a parameter for smoothness control of the fuselage shape. The boom optimization tool will then generate a fuselage shape based on the designer's inputs in a matter of seconds'. Using this tool, within a few hours, a designer can either generate a realistic fuselage shape that yields a supersonic configuration with a low-boom ground signature or quickly eliminate any configuration that cannot achieve low-boom characteristics with fuselage shaping alone. A conceptual design case study is documented to demonstrate how this boom optimization tool can be used to develop a low-boom supersonic concept from a low-drag supersonic concept. The paper also contains a study on how perturbations in the equivalent area distribution affect the ground signature shape and how new target area distributions for low-boom signatures can be constructed using superposition of equivalent area distributions derived from the Seebass-George-Darden theory. C1 [Li, Wu] NASA, Langley Res Ctr, Aeronaut Syst Anal Branch, Hampton, VA 23681 USA. [Shields, Elwood] Alliant Techsyst Inc, Space Div, Hampton, VA 23681 USA. [Le, Daniel] Univ Virginia, Charlottesville, VA 22904 USA. RP Li, W (reprint author), NASA, Langley Res Ctr, Aeronaut Syst Anal Branch, Hampton, VA 23681 USA. EM w.li@nasa.gov NR 48 TC 9 Z9 14 U1 0 U2 2 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD JUL-AUG PY 2008 VL 45 IS 4 BP 1381 EP 1397 DI 10.2514/1.35543 PG 17 WC Engineering, Aerospace SC Engineering GA 336UF UT WOS:000258389400029 ER PT J AU Mueller, RA Hardy, GH AF Mueller, Rodger A. Hardy, Gordon H. TI Pilot-force measurement with inertia and gravity compensation SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT AIAA Modeling and Simulation Technologies Conference CY AUG 20-23, 2007 CL Hilton Head, SC SP Amer Inst Aeronaut & Astronaut AB Measuring pilot force on pilot control loaders used in flight simulators is difficult due to force errors introduced by pilot control loader inertia, simulator cab motion, and gravity. Attempts to correct this problem by using strain gauges near the grip handle or in gloves have proven impractical because the devices are sensitive to grip position. This paper describes a technique for measuring the pilot control loader pilot force with compensation for all inertial effects by incorporating an accelerometer located at a specific location for each particular pilot control loader axis. There are no additional requirements on the pilot, who is only required to operate the pilot control loader in a normal manner. The pitch axis on a McFadden wheel and column pilot control loader, used at the NASA Ames Research Center, was used to demonstrate the pilot-force measurement technique with compensation for inertial effects and gravity. C1 [Mueller, Rodger A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Hardy, Gordon H.] Sci Applicat Int Corp, Moffett Field, CA 94035 USA. RP Mueller, RA (reprint author), NASA, Ames Res Ctr, Mail Stop 243-5, Moffett Field, CA 94035 USA. NR 1 TC 0 Z9 0 U1 0 U2 3 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD JUL-AUG PY 2008 VL 45 IS 4 BP 1398 EP 1404 DI 10.2514/1.34429 PG 7 WC Engineering, Aerospace SC Engineering GA 336UF UT WOS:000258389400030 ER PT J AU Owens, LR Allan, BG Gorton, SA AF Owens, Lewis R. Allan, Brian G. Gorton, Susan A. TI Boundary-layer-ingesting inlet flow control SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT AIAA 44th Aerospace Sciences Meeting and Exhibit/ASME Wind Energy Conference CY JAN 09-12, 2006 CL Reno, NV SP AIAA, ASME AB An experimental study was conducted to provide the first demonstration of an active How control system for a flush-mounted inlet with significant boundary-layer ingestion in transonic flow conditions. The effectiveness of the flow control in reducing the circumferential distortion at the engine fan-face location was assessed using a 2.5%-scale model of a boundary-layer-ingesting offset diffusing inlet. The inlet was flush mounted to the tunnel wall and ingested a large boundary layer with a boundary-layer-to-inlet height ratio of 35%. Different jet distribution patterns and jet mass-flow rates were used in the inlet to control distortion. A vane. configuration was also tested. Finally, a hybrid vane/jet configuration was tested leveraging strengths of both types of devices. Measurements were made of the onset boundary layer, the duct surface static pressures, and the mass-flow rates through the duct and the flow control actuators. The distortion and pressure recovery were measured at the aerodynamic interface plane. The data show that control jets and vanes reduce circumferential distortion to acceptable levels. The point-design vane configuration produced higher distortion levels at off-design settings. The hybrid vane/jet flow control configuration reduced the off-design distortion levels to acceptable ones and used less than 0.5% of the inlet mass flow to supply the jets. C1 [Owens, Lewis R.; Allan, Brian G.; Gorton, Susan A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Owens, Lewis R.; Allan, Brian G.; Gorton, Susan A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Owens, LR (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 37 TC 11 Z9 12 U1 1 U2 9 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD JUL-AUG PY 2008 VL 45 IS 4 BP 1431 EP 1440 DI 10.2514/1.36989 PG 10 WC Engineering, Aerospace SC Engineering GA 336UF UT WOS:000258389400033 ER PT J AU Ulbrich, CW Atlas, D AF Ulbrich, Carlton W. Atlas, David TI Radar measurement of rainfall with and without polarimetry SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID RAINDROP-SIZE DISTRIBUTION; PRECIPITATION; SPECTRA; DISDROMETER; CLOUDS; STORMS AB Raindrop size distributions (DSDs) for tropical convective storms are used to examine the relationships between the parameters of a gamma DSD, with special emphasis on their variation with the stage of the storm. Such a distinction has rarely been made before. Several storms from a variety of tropical locations are divided into storm stages according to the temporal dependence of their reflectivity factor Z, rainfall rate R, and median volume diameter D-0. In most cases it is found that the DSD parameter D-0 is approximately constant in time during the convective, or C, stage, which leads to a Z-R relation of the form Z = AR, that is, a linear relationship between Z and R. This finding implies the existence of equilibrium DSDs during the C stage. The convective stage is sometimes marked by pulsations in draft strength so that D-0, R, and Z and associated values of the shape parameter mu decrease in a quasi-transition stage before increasing once more. Theoretical relations between the differential reflectivity Z(DR) and the ratio Z/R as functions of the DSD parameter mu are derived by assuming a gamma DSD and an accurate raindrop fall speed law. It is found that data derived from disdrometer observations lie along a mu = 5 isopleth for tropical continental C stages (Puerto Rico and Brazil) and along a mu = 12 isopleth for tropical maritime C stages [Tropical Ocean and Global Atmosphere Coupled Ocean-Atmosphere Response Experiment (TOGA COARE)]. Small values of mu that occur in the weak updraft intervals do not impact the rainfall measurements because they correspond to relatively small R. The latter features imply that the measurement of rainfall for the convective stages can be performed with standard polarimetry involving only two measurables rather than three, provided knowledge of mu is available a priori. A new rain parameter diagram is presented in which isopleths of the generalized number concentration and D-0 are superimposed on the Z-R plot. It is proposed that it is possible to estimate D-0 from climatological and observable storm structural features, which, with Z, provide estimates of R. Such an approach is necessary for use with conventional radars until polarimetric radars are more widely available. C1 [Ulbrich, Carlton W.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. [Atlas, David] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Ulbrich, CW (reprint author), 106 Highland Dr, Clemson, SC 29631 USA. EM cwu@nctv.com NR 24 TC 6 Z9 6 U1 0 U2 3 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD JUL PY 2008 VL 47 IS 7 BP 1929 EP 1939 DI 10.1175/2007JAMC1804.1 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 327GT UT WOS:000257718300005 ER PT J AU Ackerman, SA Holz, RE Frey, R Eloranta, EW Maddux, BC McGill, M AF Ackerman, S. A. Holz, R. E. Frey, R. Eloranta, E. W. Maddux, B. C. McGill, M. TI Cloud detection with MODIS. Part II: Validation SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID WATER-VAPOR; CLEAR-SKY; SATELLITE; CLASSIFICATION; AEROSOL AB An assessment of the performance of the Moderate Resolution Imaging Spectroradiometer (MODIS) cloud mask algorithm for Terra and Aqua satellites is presented. The MODIS cloud mask algorithm output is compared with lidar observations from ground [Arctic High-Spectral Resolution Lidar (AHSRL)], aircraft [Cloud Physics Lidar (CPL)], and satellite-borne [Geoscience Laser Altimeter System (GLAS)] platforms. The comparison with 3 yr of coincident observations of MODIS and combined radar and lidar cloud product from the Department of Energy (DOE) Atmospheric Radiation Measurement (ARM) Program Southern Great Plains (SGP) site in Lamont, Oklahoma, indicates that the MODIS algorithm agrees with the lidar about 85% of the time. A comparison with the CPL and AHSRL indicates that the optical depth limitation of the MODIS cloud mask is approximately 0.4. While MODIS algorithm flags scenes with a cloud optical depth of 0.4 as cloudy, approximately 90% of the mislabeled scenes have optical depths less than 0.4. A comparison with the GLAS cloud dataset indicates that cloud detection in polar regions at night remains challenging with the passive infrared imager approach. In anticipation of comparisons with other satellite instruments, the sensitivity of the cloud mask algorithm to instrument characteristics (e. g., instantaneous field of view and viewing geometry) and thresholds is demonstrated. As expected, cloud amount generally increases with scan angle and instantaneous field of view (IFOV). Nadir sampling represents zonal monthly mean cloud amounts but can have large differences for regional studies when compared to full-swath-width analysis. C1 [Ackerman, S. A.; Holz, R. E.; Frey, R.] Univ Wisconsin, CIMSS, Ctr Space Sci & Engn, Madison, WI 53706 USA. [Maddux, B. C.] Univ Wisconsin, Dept Atmospher & Ocean Sci, Madison, WI 53706 USA. [McGill, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ackerman, SA (reprint author), Univ Wisconsin, CIMSS, Ctr Space Sci & Engn, 1225 W Dayton St, Madison, WI 53706 USA. EM stevea@ssec.wisc.edu RI Ackerman, Steven/G-1640-2011; McGill, Matthew/D-8176-2012 OI Ackerman, Steven/0000-0002-4476-0269; NR 26 TC 182 Z9 184 U1 3 U2 34 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD JUL PY 2008 VL 25 IS 7 BP 1073 EP 1086 DI 10.1175/2007JTECHA1053.1 PG 14 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 327GR UT WOS:000257718100002 ER PT J AU Buermann, W Saatchi, S Smith, TB Zutta, BR Chaves, JA Mila, B Graham, CH AF Buermann, Wolfgang Saatchi, Sassan Smith, Thomas B. Zutta, Brian R. Chaves, Jaime A. Mila, Borja Graham, Catherine H. TI Predicting species distributions across the Amazonian and Andean regions using remote sensing data SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE conservation biogeography; ecological niche characterization; microwave remote sensing; MODIS; optical remote sensing; QSCAT; South America; spatial scale; species distribution modelling ID CLIMATE-CHANGE; MODIS DATA; LEAF-AREA; GEOGRAPHIC DISTRIBUTIONS; CONSERVATION PRIORITIES; BIODIVERSITY HOTSPOTS; DISTRIBUTION MODELS; NICHE MODELS; VEGETATION; ALGORITHM AB Aim We explore the utility of newly available optical and microwave remote sensing data from the Moderate Resolution Imaging Spectroradiometer (MODIS) and QuikSCAT (QSCAT) instruments for species distribution modelling at regional to continental scales. Using eight Neotropical species from three taxonomic groups, we assess the extent to which remote sensing data can improve predictions of their geographic distributions. For two bird species, we investigate the specific contributions of different types of remote sensing variables to the predictions and model accuracy at the regional scale, where the benefits of the MODIS and QSCAT satellite data are expected to be most significant. Location South America, with a focus on the tropical and subtropical Andes and the Amazon Basin. Methods Potential geographic distributions of eight species, namely two birds, two mammals and four trees, were modelled with the MAXENT algorithm at 1-km resolution over the South American continent using climatic and remote sensing data separately and combined. For each species and model scenario, we assess model performance by testing the agreement between observed and simulated distributions across all thresholds and, in the case of the two focal bird species, at selected thresholds. Results Quantitative performance tests showed that models built with remote sensing and climatic layers in isolation performed well in predicting species distributions, suggesting that each of these data sets contains useful information. However, predictions created with a combination of remote sensing and climatic layers generally resulted in the best model performance across the three taxonomic groups. In Ecuador, the inclusion of remote sensing data was critical in resolving the known geographically isolated populations of the two focal bird species along the steep Amazonian-Andean elevational gradients. Within remote sensing subsets, microwave-based data were more important than optical data in the predictions of the two bird species. Main conclusions Our results suggest that the newly available remote sensing data (MODIS and QSCAT) have considerable utility in modelling the contemporary geographical distributions of species at both regional and continental scales and in predicting range shifts as a result of large-scale land-use change. C1 [Buermann, Wolfgang; Saatchi, Sassan; Smith, Thomas B.; Zutta, Brian R.; Chaves, Jaime A.; Mila, Borja] Univ Calif Los Angeles, UCLA Inst Environm, Ctr Trop Res, Los Angeles, CA 90095 USA. [Saatchi, Sassan] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Smith, Thomas B.; Zutta, Brian R.; Chaves, Jaime A.; Mila, Borja] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Graham, Catherine H.] SUNY Stony Brook, Dept Ecol & Evolut, Stony Brook, NY 11794 USA. RP Buermann, W (reprint author), Univ Calif Los Angeles, UCLA Inst Environm, Ctr Trop Res, Suite 300,619 Charles E Young Dr E, Los Angeles, CA 90095 USA. EM buermann@ucla.edu RI Graham, Catherine/A-9560-2011; OI Mila, Borja/0000-0002-6446-0079 NR 57 TC 101 Z9 104 U1 10 U2 87 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0305-0270 EI 1365-2699 J9 J BIOGEOGR JI J. Biogeogr. PD JUL PY 2008 VL 35 IS 7 BP 1160 EP 1176 DI 10.1111/j.1365-2699.2007.01858.x PG 17 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 314XQ UT WOS:000256842900003 ER PT J AU Bollasina, M Nigam, S Lau, KM AF Bollasina, Massimo Nigam, Sumant Lau, K. -M. TI Absorbing aerosols and summer monsoon evolution over South Asia: An observational portrayal SO JOURNAL OF CLIMATE LA English DT Article ID INDIAN-OCEAN EXPERIMENT; BLACK CARBON AEROSOLS; INTERANNUAL VARIABILITY; GLOBAL PRECIPITATION; NORTHEAST MONSOON; ATLANTIC-OCEAN; SATELLITE DATA; OPTICAL DEPTH; CLIMATE; TOMS AB The South Asian haze builds up from December to May, is mostly of anthropogenic origin, and absorbs part of the solar radiation. The influence of interannual variations of absorbing aerosols over the Indo-Gangetic Plain in May on the Indian summer monsoon is characterized by means of an observational analysis. Insight into how the aerosol impact is generated is also provided. It is shown that anomalous aerosol loading in late spring leads to remarkable and large-scale variations in the monsoon evolution. Excessive aerosols in May lead to reduced cloud amount and precipitation, increased surface shortwave radiation, and land surface warming. The June ( and July) monsoon anomaly associated with excessive May aerosols is of opposite sign over much of the subcontinent (although with a different pattern) with respect to May. The monsoon strengthens in June ( and July). The analysis suggests that the significant large-scale aerosol influence on monsoon circulation and hydroclimate is mediated by the heating of the land surface, pursuant to reduced cloudiness and precipitation in May. The finding of the significant role of the land surface in the realization of the aerosol impact is somewhat novel. C1 [Bollasina, Massimo; Nigam, Sumant] Univ Maryland, Dept Atmospher & Ocean Sci, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Lau, K. -M.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Bollasina, M (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, Earth Syst Sci Interdisciplinary Ctr, 3417 Comp & Space Sci Bldg, College Pk, MD 20742 USA. EM massimo@atmos.umd.edu RI Nigam, Sumant/A-8338-2009; Lau, William /E-1510-2012 OI Lau, William /0000-0002-3587-3691 NR 54 TC 70 Z9 77 U1 2 U2 15 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD JUL PY 2008 VL 21 IS 13 BP 3221 EP 3239 DI 10.1175/2007JCLI2094.1 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 326ZM UT WOS:000257698300010 ER PT J AU Masson-Delmotte, V Hou, S Ekaykin, A Jouzel, J Aristarain, A Bernardo, RT Bromwich, D Cattani, O Delmotte, M Falourd, S Frezzotti, M Gallee, H Genoni, L Isaksson, E Landais, A Helsen, MM Hoffmann, G Lopez, J Morgan, V Motoyama, H Noone, D Oerter, H Petit, JR Royer, A Uemura, R Schmidt, GA Schlosser, E Simoes, JC Steig, EJ Stenni, B Stievenard, M van den Broeke, MR de Wal, RSWV de Berg, WJV Vimeux, F White, JWC AF Masson-Delmotte, V. Hou, S. Ekaykin, A. Jouzel, J. Aristarain, A. Bernardo, R. T. Bromwich, D. Cattani, O. Delmotte, M. Falourd, S. Frezzotti, M. Gallee, H. Genoni, L. Isaksson, E. Landais, A. Helsen, M. M. Hoffmann, G. Lopez, J. Morgan, V. Motoyama, H. Noone, D. Oerter, H. Petit, J. R. Royer, A. Uemura, R. Schmidt, G. A. Schlosser, E. Simoes, J. C. Steig, E. J. Stenni, B. Stievenard, M. van den Broeke, M. R. de Wal, R. S. W. van de Berg, W. J. van Vimeux, F. White, J. W. C. TI A review of Antarctic surface snow isotopic composition: Observations, atmospheric circulation, and isotopic modeling SO JOURNAL OF CLIMATE LA English DT Review ID DRONNING MAUD LAND; NORTHERN VICTORIA-LAND; LAMBERT GLACIER BASIN; DOME EAST ANTARCTICA; SHALLOW FIRN CORES; TERRA-NOVA BAY; ICE-CORE; CLIMATE-CHANGE; DEUTERIUM EXCESS; TEMPORAL VARIABILITY AB A database of surface Antarctic snow isotopic composition is constructed using available measurements, with an estimate of data quality and local variability. Although more than 1000 locations are documented, the spatial coverage remains uneven with a majority of sites located in specific areas of East Antarctica. The database is used to analyze the spatial variations in snow isotopic composition with respect to geographical characteristics ( elevation, distance to the coast) and climatic features ( temperature, accumulation) and with a focus on deuterium excess. The capacity of theoretical isotopic, regional, and general circulation atmospheric models ( including "isotopic" models) to reproduce the observed features and assess the role of moisture advection in spatial deuterium excess fluctuations is analyzed. C1 [Masson-Delmotte, V.; Jouzel, J.; Cattani, O.; Delmotte, M.; Falourd, S.; Landais, A.; Hoffmann, G.; Royer, A.; Stievenard, M.; Vimeux, F.] CEA Saclay, IPSL CEA CNRS UVSQ UMR 1572, Lab Sci Climat & Environm, F-91191 Gif Sur Yvette, France. [Hou, S.] Chinese Acad Sci, Lab Cryosphere & Environm, Lanzhou, Peoples R China. [Ekaykin, A.] Arctic & Antarctic Res Inst, St Petersburg 199226, Russia. [Aristarain, A.] Inst Antartico Argentino, Lab Estratigraffia Glaciar & Geoquim Agua & Nieve, Mendoza, Argentina. [Bernardo, R. T.; Simoes, J. C.] Univ Fed Rio Grande do Sul, Inst Geociencias, Dept Geografia, Nucleo Pesquisas Antarcticas & Climat, Porto Alegre, RS, Brazil. [Bromwich, D.] Ohio State Univ, Columbus, OH 43210 USA. [Frezzotti, M.] ENEA, Rome, Italy. [Gallee, H.; Petit, J. R.] Univ Grenoble 1, CNRS, Lab Glaciol & Geophys Environm, F-38402 St Martin Dheres, France. [Genoni, L.; Stenni, B.] Univ Trieste, Dept Environm Geol & Marine Sci, Trieste, Italy. [Isaksson, E.] Norwegian Polar Res Inst, Tromso, Norway. [Landais, A.] Hebrew Univ Jerusalem, Inst Earth Sci, IL-91904 Jerusalem, Israel. [Helsen, M. M.; van den Broeke, M. R.; de Wal, R. S. W. van; de Berg, W. J. van] Univ Utrecht, Inst Marine & Atmospher Res, Utrecht, Netherlands. [Lopez, J.] Univ Autonoma Madrid, Dept Geol & Geoquim, Madrid, Spain. [Morgan, V.] CRC, Hobart, Tas, Australia. [Morgan, V.] Australian Antarctic Div, Hobart, Tas, Australia. [Motoyama, H.; Uemura, R.] Natl Inst Polar Res, Res Org Informat & Syst, Tokyo, Japan. [Noone, D.] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA. [Noone, D.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Oerter, H.] Alfred Wegener Inst Polar & Meeresforchung, Bremerhaven, Germany. [Schmidt, G. A.] NASA GISS, New York, NY USA. [Schlosser, E.] Univ Innsbruck, Inst Meteorol & Geophys, A-6020 Innsbruck, Austria. [Steig, E. J.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. [Vimeux, F.] IRD, UR Greatice, Paris, France. [White, J. W. C.] INSTAAR, Boulder, CO USA. RP Masson-Delmotte, V (reprint author), CEA Saclay, IPSL CEA CNRS UVSQ UMR 1572, Lab Sci Climat & Environm, Bat 701, F-91191 Gif Sur Yvette, France. EM valerie.masson@cea.fr RI Van den Broeke, Michiel/F-7867-2011; White, James/A-7845-2009; van de Berg, Willem Jan/H-4385-2011; Masson-Delmotte, Valerie/G-1995-2011; Lopez-Martinez, Jeronimo/C-5744-2011; Schmidt, Gavin/D-4427-2012; Aptel, Flo/E-6885-2013; van de wal, roderik/D-1705-2011; Steig, Eric/G-9088-2015; Ekaykin, Alexey/K-9894-2015; OI Van den Broeke, Michiel/0000-0003-4662-7565; White, James/0000-0001-6041-4684; Masson-Delmotte, Valerie/0000-0001-8296-381X; Lopez-Martinez, Jeronimo/0000-0002-1750-8287; Schmidt, Gavin/0000-0002-2258-0486; Steig, Eric/0000-0002-8191-5549; Ekaykin, Alexey/0000-0001-9819-2802; Uemura, Ryu/0000-0002-4236-0085 NR 154 TC 145 Z9 151 U1 1 U2 58 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD JUL PY 2008 VL 21 IS 13 BP 3359 EP 3387 DI 10.1175/2007JCLI2139.1 PG 29 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 326ZM UT WOS:000257698300018 ER PT J AU Baltz, EA Berenji, B Bertone, G Bergstrom, L Bloom, E Bringmann, T Chiang, J Cohen-Tanugi, J Conrad, J Edmonds, Y Edsjo, J Godfrey, G Hughes, RE Johnson, RP Lionetto, A Moiseev, AA Morselli, A Moskalenko, IV Nuss, E Ormes, JF Rando, R Sander, AJ Sellerholm, A Smith, PD Strong, AW Wai, L Wang, P Winer, BL AF Baltz, E. A. Berenji, B. Bertone, G. Bergstrom, L. Bloom, E. Bringmann, T. Chiang, J. Cohen-Tanugi, J. Conrad, J. Edmonds, Y. Edsjoe, J. Godfrey, G. Hughes, R. E. Johnson, R. P. Lionetto, A. Moiseev, A. A. Morselli, A. Moskalenko, I. V. Nuss, E. Ormes, J. F. Rando, R. Sander, A. J. Sellerholm, A. Smith, P. D. Strong, A. W. Wai, L. Wang, P. Winer, B. L. TI Pre-launch estimates for GLAST sensitivity to dark matter annihilation signals SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Review DE dark matter simulations; dark matter detectors; dark matter ID GAMMA-RAY EMISSION; INVERSE COMPTON-SCATTERING; MICROWAVE-ANISOTROPY-PROBE; MILKY-WAY HALO; GALACTIC-CENTER; EGRET DATA; OBSERVATIONAL EVIDENCE; INTERSTELLAR-MEDIUM; POWER SPECTRUM; COSMIC-RAYS AB We investigate the sensitivity of the Gamma-ray Large Area Space Telescope (GLAST) for indirectly detecting weakly interacting massive particles (WIMPs) through the gamma-ray signal that their pair annihilation produces. WIMPs are among the favorite candidates for explaining the compelling evidence that about 80% of the mass in the Universe is non-baryonic dark matter (DM). They are serendipitously motivated by various extensions of the standard model of particle physics such as supersymmetry and universal extra dimensions (UED). With its unprecedented sensitivity and its very large energy range (20 MeV to more than 300 GeV) the main instrument on board the GLAST satellite, the Large Area Telescope (LAT), will open a new window of discovery. As our estimates show, the LAT will be able to detect an indirect DM signature for a large class of WIMP models given a cuspy profile for the DM distribution. Using the current state of the art Monte Carlo and event reconstruction software developed within the LAT collaboration, we present preliminary sensitivity studies for several possible sources inside and outside the Galaxy. We also discuss the potential of the LAT to detect UED via the electron/positron channel. Diffuse background modeling and other background issues that will be important in setting limits or seeing a signal are presented. C1 Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. KIPAC, SLAC, Menlo Pk, CA 94025 USA. Inst Astrophys, F-75014 Paris, France. Ohio State Univ, Columbus, OH 43210 USA. Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. INFN Roma Tor Vergata, Rome, Italy. NASA GSFC, CRESST, AstroParticle Phys Lab, Greenbelt, MD 20771 USA. Stanford Univ, Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. Univ Montpellier, LPTA, CNRS IN2P3, F-34059 Montpellier, France. Univ Denver, Denver, CO 80208 USA. INFN, Sezione Padova, I-35131 Padua, Italy. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. RP Conrad, J (reprint author), Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. EM conrad@physto.se RI Morselli, Aldo/G-6769-2011; Rando, Riccardo/M-7179-2013; Moskalenko, Igor/A-1301-2007; OI Morselli, Aldo/0000-0002-7704-9553; Moskalenko, Igor/0000-0001-6141-458X; Rando, Riccardo/0000-0001-6992-818X; Berenji, Bijan/0000-0002-4551-772X NR 104 TC 143 Z9 143 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 JUL PY 2008 IS 7 AR 013 DI 10.1088/1475-7516/2008/07/013 PG 43 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 331OZ UT WOS:000258022800013 ER PT J AU Park, J Palazzolo, A Beach, R AF Park, Junyoung Palazzolo, Alan Beach, Raymond TI MIMO active vibration control of magnetically suspended flywheels for satellite IPAC service SO JOURNAL OF DYNAMIC SYSTEMS MEASUREMENT AND CONTROL-TRANSACTIONS OF THE ASME LA English DT Article ID ENERGY-STORAGE SYSTEM; ATTITUDE-CONTROL; BEARING; SPACECRAFT; MANEUVERS; FEEDBACK; TRACKING; WHEELS AB Theory and simulation results have demonstrated that four, variable speed flywheels could potentially provide the energy storage and attitude control functions of existing batteries and control moment gyros on a satellite. Past modeling and control algorithms were based on the assumption of rigidity in the flywheel's bearings and the satellite structure. This paper provides simulation results and theory, which eliminates this assumption utilizing control algorithms for active vibration control (AVC), flywheel shaft levitation, and integrated power transfer and attitude control (IPAC), that are effective even with low stiffness active magnetic bearings (AMBs) and flexible satellite appendages. The flywheel AVC and levitation tasks are provided by a multiple input-multiple output control law that enhances stability by reducing the dependence of the forward and backward gyroscopic poles with changes in flywheel speed. The control law is shown to be effective even for (1) large polar to transverse inertia ratios, which increases the stored energy density while causing the poles to become more speed dependent, and for (2) low bandwidth controllers shaped to suppress high frequency noise. Passive vibration dampers are designed to reduce the vibrations of flexible appendages of the satellite. Notch, low-pass, and bandpass filters are implemented in the AMB system to reduce and cancel high frequency, dynamic bearing forces and motor torques due to flywheel mass imbalance. Successful IPAC simulation results are presented with a 12% initial attitude error, large polar to transverse inertia ratio (I(P)/I(T)), structural flexibility, and unbalance mass disturbance. C1 [Park, Junyoung; Palazzolo, Alan] Texas A&M Univ, Dept Mech Engn, Vibrat Control & Electromech Lab, College Stn, TX 77843 USA. [Beach, Raymond] NASA Glenn, Power Technol Div, Cleveland, OH 44135 USA. RP Park, J (reprint author), Texas A&M Univ, Dept Mech Engn, Vibrat Control & Electromech Lab, MS 3123, College Stn, TX 77843 USA. NR 30 TC 5 Z9 5 U1 0 U2 13 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 JUL PY 2008 VL 130 IS 4 AR 041005 DI 10.1115/1.2936846 PG 22 WC Automation & Control Systems; Instruments & Instrumentation SC Automation & Control Systems; Instruments & Instrumentation GA 318ZZ UT WOS:000257132800005 ER PT J AU Hanson, TA Yilmaz, N Drozda, P Gill, W Miller, TJ Donaldson, AB AF Hanson, Thomas A. Yilmaz, Nadir Drozda, Pat Gill, Walter Miller, Timothy J. Donaldson, A. Burl TI Acoustic pyrometry using an off-the-shelf range finding system SO JOURNAL OF FIRE SCIENCES LA English DT Article DE acoustic; pyrometry; flame; temperature; measurement ID FLOW-FIELDS; TEMPERATURE; TRANSDUCERS; FLAMES AB In this study, the development and validation of a non-invasive flame temperature measurement tool from an off-the-shelf ultrasonic rangefinder is discussed. Both 'pulse-echo' and single-pass methods are tested. The application of this device to the measurement of bench top flame temperatures is presented. C1 [Yilmaz, Nadir] New Mexico Inst Min & Technol, Dept Mech Engn, Socorro, NM 87801 USA. [Hanson, Thomas A.] NASA, Jacobs Technol Inc, Lyndon B Johnson Space Ctr, White Sands Test Facil, Las Cruces, NM 88004 USA. [Drozda, Pat; Gill, Walter; Miller, Timothy J.] Sandia Natl Labs, Albuquerque, NM 87123 USA. [Donaldson, A. Burl] New Mexico State Univ, Dept Mech Engn, Las Cruces, NM 88003 USA. RP Yilmaz, N (reprint author), New Mexico Inst Min & Technol, Dept Mech Engn, Socorro, NM 87801 USA. EM yilmaznadir@yahoo.com NR 9 TC 7 Z9 7 U1 0 U2 3 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0734-9041 J9 J FIRE SCI JI J. Fire Sci. PD JUL PY 2008 VL 26 IS 4 BP 287 EP 308 DI 10.1177/0734904107087817 PG 22 WC Engineering, Multidisciplinary; Materials Science, Multidisciplinary SC Engineering; Materials Science GA 321SJ UT WOS:000257326500001 ER PT J AU Han, SC Ditmar, P AF Han, Shin-Chan Ditmar, Pavel TI Localized spectral analysis of global satellite gravity fields for recovering time-variable mass redistributions SO JOURNAL OF GEODESY LA English DT Article DE spatiospectral localization; spherical harmonic analysis; GRACE; GOCE; hydrology; earthquake ID GRAVITATIONAL SIGNATURE; GRACE; EARTHQUAKE; DYNAMICS; SYSTEM AB A spatiospectral localization method is discussed for processing the global geopotential coefficients from satellite mission data to investigate time-variable gravity. The time-variable mass variation signal usually appears associated with a particular geographical area yielding inherently regional structure, while the dependence of the satellite gravity errors on a geographical region is not so evident. The proposed localization amplifies the signal-to-noise ratio of the (non-stationary) time-variable signals in the geopotential coefficient estimates by localizing the global coefficients to the area where the signal is expected to be largest. The results based on localization of the global satellite gravity coefficients such as Gravity Recovery And Climate Experiment (GRACE) and Gravity and Ocean Circulation Explorer (GOCE) indicate that the coseismic deformation caused by great earthquakes such as the 2004 Sumatra-Andaman earthquake can be detected by the low-low tracking and the gradiometer data within the bandwidths of spherical degrees 15-30 and 25-100, respectively. However, the detection of terrestrial water storage variation by GOCE gradiometer is equivocal even after localization. C1 [Han, Shin-Chan] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Han, Shin-Chan] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Catonsville, MD 21228 USA. [Ditmar, Pavel] Delft Univ Technol, Fac Aerosp Engn, Dept Earth Observat & Space Syst DEOS, NL-2629 HS Delft, Netherlands. RP Han, SC (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Code 698, Greenbelt, MD 20771 USA. EM schan@puuoo.gsfc.nasa.gov RI Han, Shin-Chan/A-2022-2009; OI Ditmar, Pavel/0000-0002-8188-7680 NR 29 TC 15 Z9 15 U1 0 U2 4 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 JUL PY 2008 VL 82 IS 7 BP 423 EP 430 DI 10.1007/s00190-007-0194-5 PG 8 WC Geochemistry & Geophysics; Remote Sensing SC Geochemistry & Geophysics; Remote Sensing GA 321XX UT WOS:000257340900005 ER PT J AU Cavalieri, DJ Parkinson, CL AF Cavalieri, D. J. Parkinson, C. L. TI Antarctic sea ice variability and trends, 1979-2006 SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID CIRCUMPOLAR WAVE; SOUTHERN-OCEAN; TIME-SERIES; TEMPERATURE AB Analyses of 28 years (1979-2006) of Antarctic sea ice extents and areas derived from satellite passive microwave radiometers are presented and placed in the context of results obtained previously for the 20-year period 1979-1998. We present monthly averaged sea ice extents and areas, monthly deviations, yearly and seasonal averages, and their trends for the Southern Hemisphere as a whole and for each of five sectors: the Weddell Sea, the Indian Ocean, the western Pacific Ocean, the Ross Sea, and the Bellingshausen/Amundsen seas. The total Antarctic sea ice extent trend increased slightly, from 0.96 +/- 0.61% decade(-1) to 1.0 +/- 0.4% decade(-1), from the 20- to 28-year period, reflecting contrasting changes in the sector trends. The eight additional years resulted in smaller positive yearly trends in sea ice extent for the Weddell Sea (0.80 +/- 1.4% decade(-1)), the western Pacific Ocean (1.4 +/- 1.9% decade(-1)), and the Ross Sea (4.4 +/- 1.7% decade(-1)) sectors, a lessening of the negative trend for the Bellingshausen/Amundsen seas (-5.4 +/- 1.9% decade(-1)) sector, and a shift from a negative trend to a positive trend for the Indian Ocean ( 1.9 +/- 1.4% decade(-1)) sector. The trends for the Southern Hemisphere as a whole and for the Ross Sea sector are significant at the 95% level, whereas the trend for the Bellingshausen/Amundsen seas sector is significant at the 99% level. A similar pattern of yearly trend changes for the two periods is also apparent in the sea ice area time series. C1 [Cavalieri, D. J.] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD 20771 USA. RP Cavalieri, DJ (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Code 614-1, Greenbelt, MD 20771 USA. EM donald.j.cavalieri@nasa.gov RI Parkinson, Claire/E-1747-2012 OI Parkinson, Claire/0000-0001-6730-4197 NR 18 TC 102 Z9 108 U1 0 U2 24 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 EI 2169-9291 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD JUL 1 PY 2008 VL 113 IS C7 AR C07004 DI 10.1029/2007JC004564 PG 19 WC Oceanography SC Oceanography GA 323GA UT WOS:000257432800003 ER PT J AU Parkinson, CL Cavalieri, DJ AF Parkinson, Claire L. Cavalieri, Donald J. TI Arctic sea ice variability and trends, 1979-2006 SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID TIME-SERIES; INTERANNUAL VARIABILITY; POLAR BEARS; CLIMATE; OSCILLATION; TEMPERATURE; CIRCULATION; RECORD; EXTENT; COVER AB Analysis of Arctic sea ice extents derived from satellite passive-microwave data for the 28 years 1979-2006 yields an overall negative trend of -45,100 +/- 4,600 km(2)/a (-3.7 +/- 0.4%/decade) in the yearly averages, with negative ice extent trends also occurring for each of the four seasons and each of the 12 months. For the yearly averages, the largest decreases occur in the Kara and Barents seas and the Arctic Ocean, with linear least squares slopes of -10,600 +/- 2,800 km(2)/a (-7.4 +/- 2.0%/decade) and -10,100 +/- 2,200 km(2)/a (-1.5 +/- 0.3%/ decade), respectively, followed by Baffin Bay/Labrador Sea, with a slope of -8000 +/- 2000 km(2)/a (-9.0 +/- 2.3%/decade), the Greenland Sea, with a slope of -7000 +/- 1400 km(2)/a (-9.3 +/- 1.9%/decade), and Hudson Bay, with a slope of -4500 +/- 900 km(2)/a (-5.3 +/- 1.1%/decade). These are all statistically significant decreases at a 99% confidence level. The seas of Okhotsk and Japan also have a statistically significant ice decrease, although at a 95% confidence level, and the three remaining regions, the Bering Sea, Canadian Archipelago, and Gulf of St. Lawrence, have negative slopes that are not statistically significant. The 28-year trends in ice areas for the Northern Hemisphere total are also statistically significant and negative in each season, each month, and for the yearly averages. C1 [Parkinson, Claire L.] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD 20771 USA. RP Parkinson, CL (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Code 614-1, Greenbelt, MD 20771 USA. EM claire.l.parkinson@nasa.gov RI Parkinson, Claire/E-1747-2012 OI Parkinson, Claire/0000-0001-6730-4197 NR 43 TC 144 Z9 157 U1 4 U2 39 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 EI 2169-9291 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD JUL 1 PY 2008 VL 113 IS C7 AR C07003 DI 10.1029/2007JC004558 PG 28 WC Oceanography SC Oceanography GA 323GA UT WOS:000257432800002 ER PT J AU Le Deit, L Le Mouelic, S Bourgeois, O Combe, JP Mege, D Sotin, C Gendrin, A Hauber, E Mangold, N Bibring, JP AF Le Deit, Laetitia Le Mouelic, Stephane Bourgeois, Olivier Combe, Jean-Philippe Mege, Daniel Sotin, Christophe Gendrin, Aline Hauber, Ernst Mangold, Nicolas Bibring, Jean-Pierre TI Ferric oxides in East Candor Chasma, Valles Marineris (Mars) inferred from analysis of OMEGA/Mars Express data: Identification and geological interpretation SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID THERMAL EMISSION SPECTROMETER; MERIDIANI-PLANUM; EVOLUTION; DEPOSITS; MISSION; SURFACE; DECONVOLUTION; DIVERSITY; SULFATES; SPECTRA AB The mineralogical composition of the Martian surface is constrained by analyzing the data of the OMEGA visible and near infrared imaging spectrometer onboard Mars Express. Ferric signatures had previously been reported in Valles Marineris, Margaritifer Terra, and Terra Meridiani. Here we use three independent data reduction methods (Spectral Angle Mapper, a modified Spectral Mixture Analysis and Modified Gaussian Model) to detect and map ferric oxides in East Candor Chasma, a part of Valles Marineris. Ferric oxides in East Candor Chasma are concentrated in scattered formations. MOLA altimetry indicates that the ferric oxides are preferentially located in topographic lows. THEMIS, HRSC and MOC images show that the ferric oxide spectral signatures are systematically correlated with superficial deposits of low albedo, located at the foot of, or resting on Interior Layered Deposits (ILDs). This spatial distribution suggests that ferric oxides are genetically linked to ILDs. Gravity and wind-driven remobilization of ferric oxides previously formed in the ILDs can explain their accumulation around the ILDs. C1 [Le Deit, Laetitia; Le Mouelic, Stephane; Bourgeois, Olivier; Mege, Daniel; Sotin, Christophe; Mangold, Nicolas] Univ Nantes, Fac Sci & Tech, Lab Planetol & Geodynam Nantes, CNRS,UMR 6112, F-44322 Nantes 3, France. [Combe, Jean-Philippe] Bear Fight Ctr, Space Sci Inst, Winthrop, WA 98862 USA. [Sotin, Christophe] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Gendrin, Aline; Bibring, Jean-Pierre] Univ Paris 11, Inst Astrophys Spatiale, CNRS, F-91405 Orsay, France. [Hauber, Ernst] DLR, Inst Planetary Res, D-12489 Berlin, Germany. [Mangold, Nicolas] CNRS, IDES, F-91405 Orsay, France. RP Le Deit, L (reprint author), Univ Nantes, Fac Sci & Tech, Lab Planetol & Geodynam Nantes, CNRS,UMR 6112, 2 Chemin Houssiniere,BP 92208, F-44322 Nantes 3, France. EM laetitia.ledeit@univ-nantes.fr RI Mege, Daniel/A-2331-2009; OI Mege, Daniel/0000-0003-4304-9878 NR 75 TC 32 Z9 32 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUL 1 PY 2008 VL 113 IS E7 AR E07001 DI 10.1029/2007JE002950 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 323GE UT WOS:000257433200001 ER PT J AU Zhang, S Zhu, L Minus, ML Chae, HG Jagannathan, S Wong, CP Kowalik, J Roberson, LB Kumar, S AF Zhang, Shanju Zhu, Lingbo Minus, Marilyn L. Chae, Han Gi Jagannathan, Sudhakar Wong, Ching-Ping Kowalik, Janusz Roberson, Luke B. Kumar, Satish TI Solid-state spun fibers and yarns from 1-mm long carbon nanotube forests synthesized by water-assisted chemical vapor deposition SO JOURNAL OF MATERIALS SCIENCE LA English DT Article; Proceedings Paper CT Materials Science and Technology Conference and Exhibition (MS&T'07) CY SEP 16-20, 2007 CL Detroit, MI ID MECHANICAL-PROPERTIES; SINGLE; ARRAYS AB We report continuous carbon nanotube (CNT) fibers and yarns dry-drawn directly from water-assisted chemical vapor deposition (CVD) grown forests with about 1-mm height. As-drawn CNT fibers exist as aerogel and can be transformed into more compact fibers through twisting or densification with a volatile organic liquid. CNT fibers are characterized by scanning electron microscopy, X-ray photoelectron spectroscopy, Raman microscopy, and wide-angle X-ray diffraction. Mechanical properties and electrical conductivity of the post-treated CNT fibers are investigated. The resulting fibers show the work of rupture of 30 J/g and DC electrical conductivity of 5.0 x 10(4) S/m. C1 [Zhang, Shanju; Minus, Marilyn L.; Chae, Han Gi; Jagannathan, Sudhakar; Kumar, Satish] Georgia Inst Technol, Sch Polymer Text & Fiber Engn, Atlanta, GA 30332 USA. [Zhu, Lingbo; Wong, Ching-Ping] Georgia Inst Technol, Sch Mat Sci & Engn, Atlanta, GA 30332 USA. [Kowalik, Janusz] Georgia Inst Technol, Sch Chem & Biochem, Atlanta, GA 30332 USA. [Roberson, Luke B.] NASA, John F Kennedy Space Ctr, Kennedy Sapce Ctr, Kennedy Space Ctr, FL 32899 USA. RP Kumar, S (reprint author), Georgia Inst Technol, Sch Polymer Text & Fiber Engn, 801 Ferst Dr, Atlanta, GA 30332 USA. EM szhang30@mail.gatech.edu; satish.kumar@ptfe.gatech.edu RI Kumar, Satish/F-7308-2011; Zhang, Shanju/E-5119-2011; Chae, Han Gi/M-5427-2016 OI Chae, Han Gi/0000-0003-2196-0986 NR 27 TC 52 Z9 56 U1 7 U2 39 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2461 J9 J MATER SCI JI J. Mater. Sci. PD JUL PY 2008 VL 43 IS 13 BP 4356 EP 4362 DI 10.1007/s10853-008-2558-5 PG 7 WC Materials Science, Multidisciplinary SC Materials Science GA 304DL UT WOS:000256090100002 ER PT J AU Seong, M Mohanchandra, KP Lin, Y Carman, GP AF Seong, Myunghoon Mohanchandra, K. P. Lin, Yohan Carman, Gregory P. TI Development of a 'bi-layer lift-off' method for high flow rate and high frequency Nitinol MEMS valve fabrication SO JOURNAL OF MICROMECHANICS AND MICROENGINEERING LA English DT Article ID MICRO CHECK VALVES; THIN-FILM; ACTUATORS; ROBUST; ARRAY AB This paper presents modeling, fabrication and testing results for a high flow rate and high frequency nickel titanium alloy ( Nitinol) MEMS valve. ANSYSR(R) is used to evaluate several Nitinol MEMS valve structural designs with the conclusion that a pentagonal flap with five legs produces higher frequencies and higher strengths without the inherent rotation problem present in four-leg designs. The Nitinol penta-leg design was fabricated using a novel bi-layer lift-off method. A polymethylglutarimide (PMGI) polymer layer is initially used as an underlayer while a chromium layer is used as a top layer to produce a non-rotational ortho-planar Nitinol MEMS valve array without the problems inherent in conventional Nitinol wet etching. The array consists of 65 microvalves with a single valve having dimensions of 1 mm circumference, 50 mu m leg width and 8.2 mu m Nitinol thickness. Each microvalve covers an orifice of 220 mu m diameter and 500 mu m in length and is capable of producing 150 mu m vertical deflection. The Nitinol MEMS valve array was tested for flow rates in a hydraulic system as a function of applied pressure with a maximum water flow rate of 16.44 cc s(-1). C1 [Seong, Myunghoon; Mohanchandra, K. P.; Carman, Gregory P.] Univ Calif Los Angeles, Mech & Aerosp Engn Dept, Los Angeles, CA 90095 USA. [Lin, Yohan] NASA, Dryden Flight Res Ctr, Edwards AFB, CA 93523 USA. RP Seong, M (reprint author), Univ Calif Los Angeles, Mech & Aerosp Engn Dept, Los Angeles, CA 90095 USA. EM mhseong@ucla.edu NR 19 TC 7 Z9 7 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0960-1317 J9 J MICROMECH MICROENG JI J. Micromech. Microeng. PD JUL PY 2008 VL 18 IS 7 AR 075034 DI 10.1088/0960-1317/18/7/075034 PG 10 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology; Instruments & Instrumentation; Physics, Applied SC Engineering; Science & Technology - Other Topics; Instruments & Instrumentation; Physics GA 318YG UT WOS:000257128100035 ER PT J AU Melnik, R Povitsky, A Srivastava, D AF Melnik, Roderick Povitsky, Alex Srivastava, Deepak TI Mathematical and Computational Models for Transport and Coupled Processes in Micro- and Nanotechnology SO JOURNAL OF NANOSCIENCE AND NANOTECHNOLOGY LA English DT Editorial Material C1 [Melnik, Roderick] Wilfrid Laurier Univ, Fac Sci, Waterloo, ON N2L 3C5, Canada. [Povitsky, Alex] Univ Akron, Dept Mech Engn, Akron, OH 44325 USA. [Srivastava, Deepak] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Melnik, Roderick] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Melnik, Roderick] CSIRO, Sydney, NSW, Australia. [Povitsky, Alex] Concordia Univ, Montreal, PQ, Canada. [Srivastava, Deepak] NASA, Ames Ctr Nanotechnol, Moffett Field, CA USA. RP Melnik, R (reprint author), Wilfrid Laurier Univ, Fac Sci, Waterloo, ON N2L 3C5, Canada. NR 0 TC 5 Z9 5 U1 0 U2 1 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 JUL PY 2008 VL 8 IS 7 BP 3626 EP 3627 DI 10.1166/jnn.2008.001 PG 2 WC Chemistry, Multidisciplinary; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA 370QC UT WOS:000260776600049 PM 19051921 ER PT J AU Srivastava, D Makeev, MA Menon, M Osman, M AF Srivastava, Deepak Makeev, Maxim A. Menon, Madhu Osman, Mohamed TI Computational Nanomechanics and Thermal Transport in Nanotubes and Nanowires SO JOURNAL OF NANOSCIENCE AND NANOTECHNOLOGY LA English DT Article DE Carbon Nanotubes; Nanowires; Mechanical Properties; Thermal Transport ID BINDING MOLECULAR-DYNAMICS; WALL CARBON NANOTUBES; ELASTIC PROPERTIES; GRAPHITIC TUBULES; SILICON NANOWIRES; YOUNGS MODULUS; CONDUCTIVITY; SIMULATION; SCHEME; ROPES AB Representative results of computer simulation and/or modeling studies of the nanomechanical and thermal transport properties of an individual carbon nanotube, silicon nanowire, and silicon carbide nanowire systems have been reviewed and compared with available experimental observations. The investigated nanomechanical properties include different elastic moduli of carbon nanotubes, silicon nanowires, and silicon carbide nanowires, all obtained within their elastic limits. Moreover, atomistic mechanisms of elastic to plastic transition under external stresses and yielding of carbon nanotubes under experimentally feasible temperature and strain rate conditions are discussed in detail. The simulation and/or modeling results on thermal properties, presented in this work, include vibrational modes, thermal conductivity and heat pulse transport through single carbon nanotubes, and thermal conductivity of silicon nanowires. C1 [Srivastava, Deepak; Makeev, Maxim A.] NASA, Ames Res Ctr, UARC, Adv Aerosp Mat & Devices Grp, Moffett Field, CA 94035 USA. [Menon, Madhu] Univ Kentucky, Dept Phys, Lexington, KY 40506 USA. [Menon, Madhu] Univ Kentucky, Ctr Computat Sci, Lexington, KY 40506 USA. [Osman, Mohamed] Washington State Univ, Sch Elect Engn & Comp Sci, Pullman, WA 99164 USA. RP Srivastava, D (reprint author), NASA, Ames Res Ctr, UARC, Adv Aerosp Mat & Devices Grp, Moffett Field, CA 94035 USA. FU NASA [NAS2-03144]; DOE [DE-FG02-00ER45817]; US-ARO [W91INF-05-1-0372] FX Part of this work (Deepak Srivastava and Maxim A. Makeev) is supported by NASA contract NAS2-03144 to UARC at Arnes Research Center. Madhu Menon gratefully acknowledges support from DOE (DE-FG02-00ER45817) and US-ARO (W91INF-05-1-0372). The authors gratefully acknowledge their colleagues, collaborators, students and postdocs, who have contributed to the work, described and reviewed in this manuscript. In particular, authors are very thankful to C. Andersen (University of Minnesota), D. W. Brenner (North Carolina State University), 1. Ponomareva (University of Arkansas), K. J. Cho (Stanford University), A. Cummings (Washington State University), N. Mingo, (UARC, NASA Ames Research Center), E. G. Noya (University of Santiago, Spain), R. Ruoff (Northwestern University), K. Tamma (University of Minnesota), C. Y. Wei (Eloret Corporation, NASA Arnes Research Center), and L. Zhigilei (University of Virginia) for their contribution to many papers quoted in this review. NR 82 TC 7 Z9 7 U1 3 U2 20 PU AMER SCIENTIFIC PUBLISHERS PI VALENCIA PA 26650 THE OLD RD, STE 208, VALENCIA, CA 91381-0751 USA SN 1533-4880 EI 1533-4899 J9 J NANOSCI NANOTECHNO JI J. Nanosci. Nanotechnol. PD JUL PY 2008 VL 8 IS 7 BP 3628 EP 3651 DI 10.1166/jnn.2008.016 PG 24 WC Chemistry, Multidisciplinary; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA 370QC UT WOS:000260776600050 PM 19051922 ER PT J AU Lim, DSS Smol, JP Douglas, MSV AF Lim, Darlene S. S. Smol, John P. Douglas, Marianne S. V. TI Recent environmental changes on Banks Island (NWT, Canadian Arctic) quantified using fossil diatom assemblages SO JOURNAL OF PALEOLIMNOLOGY LA English DT Article DE Banks Island; Arctic; diatoms; nitrogen; paleolimnology; climate change; sediments ID CLIMATE-CHANGE; PALEOLIMNOLOGICAL EVIDENCE; WATER TEMPERATURE; ELLESMERE-ISLAND; INFERENCE MODELS; BAFFIN-ISLAND; LAKES; PONDS; VARIABLES; COMMUNITIES AB Banks Island (N.W.T.) has become a focal point for climate change studies in the Canadian Arctic. However, long-term climatic and environmental data are very sparse from this large island, as they are for the entire southwestern region of the Canadian Arctic Archipelago. In this paleolimnological study, diatom species assemblage shifts documented in cores collected from a pond and a lake on Banks Island were interpreted to represent a response to climate warming commencing in the nineteenth century. We found that, although the timing and overall nature of the species changes in the two cores were consistent, the signal was muted in the deeper site likely as a result of differences in ice cover extent and duration between lakes and ponds. A high-resolution study was also conducted from a second pond, at sub-decadal resolution, that only spanned the last similar to 60 years. In the deeper lake site, Fragilaria construens and F. pinnata dominated the assemblages, similar to those noted in other high Arctic regions where lakes are characterized by extended ice cover. In contrast, Denticula kuetzingii dominated the shallower ponds and, in the case of the pond core representing the longer time period, this taxon increased in the post-1850 sediments, likely coincident with climate warming. In all cores, diatom assemblages became more diverse and Achnanthes species (particularly A. minutissima) increased from similar to 1850 to the present, similar to changes documented in other Arctic regions. Beta diversity values calculated for the diatom species changes indicated that assemblage shifts in the Banks Island cores were of similar magnitude to those recorded in other Arctic regions with high species turnover, such as Ellesmere Island. A diatom-based Total Nitrogen (TN) transfer function previously developed for Banks Island was applied to the three (210)Pb dated cores as an exploratory tool for inferring past changes in nitrogen concentrations. In both the lake and pond cores, diatom-inferred TN concentrations tended to increase in the more recent sediments, as may be expected with warming; however these trends were not very distinct. C1 [Lim, Darlene S. S.; Douglas, Marianne S. V.] Univ Toronto, Dept Geol, PAL, Toronto, ON M5S 3B1, Canada. [Smol, John P.] Queens Univ, Dept Biol, PEARL, Kingston, ON K7L 3N6, Canada. RP Lim, DSS (reprint author), NASA, Ames Res Ctr, Mail Stop 245-3, Moffett Field, CA 94110 USA. EM dlim@mail.arc.nasa.gov RI Smol, John/A-8838-2015 NR 62 TC 12 Z9 12 U1 0 U2 10 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0921-2728 J9 J PALEOLIMNOL JI J. Paleolimn. PD JUL PY 2008 VL 40 IS 1 BP 385 EP 398 DI 10.1007/s10933-007-9168-0 PG 14 WC Environmental Sciences; Geosciences, Multidisciplinary; Limnology SC Environmental Sciences & Ecology; Geology; Marine & Freshwater Biology GA 320BL UT WOS:000257208600025 ER PT J AU Lackey, JS Valley, JW Chen, JH Stockli, DF AF Lackey, Jade Star Valley, John W. Chen, James H. Stockli, Daniel F. TI Dynamic magma systems, crustal recycling, and alteration in the central Sierra Nevada batholith: the oxygen isotope record SO JOURNAL OF PETROLOGY LA English DT Review DE zircon; crustal growth; granitoids; supracrustal; magma systems; Sierra Nevada ID FOOTHILLS METAMORPHIC BELT; TUOLUMNE INTRUSIVE SUITE; CENTRAL WHITE MOUNTAINS; YOSEMITE-NATIONAL-PARK; PENINSULAR RANGES; ACCESSORY MINERALS; EASTERN CALIFORNIA; (U-TH)/HE AGES; GRANITIC-ROCKS; HIGH-PRECISION AB Values of delta(18)O of zircon from the central Sierra Nevada batholith (SNB), California, yield fresh insight into the magmatic evolution and alteration history of this classic convergent margin batholith. Direct comparison of whole-rock and zircon (Zrc) delta(18)O provides evidence for modest (0.5), but widespread, alteration, which has complicated interpretation in previous whole-rock delta(18)O studies. Four discrete belts of delta(18)O values are recognized in the central Sierra. A small belt of plutons with relatively low delta(18)O(Zrc) values (5.2-6.0 parts per thousand) intrudes the foothills, with a sharp increase of (18)O revealing the concealed Foothills Suture; high delta(18)O(Zrc) values (7.0-8.5 parts per thousand) dominate the rest of the western SNB. East of the axis of the Sierra, delta(18)O is distinctly lower (6.75-5.75 parts per thousand), and decreases monotonically to the Sierra Crest. A sharp 1 parts per thousand increase of delta(18)O in the eastern Sierra reveals a second crustal boundary, with the fourth belt hosted in high-delta(18)O North American crust in the White Mountains and Owens and Long Valleys. Correlated O, Sr, and Pb isotope ratios reveal differences in magma generation between the western and eastern Sierra. The western Sierra experienced massive crustal recycling, with substantial melting and mobilization of accreted oceanic and volcanic arc rocks; crustal contamination affects many western SNB plutons. In contrast, the eastern Sierra was dominated by voluminous recycling of the lithospheric mantle and lower crust, with minimal crustal contamination. Batholith-wide shifts in delta(18)O occur between pulses of Cretaceous magmatism that may be linked to tectonic reorganizations of magma sources. Within intrusive suites, delta(18)O may be unchanged (Tuolumne); increase (Sonora and Whitney); or decrease (Sequoia and John Muir) with time. These trends show stable long-lived sources, or those where recycling and contamination may increase or decrease with time. Overall, delta(18)O reveals diverse magma system behavior at a range of scales in the Sierran arc. C1 [Lackey, Jade Star] Pomona Coll, Dept Geol, Claremont, CA 91711 USA. [Valley, John W.] Univ Wisconsin, Dept Geol & Geophys, Madison, WI 53706 USA. [Chen, James H.] CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA 91109 USA. [Stockli, Daniel F.] Univ Kansas, Dept Geol, Lawrence, KS 66045 USA. RP Lackey, JS (reprint author), Pomona Coll, Dept Geol, Claremont, CA 91711 USA. EM JadeStar.Lackey@pomona.edu RI Valley, John/B-3466-2011; Stockli, Daniel/N-8868-2015 OI Valley, John/0000-0003-3530-2722; Stockli, Daniel/0000-0001-7652-2129 NR 108 TC 89 Z9 89 U1 3 U2 28 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0022-3530 J9 J PETROL JI J. Petrol. PD JUL PY 2008 VL 49 IS 7 BP 1397 EP 1426 DI 10.1093/petrology/egn030 PG 30 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 322ZV UT WOS:000257414700006 ER PT J AU Baurle, RA Gaffney, RL AF Baurle, R. A. Gaffney, R. L. TI Extraction of one-dimensional flow properties from multidimensional data sets SO JOURNAL OF PROPULSION AND POWER LA English DT Article; Proceedings Paper CT AIAA 45th Aerospace Sciences Meeting and Exhibit CY JAN 08-11, 2007 CL Reno, NV SP Amer Inst Aeronaut & Astronaut ID HYPERSONIC ENGINES; THRUST LOSSES AB The engineering design and analysis of air-breathing propulsion systems relies heavily on zero- or one-dimensional properties (e.g., thrust, total pressure recovery, mixing, and combustion efficiency, etc.) for figures of merit. The extraction of these parameters from experimental data sets and/or multidimensional computational data sets is therefore an important aspect of the design process. A variety of methods exist for extracting performance measures from multidimensional data sets. Some of the information contained in the multidimensional flow is inevitably lost when any one-dimensionalization technique is applied. Hence, the unique assumptions associated with a given approach may result in one-dimensional properties that are significantly different than those extracted using alternative approaches. The purpose of this effort is to examine some of the more popular methods used for the extraction of performance measures from multidimensional data sets, reveal the strengths and weaknesses of each approach, and highlight various numerical issues that result when mapping data from a multidimensional space to a space of one dimension. C1 [Baurle, R. A.; Gaffney, R. L.] NASA Langley Res Ctr, Hampton, VA 23681 USA. RP Baurle, RA (reprint author), NASA Langley Res Ctr, Hampton, VA 23681 USA. NR 14 TC 9 Z9 10 U1 0 U2 2 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 J9 J PROPUL POWER JI J. Propul. Power PD JUL-AUG PY 2008 VL 24 IS 4 BP 704 EP 714 DI 10.2514/1.32074 PG 11 WC Engineering, Aerospace SC Engineering GA 327ID UT WOS:000257721900008 ER PT J AU Mikellides, LG Katz, I AF Mikellides, Loannis G. Katz, Ira TI Wear mechanisms in electron sources for ion propulsion, 1: Neutralizer hollow cathode SO JOURNAL OF PROPULSION AND POWER LA English DT Article; Proceedings Paper CT AIAA/ASME/SAE/ASEE 43rd Joint Propulsion Conference CY JUL 08-11, 2007 CL Cincinnati, OH SP Amer Inst Aeronaut & Astronaut, ASME, SAE, ASEE ID FLOWS; MODEL AB Upon the completion of two long-duration life tests of a 30-cm ion engine, the orifice channel of the neutralizer hollow cathode was eroded away to as much as twice its original diameter. Whereas the neutralizer cathode orifice opened significantly, no noticeable erosion of the discharge cathode orifice was observed. No quantitative explanation of these erosion trends has been established since the completion of the two life tests. A two-dimensional model of the partially ionized gas inside these devices has been developed and applied to the neutralizer hollow cathode. The numerical simulations show that the main mechanism responsible for the channel erosion is sputtering by Xe+. These ions are accelerated by the sheath along the channel and bombard the surface with kinetic energy/charge of about 17 V at the beginning of cathode life. The density of the ions inside the neutralizer orifice is computed to be as high as 2.1 X 10(22) m(-3). Because of the 3.5-times larger diameter of the discharge cathode orifice, the ion density inside the orifice is more than 40 times lower and the sheath drop 7 V lower compared with the values in the neutralizer. At these conditions, Xe+ can cause no significant sputtering of the surface. C1 [Mikellides, Loannis G.; Katz, Ira] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mikellides, LG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 18 TC 11 Z9 11 U1 5 U2 11 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 J9 J PROPUL POWER JI J. Propul. Power PD JUL-AUG PY 2008 VL 24 IS 4 BP 855 EP 865 DI 10.2514/1.33461 PG 11 WC Engineering, Aerospace SC Engineering GA 327ID UT WOS:000257721900025 ER PT J AU Mikellides, IG Katz, I Goebel, DA Jameson, KK Polk, JE AF Mikellides, Ioannis G. Katz, Ira Goebel, Dan A. Jameson, Kristina K. Polk, James E. TI Wear mechanisms in electron sources for ion propulsion, 2: Discharge hollow cathode SO JOURNAL OF PROPULSION AND POWER LA English DT Article; Proceedings Paper CT AIAA/ASME/SAE/ASEE 43rd Joint Propulsion Conference CY JUL 08-11, 2007 CL Cincinnati, OH SP Amer Inst Aeronaut & Astronaut, ASME, SAE, ASEE ID PLASMA AB The wear of the keeper electrode in discharge hollow cathodes is a major impediment to the implementation of ion propulsion onboard long-duration space science missions. The development of a predictive theoretical model for hollow cathode keeper life has long been sought, but its realization has been hindered by the complexities associated with the physics of the partially ionized gas and the associated erosion mechanisms in these devices. Thus, although several wear mechanisms have been hypothesized, a quantitative explanation of life test erosion profiles has remained incomplete. A two-dimensional model of the partially ionized gas in a discharge cathode has been developed and applied to understand the mechanisms that drove the erosion of the keeper in two long-duration life tests of a 30-cm ion thruster. An extensive set of comparisons between predictions by the numerical simulations and measurements of the plasma properties and of the erosion patterns is presented. It is found that the near-plume plasma oscillations, predicted by theory and observed by experiment, effectively enhance the resistivity of the plasma as well as the energy of ions striking the keeper. C1 [Mikellides, Ioannis G.; Katz, Ira; Goebel, Dan A.; Jameson, Kristina K.; Polk, James E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mikellides, IG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 43 TC 15 Z9 15 U1 3 U2 12 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 J9 J PROPUL POWER JI J. Propul. Power PD JUL-AUG PY 2008 VL 24 IS 4 BP 866 EP 879 DI 10.2514/1.33462 PG 14 WC Engineering, Aerospace SC Engineering GA 327ID UT WOS:000257721900026 ER PT J AU Barrett, MJ Johnson, PK AF Barrett, Michael J. Johnson, Paul K. TI Carbon-carbon recuperators in closed-brayton-cycle space power systems (vol 24, pg 609, 2008) SO JOURNAL OF PROPULSION AND POWER LA English DT Correction C1 [Barrett, Michael J.] NASA, John H Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA. [Johnson, Paul K.] Analex Corp, Cleveland, OH 44135 USA. RP Barrett, MJ (reprint author), NASA, John H Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA. NR 1 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 0748-4658 J9 J PROPUL POWER JI J. Propul. Power PD JUL-AUG PY 2008 VL 24 IS 4 BP 896 EP 896 DI 10.2514/1.38900 PG 1 WC Engineering, Aerospace SC Engineering GA 327ID UT WOS:000257721900030 ER PT J AU Rinsland, CP Luo, M Shephard, MW Clerbaux, C Boone, CD Bernath, PF Chiou, L Coheur, PF AF Rinsland, Curtis P. Luo, Ming Shephard, Mark W. Clerbaux, Cathy Boone, Chris D. Bernath, Peter F. Chiou, Linda Coheur, P. F. TI Tropospheric emission spectrometer (TES) and atmospheric chemistry experiment (ACE) measurements of tropospheric chemistry in tropical southeast Asia during a moderate El Nino in 2006 SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE remote sensing; tropospheric chemistry; pollution; spectroscopy; carbon monoxide ID MOLECULAR SPECTROSCOPIC DATABASE; CARBON-MONOXIDE; NADIR RETRIEVALS; AURA SATELLITE; SCIAMACHY; MISSION; OBJECTIVES; SYSTEMS; MODEL; DOAS AB High spectral resolution Fourier transform spectrometer (FTS) measurements of tropospheric carbon monoxide (CO) distributions show mixing ratios over Indonesia during October 2006 of similar to 200 ppbv (10(-9) per unit volume) in the middle troposphere. The elevated emissions were caused by intense and widespread Indonesian peat and forest fire emissions elevated compared to other years by the impact of a moderate El Nino/Soutern Oscillation (ENSO) event, which delayed that year's monsoon season and produced very dry conditions. Moderate resolution imaging spectrometer (MODIS) fire counts, atmospheric chemistry experiment (ACE) measurements of elevated mixing ratios of fire emission products and near infrared extinction, and back trajectory calculations for a sample measurement location near the time of maximum emissions provide additional evidence that the elevated 2006 emissions resulted primarily from the Indonesia fires. Lower CO mixing ratios measured by ACE and fewer MODIS fire counts in Indonesia during October 2005 indicate lower emissions than during 2006. Coincident profiles from the ACE agree within the uncertainties with those from the tropospheric emission spcctrometer (TES) for pressure ranges and time periods with good TES sensitivity after accounting for its lower vertical sensitivity compared with the ACE FTS. (C) 2007 Elsevier Ltd. All rights reserved. C1 [Rinsland, Curtis P.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Luo, Ming] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Shephard, Mark W.] Atmospher & Environm Res Inc, Lexington, MA 02421 USA. [Clerbaux, Cathy] Univ Paris 06, CNRS, Serv Aeron, IPSL, F-75252 Paris, France. [Boone, Chris D.; Bernath, Peter F.] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. [Bernath, Peter F.] Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. [Chiou, Linda] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. [Coheur, P. F.] Univ Libre Bruxelles, B-1050 Brussels, Belgium. RP Rinsland, CP (reprint author), NASA, Langley Res Ctr, Mail Stop 401A, Hampton, VA 23681 USA. EM curtis.p.rinsland@nasa.gov; ming.luo@jpl.nasa.gov; mshephar@aer.com; catherine.clerbaux@aero.jussieu.fr; cboone@sciborg.uwaterloo.ca; bernath@uwaterloo.ca; linda.s.chiou@nasa.gov; pfcoheur@ulb.ac.be RI Bernath, Peter/B-6567-2012; clerbaux, cathy/I-5478-2013 OI Bernath, Peter/0000-0002-1255-396X; NR 51 TC 15 Z9 15 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD JUL PY 2008 VL 109 IS 10 BP 1931 EP 1942 DI 10.1016/j.jqsrt.2007.12.020 PG 12 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 313JZ UT WOS:000256738200015 ER PT J AU Butler, JJ Johnson, BC Rice, JP Shirley, EL Barnes, RA AF Butler, J. J. Johnson, B. C. Rice, J. P. Shirley, E. L. Barnes, R. A. TI Sources of Differences in On-Orbital Total Solar Irradiance Measurements and Description of a Proposed Laboratory Intercomparison SO JOURNAL OF RESEARCH OF THE NATIONAL INSTITUTE OF STANDARDS AND TECHNOLOGY LA English DT Article DE absolute radiometric calibration; diffraction calculations; total solar irradiance (TSI); TSI uncertainty; TSI workshop; on-orbital TSI differences ID NIST AB There is a 5 W/m(2) (about 0.35 %) difference between current on-orbit Total Solar Irradiance (TSI) measurements. On 18-20 July 2005, a workshop was held at the National Institute of Standards and Technology (NIST) in Gaithersburg, Maryland that focused on understanding possible reasons for this difference, through an examination of the instrument designs, calibration approaches, and appropriate measurement equations. The instruments studied in that workshop included the Active Cavity Radiometer Irradiance Monitor III (ACRIM III) on the Active Cavity Radiometer Irradiance Monitor SATellite (ACRIMSAT), the Total Irradiance Monitor (TIM) on the Solar Radiation and Climate Experiment (SORCE), the Variability of solar IRradiance and Gravity Oscillations (VIRGO) on the Solar and Heliospheric Observatory (SOHO), and the Earth Radiation Budget Experiment (ERBE) on the Earth Radiation Budget Satellite (ERBS). Presentations for each instrument included descriptions of its design, its measurement equation and uncertainty budget, and the methods used to assess on-orbit degradation. The workshop also included a session on satellite- and ground-based instrument comparisons and a session on laboratory-based comparisons and the application of new laboratory comparison techniques. The workshop has led to investigations of the effects of diffraction and of aperture area measurements on the differences between instruments. In addition, a laboratory-based instrument comparison is proposed that uses optical power measurements (with lasers that underfill the apertures of the TSI instruments), irradiance measurements (with lasers that overfill the apertures of the TSI instrument), and a cryogenic electrical substitution radiometer as a standard for comparing the instruments. A summary of the workshop and an overview of the proposed research efforts are presented here. C1 [Butler, J. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Johnson, B. C.; Rice, J. P.; Shirley, E. L.] Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA. [Barnes, R. A.] SAIC, Beltsville, MD USA. RP Butler, JJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. EM james.j.butler@nasa.gov; cjohnson@nist.gov; joe.rice@nist.gov; eric.shirley@nist.gov; robert.a.barnes@nasa.gov RI Butler, James/D-4188-2013 FU NASA EOS Project Science Office [S-41365-F] FX The authors are grateful to Dr. Greg Kopp for many useful comments and careful reading of the manuscript. The work at NIST was supported by the NASA EOS Project Science Office (S-41365-F). NR 14 TC 16 Z9 17 U1 0 U2 5 PU US GOVERNMENT PRINTING OFFICE PI WASHINGTON PA SUPERINTENDENT DOCUMENTS,, WASHINGTON, DC 20402-9325 USA SN 1044-677X J9 J RES NATL INST STAN JI J. Res. Natl. Inst. Stand. Technol. PD JUL-AUG PY 2008 VL 113 IS 4 BP 187 EP 203 DI 10.6028/jres.113.014 PG 17 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 360TP UT WOS:000260081000001 PM 27096120 ER PT J AU Stanley, DO Martinez, RM AF Stanley, Douglas O. Martinez, Roland M. TI Comparative assessment of lunar propellant options SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article AB In July 2006, the NASA Administrator's Office and the Constellation Program Office jointly commissioned a propellant options study to perform a comprehensive detailed analysis of the major propulsion system alternatives for the planned crew exploration vehicle and lunar surface access module before the crew exploration vehicle systems requirements review. The study team, which involved over 50 NASA engineers and analysts, performed detailed modeling of the propulsion systems and the crew exploration vehicle and lunar surface access module configurations to calculate the integrated system-level impacts on payload, mass, reliability, safety, risk, and life-cycle costs. This paper presents an overview of the tools and methods used to assess the propulsion system and architecture-level effects of employing the propellant options. It also provides the architecture-level relative performance, life-cycle costs, reliability, safety, schedule, programmatic risk, and sustainability assessments for scenarios that employ a wide variety of main and auxiliary propellant combinations. It also includes a qualitative discussion of the major risks of each scenario. As a result of the study, pressure-fed hypergolic propellants were selected as the baseline for the crew exploration vehicle service module main and auxiliary propulsion systems. Pump-fed hydrogen propellants were kept on the descent stage of the lunar surface access module, but the lunar surface access module ascent stage propellant baseline was changed to pressure-fed methane for the main and auxiliary propulsion systems, with a recommendation that the trade space be kept open while more detailed configuration studies are performed. C1 [Stanley, Douglas O.] Georgia Inst Technol, Dept Aerosp Engn, Hampton, VA 23188 USA. [Martinez, Roland M.] NASA, Lyndon B Johnson Space Ctr, Constellat Program, Houston, TX 77058 USA. RP Stanley, DO (reprint author), Georgia Inst Technol, Dept Aerosp Engn, 100 Explorat Dr, Hampton, VA 23188 USA. NR 3 TC 0 Z9 0 U1 1 U2 3 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD JUL-AUG PY 2008 VL 45 IS 4 BP 776 EP 784 DI 10.2514/1.36423 PG 9 WC Engineering, Aerospace SC Engineering GA 336UH UT WOS:000258389600013 ER PT J AU Covington, MA Heinemann, JM Goldstein, HE Chen, YK Terrazas-Salinas, I Balboni, JA Olejniczak, J Martinez, ER AF Covington, M. A. Heinemann, J. M. Goldstein, H. E. Chen, Y. -K. Terrazas-Salinas, I. Balboni, J. A. Olejniczak, J. Martinez, E. R. TI Performance of a low density ablative heat shield material (vol 45, 237, 2008) SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Correction AB An evaluation of the Stardust spacecraft, forebody heat shield design was conducted to address uncertainties in original development and qualification efforts. Results are reported for additional arc jet tests and analyses done on the ablative and thermal performance of the low density ablative material used in the Stardust design for conditions simulating nominal peak convective heating conditions expected for Stardust sample return capsule Earth entry. Test data were used to adjust iteratively the thermophysical properties in an ablative response computer code to match experimental in-depth temperatures. Ablative recession rates and maximum internal temperatures were satisfactorily predicted by the computer code using derived properties for nominal peak entry heating rates and for rates 37% greater than nominal. Experimental and computer model maximum internal material temperatures were in agreement over a range of conditions and are considered to validate the Stardust heat shield design although measured in-depth temperature data show consistent temperature rise deviations that are not accurately modeled by the computer code. Predicted Stardust heat shield performance based on these results indicates that maximum attachment bond line temperatures will be considerably less than the maximum allowable of 250 degrees C, and total recession will be a small fraction of the as-designed thickness. C1 [Covington, M. A.; Heinemann, J. M.] Eloret Corp, Sunnyvale, CA 94086 USA. [Goldstein, H. E.] Adv Comp Sci Res Inst, Moffett Field, CA 94035 USA. [Chen, Y. -K.; Terrazas-Salinas, I.; Balboni, J. A.; Olejniczak, J.; Martinez, E. R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Covington, MA (reprint author), Eloret Corp, 465 S Mathilda Ave,Suite 103, Sunnyvale, CA 94086 USA. NR 15 TC 10 Z9 10 U1 1 U2 9 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD JUL-AUG PY 2008 VL 45 IS 4 BP 854 EP 864 DI 10.2514/1.38249 PG 11 WC Engineering, Aerospace SC Engineering GA 336UH UT WOS:000258389600022 ER PT J AU Parker, JS Born, GH AF Parker, Jeffrey S. Born, George H. TI Trajectory Options for DUNE, a Near-Earth Dust Telescope SO JOURNAL OF THE ASTRONAUTICAL SCIENCES LA English DT Article; Proceedings Paper CT Symposium Honoring Byron Tapley's 50 Years of Contributions CY FEB 01, 2008 CL Austin, TX ID 3-DIMENSIONAL PERIODIC-ORBITS; RESTRICTED 3-BODY PROBLEM; BOUNDARY EXPLORER IBEX AB This paper compares five mission design scenarios for the proposed Dust Near Earth (DUNE) spacecraft. DUNE's science requires it to carry a dust telescope outside of the Earth's magnetosphere, yet its communication requirements restrict it to orbits within the orbit of the Moon. The scenarios considered in this paper include trajectories that place DUNE into highly eccentric Earth orbits, lunar orbits, and lunar halo orbits. This paper concludes that the most successful mission design option for DUNE implements a lunar gravity assist to place the spacecraft in a very high Earth orbit with a raised inclination. C1 [Parker, Jeffrey S.; Born, George H.] Univ Colorado, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA. RP Parker, JS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 26 TC 0 Z9 0 U1 0 U2 3 PU AMER ASTRONAUTICAL SOC PI SPRINGFIELD PA 6352 ROLLING MILL PLACE SUITE 102, SPRINGFIELD, VA 22152 USA SN 0021-9142 J9 J ASTRONAUT SCI JI J. Astronaut. Sci. PD JUL-SEP PY 2008 VL 56 IS 3 SI SI BP 287 EP 309 PG 23 WC Engineering, Aerospace SC Engineering GA 502PA UT WOS:000270471200003 ER PT J AU Canuto, VM Cheng, Y Howard, AM Esau, IN AF Canuto, V. M. Cheng, Y. Howard, A. M. Esau, I. N. TI Stably stratified flows: A model with no Ri(cr) SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID TURBULENCE CLOSURE-MODEL; BOUNDARY-LAYER; DYNAMICAL MODEL; 3RD-ORDER MOMENTS; RICHARDSON-NUMBER; PBL MODEL; SURFACE; CONVECTION; OCEAN; HEAT AB A large set of laboratory, direct numerical simulation (DNS), and large eddy simulation (LES) data indicates that in stably stratified flows turbulent mixing exists up to Ri similar to O(100), meaning that there is practically no Ri(cr). On the other hand, traditional local second-order closure (SOC) models entail a critical Ri(cr) similar to O(1) above which turbulence ceases to exist and are therefore unable to explain the above data. The authors suggest how to modify the recent SOC model of Cheng et al. to reproduce the above data for arbitrary Ri. C1 [Canuto, V. M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Canuto, V. M.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. [Cheng, Y.] Columbia Univ, Ctr Climate Syst Res, New York, NY USA. [Howard, A. M.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA. [Esau, I. N.] Bjerknes Ctr Climate Res, Nansen Environm & Remote Sensing Ctr, Bergen, Norway. RP Canuto, VM (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM vcanuto@giss.nasa.gov RI Esau, Igor/C-6298-2008 OI Esau, Igor/0000-0003-4122-6340 NR 43 TC 49 Z9 49 U1 0 U2 11 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 JUL PY 2008 VL 65 IS 7 BP 2437 EP 2447 DI 10.1175/2007JAS2470.1 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 328KB UT WOS:000257796200024 ER PT J AU Heidmann, JD Ekkad, S AF Heidmann, James D. Ekkad, Srinath TI A novel antivortex turbine film-cooling hole concept SO JOURNAL OF TURBOMACHINERY-TRANSACTIONS OF THE ASME LA English DT Article; Proceedings Paper CT 52nd ASME Turbo Expo 2007 CY MAY 14-17, 2007 CL Montreal, CANADA SP Amer Soc Mech Engineers, Int Gas Turbine Inst ID JET; MODEL AB A novel turbine film-cooling hole shape has been conceived and designed at NASA Glenn Research Center. This "antivortex" design is unique in that it requires only easily machinable round holes, unlike shaped film-cooling holes and other advanced concepts. The hole design is intended to counteract the detrimental vorticity associated with standard circular cross-section film-cooling holes. This vorticity typically entrains hot freestream gas and is associated with jet separation from the turbine blade surface. The antivortex film-cooling hole concept has been modeled computationally for a single row of 30 deg angled holes on a flat surface using the 3D Navier-Stokes solver GLENN-HT. A blowing ratio of 1.0 and density ratios of 1.05 and 2.0 are studied. Both film effectiveness and heat transfer coefficient values are computed and compared to standard round hole cases for the same blowing rates. A net heat flux reduction is also determined using both the film effectiveness and heat transfer coefficient values to ascertain the overall effectiveness of the concept. An improvement in film effectiveness of about 0.2 and in net heat flux reduction of about 0.2 is demonstrated for the antivortex concept compared to the standard round hole for both blowing ratios. Detailed flow visualization shows that as expected, the design counteracts the detrimental vorticity of the round hole flow, allowing it to remain attached to the surface. C1 [Heidmann, James D.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Ekkad, Srinath] Louisiana State Univ, Baton Rouge, LA 70803 USA. RP Heidmann, JD (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RI Ekkad, Srinath/E-9112-2014 NR 28 TC 35 Z9 35 U1 0 U2 8 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA SN 0889-504X J9 J TURBOMACH JI J. Turbomach.-Trans. ASME PD JUL PY 2008 VL 130 IS 3 AR 031020 DI 10.1115/1.2777194 PG 9 WC Engineering, Mechanical SC Engineering GA 301FG UT WOS:000255881200020 ER PT J AU Janesick, J Elliott, T Tower, J AF Janesick, James Elliott, Tom Tower, John TI Scientific monolithic CMOS imagers come of age SO LASER FOCUS WORLD LA English DT Article AB Complementary metal-oxide semiconductor image-sensor technology has displaced charge-coupled-device technology in many commercial applications and is now moving to capture high-performance custom markets. C1 [Janesick, James] Adv Sensors Grp Sarnoff, Huntington Beach, CA 92649 USA. [Elliott, Tom] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Tower, John] David Sarnoff Res Ctr, Princeton, NJ 08543 USA. RP Janesick, J (reprint author), Adv Sensors Grp Sarnoff, 4952 Warner Ave,Suite 300, Huntington Beach, CA 92649 USA. EM cmosccd@aol.com; jtower@sarnoff.com NR 0 TC 0 Z9 0 U1 0 U2 0 PU PENNWELL PUBL CO PI NASHUA PA 98 SPIT BROOK RD, NASHUA, NH 03062-2801 USA SN 1043-8092 J9 LASER FOCUS WORLD JI Laser Focus World PD JUL PY 2008 VL 44 IS 7 BP 68 EP 71 PG 4 WC Optics SC Optics GA 327LR UT WOS:000257731100021 ER PT J AU Weeks, SJ Anthony, KRN Bakun, A Feldman, GC Hoegh-Guldberg, O AF Weeks, S. J. Anthony, K. R. N. Bakun, A. Feldman, G. C. Hoegh-Guldberg, O. TI Improved predictions of coral bleaching using seasonal baselines and higher spatial resolution SO LIMNOLOGY AND OCEANOGRAPHY LA English DT Article ID GREAT-BARRIER-REEF; CLIMATE-CHANGE; TEMPERATURE; PATTERNS; LIMITS AB Coral bleaching spread across the southern Great Barrier Reef in January 2006, after sea temperatures reached climatological summer maxima 2 months before normal. Current satellite-derived warning systems were unable to detect severe bleaching conditions in the region because of their use of a constant thermal threshold (summer maximum monthly mean) and low spatial resolution (50 km). Here it is shown that such problems can be ameliorated if the thermal threshold is adjusted for seasonal variation and a 4-km spatial resolution is used. We develop a seasonally and spatially improved thermal threshold for coral bleaching on the basis of a weekly climatology of sea surface temperatures extending from austral spring to late summer, and apply the method to two case-study sites. At both sites, and in particular at the nearshore site that was undetected by the 50-km satellite product, the seasonally adjusted thermal threshold produced a greatly improved consistency between accumulated heating and bleaching severity. The application of thermal stress algorithms that reflect the long-term mean pattern in seasonal variation allows coral bleaching to be forecast with higher precision. C1 [Weeks, S. J.; Anthony, K. R. N.; Hoegh-Guldberg, O.] Univ Queensland, Ctr Marine Studies, St Lucia, Qld 4072, Australia. [Weeks, S. J.] Univ Queensland, Ctr Remote Sensing & Spatial Informat Sci, St Lucia, Qld 4072, Australia. [Bakun, A.] Univ Miami, Pew Inst Ocean Sci, Miami, FL 33149 USA. [Feldman, G. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Weeks, SJ (reprint author), Univ Queensland, Ctr Marine Studies, St Lucia, Qld 4072, Australia. EM s.weeks@uq.edu.au RI Anthony, Kenneth/G-4299-2011; Hoegh-Guldberg, Ove/H-6169-2011; Weeks, Scarla/E-8632-2013; OI Hoegh-Guldberg, Ove/0000-0001-7510-6713; Weeks, Scarla/0000-0002-0579-7069; Bakun, Andrew/0000-0002-4366-3846 NR 15 TC 24 Z9 24 U1 2 U2 11 PU AMER SOC LIMNOLOGY OCEANOGRAPHY PI WACO PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710-4446 USA SN 0024-3590 J9 LIMNOL OCEANOGR JI Limnol. Oceanogr. PD JUL PY 2008 VL 53 IS 4 BP 1369 EP 1375 DI 10.4319/lo.2008.53.4.1369 PG 7 WC Limnology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 328BY UT WOS:000257773700015 ER PT J AU Sanchez, BV AF Sanchez, Braulio Valentin TI Normal modes of the global oceans - A review SO MARINE GEODESY LA English DT Article DE oceans; normal modes; tides; velocity potential; stream function ID PROUDMAN-FUNCTION EXPANSION; MOON TIDAL EVOLUTION; LONG-PERIOD TIDES; WORLD OCEAN; BAROMETRIC-PRESSURE; HEMISPHERICAL OCEAN; CYCLIC VARIATIONS; STOCHASTIC-MODEL; INDIAN OCEANS; EARTH AB This paper deals with the normal modes of the global oceans. More specifically, it reviews some of the work done in association with the modeling, detection, and application of the barotropic, basin-wide normal modes. The paper presents some results obtained by means of the Proudman-Rao method. The fields of tidal synthesis from a set of normal modes, and paleotides, in the context of normal modes and the evolution of the Earth-Moon system, are surveyed as well. Works associated with the detection of normal modes are discussed also. The paper closes with an analysis of possible future developments. C1 NASA, Goddard Space Flight Ctr, Planetary Geodynam Branch, Greenbelt, MD 20771 USA. RP Sanchez, BV (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Branch, Code 698, Greenbelt, MD 20771 USA. EM Braulio.V.Sanchez@nasa.gov RI Sanchez, Braulio/I-5952-2013 NR 61 TC 2 Z9 2 U1 1 U2 4 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 0149-0419 J9 MAR GEOD JI Mar. Geod. PD JUL-SEP PY 2008 VL 31 IS 3 BP 181 EP 212 DI 10.1080/01490410802265609 PG 32 WC Geochemistry & Geophysics; Oceanography; Remote Sensing SC Geochemistry & Geophysics; Oceanography; Remote Sensing GA 347MC UT WOS:000259144700004 ER PT J AU Sen, SK Agarwal, RP Shaykhian, GA AF Sen, S. K. Agarwal, Ravi P. Shaykhian, Gholam Ali TI Golden ratio versus pi as random sequence sources for Monte Carlo integration SO MATHEMATICAL AND COMPUTER MODELLING LA English DT Article ID TRAVELING-SALESMAN PROBLEM; DISCREPANCY; ALGORITHM AB The algebraic irrational number golden ratio phi = (1+root 5)/2 = one of the two roots of the algebraic equation x(2)-x-1 = 0 and the transcendental number pi = 2sin(-1)(1) = the ratio of the circumference and the diameter of any circle both have infinite number of digits with no apparent pattern. We discuss here the relative merits of these numbers as possible random sequence sources. The quality of these sequences is not judged directly based on the outcome of all known tests for the randomness of a sequence. Instead, it is determined implicitly by the accuracy of the Monte Carlo integration in a statistical sense. Since our main motive of using a random sequence is to solve real-world problems, it is more desirable if we compare the quality of the sequences based on their performances for these problems in terms of quality/accuracy of the output. We also compare these sources against those generated by a popular pseudo-random generator, viz., the Matlab rand and the quasi-random generator halton both in terms of error and time complexity. Our study demonstrates that consecutive blocks of digits of each of these numbers produce a good random sequence source. It is observed that randomly chosen blocks of digits do not have any remarkable advantage over consecutive blocks for the accuracy of the Monte Carlo integration. Also, it reveals that pi is a better source of a random sequence than phi when the accuracy of the integration is concerned. (C) 2007 Elsevier Ltd. All rights reserved. C1 [Sen, S. K.; Agarwal, Ravi P.] Florida Inst Technol, Dept Math Sci, Melbourne, FL 32901 USA. [Shaykhian, Gholam Ali] NASA, Engn Directorate, Kennedy Space Ctr, FL 32899 USA. RP Sen, SK (reprint author), Florida Inst Technol, Dept Math Sci, 150 W Univ Blvd, Melbourne, FL 32901 USA. EM sksen@fit.edu; agarwal@fit.edu; ali.shaykhian@nasa.gov NR 39 TC 4 Z9 4 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0895-7177 EI 1872-9479 J9 MATH COMPUT MODEL JI Math. Comput. Model. PD JUL PY 2008 VL 48 IS 1-2 BP 161 EP 178 DI 10.1016/j.mcm.2007.09.011 PG 18 WC Computer Science, Interdisciplinary Applications; Computer Science, Software Engineering; Mathematics, Applied SC Computer Science; Mathematics GA 302FJ UT WOS:000255953900014 ER PT J AU Bogard, DD Park, J AF Bogard, Donald D. Park, Jisun TI Ar-39-Ar-40 dating of the Zagami Martian shergottite and implications for magma origin of excess Ar-40 SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID NOBLE-GASES; ATMOSPHERIC ARGON; EJECTION TIMES; PARENT BODY; METEORITES; HISTORY; KRYPTON; MANTLE; XENON; NEON AB The Zagami shergottite experienced a complex, petrogenetic formation history (McCoy et al. 1992, 1999). Like several shergottites, Zagami contains excess Ar-40 relative to its formation age. To understand the origin of this excess Ar-40, we made Ar-39-Ar-40 analyses on plagioclase and pyroxene minerals from two phases representing different stages in the magma evolution. Surprisingly, all these separates show similar concentrations of excess Ar-40, similar to 1 x 10(-6) cm(3)/g. We present arguments against this excess Ar-40 having been introduced from the Martian atmosphere as impact glass. We also present evidence against excess Ar-40 being a partially degassed residue from a basalt that actually formed similar to 4 Gyr ago. We utilize our experimental data on Ar diffusion in Zagami and evidence that it was shock-heated to only similar to 70 degrees C, and we assume this heating occurred during an ejection from Mars similar to 3 Myr ago. With these constraints, thermal considerations necessitates either that its ejected mass was impossibly large, or that its shock-heating temperature was an order of magnitude higher than that measured. We suggest that this excess Ar-40 was inherited from the Zagami magma, and that it was introduced into the magma either by degassing of a larger volume of material or by early assimilation of old, K-rich crustal material. Similar concentrations of excess Ar-40 in the analyzed separates imply that this magma maintained a relatively constant Ar-40 concentration throughout its crystallization. This likely occurred through volatile degassing as the magma rose toward the surface and lithostatic pressure was released. These concepts have implications for excess Ar-40 in other shergottites. C1 [Bogard, Donald D.; Park, Jisun] NASA, Lyndon B Johnson Space Ctr, Code KR, ARES, Houston, TX 77058 USA. RP Bogard, DD (reprint author), NASA, Lyndon B Johnson Space Ctr, Code KR, ARES, Houston, TX 77058 USA. EM donald.d.bogard@nasa.gov FU NASA Cosmochemistry Program; NASA Postdoctoral Program FX We thank L. Nyquist and C.-Y. Shih for the Zagami mineral separates. This work was supported by the NASA Cosmochemistry Program and by a fellowship from the NASA Postdoctoral Program to J. P. We appreciate constructive comments on the paper by L. Nyquist, E. Walton, and S. Kelley. NR 59 TC 23 Z9 23 U1 0 U2 4 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 BP 1113 EP 1126 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 374ZV UT WOS:000261083100002 ER PT J AU Abell, PA Weissman, PR Hicks, MD Choi, YJ Lowry, SC AF Abell, P. A. Weissman, P. R. Hicks, M. D. Choi, Y. J. Lowry, S. C. TI Rosetta flyby target asteroid (2867) Steins: An enstatite achondrite analogue SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr ID NEAR-EARTH ASTEROIDS C1 [Abell, P. A.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Abell, P. A.] NASA Johnson Space Ctr, Houston, TX 77058 USA. [Weissman, P. R.; Hicks, M. D.; Choi, Y. J.; Lowry, S. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM abell@psi.edu NR 12 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A15 EP A15 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100007 ER PT J AU Ashley, JW Ruff, SW Christensen, PR Leshin, LA AF Ashley, J. W. Ruff, S. W. Christensen, P. R. Leshin, L. A. TI Effects of dust on thermal infrared reflectivity of iron meteorite candidates found by the mars exploration rovers SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr C1 [Ashley, J. W.; Ruff, S. W.; Christensen, P. R.] Arizona State Univ, Mars Space Flight Facil, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Ashley, J. W.] Minor Planet Res, Fountain Hills, AZ 85268 USA. [Leshin, L. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM james.ashley@asu.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 JUL PY 2008 VL 43 IS 7 SU S BP A20 EP A20 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100017 ER PT J AU Berger, EL Keller, LP Joswiak, D Matrajt, G Lauretta, DS AF Berger, E. L. Keller, L. P. Joswiak, D. Matrajt, G. Lauretta, D. S. TI Low-temperature sulfides in stardust: Tem analysis of a sphalerite/pyrrhotite assemblage from track 7 SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr C1 [Berger, E. L.; Lauretta, D. S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Keller, L. P.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Joswiak, D.; Matrajt, G.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. EM elberger@lpl.arizona.edu NR 4 TC 1 Z9 1 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A24 EP A24 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100026 ER PT J AU Chabot, NL Saslow, SA McDonough, WF Jones, JH AF Chabot, N. L. Saslow, S. A. McDonough, W. F. Jones, J. H. TI A study of Cu and Cr during iron meteorite crystallization SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr ID FRACTIONATION C1 [Chabot, N. L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Saslow, S. A.; McDonough, W. F.] Univ Maryland, College Pk, MD 20742 USA. [Jones, J. H.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM Nancy.Chabot@JHUAPL.edu RI Chabot, Nancy/F-5384-2015 OI Chabot, Nancy/0000-0001-8628-3176 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 JUL PY 2008 VL 43 IS 7 SU S BP A31 EP A31 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100039 ER PT J AU Clemett, SJ Nakamura-Messenger, K Mckay, DS AF Clemett, S. J. Nakamura-Messenger, K. Mckay, D. S. TI Molecular distribution of organic matter and mineral relationships in meteorites and interplanetary dust SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr C1 [Clemett, S. J.] NASA, ERC Inc, JSC, Houston, TX USA. [Nakamura-Messenger, K.] NASA, Jacobs Technol, JSC, Houston, TX USA. EM simonj.clemett@jsc.nasa.gov NR 4 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A33 EP A33 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100044 ER PT J AU Dauphas, N Morris, RV AF Dauphas, N. Morris, R. V. TI Iron isotopes in products of acid-sulfate basalt alteration: A prospective study for mars SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr ID MERIDIANI-PLANUM; BURNS FORMATION; HEMATITE; CONCRETIONS C1 [Dauphas, N.] Univ Chicago, Dept Geophys Sci, Origins Lab, Chicago, IL 60637 USA. [Dauphas, N.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Morris, R. V.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM dauphas@uchicago.edu RI Dauphas, Nicolas/E-4568-2011 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 JUL PY 2008 VL 43 IS 7 SU S BP A35 EP A35 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100047 ER PT J AU Fletcher, LA Bastien, R Allen, CC AF Fletcher, L. A. Bastien, R. Allen, C. C. TI A testbed for advanced cold curation of astromaterials SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr C1 [Fletcher, L. A.; Allen, C. C.] NASA, Lyndon B Johnson Space Ctr, Mail Code KT, ARES, Houston, TX 77058 USA. [Bastien, R.] Jacobs Technol, Houston, TX 77058 USA. EM lisa.a.fietcher@nasa.gov NR 1 TC 1 Z9 1 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A43 EP A43 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100064 ER PT J AU Heber, VS Baur, H Wieler, R Wiens, RC Burnett, DS AF Heber, V. S. Baur, H. Wieler, R. Wiens, R. C. Burnett, D. S. TI Argon, krypton, and xenon abundances in the solar wind measured in silicon from the genesis mission SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr C1 [Heber, V. S.; Baur, H.; Wieler, R.] ETH, IGMR, NW C, CH-8092 Zurich, Switzerland. [Wiens, R. C.] LANL, Los Alamos, NM 87544 USA. [Burnett, D. S.] CALTECH, JPL, Pasadena, CA 91109 USA. RI Wieler, Rainer/A-1355-2010; Pellin, Michael/B-5897-2008 OI Wieler, Rainer/0000-0001-5666-7494; Pellin, Michael/0000-0002-8149-9768 NR 6 TC 0 Z9 0 U1 0 U2 2 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A53 EP A53 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100084 ER PT J AU Hermalyn, B Schultz, PH Anderson, JLB Heineck, JT AF Hermalyn, B. Schultz, P. H. Anderson, J. L. B. Heineck, J. T. TI Evolution of impact ejection angles: Implications for early stage coupling SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr ID OBLIQUE IMPACTS; FLOW C1 [Hermalyn, B.; Schultz, P. H.] Brown Univ, Providence, RI 02912 USA. [Anderson, J. L. B.] Winona State Univ, Winona, MN 55987 USA. [Heineck, J. T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Brendan_Hermalyn@brown.edu 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 JUL PY 2008 VL 43 IS 7 SU S BP A54 EP A54 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100086 ER PT J AU Herrin, JS Mittlefehidt, DM Jones, JH AF Herrin, J. S. Mittlefehidt, D. M. Jones, J. H. TI Petrogenesis of Fe,Si-metals in brecciated ureilites SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr C1 [Herrin, J. S.; Mittlefehidt, D. M.; Jones, J. H.] NASA, Lyndon B Johnson Space Ctr, Houson, TX USA. EM jason.s.herrin@nasa.gov NR 12 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A55 EP A55 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100087 ER PT J AU Ito, M Messenger, S AF Ito, M. Messenger, S. TI O isotope mapping of a wark-lovering rim in a type A CAI: Constraints on its formation process SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr ID SOLAR-SYSTEM C1 [Ito, M.; Messenger, S.] NASA, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA. EM motoo.ito-l@nasa.gov; scott.r.messenger@nasa.gov NR 11 TC 1 Z9 1 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A65 EP A65 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100108 ER PT J AU Jogo, K Nakamura, T Messenger, SR Ito, M Miyamoto, T AF Jogo, K. Nakamura, T. Messenger, S. R. Ito, M. Miyamoto, T. TI Mn-Cr systematics of secondary fayalite in the Y-86009CV3 carbonaceous chondrite SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr ID CV3 CHONDRITE C1 [Jogo, K.; Nakamura, T.; Miyamoto, T.] Kyushu Univ, Dept Earth & Planetary Sci, Fukuoka 812, Japan. [Messenger, S. R.; Ito, M.] NASA, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA. EM kaori@geo.kyushu-u.ac.jp NR 5 TC 1 Z9 1 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A66 EP A66 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100110 ER PT J AU Jones, JH AF Jones, J. H. TI Parameterization of pyroxene/liquid REE partition coefficients SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr C1 [Jones, J. H.] NASA, Lyndon B Johnson Space Ctr, KR, Houston, TX 77058 USA. EM john.hjones@nasa.gov 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 JUL PY 2008 VL 43 IS 7 SU S BP A67 EP A67 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100112 ER PT J AU Karner, JM Papike, JJ Mckay, G Sutton, SR Shearer, CK Burger, P Le, L AF Karner, J. M. Papike, J. J. Mckay, G. Sutton, S. R. Shearer, C. K. Burger, P. Le, L. TI The partitioning of Cr and V between pyroxenemelt in martian basalt que 94201 SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr ID MELT C1 [Karner, J. M.; Papike, J. J.; Shearer, C. K.; Burger, P.] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA. [Mckay, G.] NASA, Lyndon B Johnson Space Ctr, Mail Code ST, Houston, TX 77058 USA. [Sutton, S. R.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. [Le, L.] ESC Grp, Houston, TX 77058 USA. EM jkamer@unm.edu NR 3 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A70 EP A70 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100117 ER PT J AU Kebukawa, Y Nakashima, S Zolensky, ME AF Kebukawa, Y. Nakashima, S. Zolensky, M. E. TI Thermal stabilities of organic matter in carbonaceous chondrites using in situ heating micro FTIR analyses SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr C1 [Kebukawa, Y.; Nakashima, S.] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan. [Zolensky, M. E.] NASA, Lyndon B Johnson Space Ctr, KT, Houston, TX 77058 USA. EM yoko.soleil@ess.sci.osaka-u.ac.jp NR 5 TC 0 Z9 0 U1 0 U2 3 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A73 EP A73 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100123 ER PT J AU Keller, LP Messenger, S AF Keller, L. P. Messenger, S. TI Relict amorphous silicates in stardust samples SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr C1 [Keller, L. P.; Messenger, S.] NASA, Lyndon B Johnson Space Ctr, ARES, Robert M Walker Lab Space Sci, Houston, TX 77058 USA. EM Lindsay.P.Keller@nasa.gov NR 5 TC 1 Z9 1 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A74 EP A74 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100125 ER PT J AU Keller, LP Flynn, GJ AF Keller, L. P. Flynn, G. J. TI Mid- and far-infrared spectra of anhydrous interplanetary dust particles SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr C1 [Keller, L. P.] NASA, Lyndon B Johnson Space Ctr, Code KR, Houston, TX 77058 USA. [Flynn, G. J.] SUNY Coll Plattsburgh, Dept Phys, Plattsburgh, NY 12901 USA. EM Lindsay.P.Keller@nasa.gov NR 4 TC 0 Z9 0 U1 1 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A73 EP A73 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100124 ER PT J AU Kelley, MS Reddy, V Gaffey, MJ AF Kelley, M. S. Reddy, V. Gaffey, M. J. TI Analyses of near-IR spectra for three asteroids in the Hungaria region SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr ID SPECTROSCOPIC SURVEY C1 [Kelley, M. S.] NASA Headquarters, Planetary Sci Div, Houston, TX USA. [Reddy, V.] Univ N Dakota, Dept Earth Syst Sci & Policy, Grand Forks, ND 58201 USA. [Gaffey, M. J.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58201 USA. EM Michael.S.Kelley@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 JUL PY 2008 VL 43 IS 7 SU S BP A74 EP A74 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100126 ER PT J AU Kita, NT Ushikubo, T Kimura, M Nyquist, LE Valley, JW AF Kita, N. T. Ushikubo, T. Kimura, M. Nyquist, L. E. Valley, J. W. TI Heterogeneous oxygen isotope ratios of olivine in chondrules from Y-793408 (H3.2) chondrite SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr C1 [Kita, N. T.; Ushikubo, T.; Valley, J. W.] Univ Wisconsin, Madison, WI 53706 USA. [Kimura, M.] Ibaraki Univ, Mito, Ibaraki, Japan. [Nyquist, L. E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX USA. EM noriko@geology.wisc.edu RI Valley, John/B-3466-2011 OI Valley, John/0000-0003-3530-2722 NR 7 TC 2 Z9 2 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A77 EP A77 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100131 ER PT J AU Koizumi, E Mikouchi, T Mckay, G Miyamoto, M AF Koizumi, E. Mikouchi, T. McKay, G. Miyamoto, M. TI Crystallization relationship of Yamato-980459 and Que 94201 depleted shergottites SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr C1 [Koizumi, E.] Remote Sensing Technol Ctr Japan, Tokyo 1060032, Japan. [Koizumi, E.; Mikouchi, T.; Miyamoto, M.] Univ Tokyo, Dept Earth & Planet Sci, Tokyo 1130033, Japan. [McKay, G.] NASA, Lyndon B Johnson Space Ctr, Mail Code KR, Houston, TX 77058 USA. EM koizumi_eisuke@restec.or.jp NR 4 TC 1 Z9 1 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A79 EP A79 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100135 ER PT J AU Martins, Z Alexander, CMOD Orzechowska, GE Elsila, JE Glavin, DP Dworkin, JP Sephton, MA Ehrenfreund, P AF Martins, Z. Alexander, C. M. O'D. Orzechowska, G. E. Elsila, J. E. Glavin, D. P. Dworkin, J. P. Sephton, M. A. Ehrenfreund, P. TI Amino acid composition of primitive CR2 chondrites SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr ID METEORITES C1 [Martins, Z.; Sephton, M. A.] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London, England. [Alexander, C. M. O'D.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. [Orzechowska, G. E.] CALTECH, JPL, Pasadena, CA 91125 USA. [Elsila, J. E.; Glavin, D. P.; Dworkin, J. P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ehrenfreund, P.] George Washington Univ, Elliott Sch Int Affairs, Inst Space Policy, Washington, DC 20052 USA. EM z.martins@imperial.ac.uk RI Elsila, Jamie/C-9952-2012; Glavin, Daniel/D-6194-2012; Martins, Zita/H-4860-2015; Dworkin, Jason/C-9417-2012 OI Glavin, Daniel/0000-0001-7779-7765; Martins, Zita/0000-0002-5420-1081; Dworkin, Jason/0000-0002-3961-8997 NR 4 TC 4 Z9 4 U1 0 U2 3 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A90 EP A90 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100157 ER PT J AU Marty, B Zimmermann, L Burnard, PG Burnett, DL Allton, JH Wiens, RC Heber, VS Wieler, R Bochsler, P Sestak, S Franchi, IA AF Marty, B. Zimmermann, L. Burnard, P. G. Burnett, D. L. Allton, J. H. Wiens, R. C. Heber, V. S. Wieler, R. Bochsler, P. Sestak, S. Franchi, I. A. TI Nitrogen isotopes in the recent solar wind: Further analysis of gold-plated concentrator frame from genesis SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr C1 [Marty, B.; Zimmermann, L.; Burnard, P. G.] Nancy Univ, CNRS, CRPG, Nancy, France. [Burnett, D. L.] CALTECH, Dept Geol Sci, Pasadena, CA 91125 USA. [Allton, J. H.] 2101 NASA Pkwy, Johnson Space Ctr, Houston, TX 77058 USA. [Wiens, R. C.] Los Alamos Natl Lab Space & Atmospher Sci, Los Alamos, NM 87544 USA. [Heber, V. S.; Wieler, R.] Swiss Fed Inst Technol, Isotope Geol & Mineral Resources, Zurich, Switzerland. Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England. EM bmarty@crpg.cnrs-nancy.fr RI Wieler, Rainer/A-1355-2010 OI Wieler, Rainer/0000-0001-5666-7494 NR 4 TC 0 Z9 0 U1 0 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A90 EP A90 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100158 ER PT J AU Mckay, DS Wentworth, SJ Thomas-Keprta, KL Clemett, SJ AF McKay, D. S. Wentworth, S. J. Thomas-Keprta, K. L. Clemett, S. J. TI Complex nanostratigraphy of volcanic surface coatings on apollo 15 green pyroclastic glass beads SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr C1 [McKay, D. S.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Wentworth, S. J.; Thomas-Keprta, K. L.; Clemett, S. J.] NASA, JSC, Mail Code JE23, ESC Grp, Houston, TX 77058 USA. EM David.S.McKay@nasa.gov NR 3 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A95 EP A95 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100167 ER PT J AU Messenger, S Ito, M Joswiak, DJ Keller, LP Stroud, RM Nakamura-Messenger, K Matrajt, G Brownlee, DE AF Messenger, S. Ito, M. Joswiak, D. J. Keller, L. P. Stroud, R. M. Nakamura-Messenger, K. Matrajt, G. Brownlee, D. E. TI Oxygen isotopic compositions of wild 2 silicates SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr C1 [Messenger, S.; Ito, M.; Keller, L. P.; Nakamura-Messenger, K.] NASA, JSC, ARES, Robert M Walker Lab Space Sci, Houston, TX USA. [Joswiak, D. J.; Matrajt, G.; Brownlee, D. E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Stroud, R. M.] USN, Res Lab, Div Mat Sci & Technol, Washington, DC 20375 USA. [Nakamura-Messenger, K.] NASA, JSC, ESCG, Houston, TX USA. EM scott.r.messenger@nasa.gov RI Stroud, Rhonda/C-5503-2008 OI Stroud, Rhonda/0000-0001-5242-8015 NR 6 TC 3 Z9 3 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A97 EP A97 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100171 ER PT J AU Mikouchi, T Mckay, G Jones, J AF Mikouchi, T. McKay, G. Jones, J. TI Petrogenesis and crystallization history of quenched angrites SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr ID PETROLOGY; ORIGIN C1 [Mikouchi, T.] Univ Tokyo, Dept Earth & Planetary Sci, Tokyo 1130033, Japan. [McKay, G.; Jones, J.] NASA, Lyndon B Johnson Space Ctr, Mail Code KR, Houston, TX 77058 USA. EM mikouchi@eps.s.u-tokyo.ac.jp NR 7 TC 2 Z9 2 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A98 EP A98 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100174 ER PT J AU Misawa, K Park, J Shih, CY Reese, Y Bogard, DD Nyquist, LE AF Misawa, K. Park, J. Shih, C. -Y. Reese, Y. Bogard, D. D. Nyquist, L. E. TI Martian metasomatic and/or alteration components preserved in maskelynitized plagioclase in shergottites? SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr ID PETROGENESIS; CONSTRAINTS C1 [Misawa, K.] Natl Inst Polar Res, Antarctic Meteorite Res Ctr, Tokyo 1738515, Japan. [Park, J.; Bogard, D. D.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Shih, C. -Y.] ESCG Jacobs Sverdrup, Houston, TX 77058 USA. [Reese, Y.] ESCG Muniz Engn, Houston, TX 77058 USA. EM misawa@nipr.ac.jp NR 7 TC 1 Z9 1 U1 0 U2 1 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A99 EP A99 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100175 ER PT J AU Mittlefehldt, DW AF Mittlefehldt, D. W. TI Petrology and geochemistry of antarctic eucrites and diogenites, and A-881394 SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr C1 [Mittlefehldt, D. W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM david.w.mittlefehldt@nasa.gov 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 JUL PY 2008 VL 43 IS 7 SU S BP A187 EP A187 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100350 ER PT J AU Mittlefehldt, DW Herrin, JS AF Mittlefehldt, David W. Herrin, Jason S. TI Petrology and geochemistry of martian meteorites LAR 06319, RBT 04261, and RBT 04262 SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr C1 [Mittlefehldt, David W.; Herrin, Jason S.] NASA, Lyndon B Johnson Space Ctr, Washington, DC 20546 USA. EM david.w.mittlefehldt@nasa.gov NR 4 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A100 EP A100 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100177 ER PT J AU Murakami, S Kato, K Fujikawa, N Terada, K Yoneda, S Arai, S Hidaka, H Okada, A Nagao, K Park, J Ebisawa, N Kusakabe, M AF Murakami, S. Kato, K. Fujikawa, N. Terada, K. Yoneda, S. Arai, S. Hidaka, H. Okada, A. Nagao, K. Park, J. Ebisawa, N. Kusakabe, M. TI Comprehensive studies of the Hiroshima H chondrite SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr C1 [Murakami, S.; Kato, K.; Fujikawa, N.] Hiroshima Childrens Museum, Naka Ku, Hiroshima 7300011, Japan. [Terada, K.; Arai, S.; Hidaka, H.] Hiroshima Univ, Dept Earth & Planetary Syst Sci, Higashihiroshima 7398526, Japan. [Yoneda, S.] Univ Tokyo, Nat Museum Nat & Sci, Shinjuku Ku, Tokyo 1690073, Japan. [Okada, A.] RIKEN, Wako, Saitama 3510198, Japan. [Nagao, K.; Ebisawa, N.] Univ Tokyo, Grad Sch Sci, Earthquake Chem Lab, Bunkyo Ku, Tokyo 1130033, Japan. [Park, J.] NASA, Lyndon B Johnson Space Ctr, Code KR, ARES, Houston, TX 77058 USA. [Kusakabe, M.] Korea Polar Res Inst, Inchon, South Korea. EM murakami@pyonta.city.hiroshimajp; terada@sci.hiroshima-u.ae.jp NR 3 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A105 EP A105 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100188 ER PT J AU Nagao, K Park, J AF Nagao, K. Park, J. TI Noble gases and cosmic-ray exposure ages of two martian shergottites, RBT 04262 and LAR 06319, recovered in Antarctica SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr C1 [Nagao, K.] Univ Tokyo, Grad Sch Sci, Earthquake Chem Lab, Bunkyo Ku, Tokyo 1130033, Japan. [Park, J.] NASA, Lyndon B Johnson Space Ctr, Code KR, ARES, Houston, TX 77058 USA. EM nagao@eqchem.s.u-tokyo.ac.jp NR 9 TC 7 Z9 7 U1 0 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A107 EP A107 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100191 ER PT J AU Nakamura-Messenger, K Keller, LP Messenger, S Clemett, SJ Zolensky, ME Palma, RL Pepin, RO Wirick, S AF Nakamura-Messenger, K. Keller, L. P. Messenger, S. Clemett, S. J. Zolensky, M. E. Palma, R. L. Pepin, R. O. Wirick, S. TI Mineralogy of interplanetary dust particles from the comet Grigg-Skjellerup dust stream collections SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr C1 [Nakamura-Messenger, K.; Keller, L. P.; Messenger, S.; Clemett, S. J.; Zolensky, M. E.] NASA, JSC, Washington, DC USA. [Palma, R. L.] Minnesota State Univ, Minneapolis, MN USA. [Palma, R. L.; Pepin, R. O.] Univ Minnesota, Minneapolis, MN 55455 USA. [Wirick, S.] SUNY Stony Brook, Stony Brook, NY USA. EM keiko.nakamura-1@nasa.gov NR 5 TC 2 Z9 2 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A111 EP A111 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100199 ER PT J AU Nuth, JA AF Nuth, Joseph A., III TI Equilibration of the oxygen isotopes in the earth-moon system SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr C1 [Nuth, Joseph A., III] NASA, Goddard Space Flight Ctr, Astrochem Lab, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. EM Joseph.A.Nuth@NASA.gov RI Nuth, Joseph/E-7085-2012 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 JUL PY 2008 VL 43 IS 7 SU S BP A118 EP A118 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100214 ER PT J AU Nyquist, LE Shih, CY Reese, YD Treiman, AH AF Nyquist, L. E. Shih, C. -Y. Reese, Y. D. Treiman, A. H. TI Early partial melting of the Gra 06128/9 Pb from Sm-Nd and Rb-Sr isotopic studies SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr ID COUNTY IAB IRON; PLAGIOCLASE-DIOPSIDE; MINERALOGY C1 [Nyquist, L. E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Shih, C. -Y.] ESCG Jacobs Sverdrup, Houston, TX 77058 USA. [Reese, Y. D.] ESCG Muniz Engn, Houston, TX 77058 USA. [Treiman, A. H.] Lunar & Planetary Inst, Houston, TX 77058 USA. EM laurence.e.nyquist@nasa.gov NR 11 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A119 EP A119 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100215 ER PT J AU Park, J Garrison, DH Bogard, DD AF Park, J. Garrison, D. H. Bogard, D. D. TI Ar-39-Ar-40 ages of the Nakhlites: A synthesis SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr ID AR-40-AR-39 C1 [Park, J.; Garrison, D. H.; Bogard, D. D.] NASA, Lyndon B Johnson Space Ctr, ARES Code KR, Houston, TX 77058 USA. [Park, J.] NASA Postdoctoral Program, Houston, TX USA. NR 13 TC 2 Z9 2 U1 0 U2 1 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A127 EP A127 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100231 ER PT J AU Reddy, V Kelley, MS Emery, JP Gaffey, MJ Bottke, WF Schaal, M Cramer, AP Takir, D AF Reddy, V. Kelley, M. S. Emery, J. P. Gaffey, M. J. Bottke, W. F. Schaal, M. Cramer, A. P. Takir, D. TI Composition of baptistina asteroid family: implications for K-T impactor link SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr ID EXTINCTION C1 [Reddy, V.] Univ N Dakota, Dept ESSP, Grand Forks, ND 58201 USA. [Kelley, M. S.] NASA Headquarters, Washington, DC USA. [Emery, J. P.] Carl Sagan Ctr, Mountain View, CA USA. [Gaffey, M. J.; Takir, D.] UND, Dept Space Studies, Grand Forks, ND USA. [Bottke, W. F.] SWRI, Dept Space Studies, Boulder, CO USA. [Schaal, M.] UND, Dept Phys, Grand Forks, ND USA. [Cramer, A. P.] Georgia So Univ, Dept Geol, Statesboro, GA 30460 USA. NR 6 TC 1 Z9 1 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A130 EP A130 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100237 ER PT J AU Righter, K Meyer, C Allton, J Warren, J Schwarz, C Clemett, S Wentworth, S McNamara, K AF Righter, K. Meyer, C. Allton, J. Warren, J. Schwarz, C. Clemett, S. Wentworth, S. McNamara, K. TI Contamination sources associated with collection and curation of Antarctic meteorites: JSC lessons learned since 1976 SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr C1 [Righter, K.; Meyer, C.; Allton, J.; Warren, J.; Schwarz, C.; Clemett, S.; Wentworth, S.; McNamara, K.] NASA, Lyndon B Johnson Space Ctr, Astromat Curat KT, Houston, TX 77058 USA. EM kevin.righter-1@nasa.gov NR 11 TC 1 Z9 1 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A189 EP A189 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100354 ER PT J AU Righter, K Danielson, LR AF Righter, K. Danielson, L. R. TI Are shergottites sulfide-saturated? SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr ID SILICATE MELTS; SULFUR; MAGMAS; MARS C1 [Righter, K.; Danielson, L. R.] NASA, Lyndon B Johnson Space Ctr, Mailcode KT, Houston, TX 77058 USA. EM kevin.righter-1@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 JUL PY 2008 VL 43 IS 7 SU S BP A131 EP A131 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100240 ER PT J AU Righter, M Lapen, TJ Righter, K Brandon, A AF Righter, M. Lapen, T. J. Righter, K. Brandon, A. TI Partitioning of HF between chromite and silicate melts: Implications for lu-hf isotopic systematics of martian meteorite ALH 84001 SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr ID SPINEL C1 [Righter, M.; Lapen, T. J.] Univ Houston, Dept Geosci, Houston, TX 77204 USA. [Righter, K.; Brandon, A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A132 EP A132 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100241 ER PT J AU Shirai, N Humayun, M Righter, K AF Shirai, N. Humayun, M. Righter, K. TI Moderately siderophile element abundances in angrites SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr ID DORBIGNY C1 [Shirai, N.; Humayun, M.] Florida State Univ, Natl High Magnet Field Lab, Tallahassee, FL 32310 USA. [Shirai, N.; Humayun, M.] Florida State Univ, Dept Geol Sci, Tallahassee, FL 32310 USA. [Righter, K.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM shirai@magnet.fsu.edu NR 8 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A144 EP A144 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100266 ER PT J AU Spencer, LM McKay, DS Gibson, EK Thomas-Keprta, KL Wentworth, SJ Clemett, SJ AF Spencer, L. M. McKay, D. S. Gibson, E. K. Thomas-Keprta, K. L. Wentworth, S. J. Clemett, S. J. TI Observation and analysis of martian meteorite y000593: Evidence of biosignatures SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr C1 [Spencer, L. M.; Thomas-Keprta, K. L.; Wentworth, S. J.; Clemett, S. J.] NASA, Lyndon B Johnson Space Ctr, ESC Grp, Houston, TX 77058 USA. NR 5 TC 1 Z9 1 U1 0 U2 1 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A145 EP A145 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100268 ER PT J AU Thomas-Keprta, KL Clemett, SJ Mckay, DS Gibson, EK Wentworth, SJ AF Thomas-Keprta, K. L. Clemett, S. J. McKay, D. S. Gibson, E. K. Wentworth, S. J. CA FEI Corp TI Reassessment of the "Life on Mars" hypothesis SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr ID MARTIAN METEORITE ALH84001 C1 [Thomas-Keprta, K. L.; Clemett, S. J.; Wentworth, S. J.] ESCG NASA, Houston, TX USA. [McKay, D. S.; Gibson, E. K.] NASA, Lyndon B Johnson Space Ctr, Washington, DC USA. [FEI Corp] FEI Co, Hillsboro, OR USA. 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 JUL PY 2008 VL 43 IS 7 SU S BP A154 EP A154 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100285 ER PT J AU Tsuchiyama, A Iida, Y Kadono, T Nakamura, T Sakamoto, K Nakano, T Uesugi, K Zolensky, ME AF Tsuchiyama, A. Iida, Y. Kadono, T. Nakamura, T. Sakamoto, K. Nakano, T. Uesugi, K. Zolensky, M. E. TI Three-dimensional morphologies and elemental distributions of stardust impact tracks SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr ID COMET 81P/WILD-2 C1 [Tsuchiyama, A.; Iida, Y.] Osaka Univ, Dept Earth & Space Sci, Grad Sch Sci, Toyonaka, Osaka 5600043, Japan. [Kadono, T.] Osaka Univ, Inst Laser Engn, Suita, Osaka 5650871, Japan. [Nakamura, T.; Sakamoto, K.] Kyushu Univ, Dept Earth & Planetary Sci, Fac Sci, Fukuoka 8128581, Japan. [Nakano, T.] Geol Survey Japan, Tsukuba, Ibaraki 3058567, Japan. [Uesugi, K.] Synchrotron Radiat Res Inst, Sayo, Hyogo 6795198, Japan. [Zolensky, M. E.] KT NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM akira@ess.sci.osaka-u.ac.jp NR 4 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A156 EP A156 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100290 ER PT J AU Westphal, AJ Allen, C Bajt, S Bastien, R Bechtel, HA Bleuet, P Borg, J Brenker, F BridgeS, J Brownlee, DE Butterworth, AL Burchell, M Burghammer, M Clark, B Cloetens, P Cody, G Ferroir, T Floss, C Flynn, G Frank, D Gainsforth, Z Gruan, E Hoppe, P Kearsleyll, A Kelley, N Lemelle, L Leroux, H Nittler, LR Lettieri, R Mendez, B Marchant, W Sandford, SA Sec, T Simionovici, A Stadermann, F Sternovsky, Z Stroud, RM Susini, J Sutton, S Tsou, P Tsuchiyama, A Tyliczszak, T Vekemans, B Vincze, L Warre, J Zolensky, ME AF Westphal, A. J. Allen, C. Bajt, S. Bastien, R. Bechtel, H. A. Bleuet, P. Borg, J. Brenker, F. Bridges, J. Brownlee, D. E. Butterworth, A. L. Burchell, M. Burghammer, M. Clark, B. Cloetens, P. Cody, G. Ferroir, T. Floss, C. Flynn, G. Frank, D. Gainsforth, Z. Gruen, E. Hoppe, P. Kearsleyll, A. Kelley, N. Lemelle, L. Leroux, H. Nittler, L. R. Lettieri, R. Mendez, B. Marchant, W. Sandford, S. A. Sec, T. Simionovici, A. Stadermann, F. Sternovsky, Z. Stroud, R. M. Susini, J. Sutton, S. Tsou, P. Tsuchiyama, A. Tyliczszak, T. Vekemans, B. Vincze, L. Warre, J. Zolensky, M. E. TI Stardust interstellar preliminary examination - First results SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr C1 [Westphal, A. J.; Butterworth, A. L.; Frank, D.; Gainsforth, Z.; Kelley, N.; Lettieri, R.; Mendez, B.; Marchant, W.] UC Berkeley, Space Sci Lab, Berkeley, CA USA. [Allen, C.; Warre, J.; Zolensky, M. E.] NASA, Lyndon B Johnson Space Ctr, Washington, DC USA. [Borg, J.] IAS, Orsay, France. [Brenker, F.] Univ Frankfurt, D-6000 Frankfurt, Germany. [Bridges, J.] Univ Leicester, Leicester LE1 7RH, Leics, England. [Brownlee, D. E.] Univ Washington, Seattle, WA 98195 USA. [Floss, C.; Stadermann, F.] Washington Univ, St Louis, MO USA. [Flynn, G.] SUNY Coll Plattsburgh, Plattsburgh, NY USA. [Gruen, E.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. [Kearsleyll, A.] Nat Hist Museum, London, England. [Leroux, H.] Univ Sci & Tech Lille Flandres Artois, F-59655 Villeneuve Dascq, France. [Nittler, L. R.] Carnegie Inst Washington, Washington, DC 20005 USA. [Simionovici, A.] Univ Grenoble, Observ Sci, Grenoble, France. [Tsuchiyama, A.] Osaka Univ, Suita, Osaka 565, Japan. [Burchell, M.] Univ Kent, Canterbury CT2 7NZ, Kent, England. [Bleuet, P.; Burghammer, M.; Susini, J.] ESRF, Grenoble, France. [Sternovsky, Z.] Univ Colorado, Boulder, CO 80309 USA. [Vekemans, B.; Vincze, L.] Univ Ghent, Ghent, Belgium. [Bajt, S.; Ferroir, T.; Lemelle, L.] ENS Lyon, Lyon, France. EM westphal@ssl.berkeley.edu RI Stroud, Rhonda/C-5503-2008; Bajt, Sasa/G-2228-2010; Hoppe, Peter/B-3032-2015 OI Stroud, Rhonda/0000-0001-5242-8015; Hoppe, Peter/0000-0003-3681-050X NR 1 TC 3 Z9 3 U1 0 U2 4 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A169 EP A169 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100315 ER PT J AU Zolensky, ME Gounelle, M Briani, G Bottke, W Young, E Dyl, K Weisberg, MK AF Zolensky, M. E. Gounelle, M. Briani, G. Bottke, W. Young, E. Dyl, K. Weisberg, M. K. TI Pieces of Kuiper belt bodies in meteorites SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT Workshop on Antarctic Meteorites - Search, Recovery, and Classification CY JUL 26-27, 2008 CL Inst Polar Res, Antarctic Meteorite Res Ctr, Matsue, JAPAN SP Natl Inst Polor Res, SOKENDAI, Graduate Univ Adv Studies, Lunar & Planetary Inst, Shimane Prefecture HO Inst Polar Res, Antarctic Meteorite Res Ctr ID SOLAR-SYSTEM; FOSSIL MICROMETEORITES; HOWARDITES; ORIGIN; PLANETS; CAPTURE C1 [Zolensky, M. E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Gounelle, M.; Briani, G.] Museum Natl Hist Nat, F-75231 Paris, France. [Bottke, W.] SW Res Inst, Boulder, CO 80302 USA. [Young, E.; Dyl, K.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Weisberg, M. K.] Kingsborough Community Coll, Brooklyn, NY 11235 USA. EM michael.e.zolensky@nasa.gov NR 14 TC 1 Z9 1 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2008 VL 43 IS 7 SU S BP A177 EP A177 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 326TZ UT WOS:000257683100331 ER PT J AU Britch, SC Linthicum, KJ Anyamba, A Tucker, CJ Pak, EW Maloney, FA Cobb, K Stanwix, E Humphries, J Spring, A Pagac, B Miller, M AF Britch, Seth C. Linthicum, Kenneth J. Anyamba, Assaf Tucker, Compton J. Pak, Edwin W. Maloney, Francis A., Jr. Cobb, Kristin Stanwix, Erin Humphries, Jeri Spring, Alexandra Pagac, Benedict Miller, Melissa TI Satellite vegetation index data as a tool to forecast population dynamics of medically important mosquitoes at military installations in the continental United States SO MILITARY MEDICINE LA English DT Article ID RIFT-VALLEY-FEVER; AEDES-ALBOPICTUS; VECTOR; VIRUS; DISEASES; EPIDEMICS; RAINFALL; AFRICA; KENYA; SAHEL AB The United States faces many existing and emerging mosquito-borne disease threats, such as West Nile virus and Rift Valley fever. An important component of strategic prevention and control plans for these and other mosquito-borne diseases is forecasting the distribution, timing, and abundance of mosquito vector populations. Populations of many medically important mosquito species are closely tied to climate, and historical climate-population associations may be used to predict future population dynamics. Using 2003-2005 U.S. Army Center for Health Promotion and Preventive Medicine mosquito surveillance data, we looked at populations of several known mosquito vectors of West Nile virus, as well as possible mosquito vectors of Rift Valley fever virus, at continental U.S. military installations. We compared population changes with concurrent patterns for a satellite-derived index of climate (normalized difference vegetation index) and observed instances of population changes appearing to be direct responses to climate. These preliminary findings are important first steps in developing an automated, climate-driven, early warning system to flag regions of the United States at elevated risk of mosquito-borne disease transmission. C1 [Britch, Seth C.; Linthicum, Kenneth J.] ARS, USDA, Ctr Med Agr & Vet Entomol, Gainesville, FL USA. [Anyamba, Assaf; Tucker, Compton J.; Pak, Edwin W.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. [Maloney, Francis A., Jr.] USA, Ctr Hlth Promot & Prevent Med W, Fort Lewis, WA 98433 USA. [Cobb, Kristin; Stanwix, Erin; Humphries, Jeri] USA, Ctr Hlth Promot & Prevent Med S, Fort Lewis, WA 98433 USA. [Spring, Alexandra; Pagac, Benedict; Miller, Melissa] USA, Ctr Hlth Promot & Prevent Med N, Fort George G Meade, MD 20755 USA. RP Britch, SC (reprint author), ARS, USDA, Ctr Med Agr & Vet Entomol, Gainesville, FL USA. NR 28 TC 13 Z9 14 U1 0 U2 4 PU ASSOC MILITARY SURG US PI BETHESDA PA 9320 OLD GEORGETOWN RD, BETHESDA, MD 20814 USA SN 0026-4075 J9 MIL MED JI Milit. Med. PD JUL PY 2008 VL 173 IS 7 BP 677 EP 683 PG 7 WC Medicine, General & Internal SC General & Internal Medicine GA 328CH UT WOS:000257774600012 PM 18700603 ER PT J AU Abdalla, FB Amara, A Capak, P Cypriano, ES Lahav, O Rhodes, J AF Abdalla, F. B. Amara, A. Capak, P. Cypriano, E. S. Lahav, O. Rhodes, J. TI Photometric redshifts for weak lensing tomography from space: the role of optical and near infrared photometry SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : statistical; galaxies : distances and redshifts; cosmology : observations ID INTRINSIC GALAXY ALIGNMENTS; PROBING DARK ENERGY; COSMIC SHEAR; POWER SPECTRUM; CONTAMINATION; REQUIREMENTS; OSCILLATIONS; CONSTRAINTS; ULTRAVIOLET; SUPERNOVAE AB We study in detail the photometric redshift requirements needed for tomographic weak gravitational lensing in order to measure accurately the dark energy equation of state. In particular, we examine how ground-based photometry (u, g, r, i, z, y) can be complemented by space-based near-infrared (near-IR) photometry (J, H), e.g. onboard the planned DUNE satellite. Using realistic photometric redshift simulations and an artificial neural network photo-z method we evaluate the figure of merit for the dark energy parameters (w(0), w(a)). We consider a DUNE-like broad optical filter supplemented with ground-based multiband optical data from surveys like the Dark Energy Survey, Pan-STARRS and LSST. We show that the dark energy figure of merit would be improved by a factor of 1.3-1.7 if IR filters are added onboard DUNE. Furthermore we show that with IR data catastrophic photo-z outliers can be removed effectively. There is an interplay between the choice of filters, the magnitude limits and the removal of outliers. We draw attention to the dependence of the results on the galaxy formation scenarios encoded into the mock galaxies, e.g. the galaxy reddening. For example, very deep u-band data could be as effective as the IR. We also find that about 10(5)-10(6) spectroscopic redshifts are needed for calibration of the full survey. C1 [Abdalla, F. B.; Cypriano, E. S.; Lahav, O.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Amara, A.] CEA Saclay, Serv Astrophys, F-91191 Gif sur Yvette, France. [Capak, P.; Rhodes, J.] CALTECH, Pasadena, CA 91125 USA. [Rhodes, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Abdalla, FB (reprint author), UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. EM fba@star.ucl.ac.uk RI Cypriano, Eduardo/C-7293-2012; OI Abdalla, Filipe/0000-0003-2063-4345 NR 38 TC 51 Z9 51 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 JUL 1 PY 2008 VL 387 IS 3 BP 969 EP 986 DI 10.1111/j.1365-2966.2008.13151.x PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 313HW UT WOS:000256732700003 ER PT J AU Halliwell, GR Shay, LK Jacob, SD Smedstad, OM Uhlhorn, EW AF Halliwell, G. R., Jr. Shay, L. K. Jacob, S. D. Smedstad, O. M. Uhlhorn, E. W. TI Improving ocean model initialization for coupled tropical cyclone forecast models using GODAE nowcasts SO MONTHLY WEATHER REVIEW LA English DT Article ID SEA-SURFACE TEMPERATURE; MIXED-LAYER RESPONSE; HURRICANE GILBERT; MAXIMUM INTENSITY; VERTICAL DIFFUSIVITIES; DATA ASSIMILATION; WIND FIELDS; COORDINATE; SYSTEM; HYCOM AB To simulate tropical cyclone (TC) intensification, coupled ocean -atmosphere prediction models must realistically reproduce the magnitude and pattern of storm-forced sea surface temperature (SST) cooling. The potential for the ocean to support intensification depends on the thermal energy available to the storm, which in turn depends on both the temperature and thickness of the upper-ocean warm layer. The ocean heat content (OHC) is used as an index of this potential. Large differences in available thermal energy associated with energetic boundary currents and ocean eddies require their accurate initialization in ocean models. Two generations of the experimental U. S. Navy ocean nowcast -forecast system based on the Hybrid Coordinate Ocean Model (HYCOM) are evaluated for this purpose in the NW Caribbean Sea and Gulf of Mexico prior to Hurricanes Isidore and Lili (2002), Ivan (2004), and Katrina (2005). Evaluations are conducted by comparison to in situ measurements, the navy's three-dimensional Modular Ocean Data Assimilation System (MODAS) temperature and salinity analyses, microwave satellite SST, and fields of OHC and 26 degrees C isotherm depth derived from satellite altimetry. Both nowcast -forecast systems represent the position of important oceanographic features with reasonable accuracy. Initial fields provided by the first-generation product had a large upper-ocean cold bias because the nowcast was initialized from a biased older-model run. SST response in a free-running Isidore simulation is improved by using initial and boundary fields with reduced cold bias generated from a HYCOM nowcast that relaxed model fields to MODAS analyses. A new climatological initialization procedure used for the second-generation nowcast system tended to reduce the cold bias, but the nowcast still could not adequately reproduce anomalously warm conditions present before all storms within the first few months following nowcast initialization. The initial cold biases in both nowcast products tended to decrease with time. A realistic free-running HYCOM simulation of the ocean response to Ivan illustrates the critical importance of correctly initializing both warm-core rings and cold-core eddies to correctly simulate the magnitude and pattern of SST cooling. C1 [Halliwell, G. R., Jr.; Shay, L. K.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, MPO, Miami, FL 33149 USA. [Jacob, S. D.] NASA, GEST, Greenbelt, MD USA. [Smedstad, O. M.] Planning Syst Inc, Stennis Space Ctr, Mississippi State, MS USA. [Uhlhorn, E. W.] NOAA, Hurricane Res Div, Miami, FL USA. RP Halliwell, GR (reprint author), Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, MPO, 4600 Rickenbacker Cswy, Miami, FL 33149 USA. EM ghalliwell@rsmas.miami.edu RI Halliwell, George/B-3046-2011; Uhlhorn, Eric/B-1336-2014 OI Halliwell, George/0000-0003-4216-070X; Uhlhorn, Eric/0000-0002-4759-5342 NR 47 TC 20 Z9 20 U1 0 U2 8 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0027-0644 J9 MON WEATHER REV JI Mon. Weather Rev. PD JUL PY 2008 VL 136 IS 7 BP 2576 EP 2591 DI 10.1175/2007MWR2154.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 330US UT WOS:000257968900018 ER PT J AU Amzajerdian, F AF Amzajerdian, Farzin TI The expanding role of lidar at NASA SO PHOTONICS SPECTRA LA English DT Article C1 [Amzajerdian, Farzin] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Amzajerdian, F (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. EM f.amzajerdian@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU LAURIN PUBL CO INC PI PITTSFIELD PA BERKSHIRE COMMON PO BOX 1146, PITTSFIELD, MA 01202 USA SN 0731-1230 J9 PHOTONIC SPECTRA JI Photon. Spect. PD JUL PY 2008 VL 42 IS 7 BP 50 EP + PG 5 WC Optics SC Optics GA 330UE UT WOS:000257967500013 ER PT J AU Wolpert, DH AF Wolpert, David H. TI Physical limits of inference SO PHYSICA D-NONLINEAR PHENOMENA LA English DT Article DE Turing machine; automata; observation; prediction; multiverse; Kolmogorov complexity ID COMPUTATION; UNDECIDABILITY; SYSTEMS; COMPUTABILITY; MECHANICS AB We show that physical devices that perform observation, prediction, or recollection share an underlying mathematical structure. We call devices with that structure "inference devices". We present a set of existence and impossibility results concerning inference devices. These results hold independent of the precise physical laws governing our universe. In a limited sense, the impossibility results establish that Laplace was wrong to claim that even in a classical, non-chaotic universe the future can be unerringly predicted, given sufficient knowledge of the present. Alternatively, these impossibility results can be viewed as a non-quantum-mechanical "uncertainty principle". The mathematics of inference devices has close connections to the mathematics of Turing Machines (TMs). In particular, the impossibility results for inference devices are similar to the Halting theorem for TMs. Furthermore, one can define an analog of Universal TMs (UTMs) for inference devices. We call those analogs "strong inference devices". We use strong inference: devices to define the "inference complexity" of an inference task, which is the analog of the Kolmogorov complexity of computing a string. A task-independent bound is derived on how much the inference complexity of an inference task can differ for two different inference devices. This is analogous to the "encoding" bound governing how much the Kolmogorov complexity of a string can differ between two UTMs used to compute: that string. However no universe can contain more than one strong inference device. So whereas the Kolmogorov complexity of a string is arbitrary up to specification of the UTM, there is no such arbitrariness in the inference complexity of an inference task. We informally discuss the philosophical implications of these results, e.g., for whether the universe "is" a computer. We also derive some graph-theoretic properties governing any set of multiple inference devices. We also present an extension of the framework to address physical devices used for control. We end with an extension of the framework to address probabilistic inference. (c) Published by Elsevier B.V. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Wolpert, DH (reprint author), NASA, Ames Res Ctr, MS 269-1, Moffett Field, CA 94035 USA. EM dhw@ptolemy.arc.nasa.gov NR 50 TC 8 Z9 8 U1 0 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0167-2789 J9 PHYSICA D JI Physica D PD JUL 1 PY 2008 VL 237 IS 9 BP 1257 EP 1281 DI 10.1016/j.physd.2008.03.040 PG 25 WC Mathematics, Applied; Physics, Multidisciplinary; Physics, Mathematical SC Mathematics; Physics GA 322DO UT WOS:000257355600010 ER PT J AU Shaw, MD Lutchyn, RM Delsing, P Echternach, PM AF Shaw, M. D. Lutchyn, R. M. Delsing, P. Echternach, P. M. TI Kinetics of nonequilibrium quasiparticle tunneling in superconducting charge qubits SO PHYSICAL REVIEW B LA English DT Article ID SINGLE; TRANSISTORS; JUNCTIONS AB We directly observe low-temperature nonequilibrium quasiparticle tunneling in charge qubits based on the single-Cooper-pair box. We measure even- and odd-state dwell-time distributions as a function of temperature, and interpret these results using a kinetic theory. While the even-state lifetime is exponentially distributed, the odd-state distribution is more heavily weighted to short times, implying that odd-to-even tunnel events are not described by a homogenous Poisson process. The mean odd-state dwell time increases sharply at low temperature, which is consistent with quasiparticles tunneling out of the island before reaching thermal equilibrium. C1 [Delsing, P.; Echternach, P. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Shaw, M. D.] Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA. [Lutchyn, R. M.] Univ Maryland, Joint Quantum Inst, Dept Phys, College Pk, MD 20742 USA. [Delsing, P.] Chalmers, S-41296 Gothenburg, Sweden. RP Echternach, PM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM pierre.m.echternach@jpl.nasa.gov RI Lutchyn, Roman/B-1873-2009; Delsing, Per/F-7288-2010 OI Delsing, Per/0000-0002-1222-3506 NR 27 TC 38 Z9 38 U1 1 U2 5 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 J9 PHYS REV B JI Phys. Rev. B PD JUL PY 2008 VL 78 IS 2 AR 024503 DI 10.1103/PhysRevB.78.024503 PG 9 WC Physics, Condensed Matter SC Physics GA 333YT UT WOS:000258190200103 ER PT J AU Sundararajan, PA Khanna, G Hughes, SA Drasco, S AF Sundararajan, Pranesh A. Khanna, Gaurav Hughes, Scott A. Drasco, Steve TI Towards adiabatic waveforms for inspiral into Kerr black holes. II. Dynamical sources and generic orbits SO PHYSICAL REVIEW D LA English DT Article ID EQUATIONS; BINARIES; FIELD; LISA AB This is the second in a series of papers whose aim is to generate adiabatic gravitational waveforms from the inspiral of stellar-mass compact objects into massive black holes. In earlier work, we presented an accurate (2+1)D finite-difference time-domain code to solve the Teukolsky equation, which evolves curvature perturbations near rotating (Kerr) black holes. The key new ingredient there was a simple but accurate model of the singular source term based on a discrete representation of the Dirac-delta function and its derivatives. Our earlier work was intended as a proof of concept, using simple circular, equatorial geodesic orbits as a test bed. Such a source is effectively static, in that the smaller body remains at the same coordinate radius and orbital inclination over an orbit. (It of course moves through axial angle, but we separate that degree of freedom from the problem. Our numerical grid has only radial, polar, and time coordinates.) We now extend the time-domain code so that it can accommodate dynamic sources that move on a variety of physically interesting world lines. We validate the code with extensive comparison to frequency-domain waveforms for cases in which the source moves along generic (inclined and eccentric) bound geodesic orbits. We also demonstrate the ability of the time-domain code to accommodate sources moving on interesting nongeodesic worldlines. We do this by computing the waveform produced by a test mass following a kludged inspiral trajectory, made of bound geodesic segments driven toward merger by an approximate radiation loss formula. C1 [Sundararajan, Pranesh A.; Hughes, Scott A.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Sundararajan, Pranesh A.; Hughes, Scott A.] MIT, Kavli Inst, Cambridge, MA 02139 USA. [Khanna, Gaurav] Univ Massachusetts, Dept Phys, Dartmouth, NS 02747, Canada. [Drasco, Steve] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Sundararajan, PA (reprint author), MIT, Dept Phys, 77 Massachusetts Ave, Cambridge, MA 02139 USA. NR 27 TC 34 Z9 34 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD JUL PY 2008 VL 78 IS 2 AR 024022 DI 10.1103/PhysRevD.78.024022 PG 13 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 340HM UT WOS:000258636700075 ER PT J AU Khazanov, G Tel'nikhin, A Kronberg, T AF Khazanov, George Tel'nikhin, Alexander Kronberg, Tatiana TI Nonlinear electron motion in a coherent whistler wave packet SO PHYSICS OF PLASMAS LA English DT Article ID RELATIVISTIC-PARTICLES; CHAOTIC MOTION; FIELD; DYNAMICS AB Map equations are derived, with which nonlinear electron motion in a coherent whistler wave packet is investigated. All solutions of these equations belong to a certain strange attractor and describe chaotic motion with the stable means. The class of solutions determined the intermittent dynamics as the control parameter of the wave-particle system increases above the appropriate critical value is found. An application of the results to the problem of the stability of Earth's radiation belts is considered. It is shown that the efficient acceleration processes take place for relativistic electrons of a few MeV. (C) 2008 American Institute of Physics. C1 [Khazanov, George] NASA, Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Huntsville, AL 35812 USA. [Tel'nikhin, Alexander; Kronberg, Tatiana] Altai State Univ, Barnaul 656049, Altai, Russia. RP Khazanov, G (reprint author), NASA, Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Huntsville, AL 35812 USA. EM George.Khazanov@nsstc.nasa.gov; kronberg@phys.asu.ru NR 23 TC 4 Z9 4 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-664X J9 PHYS PLASMAS JI Phys. Plasmas PD JUL PY 2008 VL 15 IS 7 AR 073506 DI 10.1063/1.2959121 PG 9 WC Physics, Fluids & Plasmas SC Physics GA 333TR UT WOS:000258175800073 ER PT J AU Johnson, RE Fama, M Liu, M Baragiola, RA Sittler, EC Smith, HT AF Johnson, R. E. Fama, M. Liu, M. Baragiola, R. A. Sittler, E. C., Jr. Smith, H. T. TI Sputtering of ice grains and icy satellites in Saturn's inner magnetosphere SO PLANETARY AND SPACE SCIENCE LA English DT Article DE sputtering; Saturn; icy; magnetosphere ID OUTER SOLAR-SYSTEM; WATER ICE; E-RING; ION; ENCELADUS; EJECTION; EROSION; PLASMA; TORUS; RHEA AB Icy grains and satellites orbiting in Saturn's magnetosphere are immersed in a plasma that sputters their surfaces. This limits the lifetime of the E-ring grains and ejects neutrals that orbit Saturn until they are ionized and populate its magnetosphere. Here we reevaluate the sputtering rate of ice in Saturn's inner magnetosphere using the recent Cassini data on the plasma ion density, temperature and composition [Sittler Jr., E.C., et al., 2007a. Ion and neutral sources and sinks within Saturn's inner magnetosphere: Cassini results. Planet. Space Sci. 56, 3-18.] and a recent summary of the relevant sputtering data for ice [Fama, M., Shi, J., Baragiola, R.A., 2008. Sputtering of ice by low-energy ions. Surf. Sci. 602, 156-161.]. Although the energetic (> 10 keV) ion component at Saturn is much smaller than was assumed to be the case after Voyager [Jurac, S., Johnson, R.E., Richardson, J.D., Paranicas, C., 2001a. Satellite sputtering in Saturn's magnetosphere. Planet. Space Sci. 49, 319-326; Jurac, S., Johnson, R.E., Richardson, J.D., 2001b. Saturn's E ring and production of the neutral torus. Icarus 149, 384-396.], we show that the sputtering rates are sensitive to the temperature of the thermal plasma and are still robust, so that sputtering likely determines the lifetime of the grains in Saturn's tenuous E-ring. (c) 2008 Elsevier Ltd. All rights reserved. C1 [Johnson, R. E.; Fama, M.; Liu, M.; Baragiola, R. A.] Univ Virginia, Charlottesville, VA 22904 USA. [Johnson, R. E.] NYU, Dept Phys, New York, NY 10003 USA. [Sittler, E. C., Jr.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Smith, H. T.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. RP Johnson, RE (reprint author), Univ Virginia, Charlottesville, VA 22904 USA. EM rej@virginia.edu RI Smith, Howard/H-4662-2016; OI Smith, Howard/0000-0003-3537-3360; Fama, Marcelo/0000-0003-3476-4669 NR 41 TC 30 Z9 30 U1 1 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD JUL PY 2008 VL 56 IS 9 BP 1238 EP 1243 DI 10.1016/j.pss.2008.04.003 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 332CE UT WOS:000258058600007 ER PT J AU Kuntz, KD Harrus, I McGlynn, TA Mushotzky, RF Snowden, SL AF Kuntz, K. D. Harrus, Ilana McGlynn, Thomas A. Mushotzky, Richard F. Snowden, Steven L. TI OMCat: Catalog of serendipitous sources detected with the XMM-Newton Optical Monitor SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID GALAXIES; ULTRAVIOLET; EXPLORER; NUCLEI AB The Optical Monitor Catalog of serendipitous sources (OMCat) contains entries for every source detected in the publicly available XMM-Newton Optical Monitor (OM) images taken in either the imaging or "fast" modes. Since the OM is coaligned and records data simultaneously with the X-ray telescopes on XMM-Newton, it typically produces images in one or more near-UV or optical bands for every pointing of the observatory. As of the beginning of 2006, the public archive had covered roughly 0.5% of the sky in 2950 fields. The OMCat is not dominated by sources previously undetected at other wavelengths; the bulk of the objects have optical counterparts. However, the OMCat can be used to extend optical or X-ray spectral energy distributions for known objects into the ultraviolet, to study at higher angular resolution objects detected with GALEX, or to find high-Galactic-latitude objects of interest for UV spectroscopy. C1 [Kuntz, K. D.; Harrus, Ilana] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA. [Kuntz, K. D.; Harrus, Ilana; McGlynn, Thomas A.; Mushotzky, Richard F.; Snowden, Steven L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kuntz, KD (reprint author), Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA. RI Snowden, Steven/D-5292-2012 NR 15 TC 13 Z9 13 U1 1 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUL PY 2008 VL 120 IS 869 BP 740 EP 758 DI 10.1086/590162 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 324MJ UT WOS:000257522400004 ER PT J AU Hoshi, M Endo, S Tanaka, K Ishikawa, M Straume, T Komura, K Ruhm, W Nolte, E Huber, T Nagashima, Y Seki, R Sasa, K Sueki, K Fukushima, H Egbert, SD Imanaka, T AF Hoshi, M. Endo, S. Tanaka, K. Ishikawa, M. Straume, T. Komura, K. Ruehm, W. Nolte, E. Huber, T. Nagashima, Y. Seki, R. Sasa, K. Sueki, K. Fukushima, H. Egbert, S. D. Imanaka, T. TI Intercomparison study on (152)Eu gamma ray and (36)Cl AMS measurements for development of the new Hiroshima-Nagasaki Atomic Bomb Dosimetry System 2002 (DS02) SO RADIATION AND ENVIRONMENTAL BIOPHYSICS LA English DT Article ID THERMAL-NEUTRON DISCREPANCY; GRANITE SAMPLES; RESIDUAL EU-152; LARGE DISTANCES; GE DETECTORS; RADIOACTIVITY; PART; EXPLOSION; SURVIVORS AB In the process of developing a new dosimetry system for atomic bomb survivors in Hiroshima and Nagasaki (DS02), an intercomparison study between (152)Eu and (36)Cl measurements was proposed, to reconcile the discrepancy previously observed in the Hiroshima data between measurements and calculations of thermal neutron activation products. Nine granite samples, exposed to the atomic-bomb radiation in Hiroshima within 1,200 m of the hypocenter, as well as mixed standard solutions containing known amounts of europium and chlorine that were neutron-activated by a (252)Cf source, were used for the intercomparison. Gamma-ray spectrometry for (152)Eu was carried out with ultra low-background Ge detectors at the Ogoya Underground Laboratory, Kanazawa University, while three laboratories participated in the (36)Cl measurement using accelerator mass spectrometry (AMS): The Technical University of Munich, Germany, the Lawrence Livermore National Laboratory, USA and the University of Tsukuba, Japan. Measured values for the mixed standard solutions showed good agreement among the participant laboratories. They also agreed well with activation calculations, using the neutron fluences monitored during the (252)Cf irradiation, and the corresponding activation cross-sections taken from the JENDL-3.3 library. The measured-to-calculated ratios obtained were 1.02 for (152)Eu and 0.91-1.02 for (36)Cl, respectively. Similarly, the results of the granite intercomparison indicated good agreement with the DS02 calculation for these samples. An average measured-to-calculated ratio of 0.98 was obtained for all granite intercomparison measurements. The so-called neutron discrepancy that was previously observed and that which included increasing measured-to-calculated ratios for thermal neutron activation products for increasing distances beyond 1,000 m from the hypocenter was not seen in the results of the intercomparison study. The previously claimed discrepancy could be explained by insufficient understanding of the measured data. C1 [Hoshi, M.; Endo, S.; Tanaka, K.] Hiroshima Univ, Res Inst Radiat Biol & Med, Minami Ku, Hiroshima 7348553, Japan. [Ishikawa, M.] Hokkaido Univ Hosp, Dept Med Phys, Kita Ku, Sapporo, Hokkaido 0608648, Japan. [Straume, T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Komura, K.] Kanazawa Univ, Inst Nat & Environm Technol, Low Level Radioact Lab, Nomi, Ishikawa 9231224, Japan. [Ruehm, W.] Inst Radiobiol, D-85764 Neuherberg, Germany. [Nolte, E.; Huber, T.] Tech Univ Munich, Dept Phys, D-85747 Garching, Germany. [Nagashima, Y.; Seki, R.; Sasa, K.; Sueki, K.] Univ Tsukuba, Tandem Accelerator Ctr, Tsukuba, Ibaraki 3058577, Japan. [Fukushima, H.] Japan Chem Anal Ctr, Inage Ku, Chiba 2630002, Japan. [Egbert, S. D.] Sci Applicat Int Corp, San Diego, CA 92121 USA. [Imanaka, T.] Kyoto Univ, Inst Res Reactor, Kumatori, Osaka 5900494, Japan. RP Hoshi, M (reprint author), Hiroshima Univ, Res Inst Radiat Biol & Med, Minami Ku, 1-2-3 Kasumi, Hiroshima 7348553, Japan. EM mhoshi@hiroshima-u.ac.jp RI Ishikawa, Masayori/D-9878-2012; Sueki, Keisuke/D-4337-2016; Endo, Satoru/D-9091-2012; OI Sueki, Keisuke/0000-0002-8410-9622; Endo, Satoru/0000-0001-5961-681X; Hoshi, Masaharu/0000-0001-6978-0883 NR 46 TC 4 Z9 4 U1 1 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0301-634X J9 RADIAT ENVIRON BIOPH JI Radiat. Environ. Biophys. PD JUL PY 2008 VL 47 IS 3 BP 313 EP 322 DI 10.1007/s00411-008-0166-z PG 10 WC Biology; Biophysics; Environmental Sciences; Radiology, Nuclear Medicine & Medical Imaging SC Life Sciences & Biomedicine - Other Topics; Biophysics; Environmental Sciences & Ecology; Radiology, Nuclear Medicine & Medical Imaging GA 313TS UT WOS:000256763500003 PM 18389270 ER PT J AU Cucinotta, FA Kim, MHY Willingham, V George, KA AF Cucinotta, Francis A. Kim, Myung-Hee Y. Willingham, Veronica George, Kerry A. TI Physical and biological organ dosimetry analysis for International Space Station astronauts SO RADIATION RESEARCH LA English DT Article ID LOW-EARTH-ORBIT; COMPLEX CHROMOSOME-ABERRATIONS; RADIATION CANCER-RISKS; GALACTIC COSMIC-RAYS; HUMAN-LYMPHOCYTES; BLOOD-LYMPHOCYTES; SHIELDING EFFECTIVENESS; ACCELERATED PARTICLES; LEO ENVIRONMENT; CROSS-SECTIONS AB In this study, we analyzed the biological and physical organ dose equivalents for International Space Station (ISS) astronauts. Individual physical dosimetry is difficult in space due to the complexity of the space radiation environment, which consists of protons, heavy ions and secondary neutrons, and the modification of these radiation types in tissue as well as limitations in dosimeter devices that can be worn for several months in outer space. Astronauts returning from missions to the ISS undergo biodosimetry assessment of chromosomal damage in lymphocyte cells using the multicolor fluorescence in situ hybridization (FISH) technique. Individual-based preflight dose responses for lymphocyte exposure in vitro to gamma rays were compared to those exposed to space radiation in vivo to determine an equivalent biological dose. We compared the ISS biodosimetry results, NASA's space radiation transport models of organ dose equivalents, and results from ISS and space shuttle phantom torso experiments. Physical and biological doses for 19 ISS astronauts yielded average effective doses and individual or population-based biological doses for the approximately 6-month missions of 72 mSv and 85 or 81 mGy-Eq, respectively. Analyses showed that 80% or more of organ dose equivalents on the ISS are from galactic cosmic rays and only a small contribution is from trapped protons and that GCR doses were decreased by the high level of solar activity in recent years. Comparisons of models to data showed that space radiation effective doses can be predicted to within about a +/-10% accuracy by space radiation transport models. Finally, effective dose estimates for all previous NASA missions are summarized. (C) 2008 by Radiation Research Society. C1 [Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Space Radiat Program, Houston, TX 77058 USA. [Kim, Myung-Hee Y.; Willingham, Veronica; George, Kerry A.] Wyle Labs, Life Sci Grp, Houston, TX 77058 USA. [Kim, Myung-Hee Y.] USRA Div Space Life Sci, Houston, TX 77058 USA. RP Cucinotta, FA (reprint author), NASA, Lyndon B Johnson Space Ctr, Space Radiat Program, Houston, TX 77058 USA. EM Francis.A.Cucinotta@NASA.gov OI Kim, Myung-Hee/0000-0001-5575-6858 NR 58 TC 71 Z9 76 U1 1 U2 15 PU RADIATION RESEARCH SOC PI LAWRENCE PA 810 E TENTH STREET, LAWRENCE, KS 66044 USA SN 0033-7587 J9 RADIAT RES JI Radiat. Res. PD JUL PY 2008 VL 170 IS 1 BP 127 EP 138 DI 10.1667/RR1330.1 PG 12 WC Biology; Biophysics; Radiology, Nuclear Medicine & Medical Imaging SC Life Sciences & Biomedicine - Other Topics; Biophysics; Radiology, Nuclear Medicine & Medical Imaging GA 321IN UT WOS:000257298100013 PM 18582161 ER PT J AU Vesper, SJ Wong, W Kuo, CM Pierson, DL AF Vesper, Stephen J. Wong, Wing Kuo, C. Mike Pierson, Duane L. TI Mold species in dust from the International Space Station identified and quantified by mold-specific quantitative PCR SO RESEARCH IN MICROBIOLOGY LA English DT Article DE Intenational Space Station; mold-specific quantitative PCR; Aspergillus ID MICROBIAL CHARACTERIZATION; ASTRONAUTS; RESPONSES; SPACEFLIGHT/; REACTIVATION; PENICILLIUM; VIRUS; BOARD AB Dust was collected over a period of several weeks in 2007 from HEPA filters in the U.S. Laboratory Module of the International Space Station (ISS). The dust was returned on the Space Shuttle Atlantis, mixed, sieved and the DNA was extracted. Using a DNA-based method called mold-specific quantitative PCR (MSQPCR), 39 molds were measured in the dust. Potential opportunistic pathogens Aspergillus flavus and Aspergillus niger and potential moderate toxin producers Penicillium chrysogenum and Penicillium brevicompactum were noteworthy. No cells of the potential opportunistic pathogens Asperqillus fumigatus, Aspergillus terreus, Fusarium solani or Candida albicans were detected. Published by Elsevier Masson SAS. C1 [Vesper, Stephen J.] US EPA, Natl Exposure Res Lab, Cincinnati, OH 45268 USA. [Kuo, C. Mike] WYLE Labs Inc, Houston, TX USA. [Wong, Wing] Enterprise Advisory Serv Inc, Houston, TX USA. [Pierson, Duane L.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Vesper, SJ (reprint author), US EPA, Natl Exposure Res Lab, 26 W ML King Ave,ML 314, Cincinnati, OH 45268 USA. EM vesper.stephen@epa.gov NR 19 TC 20 Z9 23 U1 0 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0923-2508 J9 RES MICROBIOL JI Res. Microbiol. PD JUL-AUG PY 2008 VL 159 IS 6 BP 432 EP 435 DI 10.1016/j.resmic.2008.06.001 PG 4 WC Microbiology SC Microbiology GA 357EN UT WOS:000259829200003 PM 18602989 ER PT J AU Smialek, JL Zhu, DM Cuy, MD AF Smialek, James L. Zhu, Dongming Cuy, Michael D. TI Moisture-induced delamination video of an oxidized thermal barrier coating SO SCRIPTA MATERIALIA LA English DT Article DE alumina scales; spallation; nickel alloys; hydrogen embrittlement; moisture effects ID OXIDATION; SEGREGATION; GROWTH; LIFE AB Physical vapor deposited thermal barrier coatings (TBCs) were thermally cycled to near-failure at It 50 degrees C. Normal failure occurred after 200-300 1 h cycles with only moderate weight gains (0.5 Mg cm(-2)). Delamination and buckling was often delayed until well after cooldown (desktop spallation), but could be instantly induced by the application of water drops, as shown in an accompanying video-recording. Moisture therefore plays a primary role in delayed desktop TBC failure. Hydrogen embrittlement is proposed as the underlying mechanism. Published by Elsevier Ltd. on behalf of Acta Materialia Inc. C1 [Smialek, James L.; Zhu, Dongming; Cuy, Michael D.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Smialek, JL (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM James.L.Smialek@grc.nasa.gov NR 15 TC 18 Z9 18 U1 1 U2 16 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1359-6462 J9 SCRIPTA MATER JI Scr. Mater. PD JUL PY 2008 VL 59 IS 1 BP 67 EP 70 DI 10.1016/j.scriptamat.2008.02.055 PG 4 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA 304PK UT WOS:000256121200017 ER PT J AU Xu, N Liu, LF Sun, X Chen, C Wang, Y Han, DD Liu, XY Han, RQ Kang, JF Yu, B AF Xu, N. Liu, L. F. Sun, X. Chen, C. Wang, Y. Han, D. D. Liu, X. Y. Han, R. Q. Kang, J. F. Yu, B. TI Bipolar switching behavior in TiN/ZnO/Pt resistive nonvolatile memory with fast switching and long retention SO SEMICONDUCTOR SCIENCE AND TECHNOLOGY LA English DT Article ID RESISTANCE; MECHANISMS AB Highly stable bipolar resistive switching behaviors of TiN/ZnO/Pt devices were demonstrated for the first time. The excellent memory characteristics including fast switching speed (< 20 ns for set and < 60 ns for reset), long retention (in the order of 10(5) s) and non-electroforming process were demonstrated. The bipolar switching behaviors can be explained by formation and rupture of the filamentary conductive path consisting of oxygen vacancies. The excellent bipolar switching behavior can be attributed to the significant amount of oxygen vacancies in ZnO film and the effect of TiN layer serving as an oxygen reservoir. C1 [Xu, N.; Liu, L. F.; Sun, X.; Chen, C.; Wang, Y.; Han, D. D.; Liu, X. Y.; Han, R. Q.; Kang, J. F.] Peking Univ, Inst Microelect, Beijing 100871, Peoples R China. [Yu, B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Xu, N (reprint author), Peking Univ, Inst Microelect, Beijing 100871, Peoples R China. EM kangjf@pku.edu.cn RI Sun, Xiao/F-5423-2012; Xu, Nuo/G-1768-2014 OI Sun, Xiao/0000-0002-7913-7186; NR 16 TC 75 Z9 75 U1 8 U2 48 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0268-1242 J9 SEMICOND SCI TECH JI Semicond. Sci. Technol. PD JUL PY 2008 VL 23 IS 7 AR 075019 DI 10.1088/0268-1242/23/7/075019 PG 4 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Condensed Matter SC Engineering; Materials Science; Physics GA 319YO UT WOS:000257201100020 ER PT J AU Green, RD Liu, CC Adler, SB AF Green, Robert D. Liu, Chung-Chiun Adler, Stuart B. TI Carbon dioxide reduction on gadolinia-doped ceria cathodes SO SOLID STATE IONICS LA English DT Article DE carbon dioxide electrolysis; impedance spectroscopy; porous electrode model; exchange rate; vacancy diffusion coefficient; thermodynamic factor ID OXIDE FUEL-CELL; STABILIZED ZIRCONIA ELECTROLYTE; CONDUCTING OXYGEN ELECTRODES; NI POINT ELECTRODES; DIRECT-OXIDATION; ELECTROCHEMICAL OXIDATION; SURFACE EXCHANGE; STEADY-STATE; ELECTRICAL CONDUCTIVITY; FLUORITE STRUCTURE AB AC impedance spectroscopy has been performed on 40 mol% gadolinia-doped ceria electrodes on yttria stabilized zirconia (YSZ) at 700-950 degrees C in reducing CO/CO2 atmospheres. Area-specific-resistance (ASR) values for this electrode were in the range of 0.8-37 Omega-cm(2), about two orders of magnitude lower than measurements on Pt electrodes and slightly lower than data on Ni-YSZ electrodes in the literature under similar temperature and partial pressure of oxygen (P-O2) conditions. A continuum-based model of this electrode is described and ail analysis performed to extract the vacancy diffusion coefficient (D-nu) and surface exchange rate coefficient (R-0) as a function of temperature and P-O2, from the impedance results. The D-nu data agree reasonably well with published measurements of the tracer diffusion coefficient (D*) based on isotope profiling by secondary ion mass spectroscopy (SIMS) and conductivity measurements on 40 mol% GDC. The R-0 values are a factor of 3 lower than the published measurements of the surface reaction rate (k) obtained from isothermal thermogravimetric relaxation, and decrease with increasing P-O2. Values of the thermodynamic factor (A) calculated from the fitted model parameters matched well with those calculated from oxygen non-stoichiometry data in the literature. Published by Elsevier B.V. C1 [Green, Robert D.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Liu, Chung-Chiun] Case Western Reserve Univ, Dept Chem Engn, Cleveland, OH 44106 USA. [Adler, Stuart B.] Univ Washington, Dept Chem Engn, Seattle, WA 98195 USA. RP Green, RD (reprint author), NASA, Glenn Res Ctr, MS 77-5,21000 Brookpk Rd, Cleveland, OH 44135 USA. EM Robert.D.Green@nasa.gov NR 73 TC 47 Z9 47 U1 9 U2 57 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0167-2738 J9 SOLID STATE IONICS JI Solid State Ion. PD JUL PY 2008 VL 179 IS 17-18 BP 647 EP 660 DI 10.1016/j.ssi.2008.04.024 PG 14 WC Chemistry, Physical; Physics, Condensed Matter SC Chemistry; Physics GA 326VB UT WOS:000257686000007 ER PT J AU Charnley, SB Rodgers, SD AF Charnley, S. B. Rodgers, S. D. TI Interstellar reservoirs of cometary matter SO SPACE SCIENCE REVIEWS LA English DT Review DE comets; radio lines : solar system; ISM : molecules; solar system : formation; astrochemistry ID O1 HALE-BOPP; LOW-MASS PROTOSTAR; ORTHO-PARA RATIO; NITROGEN ISOTOPIC FRACTIONATION; MULTIPLY DEUTERATED MOLECULES; NUCLEAR-SPIN TEMPERATURE; C/1995 O1; PROTOPLANETARY DISKS; ORGANIC-MOLECULES; IRAS 16293-2422 AB We review the evidence for the products of interstellar chemistry in volatile cometary matter. We compare the organic inventory of star-forming cores with that measured in various comets and point out the similarities and differences. The conditions necessary to fractionate interstellar molecules in the heavier isotopes of H, C, O and N are summarised and compared to the measured fractionation ratios in cometary ices. We give a list of future measurements that would shed further light on the putative connection between cometary and interstellar molecules. C1 [Charnley, S. B.; Rodgers, S. D.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. RP Charnley, SB (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, MS 245-3, Moffett Field, CA 94035 USA. EM charnley@dusty.arc.nasa.gov RI Charnley, Steven/C-9538-2012 NR 124 TC 18 Z9 18 U1 0 U2 5 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD JUL PY 2008 VL 138 IS 1-4 BP 59 EP 73 DI 10.1007/s11214-008-9331-6 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 346QT UT WOS:000259084800005 ER PT J AU Wooden, DH AF Wooden, D. H. TI Cometary refractory grains: Interstellar and nebular sources SO SPACE SCIENCE REVIEWS LA English DT Review DE comets : general; asteroids; solar system : formation; accretion disks; ISM : dust; cosmic rays ID INTERPLANETARY DUST PARTICLES; PROTOPLANETARY ACCRETION DISKS; INFRARED-ABSORPTION SPECTRA; BOPP C/1995 O1; SOLAR NEBULA; HALE-BOPP; CRYSTALLINE SILICATES; DEEP IMPACT; ION IRRADIATION; COMPOSITIONAL DEPENDENCE AB Comets are heterogeneous mixtures of interstellar and nebular materials. The degree of mixing of interstellar sources and nebular sources at different nuclear size scales holds the promise of revealing how cometary particles, cometesimals, and cometary nuclei accreted. We can ascribe cometary materials to interstellar and nebular sources and see how comets probe planet-forming process in our protoplanetary disk. Comets and cometary IDPs contain carbonaceous matter that appears to be either similar to poorly-graphitized (amorphous) carbon, a likely ISM source, or highly labile complex organics, with possible ISM or outer disk heritage. The oxygen fugacity of the solar nebula depends on the dynamical interplay between the inward migration of carbon-rich grains and of icy (water-rich) grains. Inside the water dissociation line, OH- reacts with carbon to form CO or CO2, consuming available oxygen and contributing to the canonical low oxygen fugacity. Alternatively, the influx of water vapor and/or oxygen rich dust grains from outer (cooler) disk regions can raise the oxygen fugacity. Low oxygen fugacity of the canonical solar nebula favors the condensation of Mg-rich crystalline silicates and Fe-metal, or the annealing of Fe-Mg amorphous silicates into Mg-rich crystals and Fe-metal via Fe-reduction. High oxygen fugacity nebular conditions favors the condensation of Fe-bearing to Fe-rich crystalline silicates. In the ISM, Fe-Mg amorphous silicates are prevalent, in stark contrast to Mg-rich crystalline silicates that are rare. Hence, cometary Mg-rich crystalline silicates formed in the hot, inner regions of the canonical solar nebula and they are the touchstone for models of the outward radial transport of nebular grains to the comet-forming zone. Stardust samples are dominated by Mg-rich crystalline silicates but also contain abundant Fe-bearing and Fe-rich crystalline silicates that are too large (>> 0.1 mu m) to be annealed Fe-Mg amorphous silicates. By comparison with asteroids, the Stardust Fe-bearing and Fe-rich crystalline silicates suggests partial aqueous alteration in comet nuclei. However, aqueous alteration transforms Fe-rich olivine to phyllosilicates before Mg-rich olivine, and Stardust has Mg-rich and Fe-rich olivine and no phyllosilicates. Hence, we look to a nebular source for the moderately Fe-rich to nearly pure-Fe crystalline silicates. Primitive matrices have Mg-Fe silicates but no phyllosilicates, supporting the idea that Mg-Fe silicates but not phyllosilicates are products of water-rich shocks. Chondrule-formation is a late stage process in our protoplanetary disk. Stardust samples show comet 81P/Wild 2 formed at least as late to incorporate a few chondrules, requiring radial transport of chondrules out to perhaps > 20 AU. By similar radial transport mechanisms, collisional fragments of aqueously altered asteroids, in particular achondrites that formed earlier than chondrules, might reach the comet-forming zones. However, Stardust samples do not have phyllosilicates and chondrules are rare. Hence, the nebular refractory grains in comet 81P/Wild 2, as well as other comets, appear to be pre-accretionary with respect to asteroid parent bodies. By discussing nebular pathways for the formation of Fe-rich crystalline silicates, and also phyllosilicates and carbonates, we put forth the view that comets contain both the interstellar ingredients for and the products of nebular transmutation. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Wooden, DH (reprint author), NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA. EM dwooden@mac.com NR 213 TC 53 Z9 53 U1 1 U2 8 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD JUL PY 2008 VL 138 IS 1-4 BP 75 EP 108 DI 10.1007/s11214-008-9424-2 PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 346QT UT WOS:000259084800006 ER PT J AU DiSanti, MA Mumma, MJ AF DiSanti, Michael A. Mumma, Michael J. TI Reservoirs for comets: Compositional differences based on infrared observations SO SPACE SCIENCE REVIEWS LA English DT Review DE comets; ices; composition; parent volatiles; molecular spectroscopy; infrared spectroscopy ID O1 HALE-BOPP; C/1996 B2 HYAKUTAKE; OH PROMPT EMISSION; ORTHO-PARA RATIO; CARBON-MONOXIDE; DEEP-IMPACT; ORGANIC COMPOSITION; PARENT VOLATILES; WATER PRODUCTION; EXTENDED SOURCE AB Tracing measured compositions of comets to their origins continues to be of keen interest to cometary scientists and to dynamical modelers of Solar System formation and evolution. This requires building a taxonomy of comets from both present-day dynamical reservoirs: the Kuiper Belt (hereafter KB), sampled through observation of ecliptic comets (primarily Jupiter Family comets, or JFCs), and the Oort cloud (OC), represented observationally by the long-period comets and by Halley Family comets (HFCs). Because of their short orbital periods, JFCs are subjected to more frequent exposure to solar radiation compared with OC comets. The recent apparitions of the JFCs 9P/Tempel 1 and 73P/Schwassmann-Wachmann 3 permitted detailed observations of material issuing from below their surfaces-these comets added significantly to the compositional database on this dynamical class, which is under-represented in studies of cometary parent volatiles. This chapter reviews the latest techniques developed for analysis of high-resolution spectral observations from similar to 2-5 mu m, and compares measured abundances of native ices among comets. While no clear compositional delineation can be drawn along dynamical lines, interesting comparisons can be made. The sub-surface composition of comet 9P, as revealed by the Deep Impact ejecta, was similar to the majority of OC comets studied. Meanwhile, 73P was depleted in all native ices except HCN, similar to the disintegrated OC comet C/1999 S4 (LINEAR). These results suggest that 73P may have formed in the inner giant planets' region while 9P formed farther out or, alternatively, that both JFCs formed farther from the Sun but with 73P forming later in time. C1 [DiSanti, Michael A.; Mumma, Michael J.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. RP DiSanti, MA (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Mail Stop 693, Greenbelt, MD 20771 USA. EM michael.a.disanti@nasa.gov RI mumma, michael/I-2764-2013 NR 96 TC 51 Z9 51 U1 1 U2 5 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD JUL PY 2008 VL 138 IS 1-4 BP 127 EP 145 DI 10.1007/s11214-008-9361-0 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 346QT UT WOS:000259084800008 ER PT J AU Thomas, N Alexander, C Keller, HU AF Thomas, N. Alexander, C. Keller, H. U. TI Loss of the surface layers of comet nuclei SO SPACE SCIENCE REVIEWS LA English DT Review DE comets : surface; comets : nuclei; comets : emission ID DEEP IMPACT OBSERVATIONS; DUSTY GAS-JET; INNER COMA; HALE-BOPP; WATER ICE; SPACECRAFT; TEMPERATURE; 9P/TEMPEL-1; MORPHOLOGY; EVOLUTION AB The Deep Impact observations of low thermal inertia for comet 9P/Tempel 1 are of profound importance for the observations to be made by the Rosetta spacecraft at comet 67P/Churyumov-Gerasimenko. While sub-surface sublimation is necessary to explain the observations, the depth at which this occurs is no more than 2-3 cm and possibly less. The low thermal conductivity when combined with local surface roughness (also observed with Deep Impact) implies that local variations in outgassing rates can be substantial. These variations are likely to be on scales smaller than the resolution limits of all experiments on the Rosetta orbiter. The observed physico-chemical inhomogeneity further suggests that the Rosetta lander will only provide a local snapshot of conditions in the nucleus layer. C1 [Thomas, N.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. [Alexander, C.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Keller, H. U.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. RP Thomas, N (reprint author), Univ Bern, Inst Phys, Sidlerstr 5, CH-3012 Bern, Switzerland. EM nicolas.thomas@space.unibe.ch NR 32 TC 5 Z9 5 U1 1 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD JUL PY 2008 VL 138 IS 1-4 BP 165 EP 177 DI 10.1007/s11214-008-9332-5 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 346QT UT WOS:000259084800010 ER PT J AU Gulkis, S Alexander, C AF Gulkis, S. Alexander, C. TI Composition measurements of a comet from the Rosetta orbiter spacecraft SO SPACE SCIENCE REVIEWS LA English DT Review DE comets; Rosetta; composition; spectroscopy; spacecraft instruments ID ICE; CO AB The European Space Agency (ESA) Rosetta Spacecraft, launched on March 2, 2004 toward Comet 67P/Churyumov-Gerasimenko (C-G), carries a complementary set of instruments on both the orbiter and lander (Philae) portions of the spacecraft, to measure the composition of the Comet C-G. The primary composition measuring instruments on the Orbiter are Alice, COSIMA, ICA, MIRO, OSIRIS, ROSINA and VIRTIS. These instruments collectively are capable of providing compositional information, including temporal and spatial distributions of important atomic, molecular, and ionic species, minerals, and ices in the coma and nucleus. The instruments utilize a variety of techniques and wavelength ranges to accomplish their objectives. This paper provides an overview of composition measurements that will be possible using the suite of orbiter composition measuring instruments. A table is provided that lists important species detectable (depending on abundances) with each instrument. C1 [Gulkis, S.; Alexander, C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Gulkis, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 169-506, Pasadena, CA 91109 USA. EM Samuel.Gulkis@jpl.nasa.gov NR 18 TC 5 Z9 6 U1 1 U2 8 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD JUL PY 2008 VL 138 IS 1-4 BP 259 EP 274 DI 10.1007/s11214-008-9335-2 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 346QT UT WOS:000259084800017 ER PT J AU Rignot, E AF Rignot, Eric TI Changes in West Antarctic ice stream dynamics observed with ALOS PALSAR data SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID PINE ISLAND GLACIER; RADAR INTERFEROMETRY; SOUTHERN-OCEAN; MASS-BALANCE; GREENLAND; SHEET; PENETRATION; ACCELERATION; VELOCITY; SHELF AB The Advanced Land Observation System (ALOS) Phased-Array Synthetic-Aperture Radar (PALSAR) is an L-band frequency (1.27 GHz) radar capable of continental-scale interferometric observations of ice sheet motion. Here, we show that PALSAR data yield excellent measurements of ice motion compared to C-band (5.6 GHz) radar data because of greater temporal coherence over snow and firn. We compare PALSAR velocities from year 2006 in Pine Island Bay, West Antarctica with those spanning years 1974 to 2007. Between 1996 and 2007, Pine Island Glacier sped up 42% and ungrounded over most of its ice plain. Smith Glacier accelerated 83% and ungrounded as well. Their largest speed up are recorded in 2007. Thwaites Glacier is not accelerating but widening with time and its eastern ice shelf doubled its speed. Total ice discharge from these glaciers increased 30% in 12 yr and the net mass loss increased 170% from 39 +/- 15 Gt/yr to 105 +/- 27 Gt/yr. Longer-term velocity changes suggest only a moderate loss in the 1970s. As the glaciers unground into the deeper, smoother beds inland, the mass loss from this region will grow considerably larger in years to come. C1 [Rignot, Eric] Univ Calif Irvine, Irvine, CA 92697 USA. [Rignot, Eric] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Rignot, E (reprint author), Univ Calif Irvine, Irvine, CA 92697 USA. EM erignot@uci.edu RI Rignot, Eric/A-4560-2014 OI Rignot, Eric/0000-0002-3366-0481 NR 27 TC 120 Z9 124 U1 2 U2 38 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUN 28 PY 2008 VL 35 IS 12 AR L12505 DI 10.1029/2008GL033365 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 321ML UT WOS:000257309200001 ER PT J AU McConnell, CL Highwood, EJ Coe, H Formenti, P Anderson, B Osborne, S Nava, S Desboeufs, K Chen, G Harrison, MAJ AF McConnell, C. L. Highwood, E. J. Coe, H. Formenti, P. Anderson, B. Osborne, S. Nava, S. Desboeufs, K. Chen, G. Harrison, M. A. J. TI Seasonal variations of the physical and optical characteristics of Saharan dust: Results from the Dust Outflow and Deposition to the Ocean (DODO) experiment SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID TROPICAL ATLANTIC-OCEAN; RADIATIVE PROPERTIES; MINERAL DUST; RELATIVE-HUMIDITY; EXPERIMENT SHADE; C-130 AIRCRAFT; CLIMATE MODEL; DESERT DUST; AIR-QUALITY; SEA-SALT AB [1] North African dust is important for climate through its direct radiative effect on solar and terrestrial radiation and its role in the biogeochemical system. The Dust Outflow and Deposition to the Ocean project (DODO) aimed to characterize the physical and optical properties of airborne North African dust in two seasons and to use these observations to constrain model simulations, with the ultimate aim of being able to quantify the deposition of iron to the North Atlantic Ocean. The in situ properties of dust from airborne campaigns measured during February and August 2006, based at Dakar, Senegal, are presented here. Average values of the single scattering albedo (0.99, 0.98), mass specific extinction (0.85 m(2) g(-1), 1.14 m(2) g(-1)), asymmetry parameter (0.68, 0.68), and refractive index (1.53-0.0005i, 1.53-0.0014i) for the accumulation mode were found to differ by varying degrees between the dry and wet season, respectively. It is hypothesized that these differences are due to different source regions and transport processes which also differ between the DODO campaigns. Elemental ratios of Ca/Al were found to differ between the dry and wet season (1.1 and 0.5, respectively). Differences in vertical profiles are found between seasons and between land and ocean locations and reflect the different dynamics of the seasons. Using measurements of the coarse mode size distribution and illustrative Mie calculations, the optical properties are found to be very sensitive to the presence and amount of coarse mode of mineral dust, and the importance of accurate measurements of the coarse mode of dust is highlighted. C1 [McConnell, C. L.; Highwood, E. J.] Univ Reading, Dept Meteorol, Reading RG6 6BB, Berks, England. [Anderson, B.; Chen, G.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Coe, H.] Univ Manchester, Sch Earth Atmosphere & Environm Sci, Manchester M13 9PL, Lancs, England. [Formenti, P.; Desboeufs, K.] Univ Paris 12, CNRS, LISA, F-94010 Creteil, France. [Formenti, P.; Desboeufs, K.] Univ Paris 07, F-94010 Creteil, France. [Osborne, S.; Harrison, M. A. J.] Met Off, Exeter EX1 3PB, Devon, England. [Nava, S.] Natl Inst Nucl Phys, I-50019 Florence, Italy. RP McConnell, CL (reprint author), Univ Reading, Dept Meteorol, Reading RG6 6BB, Berks, England. EM c.l.mcconnell@reading.ac.uk RI Highwood, Ellie/A-2402-2013; Coe, Hugh/C-8733-2013; Ryder, Claire/K-5969-2014 OI Ryder, Claire/0000-0002-9892-6113 NR 62 TC 80 Z9 80 U1 0 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 JUN 28 PY 2008 VL 113 IS D14 AR D14S05 DI 10.1029/2007JD009606 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 321MX UT WOS:000257310500001 ER PT J AU Tian, BJ Waliser, DE Kahn, RA Li, Q Yung, YL Tyranowski, T Geogdzhayev, IV Mishchenko, MI Torres, O Smirnov, A AF Tian, Baijun Waliser, Duane E. Kahn, Ralph A. Li, Qinbin Yung, Yuk L. Tyranowski, Tomasz Geogdzhayev, Igor V. Mishchenko, Michael I. Torres, Omar Smirnov, Alexander TI Does the Madden-Julian oscillation influence aerosol variability? SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Review ID RESOLUTION IMAGING SPECTRORADIOMETER; INTRASEASONAL CONVECTION ANOMALIES; SINGLE-SCATTERING ALBEDO; LARGE-SCALE CIRCULATION; OPTICAL DEPTH; INTERANNUAL VARIABILITY; SATELLITE MEASUREMENTS; TROPOSPHERIC AEROSOLS; SULFATE AEROSOLS; DEEP CONVECTION AB We investigate the modulation of aerosols by the Madden-Julian Oscillation (MJO) using multiple, global satellite aerosol products: aerosol index (AI) from the Total Ozone Mapping Spectrometer (TOMS) on Nimbus-7, and aerosol optical thickness (AOT) from the Moderate Resolution Imaging Spectroradiometer (MODIS) on Terra and Aqua and the Advanced Very High Resolution Radiometer (AVHRR) on NOAA satellites. A composite MJO analysis indicates that large variations in the TOMS AI and MODIS/AVHRR AOT are found over the equatorial Indian and western Pacific Oceans where MJO convection is active, as well as the tropical Africa and Atlantic Ocean where MJO convection is weak but the background aerosol level is high. A strong inverse linear relationship between the TOMS AI and rainfall anomalies, but a weaker, less coherent positive correlation between the MODIS/AVHRR AOT and rainfall anomalies, were found. The MODIS/AVHRR pattern is consistent with ground-based Aerosol Robotic Network data. These results indicate that the MJO and its associated cloudiness, rainfall, and circulation variability systematically influence the variability in remote sensing aerosol retrieval results. Several physical and retrieval algorithmic factors that may contribute to the observed aerosol-rainfall relationships are discussed. Preliminary analysis indicates that cloud contamination in the aerosol retrievals is likely to be a major contributor to the observed relationships, although we cannot exclude possible contributions from other physical mechanisms. Future research is needed to fully understand these complex aerosol-rainfall relationships. C1 [Tian, Baijun; Waliser, Duane E.; Kahn, Ralph A.; Li, Qinbin] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Geogdzhayev, Igor V.; Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Kahn, Ralph A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Smirnov, Alexander] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Torres, Omar] Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. [Yung, Yuk L.; Tyranowski, Tomasz] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Tian, BJ (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn Geol, 9258 Boelter Hall,Box 957228, Los Angeles, CA 90095 USA. EM baijun.tian@jpl.nasa.gov RI Smirnov, Alexander/C-2121-2009; Tian, Baijun/A-1141-2007; Kahn, Ralph/D-5371-2012; Torres, Omar/G-4929-2013; Mishchenko, Michael/D-4426-2012 OI Smirnov, Alexander/0000-0002-8208-1304; Tian, Baijun/0000-0001-9369-2373; Kahn, Ralph/0000-0002-5234-6359; NR 101 TC 40 Z9 40 U1 1 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 28 PY 2008 VL 113 IS D12 AR D12215 DI 10.1029/2007JD009372 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 321MT UT WOS:000257310000002 ER PT J AU Kim, SB Fukumori, I AF Kim, Seung-Bum Fukumori, Ichiro TI A near uniform basin-wide sea level fluctuation over the Japan/East Sea: A semienclosed sea with multiple straits SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID ATMOSPHERIC-PRESSURE; GEOSTROPHIC CONTROL; MEDITERRANEAN SEA; BAROTROPIC FLOW; CIRCULATION; DIFFERENCE; GIBRALTAR; MODEL AB Sea level of the Japan/East Sea observed by the TOPEX/Poseidon (T/P) satellite altimeter is analyzed using a 1/4 degrees-resolution ocean general circulation model. A significant fraction of the Japan/East Sea sea level variability is found to be spatially uniform with periods ranging from 20 d to a year. The model simulation is consistent with T/P records in terms of the basin-wide sea level fluctuation's spectral energy and coherence. The simulation indicates that the changes are barotropic in nature and controlled, notably at high frequencies, by the net mass transport through the straits of the Japan/East Sea driven by winds in the vicinity of the Korea/Tsushima and Soya Straits. A series of barotropic simulations suggest that the sea level fluctuations are the result of a dynamic balance at the straits among near-strait winds, friction, and geostrophic control. The basin-wide sea level response is a linear superposition of changes due to winds near the individual straits. In particular, a basin-wide sea level response can be established by winds near either one of the straits alone. For the specific geometry and winds, winds near the Soya Strait have a larger Strait. C1 [Kim, Seung-Bum] Remote Sensing Syst, Santa Rosa, CA 95401 USA. [Fukumori, Ichiro] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Kim, SB (reprint author), Remote Sensing Syst, 438 1st St,Suite 200, Santa Rosa, CA 95401 USA. EM kim@remss.com NR 24 TC 5 Z9 5 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD JUN 28 PY 2008 VL 113 IS C6 AR C06031 DI 10.1029/2007JC004409 PG 14 WC Oceanography SC Oceanography GA 321NQ UT WOS:000257312800001 ER PT J AU Nam, J Gorham, PW Barwick, SW Beatty, JJ Besson, DZ Binns, WR Chen, C Chen, P Clem, JM Connolly, A Dowkontt, PF DuVernois, MA Field, RC Goldstein, DJ Goodhue, A Hast, C Hebert, CL Hoover, S Israel, MH Javaid, A Kowalski, J Learned, JG Liewer, KM Link, JT Lusczek, E Matsuno, S Mercurio, BC Miki, C Miocinovic, P Naudet, CJ Ng, J Nichol, RJ Palladino, KJ Reil, K Romero-Wolf, A Rosen, M Saltzberg, D Seckel, D Varner, GS Walz, D Wu, F AF Nam, Jiwoo Gorham, P. W. Barwick, S. W. Beatty, J. J. Besson, D. Z. Binns, W. R. Chen, C. Chen, P. Clem, J. M. Connolly, A. Dowkontt, P. F. DuVernois, M. A. Field, R. C. Goldstein, D. J. Goodhue, A. Hast, C. Hebert, C. L. Hoover, S. Israel, M. H. Javaid, A. Kowalski, J. Learned, J. G. Liewer, K. M. Link, J. T. Lusczek, E. Matsuno, S. Mercurio, B. C. Miki, C. Miocinovic, P. Naudet, C. J. Ng, J. Nichol, R. J. Palladino, K. J. Reil, K. Romero-Wolf, A. Rosen, M. Saltzberg, D. Seckel, D. Varner, G. S. Walz, D. Wu, F. CA ANITA Collaboration TI Preliminary result from ANITA experiment SO MODERN PHYSICS LETTERS A LA English DT Article; Proceedings Paper CT Internatonal Symposium on Cosmology and Particle Astrophysics CY NOV 13-15, 2007 CL Taipei, TAIWAN DE UHE neutrino; GZK process; Askaryan effect ID COHERENT RADIO EMISSION; CHARGE AB The ANITA (ANtarctic Impulsive Transient Antenna) experiment is a balloon-borne neutrino telescope which consists of an array of 32 broad-band horn antennas. It successfully completed a 35 day flight over Antarctica during the 2006-2007 austral summer. The primary goal of ANITA is to search for astrophysical neutrinos with energies E > 10(19)eV by detecting radio Cherenkov signals from neutrino induced showers in the Antarctic ice. We present preliminary results from ongoing analyses of ANITA data. C1 [Nam, Jiwoo] Natl Taiwan Univ, Dept Phys, Taipei 106, Taiwan. [Nam, Jiwoo] Natl Taiwan Univ, Inst Astrophys, Taipei 106, Taiwan. [Nam, Jiwoo] Natl Taiwan Univ, Leung Ctr Cosmol & Particle Astrophys, Taipei 106, Taiwan. [Gorham, P. W.; Connolly, A.; Hebert, C. L.; Kowalski, J.; Learned, J. G.; Link, J. T.; Matsuno, S.; Miki, C.; Miocinovic, P.; Romero-Wolf, A.; Rosen, M.; Varner, G. S.] Univ Hawaii Manoa, Dept Phys & Astron, Honolulu, HI 96822 USA. [Liewer, K. M.; Naudet, C. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Beatty, J. J.; Mercurio, B. C.; Palladino, K. J.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Chen, P.; Field, R. C.; Hast, C.; Ng, J.; Reil, K.] Stanford Linear Accelerator Ctr, Menlo Pk, CA 94025 USA. [Barwick, S. W.; Goldstein, D. J.; Wu, F.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA USA. [Connolly, A.; Goodhue, A.; Hoover, S.; Saltzberg, D.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Connolly, A.; Nichol, R. J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Clem, J. M.; Javaid, A.; Seckel, D.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [DuVernois, M. A.; Lusczek, E.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Binns, W. R.; Dowkontt, P. F.; Israel, M. H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Chen, C.; Chen, P.] Natl Taiwan Univ, Dept Phys, Taipei 106, Taiwan. RP Nam, J (reprint author), Natl Taiwan Univ, Dept Phys, Taipei 106, Taiwan. EM jwnam@phys.ntu.edu.tw RI Vieregg, Abigail/D-2287-2012; Beatty, James/D-9310-2011; OI Beatty, James/0000-0003-0481-4952; Lusczek, Elizabeth/0000-0003-4680-965X NR 18 TC 1 Z9 1 U1 0 U2 0 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE SN 0217-7323 J9 MOD PHYS LETT A JI Mod. Phys. Lett. A PD JUN 28 PY 2008 VL 23 IS 17-20 BP 1419 EP 1430 DI 10.1142/S0217732308027795 PG 12 WC Physics, Nuclear; Physics, Particles & Fields; Physics, Mathematical SC Physics GA 335NK UT WOS:000258297100028 ER PT J AU Medezinski, E Broadhurst, T Umetsu, K Coe, D AF Medezinski, Elinor Broadhurst, Tom Umetsu, Keiichi Coe, Dan TI Using weak-lensing dilution to measure light properties of A1689 SO MODERN PHYSICS LETTERS A LA English DT Article; Proceedings Paper CT International Symposium on Cosmology and Particle Astrophysics CY NOV 13-15, 2007 CL Taipei, TAIWAN DE cosmology : observations; gravitational lensing; galaxies : clusters : individual (Abell 1689); galaxies : luminosity function ID GALAXY LUMINOSITY FUNCTION; COMA CLUSTER CORE; IMAGES AB Weak-lensing induced by clusters of galaxies can probe the total mass distribution out to the virial radius of the cluster, regardless of the nature of the mass or its dynamical state. To make a robust analysis, the cluster and background galaxy populations need to be separated. The E/SO sequence of a cluster defines a boundary redward of which a reliable weak-lensing signal can be obtained from background galaxies, uncontaminated by the cluster. Below this limit, the signal is diluted by the proportion of unlensed cluster members. Employing deep Subaru and HST/ACS images of the massive cluster A1689, we use this dilution effect to carefully separate between the cluster members and the background, and thus derive the cluster light profile and luminosity functions to large radius. The light profile of A1689 is found to decline steadily to the limit of the data, r < 2 h(-1)Mpc, with a constant slope, dlog(L)/dlog(r) - -1.12 zO.06. We derive a cluster luminosity function with a flat faint-end slope of alpha = -1.05 +/- 0.07, nearly independent of radius and with no faint upturn to M(i') < -12. The major advantage of this new approach is that no subtraction of far-field background counts is required. C1 [Medezinski, Elinor; Broadhurst, Tom] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Umetsu, Keiichi] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Coe, Dan] Jet Prop Lab, Pasadena, CA USA. RP Medezinski, E (reprint author), Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. NR 16 TC 1 Z9 1 U1 0 U2 1 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE SN 0217-7323 J9 MOD PHYS LETT A JI Mod. Phys. Lett. A PD JUN 28 PY 2008 VL 23 IS 17-20 BP 1521 EP 1528 DI 10.1142/S0217732308027916 PG 8 WC Physics, Nuclear; Physics, Particles & Fields; Physics, Mathematical SC Physics GA 335NK UT WOS:000258297100040 ER PT J AU Armstrong, JW Estabrook, FB Asmar, SW Iess, L Tortora, P AF Armstrong, J. W. Estabrook, F. B. Asmar, S. W. Iess, L. Tortora, P. TI Reducing antenna mechanical noise in precision spacecraft tracking SO RADIO SCIENCE LA English DT Article ID RADIO SCIENCE; CASSINI; STABILITY AB Doppler tracking of deep space probes is central to spacecraft navigation and many radio science investigations. The most sensitive Doppler observations to date were taken using the NASA/JPL Deep Space Network antenna DSS 25 (a 34 m diameter beam-waveguide station instrumented with simultaneous X-and Ka-band uplink and tropospheric scintillation calibration equipment) tracking the Cassini spacecraft. Those observations achieved Doppler fractional frequency stability (Doppler frequency fluctuation divided by center frequency, Delta f/f(o)) approximate to 3 x 10(-15) at 1000 s integration time. The leading noise in these very-high-sensitivity tracks was time-dependent unmodeled motion of the ground antenna's phase center (caused, e. g., by antenna sag as elevation angle changes, unmodeled subreflector motion, wind loading, bulk motion of the antenna as it rolled over irregularities in its azimuth ring, etc.). This antenna mechanical noise has seemed irreducible since it is not clear how to build a large, moving, steel structure with intrinsic mechanical stability better than that of current tracking stations. Here we show how intrinsic mechanical noise of a large tracking antenna can be suppressed when two-way Doppler tracking data and receive-only Doppler data from a stiffer antenna are combined with suitable delays. Using this time delay correction procedure, the mechanical noise in the final Doppler observable can be reduced to that of the stiffer antenna. We demonstrate proof-of-concept experimentally and briefly discuss some practical considerations. C1 [Armstrong, J. W.; Estabrook, F. B.; Asmar, S. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Iess, L.] Univ Roma La Sapienza, Dipartimento Ingn Aerosp & Astronaut, I-00184 Rome, Italy. [Tortora, P.] Univ Bologna, DIEM Fac Ingn 2, I-47110 Forli, Italy. RP Armstrong, JW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM john.w.armstrong@jpl.nasa.gov RI IESS, Luciano/F-4902-2011; Tortora, Paolo/J-6191-2012 OI IESS, Luciano/0000-0002-6230-5825; Tortora, Paolo/0000-0001-9259-7673 NR 19 TC 4 Z9 4 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0048-6604 J9 RADIO SCI JI Radio Sci. PD JUN 28 PY 2008 VL 43 IS 3 AR RS3010 DI 10.1029/2007RS003766 PG 7 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications GA 321OL UT WOS:000257315900001 ER PT J AU Lyatsky, W Khazanov, GV AF Lyatsky, Wladislaw Khazanov, George V. TI A new polar magnetic index of geomagnetic activity SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID SOLAR-WIND; CAP INDEX; MAGNETOSPHERE; IONOSPHERE AB We developed a new polar magnetic (PM) index of geomagnetic activity which, similarly to the existing polar cap index, was computed from magnetic field data from near-pole geomagnetic observatories. However, we used a different method for its calculation, which provided the high correlation of this index with both solar wind data and many events in geospace environment. This improves significantly the reliability of forecasting geomagnetic disturbances and such key parameters as cross-polar-cap voltage and Joule heating in high-latitude ionosphere, which play an important role in the development of global geomagnetic, ionospheric, and thermospheric disturbances. In this paper, we examined PM index in the Northern Hemisphere only. We tested the PM index for 10-year period. The correlation between PM index and upstream solar wind data for all these years is very high (the squared correlation coefficient R(2) approximate to 0.74 which corresponds to the linear correlation coefficients R approximate to 0.86). The PM index also shows the high correlation with the cross-polar-cap voltage and hemispheric Joule heating (the squared correlation coefficient R 2 between the actual and predicted values of these parameters reaches similar to 0.81 which corresponds to the linear correlation coefficients R approximate to 0.9), which results in significant increasing the prediction reliability of these parameters. Thus, the polar magnetic (PM) index of geomagnetic activity provides a significant increase in the forecasting reliability of geomagnetic disturbances and related events in geospace environment, and it may be used as an important input parameter in modeling ionospheric, magnetospheric, and thermospheric processes. C1 [Lyatsky, Wladislaw; Khazanov, George V.] NASA, George C Marshall Space Flight Ctr, Space Plasma Grp, Huntsville, AL 35805 USA. [Lyatsky, Wladislaw] Oak Ridge Associated Univ, Oak Ridge, TN USA. RP Lyatsky, W (reprint author), NASA, George C Marshall Space Flight Ctr, Space Plasma Grp, 320 Sparkman Dr, Huntsville, AL 35805 USA. EM lyatsky@cspar.uah.edu NR 25 TC 5 Z9 5 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD JUN 28 PY 2008 VL 6 IS 6 AR S06002 DI 10.1029/2007SW000382 PG 10 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 321OO UT WOS:000257316400001 ER PT J AU Gille, J Barnett, J Arter, P Barker, M Bernath, P Boone, C Cavanaugh, C Chow, J Coffey, M Craft, J Craig, C Dials, M Dean, V Eden, T Edwards, DP Francis, G Halvorson, C Harvey, L Hepplewhite, C Khosravi, R Kinnison, D Krinsky, C Lambert, A Lee, H Lyjak, L Loh, J Mankin, W Massie, S McInerney, J Moorhouse, J Nardi, B Packman, D Randall, C Reburn, J Rudolf, W Schwartz, M Serafin, J Stone, K Torpy, B Walker, K Waterfall, A Watkins, R Whitney, J Woodard, D Young, G AF Gille, John Barnett, John Arter, Philip Barker, Marion Bernath, Peter Boone, Chris Cavanaugh, Charles Chow, Jonathan Coffey, Michael Craft, James Craig, Cheryl Dials, Michael Dean, Vincil Eden, Thomas Edwards, D. P. Francis, Gene Halvorson, Chris Harvey, Lynn Hepplewhite, Christopher Khosravi, Rashid Kinnison, Douglas Krinsky, Charles Lambert, Alyn Lee, Hyunah Lyjak, Lawrence Loh, Joanne Mankin, William Massie, Steven McInerney, Joseph Moorhouse, Joseph Nardi, Bruno Packman, Daniel Randall, Cora Reburn, Jolyon Rudolf, Wayne Schwartz, Michael Serafin, John Stone, Kenneth Torpy, Brendan Walker, Kaley Waterfall, Alison Watkins, Robert Whitney, John Woodard, Douglas Young, Gregory TI High Resolution Dynamics Limb Sounder: Experiment overview, recovery, and validation of initial temperature data SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID PRE-LAUNCH CALIBRATION; HIRDLS FLIGHT INSTRUMENT; RADIANCE MEASUREMENTS; AURA; STRATOSPHERE; INVERSION; SPACE AB The High Resolution Dynamics Limb Sounder (HIRDLS) experiment was designed to provide global temperature and composition data on the region from the upper troposphere to the mesopause with vertical and horizontal resolution not previously available. The science objectives are the study of small-scale dynamics and transports, including stratosphere-troposphere exchange, upper troposphere/lower stratosphere chemistry, aerosol, cirrus and PSC distributions, and gravity waves. The instrument features 21 channels, low noise levels, high vertical resolution, and a mechanical cooler for long life. During launch most of the optical aperture became obscured, so that only a potion of an optical beam width at a large azimuth from the orbital plane on the side away from the Sun can see the atmosphere. Irrecoverable loss of capabilities include limitation of coverage to the region 65 degrees S-82 degrees N and inability to obtain longitudinal resolution finer than an orbital spacing. While this optical blockage also impacted radiometric performance, extensive effort has gone into developing corrections for the several effects of the obstruction, so that radiances from some of the channels can be put into retrievals for temperature. Changes were also necessary for the retrieval algorithm. The validation of the resulting temperature retrievals is presented to demonstrate the effectiveness of these corrections. The random errors range from similar to 0.5 K at 20 km to similar to 1.0 at 60 km, close to those predicted. Comparisons with high-resolution radiosondes, lidars, ACE-FTS, and ECMWF analyses give a consistent picture of HIRDLS temperatures being 1-2 K warm from 200 to 10 hPa and within +/- 2 K of standards from 200 to 2 hPa (but warmer in the region of the tropical tropopause), above which HIRDLS appears to be cold. Comparisons show that both COSMIC and HIRDLS can see small vertical features down to about 2 km wavelength. While further improvements in the data are expected, these data will allow HIRDLS to provide important support toward reaching the Aura objectives. C1 [Gille, John; Craft, James; Dean, Vincil; Krinsky, Charles; Loh, Joanne; McInerney, Joseph; Torpy, Brendan; Young, Gregory] Univ Colorado, Ctr Limb Atmospher Sounding, Boulder, CO 80309 USA. [Barker, Marion; Craft, James; Rudolf, Wayne; Serafin, John] Lockheed Martin Adv Technol Ctr, Palo Alto, CA 94304 USA. [Barnett, John; Hepplewhite, Christopher; Moorhouse, Joseph; Watkins, Robert; Whitney, John] Univ Oxford, Dept Phys, Oxford OX1 3PU, England. [Bernath, Peter] Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. [Boone, Chris] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. [Cavanaugh, Charles; Coffey, Michael; Craig, Cheryl; Eden, Thomas; Edwards, D. P.; Francis, Gene; Halvorson, Chris; Khosravi, Rashid; Kinnison, Douglas; Lambert, Alyn; Mankin, William; Massie, Steven; Nardi, Bruno; Packman, Daniel] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Dials, Michael] Ball Aerosp & Technol Corp, Boulder, CO 80301 USA. [Harvey, Lynn; Randall, Cora] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA. [Lyjak, Lawrence] NOAA, Natl Weather Serv, Silver Spring, MD 20910 USA. [Reburn, Jolyon] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Schwartz, Michael] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Stone, Kenneth] ERT Inc, Aurora, CO 80011 USA. [Walker, Kaley] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. RP Gille, J (reprint author), Univ Colorado, Ctr Limb Atmospher Sounding, Boulder, CO 80309 USA. EM gille@ucar.edu RI Bernath, Peter/B-6567-2012; Schwartz, Michael/F-5172-2016; Randall, Cora/L-8760-2014 OI Bernath, Peter/0000-0002-1255-396X; Schwartz, Michael/0000-0001-6169-5094; Randall, Cora/0000-0002-4313-4397 NR 34 TC 82 Z9 82 U1 1 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 27 PY 2008 VL 113 IS D16 AR D16S43 DI 10.1029/2007JD008824 PG 23 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 321NB UT WOS:000257311200001 ER PT J AU Bass, DS Talley, KP AF Bass, Deborah S. Talley, Kevin P. TI Phoenix surface mission operations processes SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article AB We present an overview of Phoenix Mars Scout Mission (Phoenix) surface operations process design with an emphasis on the science portion of the process. We describe the drivers and constraints on Phoenix operations and the resulting choices that the development team made to accommodate these constraints. The two most important drivers on Phoenix operations are the choice of orbiter relay only for data and the limited amount of data storage on the lander. These two combine to regulate the amount of data the spacecraft can collect, save, and transmit on any given sol. We discuss the interplay between the daily (tactical) and long-term/multiday (strategic) processes and finish with lessons learned for future mission operations design. Integration of mostly complete engineering requirements toward the front end of the tactical process, as well as the multiday nature of science acquisition, results in particular design decisions that have not been incorporated in previous ground operations planning. C1 [Bass, Deborah S.; Talley, Kevin P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bass, DS (reprint author), CALTECH, Jet Prop Lab, Mail Stop 264-623, Pasadena, CA 91109 USA. EM deborah.bass@jpl.nasa.gov NR 1 TC 4 Z9 4 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUN 26 PY 2008 VL 113 AR E00A06 DI 10.1029/2007JE003051 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321NV UT WOS:000257313500003 ER PT J AU Fleischer, I Klingelhofer, G Schroder, C Morris, RV Hahn, M Rodionov, D Gellert, R de Souza, PA AF Fleischer, I. Klingelhoefer, G. Schroeder, C. Morris, R. V. Hahn, M. Rodionov, D. Gellert, R. de Souza, P. A. TI Depth selective Mossbauer spectroscopy: Analysis and simulation of 6.4 keV and 14.4 keV spectra obtained from rocks at Gusev Crater, Mars, and layered laboratory samples SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID SPIRIT ROVER; MIMOS-II; SPECTROMETER; HEMATITE; SOILS; MINERALOGY; ELECTRONS; IMPACT; CEMS AB The miniaturized Mossbauer spectrometer (MIMOS) II Mossbauer spectrometers on the Mars Exploration Rovers (MER) simultaneously obtained 6.4 keV and 14.4 keV Mossbauer spectra from rock and soil targets. Because photons with lower energy have a shallower penetration depth, 6.4 keV spectra contain more mineralogical information about the near-surface region of a sample than do 14.4 keV spectra. The influence of surface layers of varying composition and thickness on Mossbauer spectra was investigated by Monte Carlo simulation and by measurement using a copy of the MER MIMOS II instrument and samples with one or two layers of known thicknesses. Thin sections of minerals or metallic Fe foil on top of a thick mineral sample were used to produce samples with thin layers of known thickness on a thick substrate. Monte Carlo simulation of MER spectra obtained on the rock Mazatzal, which displays a coating on a basaltic substrate, and other Adirondack Class rocks results in a calculated thickness of 10 mm for the Mazatzal surface layer. The 6.4 keV spectra obtained on Adirondack Class rocks, on laboratory samples, and in Monte Carlo calculations show an apparent olivine enrichment which is not related to any observable surface layer. C1 [Fleischer, I.; Klingelhoefer, G.; Hahn, M.; Rodionov, D.] Johannes Gutenberg Univ Mainz, Inst Anorgan & Analyt Chem, D-55128 Mainz, Germany. [Schroeder, C.; Morris, R. V.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Rodionov, D.] Space Res Inst IKI, Moscow 117997, Russia. [Gellert, R.] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada. [de Souza, P. A.] Vallourec Res Ctr, Aulnoye Aymeries, France. RP Fleischer, I (reprint author), Johannes Gutenberg Univ Mainz, Inst Anorgan & Analyt Chem, D-55128 Mainz, Germany. EM fleischi@uni-mainz.de RI de Souza, Paulo/B-8961-2008; Schroder, Christian/B-3870-2009; Centre, TasICT/D-1212-2011 OI de Souza, Paulo/0000-0002-0091-8925; Schroder, Christian/0000-0002-7935-6039; NR 44 TC 12 Z9 12 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUN 26 PY 2008 VL 113 IS E6 AR E06S21 DI 10.1029/2007JE003022 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321NT UT WOS:000257313300001 ER PT J AU Pathak, J Michelangeli, DV Komguem, L Whiteway, J Tamppari, LK AF Pathak, Jagruti Michelangeli, Diane V. Komguem, Leonce Whiteway, James Tamppari, Leslie K. TI Simulating Martian boundary layer water ice clouds and the lidar measurements for the Phoenix mission SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID T-MATRIX METHOD; MARS-PATHFINDER; DUST; AEROSOLS; LANDER; MODEL; SCATTERERS; IMAGER AB Diurnal variation of ground fog and water ice cloud formation at the NASA Phoenix lander site is investigated using a one-dimensional Mars Microphysical Model (MMM) coupled with the results from the one-dimensional University of Helsinki atmospheric boundary layer (ABL) model. Phoenix is scheduled to reach Mars in May 2008 and land in the northern plains ( 65 degrees-72 degrees N). Observations from Mars Global Surveyor Thermal Emission Spectrometer for the proposed landing site and season L(s) = 76 degrees-125 degrees have been used for the model initialization, both in the ABL and MMM. The diurnal variations of temperature and eddy diffusion coefficients produced by the uncoupled ABL are then applied to the MMM. Extinction and backscattering coefficients and lidar ratios are presented for the simulated dust and water ice clouds at the Phoenix location. Results of the dust and ice clouds are then used to simulate the Phoenix lidar measurements at two wavelengths, 532 and 1064 nm. C1 [Pathak, Jagruti; Michelangeli, Diane V.; Komguem, Leonce; Whiteway, James] York Univ, Dept Earth & Space Sci & Engn, N York, ON M3J 1P3, Canada. [Tamppari, Leslie K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Pathak, J (reprint author), York Univ, Dept Earth & Space Sci & Engn, 4700 Keele St, N York, ON M3J 1P3, Canada. EM jagruti@yorku.ca NR 27 TC 9 Z9 9 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUN 26 PY 2008 VL 113 AR E00A05 DI 10.1029/2007JE002967 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321NV UT WOS:000257313500001 ER PT J AU Chandler, D Chapman, C Morrison, D Shoemaker, C Schweickart, R Ostro, S Marsden, B Gehrels, T Milani, A AF Chandler, David Chapman, Clark Morrison, David Shoemaker, Carolyn Schweickart, Rusty Ostro, Steve Marsden, Brian Gehrels, Tom Milani, Andrea TI Planetary science: The burger bar that saved the world SO NATURE LA English DT Editorial Material C1 [Chapman, Clark] SW Res Inst, Boulder, CO USA. [Morrison, David] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ostro, Steve] NASA, Jet Prop Lab, Pasadena, CA USA. [Marsden, Brian] Int Astron Unions Minor Planet Ctr, Cambridge, MA USA. [Gehrels, Tom] Univ Arizona, Tucson, AZ USA. [Milani, Andrea] Univ Pisa, Pisa, Italy. NR 0 TC 0 Z9 0 U1 0 U2 4 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JUN 26 PY 2008 VL 453 IS 7199 BP 1164 EP 1168 DI 10.1038/4531164a PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 318FA UT WOS:000257075800014 PM 18580921 ER PT J AU Andrews-Hanna, JC Zuber, MT Banerdt, WB AF Andrews-Hanna, Jeffrey C. Zuber, Maria T. Banerdt, W. Bruce TI The Borealis basin and the origin of the martian crustal dichotomy SO NATURE LA English DT Article ID INTERNAL STRUCTURE; MANTLE CONVECTION; GIANT IMPACTS; MARS; EVOLUTION; TOPOGRAPHY AB The most prominent feature on the surface of Mars is the near-hemispheric dichotomy between the southern highlands and northern lowlands. The root of this dichotomy is a change in crustal thickness along an apparently irregular boundary, which can be traced around the planet, except where it is presumably buried beneath the Tharsis volcanic rise(1,2). The isostatic compensation of these distinct provinces(2,3) and the ancient population of impact craters buried beneath the young lowlands surface(4) suggest that the dichotomy is one of the most ancient features on the planet(3). However, the origin of this dichotomy has remained uncertain, with little evidence to distinguish between the suggested causes: a giant impact(5,6) or mantle convection/ overturn(7-9). Here we use the gravity(10) and topography(11) of Mars to constrain the location of the dichotomy boundary beneath Tharsis, taking advantage of the different modes of compensation for Tharsis and the dichotomy to separate their effects. We find that the dichotomy boundary along its entire path around the planet is accurately fitted by an ellipse measuring approximately 10,600 by 8,500 km, centred at 67 degrees N, 208 degrees E. We suggest that the elliptical nature of the crustal dichotomy is most simply explained by a giant impact, representing the largest such structure thus far identified in the Solar System. C1 [Andrews-Hanna, Jeffrey C.; Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Banerdt, W. Bruce] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Andrews-Hanna, JC (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM jhanna@mit.edu NR 34 TC 114 Z9 114 U1 1 U2 17 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JUN 26 PY 2008 VL 453 IS 7199 BP 1212 EP U27 DI 10.1038/nature07011 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 318FA UT WOS:000257075800036 PM 18580944 ER PT J AU Read, KA Mahajan, AS Carpenter, LJ Evans, MJ Faria, BVE Heard, DE Hopkins, JR Lee, JD Moller, SJ Lewis, AC Mendes, L McQuaid, JB Oetjen, H Saiz-Lopez, A Pilling, MJ Plane, JMC AF Read, Katie A. Mahajan, Anoop S. Carpenter, Lucy J. Evans, Mathew J. Faria, Bruno V. E. Heard, Dwayne E. Hopkins, James R. Lee, James D. Moller, Sarah J. Lewis, Alastair C. Mendes, Luis McQuaid, James B. Oetjen, Hilke Saiz-Lopez, Alfonso Pilling, Michael J. Plane, John M. C. TI Extensive halogen-mediated ozone destruction over the tropical Atlantic Ocean SO NATURE LA English DT Article ID MARINE BOUNDARY-LAYER; TROPOSPHERIC CHEMISTRY; BROMINE CHEMISTRY; MODEL; SIMULATION; BRO; OH AB Increasing tropospheric ozone levels over the past 150 years have led to a significant climate perturbation(1); the prediction of future trends in tropospheric ozone will require a full understanding of both its precursor emissions and its destruction processes. A large proportion of tropospheric ozone loss occurs in the tropical marine boundary layer(2,3) and is thought to be driven primarily by high ozone photolysis rates in the presence of high concentrations of water vapour. A further reduction in the tropospheric ozone burden through bromine and iodine emitted from open- ocean marine sources has been postulated by numerical models(4-7), but thus far has not been verified by observations. Here we report eight months of spectroscopic measurements at the Cape Verde Observatory indicative of the ubiquitous daytime presence of bromine monoxide and iodine monoxide in the tropical marine boundary layer. A year- round data set of co- located in situ surface trace gas measurements made in conjunction with low- level aircraft observations shows that the mean daily observed ozone loss is similar to 50 per cent greater than that simulated by a global chemistry model using a classical photochemistry scheme that excludes halogen chemistry. We perform box model calculations that indicate that the observed halogen concentrations induce the extra ozone loss required for the models to match observations. Our results show that halogen chemistry has a significant and extensive influence on photochemical ozone loss in the tropical Atlantic Ocean boundary layer. The omission of halogen sources and their chemistry in atmospheric models may lead to significant errors in calculations of global ozone budgets, tropospheric oxidizing capacity and methane oxidation rates, both historically and in the future. C1 [Read, Katie A.; Carpenter, Lucy J.; Moller, Sarah J.] Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. [Mahajan, Anoop S.; Heard, Dwayne E.; Oetjen, Hilke; Pilling, Michael J.; Plane, John M. C.] Univ Leeds, Sch Chem, Leeds LS2 9JT, W Yorkshire, England. [Evans, Mathew J.; McQuaid, James B.] Univ Leeds, SEE, Leeds LS2 9JT, W Yorkshire, England. [Faria, Bruno V. E.; Mendes, Luis] INMG, Mindelo, Cape Verde. [Hopkins, James R.; Lee, James D.; Lewis, Alastair C.] Univ York, NCAS, York YO10 5DD, N Yorkshire, England. [Saiz-Lopez, Alfonso] CALTECH, Jet Prop Lab, Div Earth & Space Sci, Pasadena, CA 91109 USA. RP Carpenter, LJ (reprint author), Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. EM ljc4@york.ac.uk; j.m.c.plane@leeds.ac.uk RI McQuaid, Jim/C-7450-2011; Mahajan, Anoop/D-2714-2012; Evans, Mathew/A-3886-2012; Carpenter, Lucy/E-6742-2013; Mason, Robert/A-6829-2011; Saiz-Lopez, Alfonso/B-3759-2015; Lewis, Alastair/A-6721-2008; Plane, John/C-7444-2015; Oetjen, Hilke/H-3708-2016 OI Carpenter, Lucy/0000-0002-6257-3950; Heard, Dwayne/0000-0002-0357-6238; McQuaid, Jim/0000-0001-8702-0415; Mahajan, Anoop/0000-0002-2909-5432; Evans, Mathew/0000-0003-4775-032X; Saiz-Lopez, Alfonso/0000-0002-0060-1581; Lewis, Alastair/0000-0002-4075-3651; Plane, John/0000-0003-3648-6893; Oetjen, Hilke/0000-0002-3542-1337 NR 26 TC 202 Z9 203 U1 7 U2 90 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD JUN 26 PY 2008 VL 453 IS 7199 BP 1232 EP 1235 DI 10.1038/nature07035 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 318FA UT WOS:000257075800041 PM 18580948 ER PT J AU Luo, YL Xu, KM Morrison, H McFarquhar, GM Wang, Z Zhang, G AF Luo, Yali Xu, Kuan-Man Morrison, Hugh McFarquhar, Greg M. Wang, Zhien Zhang, Gong TI Multi-layer arctic mixed-phase clouds simulated by a cloud-resolving model: Comparison with ARM observations and sensitivity experiments SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID ATMOSPHERIC RADIATION; STRATUS CLOUDS; NUMERICAL-SIMULATION; AEROSOL ACTIVATION; STRATIFORM CLOUDS; BOUNDARY-LAYER; ICE PARTICLES; BEAUFORT SEA; PARAMETERIZATION; CLIMATE AB A cloud-resolving model (CRM) is used to simulate the multiple-layer mixed-phase stratiform (MPS) clouds that occurred during a three-and-a-half day subperiod of the Department of Energy-Atmospheric Radiation Measurement Program's Mixed-Phase Arctic Cloud Experiment (M-PACE) and to examine physical processes responsible for multilayer production and evolution. The CRM with a two-moment cloud microphysics is initialized with concurrent meteorological, aerosol, and ice nucleus measurements and is driven by time-varying large-scale advective tendencies of temperature and moisture and surface sensible and latent heat fluxes. The CRM reproduces the dominant occurrences of the single- and double-layer MPS clouds as revealed by the M-PACE observations although the simulated first cloud layer is lower and the second cloud layer is thicker compared to observations. The aircraft measurements suggest that the CRM qualitatively captures the major characteristics in the vertical distribution and interperiod variation of liquid water content (LWC), droplet number concentration, total ice water content (IWC), and ice crystal number concentration (n(is)). However, the magnitude of LWC is overestimated and those of IWC and nis are underestimated. In particular, the simulated n(is) is one order of magnitude smaller than the observed. Sensitivity experiments suggest that both the surface fluxes and large-scale advection control the formation of the lower cloud layer while the large-scale advection initiates the formation of the upper cloud layer but the maintenance of multilayer structures relies on the longwave (LW) radiative effect. The LW cooling near cloud top produces a more saturated environment and a stronger dynamical circulation while cloud base radiative warming of the upper layer creates the stability gap between the two cloud layers. Both cloud layers are sensitive to ice-forming nuclei number concentration since ice-phase microphysics provides a strong sink of cloud liquid water mass. C1 [Luo, Yali] Chinese Acad Meteorol Sci, State Key Lab Severe Weather, Beijing 100081, Peoples R China. [McFarquhar, Greg M.; Zhang, Gong] Univ Illinois, Dept Atmospher Sci, Urbana, IL 61801 USA. [Morrison, Hugh] Natl Ctr Atmospher Res, MMM, Boulder, CO 80307 USA. [Wang, Zhien] Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82071 USA. [Xu, Kuan-Man] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA. RP Luo, YL (reprint author), Chinese Acad Meteorol Sci, State Key Lab Severe Weather, 46 Zhong Guan Cun S Ave, Beijing 100081, Peoples R China. EM yali@cams.cma.gov.cn RI Wang, Zhien/F-4857-2011; Xu, Kuan-Man/B-7557-2013; OI Xu, Kuan-Man/0000-0001-7851-2629; McFarquhar, Greg/0000-0003-0950-0135 NR 55 TC 16 Z9 16 U1 0 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 25 PY 2008 VL 113 IS D12 AR D12208 DI 10.1029/2007JD009563 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 321MQ UT WOS:000257309700006 ER PT J AU Santee, ML MacKenzie, IA Manney, GL Chipperfield, MP Bernath, PF Walker, KA Boone, CD Froidevaux, L Livesey, NJ Waters, JW AF Santee, M. L. MacKenzie, I. A. Manney, G. L. Chipperfield, M. P. Bernath, P. F. Walker, K. A. Boone, C. D. Froidevaux, L. Livesey, N. J. Waters, J. W. TI A study of stratospheric chlorine partitioning based on new satellite measurements and modeling SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Review ID CHEMICAL-TRANSPORT MODEL; HALOGEN OCCULTATION EXPERIMENT; ATMOSPHERIC TRACE GASES; ARCTIC WINTER 2002/2003; POLAR VORTEX; OZONE LOSS; FTIR MEASUREMENTS; CLO DIMER; SOUTHERN-HEMISPHERE; ANTARCTIC VORTEX AB Two recent satellite instruments, the Microwave Limb Sounder (MLS) on Aura and the Atmospheric Chemistry Experiment Fourier Transform Spectrometer (ACE-FTS) on SCISAT-1, provide an unparalleled opportunity to investigate stratospheric chlorine partitioning. We use measurements of ClO, HCl, ClONO2, and other species from MLS and ACE-FTS to study the evolution of reactive and reservoir chlorine throughout the lower stratosphere during two Arctic and two Antarctic winters characterizing both relatively cold and relatively warm and disturbed conditions in each hemisphere. At middle latitudes, and at high latitudes at the beginning of winter, HCl greatly exceeds ClONO2, representing similar to 0.7-0.8 of estimated total inorganic chlorine. Nearly complete chlorine activation is seen inside the winter polar vortices. In the Arctic, chlorine recovery follows different paths in the two winters: In 2004/2005, deactivation initially takes place through reformation of ClONO2, then both reservoirs are produced concurrently but ClONO2 continues to significantly exceed HCl, and finally slow repartitioning between ClONO2 and HCl occurs; in 2005/2006, HCl and ClONO2 rise at comparable rates in some regions. In the Antarctic, chlorine deactivation proceeds in a similar manner in both winters, with a rapid rise in HCl accompanying the decrease in ClO. The measurements are compared to customized runs of the SLIMCAT three-dimensional chemical transport model. Measured and modeled values typically agree well outside the winter polar regions. In contrast, partly because of the equilibrium scheme used to parameterize polar stratospheric clouds, the model overestimates the magnitude, spatial extent, and duration of chlorine activation inside the polar vortices. C1 [Santee, M. L.; Manney, G. L.; Froidevaux, L.; Livesey, N. J.; Waters, J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [MacKenzie, I. A.] Univ Edinburgh, Sch Geosci, Edinburgh EH9 3JN, Midlothian, Scotland. [Chipperfield, M. P.] Univ Leeds, Sch Environm, Leeds LS2 9JT, W Yorkshire, England. [Bernath, P. F.; Boone, C. D.] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. RP Santee, ML (reprint author), CALTECH, Jet Prop Lab, Mail Stop 183-701,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mls@mls.jpl.nasa.gov RI Bernath, Peter/B-6567-2012; mackenzie, ian/E-9320-2013; Chipperfield, Martyn/H-6359-2013 OI Bernath, Peter/0000-0002-1255-396X; Chipperfield, Martyn/0000-0002-6803-4149 NR 116 TC 49 Z9 49 U1 4 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 25 PY 2008 VL 113 IS D12 AR D12307 DI 10.1029/2007JD009057 PG 25 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 321MQ UT WOS:000257309700001 ER PT J AU Milkovich, SM Plaut, JJ AF Milkovich, Sarah M. Plaut, Jeffrey J. TI Martian South Polar Layered Deposit stratigraphy and implications for accumulation history SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID ASTRONOMICAL THEORY; MARS; MISSION; AGES AB We examine the stratigraphy of the Martian South Polar Layered Deposits (SPLD) exposed on scarp walls throughout the deposit using THEMIS visible (17 m/pxl) images from the Mars Odyssey spacecraft. By correlating marker layers and packets of layers among multiple locations, we are able to identify three sequences of layers within the SPLD, each with a different areal extent. While certain layers are correlatable over hundreds of km, implying widespread deposition of polar material, the absence of several identified layer sequences in some regions, notably the Promethei Lingula region, as well as the presence of several unconformities, indicates that deposition and sublimation or erosion of these deposits has not been uniform around the SPLD. This is further supported by the fact that individual layers display variations in thickness greater than a factor of 4 over hundreds of kilometers. Using these observations we propose an internal structure for the SPLD, with individual layers roughly following a dome-like shape toward the center of the deposit, and becoming more planar toward the margins. We infer that the SPLD underwent at least three major periods of layer accumulation; each period is distinguished by a change in areal extent of net accumulation. The changes in areal extent of the layer sequences may be due to changes in Martian climate causing episodes of significant erosion of the SPLD between the deposition of each sequence or causing wide variations in accumulation zones of the SPLD over the history of these deposits. C1 [Milkovich, Sarah M.; Plaut, Jeffrey J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Milkovich, SM (reprint author), CALTECH, Jet Prop Lab, M-S 183-501,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM sarah.m.milkovich@jpl.nasa.gov NR 31 TC 13 Z9 13 U1 2 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 JUN 25 PY 2008 VL 113 IS E6 AR E06007 DI 10.1029/2007JE002987 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321NS UT WOS:000257313200002 ER PT J AU Malone, CP Johnson, PV McConkey, JW Kanik, I AF Malone, C. P. Johnson, P. V. McConkey, J. W. Kanik, I. TI Cross sections for the OII (83.4 nm) emission from electron impact on O-2 SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ATOMIC OXYGEN; DISSOCIATIVE EXCITATION; EXTREME ULTRAVIOLET; MOLECULAR-HYDROGEN; O-I; TRANSITION; ATMOSPHERE; RADIATION; EUV; PHOTOEMISSION AB Vacuum ultraviolet emissions resulting from electron impact on O-2 have been studied at 100, 200, and 300 eV. The ratio of the 83.4 nm and 130.4 nm emissions were used in combination with the recently revised recommendation of the OI (130.4 nm) cross section to determine the O II (83.4 nm) cross sections. The present results are compared with existing measurements and resolve the controversy that has existed regarding the magnitude and shape of the 83.4nm emission cross section. We recommend an O II (83.4 nm) emission cross section of (1.50 +/- 0.17) x 10(-18) cm(2) at 100 eV. C1 [Malone, C. P.; Johnson, P. V.; McConkey, J. W.; Kanik, I.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [McConkey, J. W.] Univ Windsor, Dept Phys, Windsor, ON N9B 3P4, Canada. RP Malone, CP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Johnson, Paul/D-4001-2009; Malone, Charles/A-6294-2010 OI Johnson, Paul/0000-0002-0186-8456; Malone, Charles/0000-0001-8418-1539 NR 42 TC 3 Z9 3 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 JUN 25 PY 2008 VL 113 IS A6 AR A06309 DI 10.1029/2008JA013160 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 321OD UT WOS:000257314700004 ER PT J AU Singh, M Shpargel, TP Asthana, R AF Singh, M. Shpargel, T. P. Asthana, R. TI Braze oxidation behavior and joint microstructure in YSZ/steel joints made using palladium brazes for SOFC applications SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES MICROSTRUCTURE AND PROCESSING LA English DT Article DE joining; yttria-stabilized zirconia; palladium brazes; microscopy; oxidation ID SYSTEMS; WETTABILITY; ZIRCONIA; METALS AB Two palladium-base brazes (Palco and Palni), and two silver-base brazes containing palladium as an alloying element (Palcusil-10 and Palcusil-15) were evaluated for oxidation resistance at 750 degrees C, and used in joining yttria-stabilized zirconia (YSZ) to a corrosion-resistant ferritic stainless steel for possible use in solid oxide fuel cell (SOFC) interconnects. Thermogravimetric analysis (TGA), and optical and scanning electron microscopy (SEM) coupled with energy dispersive spectrometry (EDS) were used to evaluate the braze oxidation behavior and the microstructure of the YSZ/braze/steel joints. Knoop microhardness testing was used to develop hardness profiles across the joint region. The TGA results showed that Palco and Palni exhibited the fastest and the slowest oxidation kinetics, respectively, with Palcusil-10 and Palcusil-15 exhibiting oxidation kinetics intermediate between Palco and Palni. The EDS analysis revealed the dissolution of YSZ and steel constituents in braze, and of braze constituents in the YSZ and steel, which led to metallurgically sound joints. The microhardness profiles exhibited a sharper discontinuity at the YSZ/braze interface than at the steel/braze interface, with a peak hardness of similar to 1000 KHN in YSZ and 150-180 KHN in the steel substrate. (C) 2007 Published by Elsevier B.V. C1 [Singh, M.] NASA Glenn Res Ctr, Ohio Aerosp Inst, Cleveland, OH 44135 USA. [Shpargel, T. P.] NASA Glenn Res Ctr, ASRC Aerosp, Cleveland, OH 44135 USA. [Asthana, R.] Univ Wisconsin Stout, Engn & Technol Dept, Menomonie, WI 54751 USA. RP Singh, M (reprint author), NASA Glenn Res Ctr, Ohio Aerosp Inst, Cleveland, OH 44135 USA. EM Mrityunjay.Sing-1@nasa.gov NR 25 TC 14 Z9 14 U1 0 U2 12 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0921-5093 J9 MAT SCI ENG A-STRUCT JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process. PD JUN 25 PY 2008 VL 485 IS 1-2 BP 695 EP 702 DI 10.1016/j.msea.2007.08.032 PG 8 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA 305RA UT WOS:000256194300089 ER PT J AU Sud, YC Walker, GK Zhou, YP Schmidt, GA Lau, KM Cahalan, RF AF Sud, Y. C. Walker, G. K. Zhou, Y. P. Schmidt, Gavin A. Lau, K. -M. Cahalan, Robert F. TI Effects of doubled CO(2) on tropical sea surface temperatures (SSTs) for onset of deep convection and maximum SST: Simulations based inferences SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID CIRRUS-CLOUD THERMOSTAT; INFRARED IRIS; WATER-VAPOR; CLIMATE; OCEAN; REANALYSIS; SATELLITE; FEEDBACK; EARTH AB A primary concern of CO2-induced warming is the associated rise of tropical (10S-10N) sea-surface temperatures (SSTs). GISS Model-E was used to produce two sets of simulations-one with the present-day and one with doubled CO(2) in the atmosphere. The intrinsic usefulness of model guidance in the tropics was confirmed when the model simulated realistic convective coupling between SSTs and atmospheric soundings and that the simulated-data correlations between SSTs and 300 hPa moist-static energies were similar to the observed. Model predicted SST limits for (i) the onset of deep convection and (ii) maximum SST, increased in the doubled CO(2) environment. Changes in cloud heights, cloud frequencies, and cloud mass-fractions showed that convective-cloud changes increased the SSTs, while warmer mixed-layer of the doubled CO(2) contained similar to 10% more water vapor; clearly that would be conducive to more intense storms and hurricanes. C1 [Sud, Y. C.; Lau, K. -M.; Cahalan, Robert F.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Schmidt, Gavin A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Walker, G. K.] Sci Applicat Int Corp, Beltsville, MD 20771 USA. [Zhou, Y. P.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol, Baltimore, MD 21228 USA. RP Sud, YC (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. EM yogesh.c.sud@nasa.gov; gregory.k.walker@nasa.gov; yaping.zhou-1@nasa.gov; gavin.a.schmidt@nasa.gov; william.k.lau@nasa.gov; robert.f.cahalan@nasa.gov RI Schmidt, Gavin/D-4427-2012; Cahalan, Robert/E-3462-2012; Lau, William /E-1510-2012 OI Schmidt, Gavin/0000-0002-2258-0486; Cahalan, Robert/0000-0001-9724-1270; Lau, William /0000-0002-3587-3691 NR 26 TC 9 Z9 9 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 JUN 24 PY 2008 VL 35 IS 12 AR L12707 DI 10.1029/2008GL033872 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 321MB UT WOS:000257308200005 ER PT J AU Coffey, MT Hannigan, JW Goldman, A Kinnison, D Gille, JC Barnett, JJ Froidevaux, L Lambert, A Santee, M Livesey, N Fisher, B Kulawik, SS Beer, R AF Coffey, M. T. Hannigan, J. W. Goldman, A. Kinnison, D. Gille, J. C. Barnett, J. J. Froidevaux, L. Lambert, A. Santee, M. Livesey, N. Fisher, B. Kulawik, S. S. Beer, R. TI Airborne Fourier transform spectrometer observations in support of EOS Aura validation SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID INFRARED SPECTROSCOPIC MEASUREMENTS; HIGH-RESOLUTION; STRATOSPHERIC CONSTITUENTS; ERROR ANALYSIS; TRACE GASES; ANTARCTICA; PROFILES; NO2 AB Nearly coincident observations of HNO3, HCl, N2O, and H2O in the vicinity of the northern polar vortex during the NASA Polar Aura Validation Experiment (PAVE) in January and February 2005 have shown reasonably good agreement between aircraft-borne infrared spectrometer results and results from High Resolution Dynamics Limb Sounder (HIRDLS), Microwave Limb Sounder (MLS), and Tropospheric Emission Spectrometer (TES) instruments aboard the EOS Aura satellite. Mixing ratio profile and column results show that special attention must be given to retrievals that may be disturbed by the dynamics and chemical processing of the polar vortex. Largest differences occur on days when observations were made in regions of the vortex with large gradients in wind and potential vorticity, and the differences were especially noticeable in results for HNO3 and HCl, whose profiles may be dramatically changed by vortex activity. The mean difference between coincident column observations by MLS and the Fourier transform spectrometer (FTS) is 2.4%, VMR profile amounts generally are in good agreement between the satellite observations where they are available. The average difference between coincident HCl column observations by MLS and the FTS is 4.6%. C1 [Coffey, M. T.; Hannigan, J. W.; Kinnison, D.; Gille, J. C.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Barnett, J. J.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England. [Froidevaux, L.; Lambert, A.; Santee, M.; Livesey, N.; Fisher, B.; Kulawik, S. S.; Beer, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Goldman, A.] Univ Denver, Denver, CO 80208 USA. RP Coffey, MT (reprint author), Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. EM coffey@ucar.edu NR 28 TC 5 Z9 5 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 JUN 24 PY 2008 VL 113 IS D16 AR D16S42 DI 10.1029/2007JD008833 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 321NA UT WOS:000257310800001 ER PT J AU Kim, S Zimmerman, JD Focardi, P Gossard, AC Wu, DH Sherwin, MS AF Kim, Sangwoo Zimmerman, Jeramy D. Focardi, Paolo Gossard, Arthur C. Wu, Dong Ho Sherwin, Mark S. TI Room temperature terahertz detection based on bulk plasmons in antenna-coupled GaAs field effect transistors SO APPLIED PHYSICS LETTERS LA English DT Article AB A first generation of antenna-coupled GaAs metal-semiconductor-field-effect-transistors (MESFETs) is fabricated, modeled, and tested for room-temperature terahertz detection. For fixed excitation frequencies between 0.14 and 1 THz, the source-drain current (signal) is monitored as the gate and drain voltages are varied. The signal shows resonances when applied voltages sweep the charge density in the MESFET through values at which the bulk plasmon is resonant with the excitation frequency. For these unoptimized devices, the measured system noise-equivalent power is similar to 5x10(-8) W/Hz(1/2); the electronics-limited response time is 10 ns. (c) 2008 American Institute of Physics. C1 [Kim, Sangwoo; Sherwin, Mark S.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Zimmerman, Jeramy D.; Gossard, Arthur C.] Univ Calif Santa Barbara, Dept Mat, Santa Barbara, CA 93106 USA. [Focardi, Paolo] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wu, Dong Ho] USN, Res Lab, Washington, DC 20375 USA. RP Kim, S (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. EM swkim@physics.ucsb.edu RI Zimmerman, Jeramy/C-2273-2009 OI Zimmerman, Jeramy/0000-0001-8936-5345 NR 12 TC 27 Z9 27 U1 0 U2 2 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD JUN 23 PY 2008 VL 92 IS 25 AR 253508 DI 10.1063/1.2947587 PG 3 WC Physics, Applied SC Physics GA 320KC UT WOS:000257231200088 ER PT J AU Hemmer, MJ Cripe, GM Hemmer, BL Goodman, LR Salinas, KA Fournie, JW Walker, CC AF Hemmer, Michael J. Cripe, Geraldine M. Hemmer, Becky L. Goodman, Larry R. Salinas, Kimberly A. Fournie, John W. Walker, Calvin C. TI Comparison of estrogen-responsive plasma protein biomarkers and reproductive endpoints in sheepshead minnows exposed to 17 beta-trenbolone SO AQUATIC TOXICOLOGY LA English DT Article DE protein profiling; MALDI; androgen; trenbolone; fish; biomarker ID MEDAKA ORYZIAS-LATIPES; ENVIRONMENTALLY RELEVANT CONCENTRATIONS; GROWTH PROMOTER 17-BETA-TRENBOLONE; TROUT ONCORHYNCHUS-MYKISS; ZEBRAFISH DANIO-RERIO; FATHEAD MINNOW; PIMEPHALES-PROMELAS; IN-VIVO; CYPRINODON-VARIEGATUS; GENE-EXPRESSION AB Protein profiling can be used for detection of biomarkers that can be applied diagnostically to screen chemicals for endocrine modifying activity. In previous studies, mass spectral analysis revealed four peptides (2950.5, 2972.5, 3003.4, 3025.5 m/z) in the plasma of estrogen agonist-treated male and gravid female sheepshead minnows (Cyprinodon variegatus, SHM), which served as distinct estrogenic biomarkers. In this study, a 21-day reproductive assay with adult SHM was conducted to investigate possible dose-related effects of the synthetic androgen, 17 beta-trenbolone, on expression of these four estrogen-responsive peptides. In addition, the response of the peptide biomarkers were compared to traditional reproductive endpoints of fecundity, histopathology, secondary sex characteristics, length, weight, hepatosomatic index, female gonadosomatic index and plasma vitellogenin (VTG) levels. Fish were continuously exposed to 0.005, 0.05, and 5.0 mu g/l, a solvent control (triethylene glycol, TEG), and a seawater control (SW) using an intermittent flow-through dosing system. Plasma was analyzed for the presence of the four peptide biomarkers by MALDI-TOF MS and VTG protein by quantitative ELISA. Male fish from the trenbolone treatments and controls showed no expression of the four peptide biomarkers or measurable levels of VTG. The estrogen-responsive biomarkers and plasma VTG were constitutively expressed in females from the SW, TEG, 0.005 and 0.05 mu g/l exposures. All four peptide biomarkers were significantly reduced (p < 0.0002 to p < 0.005) at the 5.0 mu g/l treatment level which corresponded with significant reductions in fecundity and changes in ovarian morphology. A distinct but non-significant reduction in VTG was also observed in female fish from the 5.0 mu g/l treatment. Results of this study suggest application of these estrogen-responsive protein biomarkers may be a cost effective alternative to fecundity measures which are labor intensive and expensive to conduct. Published by Elsevier B.V. C1 [Hemmer, Michael J.; Cripe, Geraldine M.; Hemmer, Becky L.; Goodman, Larry R.; Salinas, Kimberly A.; Fournie, John W.] US EPA, Off Res & Dev, Natl Hlth & Environm Effects Res Lab, Gulf Ecol Div, Gulf Breeze, FL 32561 USA. [Walker, Calvin C.] US Natl Ocean & Atmospher Adm, Natl Marine Fisheries Serv, Pascagoula, MS 39568 USA. RP Hemmer, MJ (reprint author), US EPA, Off Res & Dev, Natl Hlth & Environm Effects Res Lab, Gulf Ecol Div, 1 Sabine Isl Dr, Gulf Breeze, FL 32561 USA. EM hemmer.michael@epa.gov NR 55 TC 17 Z9 18 U1 3 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0166-445X EI 1879-1514 J9 AQUAT TOXICOL JI Aquat. Toxicol. PD JUN 23 PY 2008 VL 88 IS 2 BP 128 EP 136 DI 10.1016/j.aquatox.2008.04.001 PG 9 WC Marine & Freshwater Biology; Toxicology SC Marine & Freshwater Biology; Toxicology GA 322JB UT WOS:000257369900005 PM 18495259 ER PT J AU Wan, W Liu, L Pi, X Zhang, ML Ning, B Xiong, J Ding, F AF Wan, W. Liu, L. Pi, X. Zhang, M. -L. Ning, B. Xiong, J. Ding, F. TI Wavenumber-4 patterns of the total electron content over the low latitude ionosphere SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID NONMIGRATING DIURNAL TIDES; LATENT-HEAT RELEASE; THERMOSPHERE AB The global ionospheric maps (GIMs) produced by JPL are used to investigate the longitudinal structure of the low latitude ionosphere. As a proxy of the ionization parameter at low latitudes, the latitudinally integrated total electron content (ITEC) is first extracted from low latitude GIMs and then Fourier filtered to obtain the wavenumber-4 components. We then study in detail the diurnal, seasonal and solar cycle variations of the wave patterns. It is found that the wavenumber-4 patterns are intense and well developed in boreal summer and early boreal autumn, but quite weak in boreal winter. This seasonal variation is consistent with that of the zonal wind of the non-migrating tide mode DE3. We also found that the wavenumber-4 patterns shift eastward with a shifting speed that is smaller in daytime than at night. This is attributed to the contribution of both the eastward propagation of DE3 in E-region and the zonal E x B ion drifts in F-region. Our results support the suggestion that the longitudinal wavenumber-4 structure of the low latitude ionosphere should be originated from the non-migrating tide mode DE3. C1 [Wan, W.; Liu, L.; Zhang, M. -L.; Ning, B.; Xiong, J.; Ding, F.] Chinese Acad Sci, Inst Geol & Geophys, Beijing 100029, Peoples R China. [Pi, X.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Wan, W (reprint author), Chinese Acad Sci, Inst Geol & Geophys, Beijing 100029, Peoples R China. EM wanw@mail.iggcas.ac.cn RI Liu, Libo/A-2370-2012; Ding, Feng/C-3249-2013 OI Liu, Libo/0000-0001-5773-0184; NR 26 TC 97 Z9 104 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUN 21 PY 2008 VL 35 IS 12 AR L12104 DI 10.1029/2008GL033755 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 317XC UT WOS:000257052700001 ER PT J AU Ichoku, C Martins, JV Kaufman, YJ Wooster, MJ Freeborn, PH Hao, WM Baker, S Ryan, CA Nordgren, BL AF Ichoku, Charles Martins, J. Vanderlei Kaufman, Yoram J. Wooster, Martin J. Freeborn, Patrick H. Hao, Wei Min Baker, Stephen Ryan, Cecily A. Nordgren, Bryce L. TI Laboratory investigation of fire radiative energy and smoke aerosol emissions SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID BIOMASS-BURNING EMISSIONS; OPTICAL-PROPERTIES; PARTICLES; SATELLITE; MODIS; CALIFORNIA; CARBON; GASES AB Fuel biomass samples from southern Africa and the United States were burned in a laboratory combustion chamber while measuring the biomass consumption rate, the fire radiative energy (FRE) release rate (R-fre), and the smoke concentrations of carbon monoxide (CO), carbon dioxide (CO2), and particulate matter (PM). The PM mass emission rate (R-PM) was quantified from aerosol optical thickness (AOT) derived from smoke extinction measurements using a custom-made laser transmissometer. The R-PM and Rfre time series for each fire were integrated to total PM mass and FRE, respectively, the ratio of which represents its FRE-based PM emission coefficient (C-e(PM)). A strong correlation (r(2) = 0.82) was found between the total FRE and total PM mass, from which an average C-e(PM) value of 0.03 kg MJ(-1) was calculated. This value agrees with those derived similarly from satellite-borne measurements of R-fre and AOT acquired over large-scale wildfires. C1 [Ichoku, Charles] NASA, Goddard Space Flight Ctr, Climate & Radiat Branch, Greenbelt, MD 20771 USA. [Martins, J. Vanderlei] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA. [Hao, Wei Min; Baker, Stephen; Ryan, Cecily A.; Nordgren, Bryce L.] US Forest Serv, Fire Sci Lab, Rocky Mt Res Stn, USDA, Missoula, MT 59808 USA. [Wooster, Martin J.; Freeborn, Patrick H.] Kings Coll London, Dept Geog, London WC2R 2LS, England. RP Ichoku, C (reprint author), NASA, Goddard Space Flight Ctr, Climate & Radiat Branch, Code 913,Bldg 33, Greenbelt, MD 20771 USA. EM ichoku@climate.gsfc.nasa.gov RI Ichoku, Charles/E-1857-2012 OI Ichoku, Charles/0000-0003-3244-4549 NR 35 TC 10 Z9 10 U1 1 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 21 PY 2008 VL 113 IS D14 AR D14S09 DI 10.1029/2007JD009659 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 317YL UT WOS:000257056200001 ER PT J AU Petropavlovskikh, I Froidevaux, L Shetter, R Hall, S Ullmann, K Bhartia, PK Kroon, M Levelt, P AF Petropavlovskikh, I. Froidevaux, L. Shetter, R. Hall, S. Ullmann, K. Bhartia, P. K. Kroon, M. Levelt, P. TI In-flight validation of Aura MLS ozone with CAFS partial ozone columns SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID EOS MLS; SATELLITE; BREWER; DOBSON AB A comprehensive data set of partial ozone columns was derived from the charge-coupled device (CCD) Actinic Flux Spectroradiometer (CAFS) measurements taken during the Polar 2005, Houston 2005, and Costa Rica 2006 Aura Validation Experiments (AVE). It was used to validate the colocated daytime Aura Microwave Limb Sounder (MLS) partial ozone columns along the aircraft tracks over diverse geophysical conditions. Results show that the MLS v. 1.5 and CAFS ozone columns agree to better than 3% at pressure levels of 100 and 146 hPa, and to better than 5% at 215 hPa level. The partial ozone column differences between the two systems were the largest during the Polar AVE ( PAVE) 2005 campaign ( polar region, similar to 250 hPa pressure level), and the smallest during the CRAVE 2006 campaign ( tropics, similar to 100 hPa pressure level). Overall, the averaged bias between the MLS and CAFS partial ozone column is about 2%, and the standard deviation of the differences is about 2%. The v. 2.2 update of the MLS data tends to reduce the bias to less than 1%. In addition, the AVE 2005 campaign uncovered an altitude-dependent bias, where the MLS partial ozone columns above 100 and 146 hPa pressure levels were about 1% higher than the CAFS derived columns, while the bias increased to about 3% in partial columns integrated above 215 hPa. However, the MLS and CAFS data track each other closely over a wide range of atmospheric conditions, and the differences lie within the combined uncertainties of the two data sets. C1 [Froidevaux, L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Shetter, R.; Hall, S.; Ullmann, K.] NCAR, ESSL, Div Atmospher Chem, Boulder, CO 80303 USA. [Bhartia, P. K.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Greenbelt, MD 20771 USA. [Kroon, M.; Levelt, P.] Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands. [Petropavlovskikh, I.] Univ Colorado, NOAA, Cooperat Inst Res Environm Sci, ESRL,GMD, Boulder, CO 80309 USA. RP Petropavlovskikh, I (reprint author), Univ Colorado, NOAA, Cooperat Inst Res Environm Sci, ESRL,GMD, Boulder, CO 80309 USA. EM irina.petro@noaa.gov RI Bhartia, Pawan/A-4209-2016 OI Bhartia, Pawan/0000-0001-8307-9137 NR 25 TC 4 Z9 4 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 21 PY 2008 VL 113 IS D16 AR D16S41 DI 10.1029/2007JD008690 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 317YP UT WOS:000257056600001 ER PT J AU Coe, MJ Schurch, M Corbet, RHD Galache, J McBride, VA Townsend, LJ Udalski, A AF Coe, M. J. Schurch, M. Corbet, R. H. D. Galache, J. McBride, V. A. Townsend, L. J. Udalski, A. TI An optical and X-ray study of the counterpart to the Small Magellanic Cloud X-ray binary pulsar system SXP327 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars : neutron; X-rays : binaries ID CATALOG; SMC AB Optical and X-ray observations are presented here of a newly reported X-ray transient system in the Small Magellanic Cloud. The data reveal many previously unknown X-ray detections of this system and clear evidence for a 45.99 d binary period. In addition, the optical photometry shows recurring outburst features at the binary period which may be well indicative of the neutron star interacting with a circumstellar disc around a Be star. C1 [Coe, M. J.; Schurch, M.; McBride, V. A.; Townsend, L. J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Corbet, R. H. D.] Univ Maryland, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Galache, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Udalski, A.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Coe, MJ (reprint author), Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. EM m.j.coe@soton.ac.uk NR 17 TC 7 Z9 7 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 21 PY 2008 VL 387 IS 2 BP 724 EP 728 DI 10.1111/j.1365-2966.2008.13257.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 312RO UT WOS:000256688700018 ER PT J AU Georgiev, GT Butler, JJ AF Georgiev, Georgi T. Butler, James J. TI Laboratory-based bidirectional reflectance distribution functions of radiometric tarps SO APPLIED OPTICS LA English DT Article ID CALIBRATION; SPECTRALON AB Laboratory-based bidirectional reflectance distribution functions (BRDFs) of radiometric tarp samples used in the vicarious calibration of Earth remote sensing satellite instruments are presented in this paper. The results illustrate the BRDF dependence on the orientation of the tarps' weft and warp threads. The study was performed using the GSFC scatterometer at incident zenith angles of 0 degrees, 10 degrees, and 30 degrees; scatter zenith angles from 0 degrees to 60 degrees; and scatter azimuth angles of 0 degrees, 45 degrees, 90 degrees, 135 degrees, and 180 degrees. The wavelengths were 485 nm, 550 nm, 633 nm, and 800 nm. The tarp's weft and warp dependence on BRDF is well defined at all measurement geometries and wavelengths. The BRDF difference can be as high as 8% at 0 degrees incident angle and 12% at 30 degrees incident angle. The fitted BRDF data show a very small discrepancy from the measured ones. New data on the forward and backscatter properties of radiometric tarps are reported. The backward scatter is well pronounced for the white samples. The black sample has well-pronounced forward scatter. The provided BRDF characterization of radiometric tarps is an excellent reference for anyone interested in using tarps for radiometric calibrations. The results are NIST traceable. (c) 2008 Optical Society of America. C1 [Georgiev, Georgi T.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Butler, James J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Georgiev, GT (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA. EM georgi.t.georgiev@nasa.gov RI Butler, James/D-4188-2013 NR 19 TC 12 Z9 12 U1 1 U2 1 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD JUN 20 PY 2008 VL 47 IS 18 BP 3313 EP 3323 DI 10.1364/AO.47.003313 PG 11 WC Optics SC Optics GA 323ZG UT WOS:000257486700013 PM 18566627 ER PT J AU Kadler, M Ros, E Perucho, M Kovalev, YY Homan, DC Agudo, I Kellermann, KI Aller, MF Aller, HD Lister, ML Zensus, JA AF Kadler, M. Ros, E. Perucho, M. Kovalev, Y. Y. Homan, D. C. Agudo, I. Kellermann, K. I. Aller, M. F. Aller, H. D. Lister, M. L. Zensus, J. A. TI The trails of superluminal jet components in 3C 111 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (3C111); galaxies : jets; galaxies : nuclei ID ACTIVE GALACTIC NUCLEI; BASE-LINE ARRAY; RADIO GALAXY; RELATIVISTIC JETS; VLBA EXPERIMENTS; SCALE STRUCTURE; EXTRAGALACTIC SOURCES; BL LACERTAE; X-RAY; QUASARS AB In 1996 a major radio flux density outburst occurred in the broad-line radio galaxy 3C 111. It was followed by a particularly bright plasma ejection associated with a superluminal jet component, which has shaped the parsec-scale structure of 3C 111 for almost a decade. Here we present results from 18 epochs of Very Long Baseline Array (VLBA) observations conducted since 1995 as part of the VLBA 2 cm Survey and MOJAVE monitoring programs. This major event allows us to study a variety of processes associated with outbursts of radio-loud AGNs in much greater detail than has been possible in other cases: the primary perturbation gives rise to the formation of a leading and a following component, which are interpreted as a forward and a backward shock. Both components evolve in characteristically different ways and allow us to draw conclusions about the work flow of jet-production events; the expansion, acceleration and recollimation of the ejected jet plasma in an environment with steep pressure and density gradients are revealed; trailing components are formed in the wake of the primary perturbation, possibly as a result of coupling to Kelvin-Helmholtz instability pinching modes from the interaction of the jet with the external medium. The interaction of the jet with its ambient medium is further described by the linear-polarization signature of jet components traveling along the jet and passing a region of steep pressure/density gradients. C1 [Kadler, M.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Kadler, M.; Ros, E.; Perucho, M.; Kovalev, Y. Y.; Agudo, I.; Zensus, J. A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Kovalev, Y. Y.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [Homan, D. C.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Agudo, I.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Kellermann, K. I.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Aller, M. F.; Aller, H. D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Lister, M. L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. RP Kadler, M (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt Rd, Greenbelt, MD 20771 USA. EM mkadler@milkyway.gsfc.nasa.gov; ros@mpifr-bonn.mpg.de; perucho@mpifr-bonn.mpg.de; ykovalev@mpifr-bonn.mpg.de; homand@denison.edu; iagudo@iaa.es; kkellerm@nrao.edu; mfa@umich.edu; haller@umich.edu; mlister@physics.purdue.edu; azensus@mpifr-bonn.mpg.de RI Kovalev, Yuri/J-5671-2013; Agudo, Ivan/G-1701-2015; Perucho, Manel/A-9528-2017; OI Kovalev, Yuri/0000-0001-9303-3263; Agudo, Ivan/0000-0002-3777-6182; Perucho, Manel/0000-0003-2784-0379; Ros, Eduardo/0000-0001-9503-4892; Kadler, Matthias/0000-0001-5606-6154 NR 54 TC 15 Z9 15 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 JUN 20 PY 2008 VL 680 IS 2 BP 867 EP 884 DI 10.1086/529539 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 313PL UT WOS:000256752400004 ER PT J AU Cannizzo, JK Gehrels, N Vishniac, ET AF Cannizzo, J. K. Gehrels, N. Vishniac, E. T. TI Glimm's method for relativistic hydrodynamics SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; methods : numerical; relativity ID GAMMA-RAY BURST; 28 FEBRUARY 1997; HYPERBOLIC SYSTEMS; RIEMANN PROBLEM; FLUID-DYNAMICS; AFTERGLOW; JETS; CODE; EQUATIONS; FLOWS AB We present the results of standard one-dimensional test problems in relativistic hydrodynamics using Glimm's ( random choice) method and compare them to results obtained using finite differencing methods. For problems containing profiles with sharp edges, such as shocks, we find Glimm's method yields global errors similar to 1-3 orders of magnitude smaller than the traditional techniques. The strongest differences are seen for problems in which a shear field is superposed. For smooth flows, Glimm's method is inferior to standard methods. The location of specific features can be off by up to two grid points with respect to an exact solution in Glimm's method, and furthermore, curved states are not modeled optimally, since the method idealizes solutions as being composed of piecewise constant states. Thus, although Glimm's method is superior at correctly resolving sharp features, especially in the presence of shear, for realistic applications in which one typically finds smooth flows plus strong gradients or discontinuities, standard finite-difference methods yield smaller global errors. Glimm's method may prove useful in certain applications such as GRB afterglow shock propagation into a uniform medium. C1 [Cannizzo, J. K.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Cannizzo, J. K.] Univ Maryland, CRESST, Joint Ctr Astrophys, Baltimore, MD 21250 USA. [Vishniac, E. T.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. RP Cannizzo, JK (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RI Gehrels, Neil/D-2971-2012; OI Vishniac, Ethan/0000-0002-2307-3857 NR 39 TC 1 Z9 1 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 JUN 20 PY 2008 VL 680 IS 2 BP 885 EP 896 DI 10.1086/587164 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 313PL UT WOS:000256752400005 ER PT J AU Deharveng, JM Small, T Barlow, TA Peroux, C Milliard, B Friedman, PG Martin, DC Morrissey, P Schiminovich, D Forster, K Seibert, M Wyder, TK Bianchi, L Donas, J Heckman, TM Lee, YW Madore, BF Neff, SG Rich, RM Szalay, AS Welsh, BY Yi, SK AF Deharveng, Jean-Michel Small, Todd Barlow, Tom A. Peroux, Celine Milliard, Bruno Friedman, Peter G. Martin, D. Christopher Morrissey, Patrick Schiminovich, David Forster, Karl Seibert, Mark Wyder, Ted K. Bianchi, Luciana Donas, Jose Heckman, Timothy M. Lee, Young-Wook Madore, Barry F. Neff, Susan G. Rich, R. Michael Szalay, Alex S. Welsh, Barry Y. Yi, Sukyoung K. TI Ly alpha-emitting galaxies at 0.2 < z < 0.35 from GALEX spectroscopy SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : evolution; galaxies : ISM; galaxies : luminosity function, mass function; galaxies : starburst; ultraviolet : galaxies ID LYMAN-BREAK GALAXIES; STAR-FORMATION RATE; DIGITAL SKY SURVEY; REST-FRAME ULTRAVIOLET; ACTIVE GALACTIC NUCLEI; SUBARU DEEP FIELD; LUMINOSITY FUNCTION; H-ALPHA; HIGH-REDSHIFT; FORMING GALAXIES AB We have used the GALEX (Galaxy Evolution Explorer) spectroscopic survey mode, with a resolution of similar to 8 angstrom in the far-ultraviolet (FUV; 1350-1750 angstrom) and similar to 20 angstrom in the near-ultraviolet (NUV; 1950-2750 angstrom) for a systematic search of Ly alpha-emitting galaxies at low redshift. Our aim is to fill a gap between high-redshift surveys and a small set of objects studied in detail in the nearby universe. A blind search of 7018 spectra extracted in five deep exposures (5.65 deg(2)) has resulted in 96 Ly alpha-emitting galaxy candidates in the FUV domain after accounting for broad-line AGNs. The Ly alpha equivalent widths (EWs) are consistent with stellar population model predictions and show no trends as a function of UV color or UV luminosity, with the exception of a possible decrease in the most luminous objects that may be due to small-number statistics. The objects' distribution in EW is similar to that at z similar to 3, but their fraction among star-forming galaxies is smaller. Avoiding uncertain candidates, a subsample of 66 objects in the range 0.2 < z < 0.35 has been used to build a Ly alpha luminosity function (LF). The incompleteness due to objects with significant Ly alpha emission but a UV continuum too low for spectral extraction has been evaluated. A comparison with H alpha LFs in the same redshift domain is consistent with an average Ly alpha/H alpha of similar to 1 in about 15% of the star-forming galaxies. A comparison with high-redshift Ly alpha LFs implies an increase of the Ly alpha luminosity density by a factor of about 16 from z similar to 0.3 to z similar to 3. By comparison with the factor of 5 increase in the UV luminosity density in the same redshift range, this suggests an increase of the average Ly alpha escape fraction with redshift. C1 [Deharveng, Jean-Michel; Peroux, Celine; Milliard, Bruno; Donas, Jose] Univ Aix Marseille 1, CNRS, UMR 6110, Astrophys Lab, F-13376 Marseille 12, France. [Small, Todd; Barlow, Tom A.; Friedman, Peter G.; Martin, D. Christopher; Morrissey, Patrick; Forster, Karl; Seibert, Mark; Wyder, Ted K.] CALTECH, Pasadena, CA 91125 USA. [Schiminovich, David] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Heckman, Timothy M.; Szalay, Alex S.] Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA. [Lee, Young-Wook; Yi, Sukyoung K.] Yonsei Univ, Ctr Space Astrophys, Seoul 120749, South Korea. [Madore, Barry F.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Neff, Susan G.] NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. [Rich, R. Michael] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Welsh, Barry Y.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Deharveng, JM (reprint author), Univ Aix Marseille 1, CNRS, UMR 6110, Astrophys Lab, BP 8, F-13376 Marseille 12, France. NR 64 TC 63 Z9 63 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2008 VL 680 IS 2 BP 1072 EP 1082 DI 10.1086/587953 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 313PL UT WOS:000256752400019 ER PT J AU Goldsmith, PF Pandian, JD Deshpande, AA AF Goldsmith, Paul F. Pandian, Jagadheep D. Deshpande, Avinash A. TI A search for 6.7 GHz methanol masers in M33 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (M33); ISM : individual (methanol); ISM : molecules; masers ID GALACTIC PLANE SURVEY; EXTRAGALACTIC METHANOL; MAGELLANIC CLOUDS; MOLECULAR CLOUDS; GENERAL CATALOG; SPIRAL GALAXIES; STAR-FORMATION; HII-REGIONS; ABUNDANCES; TRANSITION AB We report the negative results from a search for 6.7 GHz methanol masers in the nearby spiral galaxy M33. We observed 14 GMCs in the central 4 kpc of the Galaxy, and found 3 sigma upper limits to the flux density of similar to 4 mJy at a velocity resolution of 0.35 km s(-1). By velocity shifting and combining the spectra from the positions observed, we obtain an effective 3 sigma upper limit on the average emission of similar to 1 mJy in a 0.25 km s(-1) channel. These limits lie significantly below what we would expect based on our estimates of the methanol maser luminosity function in the Milky Way. One possible explanation for the absence of detectable methanol masers appears to be the metallicity of M33, which is somewhat less than that of the Milky Way. C1 [Goldsmith, Paul F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Pandian, Jagadheep D.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Pandian, Jagadheep D.] Cornell Univ, Dept Astron, Ithaca, NY USA. [Deshpande, Avinash A.] Raman Res Inst, Bangalore 560080, Karnataka, India. RP Goldsmith, PF (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM paul.f.goldsmith@jpl.nasa.gov; jpandian@mpifr-bonn.mpg.de; desh@rri.res.in RI Deshpande, Avinash/D-4868-2012; Astronomy & Astrophysics Group, Raman Res Institute/D-4046-2012; M, Manjunath/N-4000-2014; Goldsmith, Paul/H-3159-2016 OI M, Manjunath/0000-0001-8710-0730; NR 34 TC 6 Z9 6 U1 1 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2008 VL 680 IS 2 BP 1132 EP 1136 DI 10.1086/524651 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 313PL UT WOS:000256752400023 ER PT J AU Katsuda, S Tsunemi, H Kimura, M Mori, K AF Katsuda, Satoru Tsunemi, Hiroshi Kimura, Masashi Mori, Koji TI Chandra observations of the northeastern rim of the Cygnus Loop SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : abundances; ISM : individual (Cygnus loop); supernova remnants; X-rays : ISM ID X-RAY SPECTROSCOPY; NONRADIATIVE SHOCK-WAVE; VELA SHRAPNEL-A; SUPERNOVA REMNANT; SOUTHWESTERN RIM; PLASMA STRUCTURE; EMISSION; SUZAKU; CLOUD; ULTRAVIOLET AB We present results from spatially resolved spectral analyses of the northeastern ( NE) rim of the Cygnus Loop supernova remnant (SNR) based on two Chandra observations. One pointing includes northern outermost abundance-enhanced regions discovered by recent Suzaku observations, while the other pointing is located on regions with "normal" abundances in the NE rim of the Cygnus Loop. The superior spatial resolving power of Chandra allows us to reveal that the abundance-enhanced region is concentrated in a similar to 20000 thickness region behind the shock front. We confirm absolute metal abundances (i.e., relative to H), as well as abundance ratios between metals, are consistent with those of the solar values within a factor of similar to 2. Also, we find that the emission measure in the region gradually decreases toward the shock front. These features are in contrast with those of the ejecta fragments around the Vela SNR, which leads us to believe that the abundance enhancements are not likely due to metal-rich ejecta. We suggest that the origin of the plasma in this region is the interstellar medium ( ISM). In the "normal" abundance regions, we confirm that abundances are depleted to the solar values by a factor of similar to 5 that is not expected in the ISM around the Cygnus Loop. Introduction of nonthermal emission in our model fitting cannot naturally resolve the abundance-depletion problem. The origin of the depletion still remains as an open question. C1 [Katsuda, Satoru; Tsunemi, Hiroshi; Kimura, Masashi] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Osaka 5600043, Japan. [Mori, Koji] Miyazaki Univ, Fac Engn, Dept Appl Phys, Miyazaki 8892192, Japan. RP Katsuda, S (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. RI XRAY, SUZAKU/A-1808-2009 NR 38 TC 15 Z9 16 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2008 VL 680 IS 2 BP 1198 EP 1205 DI 10.1086/588188 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 313PL UT WOS:000256752400030 ER PT J AU Mattioda, AL Rutter, L Parkhill, J Head-Gordon, M Lee, TJ Allamandola, LJ AF Mattioda, Andrew L. Rutter, Lindsay Parkhill, John Head-Gordon, Martin Lee, Timothy J. Allamandola, Louis J. TI Near-infrared spectroscopy of nitrogenated polycyclic aromatic hydrocarbon cations from 0.7 to 2.5 mu m SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; dust, extinction; ISM : general; ISM : molecules; molecular data ID ELECTRONIC ABSORPTION-SPECTROSCOPY; DIFFUSE INTERSTELLAR-MEDIUM; RADICAL CATIONS; MU-M; VIBRATIONAL-SPECTRA; LARGE MOLECULES; EXCITED-STATES; SMALL GRAINS; PAH MODEL; EMISSION AB The near-infrared (NIR) spectra and absolute band strengths of 10 nitrogenated polycyclic aromatic hydrocarbon (PANH) radical cations isolated in an argon matrix are presented and compared with the spectra of their parent polycyclic aromatic hydrocarbon (PAH) radical cations. The 0.7-2.5 mu m (14,500-4000 cm(-1)) spectrum for the open-shell cation forms of two nitrogenated anthracenes (C(13)H(9)N and C(12)H(8)N(2)), four isomeric nitrogenated benzanthracenes (C(17)H(11)N), and four isomeric nitrogenated dibenzanthracenes (C(21)H(13)N) are reported. These ionized PANHs have allowed electronic transitions that give rise to strong absorption bands in the NIR. Low-lying excited states for these PANH ions are computed using time-dependent density functional theory (TDDFT). The resulting vertical excitation spectrum characterizes the transitions, and leads to a simple model that predicts the qualitative trends in absorption energy. The direction of the shift depends on the position of the nitrogen atom within the PANH and the relative magnitudes of the donor and acceptor molecular orbitals involved in the transitions. As with non-nitrogenated PAHs, ionized interstellar PANHs can be expected to contribute to the mid-IR emission features from UV-rich as well as UV-poor regions, and add weak, broad band structure to the NIR region of the interstellar extinction curve. C1 [Mattioda, Andrew L.; Rutter, Lindsay; Lee, Timothy J.; Allamandola, Louis J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Mattioda, Andrew L.; Rutter, Lindsay] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. [Rutter, Lindsay] Penn State Univ, University Pk, PA 16802 USA. [Parkhill, John; Head-Gordon, Martin] Univ Calif Berkeley, Berkeley, CA 94720 USA. RP Mattioda, AL (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Andrew.L.Mattioda@nasa.gov RI Lee, Timothy/K-2838-2012 NR 46 TC 23 Z9 23 U1 0 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2008 VL 680 IS 2 BP 1243 EP 1255 DI 10.1086/529484 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 313PL UT WOS:000256752400034 ER PT J AU Spezzi, L Alcala, JM Covino, E Frasca, A Gandolfi, D Oliveira, I Chapman, N Evans, NJ Huard, TL Jorgensen, JK Merin, B Stapelfeldt, KR AF Spezzi, Loredana Alcala, Juan M. Covino, Elvira Frasca, Antonio Gandolfi, Davide Oliveira, Isa Chapman, Nicholas Evans, Neal J., II Huard, Tracy L. Jorgensen, Jes K. Merin, Bruno Stapelfeldt, Karl R. TI The young population of the Chamaeleon II dark cloud SO ASTROPHYSICAL JOURNAL LA English DT Review DE circumstellar matter; infrared : stars; planetary systems : protoplanetary disks; stars : formation; stars : low-mass; brown dwarfs; stars : pre-main-sequence ID LOW-MASS STARS; T-TAURI STARS; SPITZER C2D SURVEY; ALL-SKY SURVEY; BROWN DWARF POPULATION; CIRCUMSTELLAR DISK MASSES; ORION NEBULA CLUSTER; FORMING REGION; INTERSTELLAR CLOUDS; STELLAR OBJECTS AB We discuss the results of the optical spectroscopic follow-up of pre-main-sequence (PMS) objects and candidates selected in the Chamaeleon II dark cloud based on data from the Spitzer Legacy survey "From Molecular Cores to Planet Forming Disks" (c2d) and from previous surveys. Our sample includes both objects with infrared excess selected according to c2d criteria and referred to as young stellar objects and other cloud members and candidates selected from complementary optical and near-infrared data. We characterize the sample of objects by deriving their physical parameters. The vast majority of objects have masses M <= 1 M-circle dot and ages < 6 Myr. Several of the PMS objects and candidates lie very close to or below the hydrogen-burning limit. A first estimate of the slope of the initial mass function in Cha II is consistent with that of other T associations. The star formation efficiency in the cloud (1%-4%) is consistent with our own estimates for Taurus and Lupus, but significantly lower than for Cha I. This might mean that different star formation activities in the Chamaeleon clouds may reflect a different history of star formation. We also find that the Cha II cloud is turning some 8 M-circle dot into stars every megayear, which is less than the star formation rate in the other c2d clouds. However, the star formation rate is not steady and evidence is found that the star formation in Cha II might have occurred very rapidly. The H alpha emission of the Cha II PMS objects, as well as possible correlations between their stellar and disk properties, is also investigated. C1 [Spezzi, Loredana; Alcala, Juan M.; Covino, Elvira] INAF OA Capodimonte, I-80131 Naples, Italy. [Spezzi, Loredana; Frasca, Antonio; Gandolfi, Davide] INAF OA Catania, I-95123 Catania, Italy. [Oliveira, Isa] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Oliveira, Isa] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Chapman, Nicholas] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Evans, Neal J., II] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Huard, Tracy L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jorgensen, Jes K.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Merin, Bruno] European Space Agcy, Res & Sci Support Dept, ESTEC, NL-2200 AG Noordwijk, Netherlands. [Stapelfeldt, Karl R.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Spezzi, L (reprint author), INAF OA Capodimonte, I-80131 Naples, Italy. EM lspezzi@oact.inaf.it; afr@oact.inaf.it; isa@gps.caltech.edu; chapman@astro.umd.edu; nje@astro.as.utexas.edu; thuard@cfa.harvard.edu; jes@astro.uni-bonn.de; bmerin@rssd.esa.int; krs@exoplanet.jpl.nasa.gov RI Stapelfeldt, Karl/D-2721-2012; OI Alcala, Juan Manuel/0000-0001-8657-095X; Frasca, Antonio/0000-0002-0474-0896; Covino, Elvira/0000-0002-6187-6685; Gandolfi, Davide/0000-0001-8627-9628; Merin, Bruno/0000-0002-8555-3012 NR 112 TC 57 Z9 57 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2008 VL 680 IS 2 BP 1295 EP 1318 DI 10.1086/587931 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 313PL UT WOS:000256752400038 ER PT J AU Miller, JM Raymond, J Reynolds, CS Fabian, AC Kallman, TR Homan, J AF Miller, J. M. Raymond, J. Reynolds, C. S. Fabian, A. C. Kallman, T. R. Homan, J. TI The accretion disk wind in the black hole GRO J1655-40 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries : spectroscopic (GRO J1655-40); black hole physics; relativity ID RESOLVED ULTRAVIOLET SPECTROSCOPY; GRO J1655-40; EXPLORER OBSERVATIONS; ABSORPTION-LINES; ATOMIC DATABASE; EMISSION-LINES; DRIVEN; MASS; SPECTRA; CHANDRA AB We report on simultaneous Chandra HETGS and RXTE observations of the transient stellar-mass black hole GRO J1655-40, made during its 2005 outburst. Chandra reveals a line-rich X-ray absorption spectrum consistent with a disk wind. Prior modeling of the spectrum suggested that the wind may be magnetically driven, potentially providing insights into the nature of disk accretion onto black holes. In this paper, we present results obtained with new models for this spectrum, generated using three independent photoionization codes: XSTAR, Cloudy, and our own code. Fits to the spectrum in particular narrow wavelength ranges, in evenly spaced wavelength slices, and across a broad wavelength band all strongly prefer a combination of high density, high ionization, and small inner radius. Indeed, the results obtained from all three codes require a wind that originates more than 10 times closer to the black hole and carrying a mass flux that is on the order of 1000 times higher than predicted by thermal driving models. If seminal work on thermally driven disk winds is robust, magnetic forces may play a role in driving the disk wind in GRO J1655-40. However, even these modeling efforts must be regarded as crude given the complexity of the spectra. We discuss these results in the context of accretion flows in black holes and other compact objects. C1 [Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Raymond, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England. [Kallman, T. R.] NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. [Homan, J.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Miller, JM (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM jonmm@umich.edu NR 57 TC 87 Z9 87 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2008 VL 680 IS 2 BP 1359 EP 1377 DI 10.1086/588521 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 313PL UT WOS:000256752400042 ER PT J AU Harding, AK Stern, JV Dyks, J Frackowiak, M AF Harding, Alice K. Stern, Julie V. Dyks, Jaroslaw Frackowiak, Michal TI High-altitude emission from pulsar slot gaps: The crab pulsar SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; gamma rays : theory; pulsars : general; radiation mechanisms : nonthermal; stars : neutron; X-rays : stars ID GAMMA-RAY PULSARS; HIGH-ENERGY EMISSION; RADIO-EMISSION; POLAR CAPS; X-RAY; SYNCHROTRON ABSORPTION; PARTICLE-ACCELERATION; OUTER MAGNETOSPHERE; PAIR FORMATION; BEAM GEOMETRY AB We present results of a 3D model of optical-to-gamma-ray emission from the slot gap accelerator of a rotation-powered pulsar. Primary electrons accelerating to high altitudes in the unscreened electric field of the slot gap reach radiation reaction limited Lorentz factors of similar to 2x10(7),while electron-positron pairs from lower altitude cascades flow along field lines interior to the slot gap. The curvature, synchrotron, and inverse Compton radiation of both primary electrons and pairs produce a broad spectrum of emission from infrared to GeV energies. Both primaries and pairs undergo cyclotron resonant absorption of radio photons, allowing them to maintain significant pitch angles. Synchrotron radiation from pairs with a power-law energy spectrum from gamma = 10(2) to 10(5), dominate the spectrum up to similar to 10 MeV. Synchrotron and curvature radiation of primaries dominates from 10 MeV up to a few GeV. We examine the energy-dependent pulse profiles and phase-resolved spectra for parameters of the Crab pulsar as a function of magnetic inclination alpha and viewing angle zeta, comparing to broadband data. In most cases, the pulse profiles are dominated by caustics on trailing field lines. We also explore the relation of the high-energy and the radio profiles, as well as the possibility of caustic formation in the radio cone emission. We find that the Crab pulsar profiles and spectrum can be reasonably well reproduced by a model with alpha = 45 degrees and zeta similar to 100 degrees or 80 degrees. This model predicts that the slot gap emission below 200 MeV will exhibit correlations in time and phase with the radio emission. C1 [Harding, Alice K.; Stern, Julie V.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Stern, Julie V.] SUNY Stony Brook, Stony Brook, NY 11794 USA. [Dyks, Jaroslaw; Frackowiak, Michal] Nicholas Copernicus Astron Ctr, Torun, Poland. RP Harding, AK (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. EM redbeard@openlabs.pl RI Harding, Alice/D-3160-2012 NR 47 TC 96 Z9 96 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 JUN 20 PY 2008 VL 680 IS 2 BP 1378 EP 1393 DI 10.1086/588037 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 313PL UT WOS:000256752400043 ER PT J AU Jess, DB Mathioudakis, M Erdelyi, R Verth, G McAteer, RTJ Keenan, FP AF Jess, D. B. Mathioudakis, M. Erdelyi, R. Verth, G. McAteer, R. T. J. Keenan, F. P. TI Discovery of spatial periodicities in a coronal loop using automated edge-tracking algorithms SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods : data analysis; Sun : corona; Sun : evolution; Sun : oscillations; techniques : image processing ID ACTIVE-REGION OSCILLATIONS; TRANSVERSE OSCILLATIONS; DENSITY STRATIFICATION; AMPLITUDE PROFILE; TRANSITION-REGION; WAVE-PROPAGATION; TRACE; FLARE AB A new method for automated coronal loop tracking, in both spatial and temporal domains, is presented. Applying this technique to TRACE data, obtained using the 171 angstrom filter on 1998 July 14, we detect a coronal loop undergoing a 270 s kink-mode oscillation, as previously found by Aschwanden et al. However, we also detect flare-induced, and previously unnoticed, spatial periodicities on a scale of 3500 km, which occur along the coronal loop edge. Furthermore, we establish a reduction in oscillatory power for these spatial periodicities of 45% over a 222 s interval. We relate the reduction in detected oscillatory power to the physical damping of these loop-top oscillations. C1 [Jess, D. B.; Mathioudakis, M.; Keenan, F. P.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Jess, D. B.; McAteer, R. T. J.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. [Erdelyi, R.; Verth, G.] Univ Sheffield, Dept Appl Math, SP2RC, Sheffield S3 7RH, S Yorkshire, England. [McAteer, R. T. J.] Catholic Univ Amer, Washington, DC 20064 USA. RP Jess, DB (reprint author), Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. EM djess01@qub.ac.uk RI McAteer, R. T. James/D-3736-2011 NR 30 TC 12 Z9 12 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 JUN 20 PY 2008 VL 680 IS 2 BP 1523 EP 1531 DI 10.1086/587735 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 313PL UT WOS:000256752400058 ER PT J AU Zhukov, AN Saez, F Lamy, P Llebaria, A Stenborg, G AF Zhukov, A. N. Saez, F. Lamy, P. Llebaria, A. Stenborg, G. TI The origin of polar streamers in the solar corona SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : corona; Sun : magnetic fields ID HELIOSPHERIC CURRENT SHEET; MAGNETIC-FIELDS; 3-DIMENSIONAL STRUCTURE; EVOLUTION; FILAMENTS; PHASE; MODEL; HOLES; INTERPLANETARY; CAVITIES AB We investigate the large-scale three-dimensional (3D) structure of the solar corona near the maximum of the 23rd solar cycle in an attempt to determine the origin of polar streamers. We use a model that allows us to simulate the quasi-stationary configuration of the large-scale coronal density distribution. The coronal neutral line, as given by the potential field source surface (PFSS) model, serves as a proxy for mid-and low-latitude current sheets. We investigate the contribution of possible polar coronal current sheets associated with large-scale photospheric magnetic neutral lines around the poles of the Sun (polar crown neutral lines). Positions of polar neutral lines are radially extrapolated outward to obtain the configuration of polar current sheets. Coronal plasma sheets are centered around introduced current sheets. Streamer positions during Carrington rotation 1965, near the activity maximum, are calculated. Simulated synoptic maps of the coronal brightness are compared with those obtained from observations by the LASCO C2 coronagraph on board the SOHO spacecraft. We demonstrate that polar streamers are "classical'' streamers situated above low-lying loops (observed by SOHO EIT) connecting the regions of opposite magnetic polarity on two sides of polar crown neutral lines. Polar streamer configurations obtained from our model are close to those observed by LASCO. Our results suggest that the PFSS model cannot adequately describe the configuration of streamers during the epoch of high solar activity. The representation of the streamer belt as a single tilted and warped current sheet becomes questionable. Multiple coronal current sheets may better correspond to the observed streamer configurations. C1 [Zhukov, A. N.] Observ Royal Belgique, Solar Terr Ctr Excellence SIDC, B-1180 Brussels, Belgium. [Zhukov, A. N.] Moscow MV Lomonosov State Univ, Skobeltsyn Inst Nucl Phys, Moscow 119992, Russia. [Saez, F.; Lamy, P.; Llebaria, A.] Lab Astrophys Marseille, F-13376 Marseille, France. [Stenborg, G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Stenborg, G.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. RP Zhukov, AN (reprint author), Observ Royal Belgique, Solar Terr Ctr Excellence SIDC, Ave Circulaire 3, B-1180 Brussels, Belgium. EM andrei.zhukov@sidc.be NR 55 TC 6 Z9 6 U1 1 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2008 VL 680 IS 2 BP 1532 EP 1541 DI 10.1086/587924 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 313PL UT WOS:000256752400059 ER PT J AU Angel, R Worden, SP Borra, EF Eisenstein, DJ Foing, B Hickson, P Josset, JL Ma, KB Seddiki, O Sivanandam, S Thibault, S van Susante, P AF Angel, Roger Worden, Simon P. Borra, Ermanno F. Eisenstein, Daniel J. Foing, Bernard Hickson, Paul Josset, Jean-Luc Ma, Ki Bui Seddiki, Omar Sivanandam, Suresh Thibault, Simon van Susante, Paul TI A cryogenic liquid-mirror telescope on the moon to study the early universe SO ASTROPHYSICAL JOURNAL LA English DT Article DE early universe; infrared : general; Moon; telescopes ID DIGITAL SKY SURVEY; LUNAR TELESCOPE; SPACE-TELESCOPE; ORBITAL DEBRIS; PRIMORDIAL GAS; COSMOLOGY; GALAXIES; STARS; Z-SIMILAR-TO-6; FRAGMENTATION AB We have studied the feasibility and scientific potential of zenith observing liquid-mirror telescopes having 20-100m diameters located on the Moon. They would carry out deep infrared surveys to study the distant universe and follow up discoveries made with the 6 m James Webb Space Telescope (JWST), with more detailed images and spectroscopic studies. They could detect objects 100 times fainter than JWST, observing the first high-redshift stars in the early universe and their assembly into galaxies. We explored the scientific opportunities, key technologies, and optimum location of such telescopes. We have demonstrated critical technologies. For example, the primary mirror would necessitate a high-reflectivity liquid that does not evaporate in the lunar vacuum and remains liquid at less than 100 K. We have made a crucial demonstration by successfully coating an ionic liquid that has negligible vapor pressure. We also successfully experimented with a liquid mirror spinning on a superconducting bearing, as will be needed for the cryogenic, vacuum environment of the telescope. We have investigated issues related to lunar locations, concluding that locations within a few kilometers of a pole are ideal for deep sky cover and long integration times. We have located ridges and crater rims within 0.5 degrees of the north pole that are illuminated for at least some sun angles during lunar winter, providing power and temperature control. We also have identified potential problems, like lunar dust. Issues raised by our preliminary study demand additional in-depth analyses. These issues must be fully examined as part of a scientific debate that we hope to start with the present article. C1 [Angel, Roger; Eisenstein, Daniel J.; Sivanandam, Suresh] Univ Arizona, Steward Observ, Tucson, AZ 85751 USA. [Worden, Simon P.] NASA, Ames Res Ctr, Off Director, Moffett Field, CA 94035 USA. [Borra, Ermanno F.; Seddiki, Omar] Univ Laval, Fac Sci & Genie, Quebec City, PQ G1K 7P4, Canada. [Foing, Bernard] ESA ESTEC SCI S, NL-2200 AG Noordwijk, Netherlands. [Hickson, Paul] Univ British Columbia, Dept Phys, Vancouver, BC V6T 1Z1, Canada. [Josset, Jean-Luc] Space X Space Explorat Inst, CH-2007 Neuchatel, Switzerland. [Ma, Ki Bui] Univ Houston, Texas Ctr Superconduct, Houston, TX 77204 USA. [Thibault, Simon] Immervision, Montreal, PQ H3A 2A5, Canada. [van Susante, Paul] Colorado Sch Mines, Div Engn, Golden, CO 80401 USA. RP Angel, R (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85751 USA. NR 51 TC 10 Z9 10 U1 0 U2 14 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 JUN 20 PY 2008 VL 680 IS 2 BP 1582 EP 1594 DI 10.1086/588034 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 313PL UT WOS:000256752400064 ER PT J AU Milligan, RO AF Milligan, Ryan O. TI A hot microflare observed with RHESSI and Hinode SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun : atmospheric motions; Sun : flares; Sun : UV radiation; Sun : X-rays, gamma rays ID X-RAY-SPECTRUM; CHROMOSPHERIC EVAPORATION; SOLAR-FLARE; SPECTROMETER; MISSION; MODEL; CDS AB RHESSI and Hinode observations of a GOES B-class flare are combined to investigate the origin of 15 MK plasma. The absence of any detectable hard X-ray emission coupled with weak blueshifted emission lines ( indicating upward velocities averaging only 14 km s(-1)) suggests that this was a result of direct heating in the corona, as opposed to nonthermal electron precipitation causing chromospheric evaporation. These findings are in agreement with a recent hydrodynamical simulation of microflare plasmas that found that higher temperatures can be attained when less energy is used to accelerate electrons out of the thermal distribution. In addition, unusual redshifts in the 2 MK Fe xv line (indicating downward velocities of similar to 14 km s(-1)) were observed cospatial with one of the flare ribbons during the event. Downflows of such high-temperature plasma are not predicted by any common flare model. C1 NASA, Goddard Space Flight Ctr, Solar Phys Lab Code 671, Heliophys Sci Div, Greenbelt, MD 20771 USA. RP Milligan, RO (reprint author), NASA, Goddard Space Flight Ctr, Solar Phys Lab Code 671, Heliophys Sci Div, Greenbelt, MD 20771 USA. NR 24 TC 19 Z9 20 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 20 PY 2008 VL 680 IS 2 BP L157 EP L160 DI 10.1086/589856 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 313DZ UT WOS:000256722600016 ER PT J AU Romano, P Sidoli, L Mangano, V Vercellone, S Kennea, JA Cusumano, G Krimm, HA Burrows, DN Gehrels, N AF Romano, P. Sidoli, L. Mangano, V. Vercellone, S. Kennea, J. A. Cusumano, G. Krimm, H. A. Burrows, D. N. Gehrels, N. TI Monitoring supergiant fast X-ray transients with Swift. II. Rise to the outburst in IGR J16479-4514 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE stars : individual (IGR J16479-4514); X-rays : individual (IGR J16479-4514) ID INTEGRAL OBSERVATIONS; J11215-5952 AB IGR J16479- 4514 is a supergiant fast X-ray transient (SFXT), a new class of high-mass X-ray binaries, whose number is rapidly growing thanks to the INTEGRAL observations of the Galactic plane. It has been regularly monitored with Swift XRT since 2007 November to study the quiescent emission, the outburst properties, and their recurrence. A new bright outburst, reaching fluxes above 10(-9) erg cm(-2) s(-1), was caught by the Swift BAT. Swift immediately repointed at the target with the narrow-field instruments so that, for the first time, an outburst from an SFXT where a periodicity in the outburst recurrence is unknown could be observed simultaneously in the 0.2-150 keV energy band. The X-ray emission is highly variable and spans almost 4 orders of magnitude in count rate during the Swift XRT observations covering a few days before and after the bright peak. The Xray spectrum in outburst is hard and highly absorbed. The power-law fit resulted in a photon index of 0.98 +/- 0.07, and in an absorbing column density of similar to 5 x 10(22) cm(-2). These observations demonstrate that in this source (similarly to what was observed during the 2007 outburst from the periodic SFXT IGR J11215-5952), the accretion phase lasts much longer than a few hours. C1 [Romano, P.; Mangano, V.; Cusumano, G.] INAF, Ist Astrofis Spaziale & Fis Cosm, I-90146 Palermo, Italy. [Vercellone, S.] INAF, Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Kennea, J. A.; Burrows, D. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Krimm, H. A.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Krimm, H. A.] Univ Space Res Assoc, Columbia, MD USA. RP Romano, P (reprint author), INAF, Ist Astrofis Spaziale & Fis Cosm, Via U La Malfa 153, I-90146 Palermo, Italy. RI Gehrels, Neil/D-2971-2012; OI Sidoli, Lara/0000-0001-9705-2883 NR 19 TC 29 Z9 29 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 20 PY 2008 VL 680 IS 2 BP L137 EP L140 DI 10.1086/590082 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 313DZ UT WOS:000256722600011 ER PT J AU Siddon, EC Siddon, CE Stekoll, MS AF Siddon, Elizabeth Calvert Siddon, Christopher E. Stekoll, Michael S. TI Community level effects of Nereocystis luetkeana in southeastern Alaska SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE fish; habitat complexity; invertebrate assemblages; kelp; Nereocystis luetkeana; essential fish habitat ID TEMPERATE REEF FISH; JUVENILE COD GADUS; KELP FOREST; HABITAT CHARACTERISTICS; PARALABRAX-CLATHRATUS; LAMINARIA-HYPERBOREA; RECRUITMENT PATTERNS; CENTRAL CALIFORNIA; WASHINGTON-STATE; SEA OTTERS AB A multispecies approach was used to examine the role of the canopy forming kelp, Nereocystis luetkeana, in structuring kelp communities near Juneau, Alaska (58 degrees 22'53 N, 134 degrees 38'45 W). Large-scale (1500 m(2)) manipulations were used to test direct and indirect effects of Nereocystis on faunal assemblages. Fish and invertebrate abundances were quantified in relation to canopy (canopy, no canopy), depth (bottom, surface), and season (summer, winter) using Standard Monitoring Units for Recruitment of Fish (SMURFs), light traps, and visual surveys. Lacuna vincta directly utilized the canopy of Nereocystis with greatest abundances at canopy sites during the summer. In contrast, a direct negative effect of Nereocystis was observed for schooling Gadidae fishes: six times more fish were observed at sites without canopy kelp. The abundance of juvenile benthic fishes was twice as high at the bottom of sites containing Nereocystis as compared to no canopy sites, providing strong evidence for an indirect effect of canopy presence on community structure. Other invertebrate abundances (i.e., amphipods, copepods) were greater within the bottom strata (sub-canopy) of all sites, regardless of canopy or season. Our results illustrate the importance of a multispecies approach and present novel information for a little-studied, high-latitude kelp system. Published by Elsevier B.V. C1 [Siddon, Elizabeth Calvert; Siddon, Christopher E.; Stekoll, Michael S.] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Juneau, AK 99801 USA. [Stekoll, Michael S.] Univ Alaska SE, Dept Nat Sci, Juneau, AK 99801 USA. RP Siddon, EC (reprint author), Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Natl Ocean & Atmospher Adm, 17109 Point Lena Loop Rd, Juneau, AK 99801 USA. EM Elizabeth.Siddon@noaa.gov NR 67 TC 7 Z9 7 U1 6 U2 19 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD JUN 20 PY 2008 VL 361 IS 1 BP 8 EP 15 DI 10.1016/j.jembe.2008.03.015 PG 8 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 330PQ UT WOS:000257955700002 ER PT J AU Fatoyinbo, TE Simard, M Washington-Allen, RA Shugart, HH AF Fatoyinbo, Temilola E. Simard, Marc Washington-Allen, Robert A. Shugart, Herman H. TI Landscape-scale extent, height, biomass, and carbon estimation of Mozambique's mangrove forests with Landsat ETM+ and Shuttle Radar Topography Mission elevation data SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article ID GROUND BIOMASS; ECOSYSTEMS; PRODUCTIVITY; MADAGASCAR; LITTERFALL; DYNAMICS; IMAGERY; FUTURE; COVER; KENYA AB Mangroves are salt tolerant plants that grow within the intertidal zone along tropical and subtropical coasts. They are important barriers for mitigating coastal disturbances, provide habitat for over 1300 animal species and are one of the most productive ecosystems. Mozambique's mangroves extend along 2700 km and cover one of the largest areas in Africa. The purpose of this study was to determine the countrywide mean tree height spatial distribution and biomass of Mozambique's mangrove forests using Landsat ETM+ and Shuttle Radar Topography Mission (SRTM) data. The SRTM data were calibrated using the Landsat derived land-cover map and height calibration equations. Stand-specific canopy height-biomass allometric equations developed from field measurements and published height-biomass equations were used to calculate aboveground biomass of the mangrove forests on a landscape scale. The results showed that mangrove forests covered a total of 2909 km 2 in Mozambique, a 27% smaller area than previously estimated. The SRTM calibration indicated that average tree heights changed with geographical settings. Even though the coast of Mozambique spans across 16 degrees latitude, we did not find a relationship between latitude and biomass. These results confirm that geological setting has a greater influence than latitude alone on mangrove production. The total mangrove dry aboveground biomass in Mozambique was 23.6 million tons and the total carbon was 11.8 million tons. C1 [Fatoyinbo, Temilola E.; Washington-Allen, Robert A.; Shugart, Herman H.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA. [Simard, Marc] CALTECH, Jet Prop Lab, Radar & Engn Sect, Pasadena, CA 91109 USA. [Washington-Allen, Robert A.] Texas A&M Univ, Dept Ecosyst Sci & Management, College Stn, TX 77843 USA. RP Fatoyinbo, TE (reprint author), Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA. EM tef3p@virginia.edu RI Fatoyinbo, Temilola/G-6104-2012; Simard, Marc/H-3516-2013; Shugart, Herman/C-5156-2009 OI Fatoyinbo, Temilola/0000-0002-1130-6748; Simard, Marc/0000-0002-9442-4562; NR 75 TC 24 Z9 26 U1 3 U2 18 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-8953 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD JUN 20 PY 2008 VL 113 IS G2 AR G02S06 DI 10.1029/2007JG000551 PG 13 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 317YU UT WOS:000257057100001 ER PT J AU Moore, TE Fok, MC Delcourt, DC Slinker, SP Fedder, JA AF Moore, T. E. Fok, M. -C. Delcourt, D. C. Slinker, S. P. Fedder, J. A. TI Plasma plume circulation and impact in an MHD substorm SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID SOLAR-WIND; OUTER PLASMASPHERE; RING CURRENT; DENSITY; EVENTS; SHEET; MODEL AB We investigate the fate of a plasmaspheric plume generated by a discrete period of southward interplanetary magnetic field (IMF) to assess its contribution to plasma sheet and ring current pressure and compare with that for other sources. We use test particle motions in Lyon-Fedder-Mobarry (LFM) global circulation model fields. The inner magnetosphere is simulated with the Comprehensive Ring Current Model (CRCM) model of Fok and Wolf, driven by the transpolar potential developed by the LFM magnetosphere. A variant of the Ober plasmasphere model is embedded within the models and driven by them. Global circulation is stimulated by a period of southward IMF embedded within a long interval of northward IMF. This leads to the production of a well-defined plasmaspheric plume, enhancing the plasma density sunward of the plasmasphere. Test particles are launched with the properties of plasmaspheric ions on the L = 6.6 R(E) shell and weighted with densities as specified by the Ober model, as it responds to convection imposed by CRCM. Particles are tracked until they are lost from the system downstream or into the atmosphere, using the Delcourt full equations of motion, implemented for finite element fields. Results are compared with earlier computations of polar and auroral wind outflows. The plume produces an enhanced flow of plasma similar to 10 times the normal polar wind global fluence. However, we find that most of the "plasmaspheric wind'' is lost from the magnetosphere such that its contribution to the ring current energy density is comparable to that of the normal polar wind for this type of event. C1 [Moore, T. E.; Fok, M. -C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Delcourt, D. C.] Ctr Etud Environm Terr & Planetaires, UMR 8639, F-94107 St Maur Des Fosses, France. [Slinker, S. P.] USN, Res Lab, Washington, DC 20375 USA. [Fedder, J. A.] Icarus Res Inc, Bethesda, MD 20814 USA. RP Moore, TE (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd,Code 670, Greenbelt, MD 20771 USA. EM thomas.e.moore@nasa.gov RI Moore, Thomas/D-4675-2012; Fok, Mei-Ching/D-1626-2012 OI Moore, Thomas/0000-0002-3150-1137; NR 27 TC 15 Z9 15 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUN 20 PY 2008 VL 113 IS A6 AR A06219 DI 10.1029/2008JA013050 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 317ZU UT WOS:000257060200002 ER PT J AU Pawson, S Stolarski, RS Douglass, AR Newman, PA Nielsen, JE Frith, SM Gupta, ML AF Pawson, Steven Stolarski, Richard S. Douglass, Anne R. Newman, Paul A. Nielsen, J. Eric Frith, Stacey M. Gupta, Mohan L. TI Goddard Earth Observing System chemistry-climate model simulations of stratospheric ozone-temperature coupling between 1950 and 2005 SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID GENERAL-CIRCULATION MODEL; INTERACTIVE CHEMISTRY; TROPICAL STRATOSPHERE; MIDDLE ATMOSPHERE; TRANSPORT MODEL; TROPOSPHERE; SENSITIVITY; TRENDS; DEPLETION; DYNAMICS AB Links between the stratospheric thermal structure and the ozone distribution are explored in the Goddard Earth Observing System chemistry-climate model (CCM). Ozone and temperature fields are validated using estimates based on observations. An experimental strategy is used to explore sensitivities of temperature and ozone using the CCM alongside the underlying general circulation model (GCM) with ozone specified from either observations or from a chemistry-transport model (CTM), which uses the same chemical modules as the CCM. In the CTM, upper stratospheric ozone is biased low compared to observations; GCM experiments reveal that using CTM ozone reduces a warm temperature bias near the stratopause in the GCM, and this improvement is also seen in the CCM. Near 5 hPa, the global-mean ozone profile is biased low in the CTM but is close to observations in the CCM, which suggests that the temperature feedbacks are important in simulating the ozone distribution in the middle stratosphere. In the low stratosphere there is a high bias in simulated ozone, which forces a warm bias in the CCM. The high ozone also leads to an overestimate in total column ozone of several tens of Dobson units in the polar regions. In the late part of the twentieth century the seasonal activation of chlorine, especially over Antarctica, destroys ozone as expected, so that chlorine-induced ozone decreases are overestimated in the CCM compared to the real atmosphere. Ozone-change experiments reveal that the thermal structures of the GCM and CCM respond in a similar manner to ozone differences between 1980 and 2000, with a peak ozone-induced temperature change of about 1.5 K (over 20 years) near the stratopause, which is at the low end of the range computed by other models. Greenhouse-gas-induced cooling increases with altitude and, near the stratopause, contributes an additional 1.3 K to the cooling near 1 hPa between 1980 and 2000. In the Antarctic, the ozone hole is simulated with some success by the CCM. As with many other models, the polar vortex is too persistent in late winter, but counteracting this, the CCM undergoes too much midwinter variability, meaning the ozone hole is more variable than it is in the real atmosphere. Temperature decreases associated with the ozone hole in the CCM are similar to those computed with other models. C1 [Pawson, Steven; Nielsen, J. Eric] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Gupta, Mohan L.] FAA, Washington, DC 20591 USA. [Stolarski, Richard S.; Douglass, Anne R.; Newman, Paul A.; Frith, Stacey M.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Greenbelt, MD 20771 USA. RP Pawson, S (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Mail Code 610-1, Greenbelt, MD 20771 USA. EM steven.pawson@nasa.gov RI Douglass, Anne/D-4655-2012; Newman, Paul/D-6208-2012; Stolarski, Richard/B-8499-2013; Pawson, Steven/I-1865-2014 OI Newman, Paul/0000-0003-1139-2508; Stolarski, Richard/0000-0001-8722-4012; Pawson, Steven/0000-0003-0200-717X NR 52 TC 98 Z9 99 U1 0 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 19 PY 2008 VL 113 IS D12 AR D12103 DI 10.1029/2007JD009511 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 317YC UT WOS:000257055300005 ER PT J AU Arvidson, R Adams, D Bonfiglio, G Christensen, P Cull, S Golombek, M Guinn, J Guinness, E Heet, T Kirk, R Knudson, A Malin, M Mellon, M McEwen, A Mushkin, A Parker, T Seelos, F Seelos, K Smith, P Spencer, D Stein, T Tamppari, L AF Arvidson, R. Adams, D. Bonfiglio, G. Christensen, P. Cull, S. Golombek, M. Guinn, J. Guinness, E. Heet, T. Kirk, R. Knudson, A. Malin, M. Mellon, M. McEwen, A. Mushkin, A. Parker, T. Seelos, F. Seelos, K. Smith, P. Spencer, D. Stein, T. Tamppari, L. TI Mars Exploration Program 2007 Phoenix landing site selection and characteristics SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID SIZE-FREQUENCY DISTRIBUTIONS; HEMISPHERE; ROCKS; ICE AB [1] To ensure a successful touchdown and subsequent surface operations, the Mars Exploration Program 2007 Phoenix Lander must land within 65 degrees to 72 degrees north latitude, at an elevation less than -3.5 km. The landing site must have relatively low wind velocities and rock and slope distributions similar to or more benign than those found at the Viking Lander 2 site. Also, the site must have a soil cover of at least several centimeters over ice or icy soil to meet science objectives of evaluating the environmental and habitability implications of past and current near-polar environments. The most challenging aspects of site selection were the extensive rock fields associated with crater rims and ejecta deposits and the centers of polygons associated with patterned ground. An extensive acquisition campaign of Odyssey Thermal Emission Imaging Spectrometer predawn thermal IR images, together with similar to 0.31 m/pixel Mars Reconnaissance Orbiter High Resolution Imaging Science Experiment images was implemented to find regions with acceptable rock populations and to support Monte Carlo landing simulations. The chosen site is located at 68.16 degrees north latitude, 233.35 degrees east longitude (areocentric), within a similar to 50 km wide (N-S) by similar to 300 km long (E-W) valley of relatively rock-free plains. Surfaces within the eastern portion of the valley are differentially eroded ejecta deposits from the relatively recent similar to 10-km-wide Heimdall crater and have fewer rocks than plains on the western portion of the valley. All surfaces exhibit polygonal ground, which is associated with fracture of icy soils, and are predicted to have only several centimeters of poorly sorted basaltic sand and dust over icy soil deposits. C1 [Arvidson, R.; Cull, S.; Guinness, E.; Heet, T.; Knudson, A.; Stein, T.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Adams, D.; Bonfiglio, G.; Golombek, M.; Guinn, J.; Parker, T.; Spencer, D.; Tamppari, L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [McEwen, A.; Smith, P.] Arizona State Univ, Dept Planetary Sci, Tempe, AZ 85287 USA. [Mellon, M.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80310 USA. [Mushkin, A.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. [Seelos, F.; Seelos, K.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Arvidson, R (reprint author), Washington Univ, Dept Earth & Planetary Sci, Campus Box 1169, St Louis, MO 63130 USA. EM arvidson@wunder.wustl.edu RI Seelos, Kimberly/F-4647-2015; Mellon, Michael/C-3456-2016; Seelos, Frank/C-7875-2016 OI Seelos, Kimberly/0000-0001-7236-0580; Seelos, Frank/0000-0001-9721-941X NR 38 TC 37 Z9 37 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUN 19 PY 2008 VL 113 AR E00A03 DI 10.1029/2007JE003021 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 318OR UT WOS:000257102000001 ER PT J AU Gunnarsdottir, HM Linscott, IR Callas, JL Cousins, MD Simpson, RA Tyler, GL AF Gunnarsdottir, H. M. Linscott, I. R. Callas, J. L. Cousins, M. D. Simpson, R. A. Tyler, G. L. TI Root-mean-square surface slopes of Phoenix landing sites with 75-cm bistatic radar received by Mars Odyssey SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID ORBITER LASER ALTIMETER; SCALE ROUGHNESS; MOLA DATA; DISTRIBUTIONS; MOON AB [1] Between August and December 2005, we conducted 76 oblique-incidence scattering experiments using the SRI International 46-m antenna in the Stanford foothills to illuminate Mars for 20-min periods with an unmodulated, 75-cm lambda, circularly polarized wave. The direct signal and a Martian surface echo, separated by differential Doppler frequency shifts, were received simultaneously by the one-bit receiver on board the Mars Odyssey spacecraft. Four of the proposed Phoenix landing regions, denoted A - D, were probed by at least one experiment. The surface echoes are characterized by both fluctuating amplitude and varying spectral width, which are responses to surface reflectivity and roughness variations. Our analysis of the echo data is based on quasi-specular scattering theory and makes use of high-resolution Mars Orbiter Laser Altimeter (MOLA) topographic maps to model the scattering surface in three dimensions along the specular track of the echo. We find MOLA topography sufficient to model scattering at 75-cm lambda, indicating that the effective horizontal scales being sensed by the radar are at or larger than the MOLA grid spacing of 150 - 500 m. We find that the RMS surface slopes for the proposed Phoenix landing regions, as determined using the Hagfors scattering law and applicable to those scales, rarely exceed 1 degrees, except in the presence of large craters and other surface irregularities. C1 [Gunnarsdottir, H. M.; Linscott, I. R.; Simpson, R. A.; Tyler, G. L.] Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA. [Cousins, M. D.] SRI Int, Menlo Pk, CA 94025 USA. [Callas, J. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Gunnarsdottir, HM (reprint author), Stanford Univ, Dept Elect Engn, 350 Serra Mall 325, Stanford, CA 94305 USA. EM hrefna@stanford.edu NR 16 TC 2 Z9 2 U1 1 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUN 19 PY 2008 VL 113 AR E00A02 DI 10.1029/2007JE003040 PG 7 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 318OR UT WOS:000257102000002 ER PT J AU Schmidt, ME Ruff, SW Mccoy, TJ Farrand, WH Johnson, JR Gellert, R Ming, DW Morris, RV Cabrol, N Lewis, KW Schroeder, C AF Schmidt, Mariek E. Ruff, Steven W. McCoy, Timothy J. Farrand, William H. Johnson, Jeffrey R. Gellert, Ralf Ming, Douglas W. Morris, Richard V. Cabrol, Nathalie Lewis, Kevin W. Schroeder, Christian TI Hydrothermal origin of halogens at Home Plate, Gusev Crater SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID MARTIAN METEORITES; MERIDIANI-PLANUM; SPIRIT ROVER; MARS; ASSEMBLAGES; CHEMISTRY; CHLORINE; MAGMAS; FLUIDS; SOILS AB In the Inner Basin of the Columbia Hills, Gusev Crater is Home Plate, an 80 m platform of layered clastic rocks of the Barnhill class with microscopic and macroscopic textures, including a bomb sag, suggestive of a phreatomagmatic origin. We present data acquired by the Spirit Mars Exploration Rover by Alpha Particle X-Ray Spectrometer (APXS), Mossbauer Spectrometer, Miniature Thermal Emission Spectrometer (Mini-TES), and Panoramic Camera (Pancam) for the Barnhill class rocks and nearby vesicular Irvine class basalts. In major element concentrations (e. g., SiO2, Al2O3, MgO, and FeO*), the two rock classes are similar, suggesting that they are derived from a similar magmatic source. The Barnhill class, however, has higher abundances of Cl, Br, Zn, and Ge with comparable SO3 to the Irvine basalts. Nanophase ferric oxide (np ox) and volcanic glass were detected in the Barnhill class rocks by Mossbauer and Mini-TES, respectively, and imply greater alteration and cooling rates in the Barnhill than in the Irvine class rocks. The high volatile elements in the Barnhill class agree with volcanic textures that imply interaction with a briny groundwater during eruption and (or) by later alteration. Differences in composition between the Barnhill and Irvine classes allow the fingerprinting of a Na-Mg-Zn-Ge-Cl-Br (+/- Fe +/- Ca +/- CO2) brine with low S. Nearby sulfate salt soils of fumarolic origin may reflect fractionation of an acidic S-rich vapor during boiling of a hydrothermal brine at depth. Persistent groundwater was likely present during and after the formation of Home Plate. C1 [Schmidt, Mariek E.; McCoy, Timothy J.] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA. [Ming, Douglas W.; Morris, Richard V.; Schroeder, Christian] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Ruff, Steven W.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Lewis, Kevin W.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Johnson, Jeffrey R.] US Geol Survey, Astrogeol Team, Flagstaff, AZ 86001 USA. [Gellert, Ralf] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada. [Cabrol, Nathalie] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Farrand, William H.] Space Sci Inst, Boulder, CO 80301 USA. RP Schmidt, ME (reprint author), Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, 10th & Constitution Ave, Washington, DC 20560 USA. EM schmidtm@si.edu RI Schroder, Christian/B-3870-2009; Lewis, Kevin/E-5557-2012; Johnson, Jeffrey/F-3972-2015 OI Schroder, Christian/0000-0002-7935-6039; NR 74 TC 41 Z9 41 U1 1 U2 19 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUN 19 PY 2008 VL 113 IS E6 AR E06S12 DI 10.1029/2007JE003027 PG 21 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 317ZK UT WOS:000257058800001 ER PT J AU Sullivan, R Arvidson, R Bell, JF Gellert, R Golombek, M Greeley, R Herkenhoff, K Johnson, J Thompson, S Whelley, P Wray, J AF Sullivan, R. Arvidson, R. Bell, J. F., III Gellert, R. Golombek, M. Greeley, R. Herkenhoff, K. Johnson, J. Thompson, S. Whelley, P. Wray, J. TI Wind-driven particle mobility on mars: Insights from Mars Exploration Rover observations at "El Dorado" and surroundings at Gusev Crater SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Review ID MAGNETIC-PROPERTIES EXPERIMENTS; GENERAL-CIRCULATION MODEL; ORBITER CAMERA; SAND TRANSPORT; SPIRIT ROVER; AEOLIAN SAND; PHYSICAL-PROPERTIES; TUNNEL SIMULATIONS; ATMOSPHERIC DUST; MERIDIANI-PLANUM AB The ripple field known as "El Dorado'' was a unique stop on Spirit's traverse where dust-raising, active mafic sand ripples and larger inactive coarse-grained ripples interact, illuminating several long-standing issues of Martian dust mobility, sand mobility, and the origin of transverse aeolian ridges. Strong regional wind events endured by Spirit caused perceptible migration of ripple crests in deposits SSE of El Dorado, erasure of tracks in sandy areas, and changes to dust mantling the site. Localized thermal vortices swept across El Dorado, leaving paths of reduced dust but without perceptibly damaging nearly cohesionless sandy ripple crests. From orbit, winds responsible for frequently raising clay-sized dust into the atmosphere do not seem to significantly affect dunes composed of (more easily entrained) sand-sized particles, a long-standing paradox. This disparity between dust mobilization and sand mobilization on Mars is due largely to two factors: (1) dust occurs on the surface as fragile, low-density, sand-sized aggregates that are easily entrained and disrupted, compared with clay-sized air fall particles; and (2) induration of regolith is pervasive. Light-toned bed forms investigated at Gusev are coarse-grained ripples, an interpretation we propose for many of the smallest linear, light-toned bed forms of uncertain origin seen in high-resolution orbital images across Mars. On Earth, wind can organize bimodal or poorly sorted loose sediment into coarse-grained ripples. Coarse-grained ripples could be relatively common on Mars because development of durable, well-sorted sediments analogous to terrestrial aeolian quartz sand deposits is restricted by the lack of free quartz and limited hydraulic sediment processing. C1 [Sullivan, R.; Bell, J. F., III; Wray, J.] Cornell Univ, Dept Astron, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [Arvidson, R.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Gellert, R.] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada. [Golombek, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Greeley, R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Herkenhoff, K.; Johnson, J.] US Geol Survey, Flagstaff, AZ 86001 USA. [Thompson, S.] Univ Nevada, Dept Geol Sci, Reno, NV 89557 USA. [Whelley, P.] SUNY Buffalo, Dept Geol, Buffalo, NY 14260 USA. RP Sullivan, R (reprint author), Cornell Univ, Dept Astron, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. EM rjs33@cornell.edu RI Wray, James/B-8457-2008; Whelley, Patrick/B-9560-2012 OI Wray, James/0000-0001-5559-2179; Whelley, Patrick/0000-0003-3266-9772 NR 134 TC 98 Z9 98 U1 4 U2 25 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUN 19 PY 2008 VL 113 IS E6 AR E06S07 DI 10.1029/2008JE003101 PG 70 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 317ZK UT WOS:000257058800002 ER PT J AU Krotkov, NA McClure, B Dickerson, RR Carn, SA Li, C Bhartia, PK Yang, K Krueger, AJ Li, ZQ Levelt, PF Chen, HB Wang, PC Lu, DR AF Krotkov, Nickolay A. McClure, Brittany Dickerson, Russell R. Carn, Simon A. Li, Can Bhartia, Pawan K. Yang, Kai Krueger, Arlin J. Li, Zhanqing Levelt, Pieternel F. Chen, Hongbin Wang, Pucai Lu, Daren TI Validation of SO2 retrievals from the Ozone Monitoring Instrument over NE China SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID RADIATIVE PROPERTIES; AEROSOL; EMISSIONS; MISSION; GOME; NEPHELOMETER; SCIAMACHY; INVENTORY; PERIOD; MODEL AB The Dutch-Finnish Ozone Monitoring Instrument (OMI) launched on the NASA Aura satellite in July 2004 offers unprecedented spatial resolution, coupled with contiguous daily global coverage, for space-based UV measurements of sulfur dioxide (SO2). We present a first validation of the OMI SO2 data with in situ aircraft measurements in NE China in April 2005. The study demonstrates that OMI can distinguish between background SO2 conditions and heavy pollution on a daily basis. The noise (expressed as the standard deviation, sigma) is similar to 1.5 DU (Dobson units; 1 DU = 2.69 . 10(16) molecules/cm(2)) for instantaneous field of view boundary layer (PBL) SO2 data. Temporal and spatial averaging can reduce the noise to sigma similar to 0.3 DU over a remote region of the South Pacific; the long-term average over this remote location was within 0.1 DU of zero. Under polluted conditions collection 2 OMI data are higher than aircraft measurements by a factor of two. Improved calibrations of the radiance and irradiance data ( collection 3) result in better agreement with aircraft measurements on polluted days. The air mass-corrected collection 3 data still show positive bias and sensitivity to UV absorbing aerosols. The difference between the in situ data and the OMI SO2 measurements within 30 km of the aircraft profiles was about 1 DU, equivalent to similar to 5 ppb from 0 to 3000 m altitude. Quantifying the SO2 and aerosol profiles and spectral dependence of aerosol absorption between 310 and 330 nm are critical for an accurate estimate of SO2 from satellite UV measurements. C1 [Krotkov, Nickolay A.; Yang, Kai] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [McClure, Brittany; Dickerson, Russell R.] Univ Maryland, Dept Chem, College Pk, MD 20742 USA. [McClure, Brittany; Dickerson, Russell R.; Li, Can; Li, Zhanqing] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Carn, Simon A.; Krueger, Arlin J.] Univ Maryland Baltimore Cty, Joint Res Earth Syst Technol, Baltimore, MD 21250 USA. [Bhartia, Pawan K.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Levelt, Pieternel F.] Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands. [Chen, Hongbin; Wang, Pucai; Lu, Daren] Chinese Acad Sci, Inst Atmospher Phys, Beijing 100021, Peoples R China. RP Krotkov, NA (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. EM krotkov@mhatter.gsfc.nasa.gov RI Li, Zhanqing/F-4424-2010; Li, Can/F-6867-2011; Krotkov, Nickolay/E-1541-2012; Bhartia, Pawan/A-4209-2016; Dickerson, Russell/F-2857-2010 OI Li, Zhanqing/0000-0001-6737-382X; Krotkov, Nickolay/0000-0001-6170-6750; Bhartia, Pawan/0000-0001-8307-9137; Dickerson, Russell/0000-0003-0206-3083 NR 45 TC 75 Z9 80 U1 0 U2 19 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 18 PY 2008 VL 113 IS D16 AR D16S40 DI 10.1029/2007JD008818 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 317YM UT WOS:000257056300001 ER PT J AU Pieters, CM Klima, RL Hiroi, T Dyar, MD Lane, MD Treiman, AH Noble, SK Sunshine, JM Bishop, JL AF Pieters, Carle M. Klima, Rachel L. Hiroi, Takahiro Dyar, M. Darby Lane, Melissa D. Treiman, Allan H. Noble, Sarah K. Sunshine, Jessica M. Bishop, Janice L. TI Martian dunite NWA 2737: Integrated spectroscopic analyses of brown olivine SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID PARTICULATE SURFACES; REFLECTANCE SPECTRA; INFRARED-SPECTRA; SNC METEORITES; PARTICLE-SIZE; UPPER-MANTLE; EMISSION; MINERALS; MARS; IRON AB A second Martian meteorite has been identified that is composed primarily of heavily shocked dunite, Northwest Africa (NWA) 2737. This meteorite has several similarities to the Chassigny dunite cumulate, but the olivine is more Mg rich and, most notably, is very dark and visually brown. Carefully coordinated analyses of NWA 2737 whole-rock and olivine separates were undertaken using visible and near-infrared reflectance, midinfrared emission and reflectance, and Mossbauer spectroscopic studies of the same samples along with detailed petrography, chemistry, scanning electron microscopy, and transmission electron microscopy analyses. Midinfrared spectra of this sample indicate that the olivine is fully crystalline and that its molecular structure remains intact. The unusual color and spectral properties that extend from the visible through the near-infrared part of the spectrum are shown to be due to nanophase metallic iron particles dispersed throughout the olivine during a major shock event on Mars. Although a minor amount of Fe(3+) is present, it cannot account for the well-documented unusual optical properties of Martian meteorite NWA 2737. Perhaps unique to the Martian environment, this "brown'' olivine exhibits spectral properties that can potentially be used to remotely explore the pressure-temperature history of surface geology as well as assess surface composition. C1 [Pieters, Carle M.; Klima, Rachel L.; Hiroi, Takahiro] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Bishop, Janice L.] NASA Ames Res Ctr, Mountain View, CA 94043 USA. [Dyar, M. Darby] Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA. [Lane, Melissa D.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Noble, Sarah K.] Johnson Space Ctr, Astromat Res & Explorat Sci Div, Houston, TX 77058 USA. [Sunshine, Jessica M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Treiman, Allan H.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Bishop, Janice L.] Search Extraterrestrial Intelligence Inst, Mountain View, CA USA. RP Pieters, CM (reprint author), Brown Univ, Dept Geol Sci, 324 Brook St, Providence, RI 02912 USA. EM carle_pieters@brown.edu RI Noble, Sarah/D-7614-2012 NR 54 TC 24 Z9 24 U1 1 U2 7 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 JUN 18 PY 2008 VL 113 IS E6 AR E06004 DI 10.1029/2007JE002939 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 317ZJ UT WOS:000257058700001 ER PT J AU Rietmeijer, FJM Pun, A Nuth, JA AF Rietmeijer, Frans J. M. Pun, Aurora Nuth, Joseph A., III TI A deep metastable eutectic iron-aluminate SO CHEMICAL PHYSICS LETTERS LA English DT Article ID CONDENSATION; SYSTEM; ENVIRONMENTS; SILICATES; SMOKES AB A small number of amorphous nanograins with a silica-free, iron-alumina composition was formed during laboratory condensation of a low-silica Al-Fe-SiO-H(2)-O(2) vapor. Very rapid cooling of the vapor created conditions that were conducive to the formation of deep metastable eutectic compounds with a specific composition. High Fe(2+)/Fe(3+) ratios during condensation are reflected in the 1.8FeO center dot 0.6Fe(2)O(3) center dot Al(2)O(3) composition of this amorphous deep metastable eutectic compound. (c) 2008 Elsevier B.V. All rights reserved. C1 [Rietmeijer, Frans J. M.; Pun, Aurora] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. [Nuth, Joseph A., III] NASA, Goddard Space Flight Ctr, Astrochem Lab, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. RP Rietmeijer, FJM (reprint author), Univ New Mexico, Dept Earth & Planetary Sci, MSC03-2040, Albuquerque, NM 87131 USA. EM fransjmr@unm.edu RI Nuth, Joseph/E-7085-2012 NR 18 TC 3 Z9 3 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2614 J9 CHEM PHYS LETT JI Chem. Phys. Lett. PD JUN 17 PY 2008 VL 458 IS 4-6 BP 355 EP 358 DI 10.1016/j.cplett.2008.05.020 PG 4 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 309GT UT WOS:000256449400022 ER PT J AU Minnis, P Yost, CR Sun-Mack, S Chen, Y AF Minnis, Patrick Yost, Chris R. Sun-Mack, Sunny Chen, Yan TI Estimating the top altitude of optically thick ice clouds from thermal infrared satellite observations using CALIPSO data SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID LIDAR AB The difference between cloud-top altitude Z(top) and infrared effective radiating height Z(eff) for optically thick ice clouds is examined using April 2007 data taken by the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) and the Moderate-Resolution Imaging Spectroradiometer (MODIS). For even days, the difference Delta Z between CALIPSO Z(top) and MODIS Z(eff) is 1.58 +/- 1.26 km. The linear fit between Z(top) and Z(eff), applied to odd-day data, yields a difference of 0.03 +/- 1.21 km and can be used to estimate Z(top) from any infrared-based Z(eff) for thick ice clouds. Random errors appear to be due primarily to variations in cloud ice-water content (IWC). Radiative transfer calculations show that Delta Z corresponds to an optical depth of similar to 1, which based on observed ice-particle sizes yields an average cloud-top IWC of similar to 0.015 gm(-3), a value consistent with in situ measurements. The analysis indicates potential for deriving cloud-top IWC using dual-satellite data. C1 [Minnis, Patrick] NASA, Langley Res Ctr, Hampton, VA USA. [Yost, Chris R.; Sun-Mack, Sunny; Chen, Yan] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. RP Minnis, P (reprint author), NASA, Langley Res Ctr, Hampton, VA USA. EM patrick.minnis@nasa.gov RI Minnis, Patrick/G-1902-2010 OI Minnis, Patrick/0000-0002-4733-6148 NR 14 TC 46 Z9 48 U1 1 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUN 17 PY 2008 VL 35 IS 12 AR L12801 DI 10.1029/2008GL033947 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 317WI UT WOS:000257050700003 ER PT J AU Mccoy, TJ Sims, M Schmidt, ME Edwards, L Tornabene, LL Crumpler, LS Cohen, BA Soderblom, LA Blaney, DL Squyres, SW Arvidson, RE Rice, JW Treguier, E d'Uston, C Grant, JA McSween, HY Golombek, MP Haldemann, AFC de Souza, PA AF McCoy, T. J. Sims, M. Schmidt, M. E. Edwards, L. Tornabene, L. L. Crumpler, L. S. Cohen, B. A. Soderblom, L. A. Blaney, D. L. Squyres, S. W. Arvidson, R. E. Rice, J. W., Jr. Treguier, E. d'Uston, C. Grant, J. A. McSween, H. Y., Jr. Golombek, M. P. Haldemann, A. F. C. de Souza, P. A., Jr. TI Structure, stratigraphy, and origin of Husband Hill, Columbia Hills, Gusev Crater, Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID ROVER; SPIRIT AB The strike and dip of lithologic units imaged in stereo by the Spirit rover in the Columbia Hills using three-dimensional imaging software shows that measured dips (15-32 degrees) for bedding on the main edifice of the Columbia Hill are steeper than local topography (similar to 8-10 degrees). Outcrops measured on West Spur are conformable in strike with shallower dips (7-15 degrees) than observed on Husband Hill. Dips are consistent with observed strata draping the Columbia Hills. Initial uplift was likely related either to the formation of the Gusev Crater central peak or ring or through mutual interference of overlapping crater rims. Uplift was followed by subsequent draping by a series of impact and volcaniclastic materials that experienced temporally and spatially variable aqueous infiltration, cementation, and alteration episodically during or after deposition. West Spur likely represents a spatially isolated depositional event. Erosion by a variety of processes, including mass wasting, removed tens of meters of materials and formed the Tennessee Valley primarily after deposition. This was followed by eruption of the Adirondack-class plains basalt lava flows which embayed the Columbia Hills. Minor erosion, impact, and aeolian processes have subsequently modified the Columbia Hills. C1 [McCoy, T. J.; Schmidt, M. E.] Smithsonian Inst, Natl Museum Amer Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Sims, M.; Edwards, L.] NASA Ames, Intelligent Syst Div, Moffett Field, CA 94035 USA. [Tornabene, L. L.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Cohen, B. A.] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA. [Soderblom, L. A.] US Geol Survey, Branch Astrogeol, Flagstaff, AZ 86001 USA. [Blaney, D. L.; Golombek, M. P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Arvidson, R. E.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Crumpler, L. S.] New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA. [Treguier, E.; d'Uston, C.] Ctr Etud Spatiale Rayonnements, OMP, F-31400 Toulouse, France. [Grant, J. A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Haldemann, A. F. C.] European Space Technol Ctr, European Space Agcy, HME ME, NL-2200 AG Noordwijk, Netherlands. [McSween, H. Y., Jr.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Rice, J. W., Jr.] Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. [Squyres, S. W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [de Souza, P. A., Jr.] Vallourec Res Ctr, Aulnoye Aymeries, France. RP Mccoy, TJ (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Dept Mineral Sci, Washington, DC 20560 USA. EM mccoyt@si.edu RI de Souza, Paulo/B-8961-2008; Centre, TasICT/D-1212-2011; OI de Souza, Paulo/0000-0002-0091-8925; Treguier, Erwan/0000-0002-7347-2805 NR 48 TC 23 Z9 23 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUN 17 PY 2008 VL 113 IS E6 AR E06S03 DI 10.1029/2007JE003041 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 317ZI UT WOS:000257058600002 ER PT J AU Masek, JG Huang, CQ Wolfe, R Cohen, W Hall, F Kutler, J Nelson, P AF Masek, Jeffrey G. Huang, Chengquan Wolfe, Robert Cohen, Warren Hall, Forrest Kutler, Jonathan Nelson, Peder TI North American forest disturbance mapped from a decadal Landsat record SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE remote sensing; Landsat; change detection; forestry; disturbance ID FIRE FREQUENCY; MODIS DATA; BOREAL FOREST; TASSELLED CAP; UNITED-STATES; COVER DATA; DATA SET; CARBON; IMAGERY; TRANSFORMATION AB Forest disturbance and recovery are critical ecosystem processes, but the spatial pattern of disturbance has never been mapped across North America. The LEDAPS (Landsat Ecosystem Disturbance Adaptive Processing System) project has assembled a wall-to-wall record of stand-clearing disturbance (clearcut harvest, fire) for the United States and Canada for the period 1990-2000 using the Landsat satellite archive. Landsat TM and ETM+ data were first converted to surface reflectance using the MODIS/6S atmospheric correction approach. Disturbance and early recovery were mapped using the temporal change in a Tasseled-Cap "Disturbance Index" calculated from the early (similar to 1990) and later (similar to 2000) images. Validation of the continental mapping has been carried out using a sample of biennial Landsat time series from 23 locations across the United States. Although a significant amount of disturbance (30-60%) cannot be mapped due to the long interval between image acquisition dates, the biennial analyses allow a first-order correction of the decadal mapping. Our results indicate disturbance rates of up to 2-3% per year are common across the US and Canada due primarily to harvest and forest fire. Rates are highest in the southeastern US, the Pacific Northwest, Maine, and Quebec. The mean disturbance rate for the conterminous United States (the "lower 48" states and District of Columbia) is calculated as 0.9 +/-0.2% per year, corresponding to a turnover period of 110 years. (C) 2008 Elsevier Inc. All rights reserved. C1 [Masek, Jeffrey G.; Wolfe, Robert; Kutler, Jonathan] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA. [Huang, Chengquan] Univ Maryland, Dept Geog, College Pk, MD 20742 USA. [Cohen, Warren; Nelson, Peder] US Forest Serv, Pacific NW Res Stn, Corvallis, OR 97331 USA. [Hall, Forrest] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. RP Masek, JG (reprint author), NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA. EM jeffrey.G.Masek@nasa.gov RI Masek, Jeffrey/D-7673-2012; Wolfe, Robert/E-1485-2012; OI Wolfe, Robert/0000-0002-0915-1855; Huang, Chengquan/0000-0003-0055-9798 NR 45 TC 199 Z9 214 U1 10 U2 83 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD JUN 16 PY 2008 VL 112 IS 6 BP 2914 EP 2926 DI 10.1016/j.rse.2008.02.010 PG 13 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 316YR UT WOS:000256986400015 ER PT J AU Ichoku, C Giglio, L Wooster, MJ Remer, LA AF Ichoku, Charles Giglio, Louis Wooster, Martin J. Remer, Lorraine A. TI Global characterization of biomass-burning patterns using satellite measurements of fire radiative energy SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE biomass burning; wildfire; fire radiative power (FRP); fire radiative energy (FRE); MODIS ID MODIS; SYSTEM; AVHRR; EARTH AB Remote sensing is the most practical means of measuring energy release from large open-air biomass burning. Satellite measurement of fire radiative energy (FRE) release rate or power (FRP) enables distinction between fires of different strengths. Based on a 1-km resolution fire data acquired globally by the MODerate-resolution Imaging Spectro-radiometer (MODIS) sensor aboard the Terra and Aqua satellites from 2000 to 2006, instantaneous FRP values ranged between 0.02 MW and 1866 MW, with global daily means ranging between 20 and 40 MW. Regionally, at the Aqua-MODIS afternoon overpass, the mean FRP values for Alaska, Western US, Western Australia, Quebec and the rest of Canada are significantly higher than these global means, with Quebec having the overall highest value of 85 MW. Analysis of regional mean FRP per unit area of land (FRP flux) shows that at peak fire season in certain regions, fires can be responsible for up to 0.2 W/m(2) at peak time of day. Zambia has the highest regional monthly mean FRP flux of similar to 0.045 W/m(2) at peak time of day and season, while the Middle East has the lowest value of similar to 0.0005 W/m(2). A simple scheme based on FRP has been devised to classify fires into five categories, to facilitate fire rating by strength, similar to earthquakes and hurricanes. The scheme uses MODIS measurements of FRP at 1-km resolution as follows: category 1 (< 100 MW), category 2 (100 to < 500 MW), category 3 (500 to < 1000 MW), category 4 (1000 to < 1500 MW), category 5 (2:1500 MW). In most regions of the world, over 90% of fires fall into category 1, while only less than 1% fall into each of categories 3 to 5, although these Proportions may differ significantly from day to day and by season. The frequency of occurrence of the larger fires is region specific, and could not be explained by ecosystem type alone. Time-series analysis of the proportions of higher category fires based on MODIS-measured FRP from 2002 to 2006 does not show any noticeable trend because of the short time period. (C) 2008 Elsevier Inc. All rights reserved. C1 [Ichoku, Charles; Giglio, Louis; Remer, Lorraine A.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ichoku, Charles] Univ Maryland, ESSIC, College Pk, MD 20742 USA. [Giglio, Louis] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Wooster, Martin J.] Kings Coll London, Dept Geog, Strand, London WC2R 2LS, England. RP Ichoku, C (reprint author), NASA Goddard Space Flight Ctr, Code 613-2, Greenbelt, MD 20771 USA. EM Charles.Ichoku@nasa.gov RI Ichoku, Charles/E-1857-2012 OI Ichoku, Charles/0000-0003-3244-4549 NR 18 TC 73 Z9 76 U1 4 U2 25 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD JUN 16 PY 2008 VL 112 IS 6 BP 2950 EP 2962 DI 10.1016/j.rse.2008.02.009 PG 13 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 316YR UT WOS:000256986400018 ER PT J AU Schaeffer, BA Morrison, JM Kamykowski, D Feldman, GC Xie, L Liu, YY Sweet, W McCulloch, A Banks, S AF Schaeffer, Blake A. Morrison, John M. Kamykowski, Daniel Feldman, Gene C. Xie, Lian Liu, Yanyun Sweet, William McCulloch, Anita Banks, Stuart TI Phytoplankton biomass distribution and identification of productive habitats within the Galapagos Marine Reserve by MODIS, a surface acquisition system, and in-situ measurements SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE chlorophyll a; MODIS; surface acquisition system; Galapagos Marine Reserve; phytoplankton; biomass; El Nino; productive habitats ID EASTERN TROPICAL PACIFIC; NINO-SOUTHERN OSCILLATION; OCEAN MODEL HYCOM; EL-NINO; EQUATORIAL PACIFIC; VERTICAL COORDINATE; ISLANDS; ARCHIPELAGO; PENGUIN; IRON AB The Galapagos Marine Reserve (GMR) is one of the most diverse ecosystems in the world. Phytoplankton are the base of the ecosystem food chain for many higher trophic organisms, so identifying phytoplankton biomass distribution is the first step in understanding the dynamic environment for effective management of the GMR. Moderate Resolution Imaging Spectroradiometer (MODIS) and hyperspectral surface acquisition system derived chlorophyll, in-situ chlorophyll fluorescence, nitrate, salinity, and temperature were collected from March 2005 to the onset of a mild El Nino in November 2006. Islands in the eastern GMR, such as San Cristobal and Espanola, are the first to experience impacts of El Nino and southern migration of the Equatorial Front. Productive habitats were defined as surface waters with salinities > 34, temperatures < 24 degrees C, and chlorophyll a > 0.4 mg m(-3). Six temporally variable productive habitats identified were: west of Isabela Island, southwest of Floreana Island, south of Santa Cruz, between Santiago and Santa Cruz Islands, and on the eastern side near San Cristobal Island. Model results coupled with surface acquisition system derived chlorophyll indicated productive habitats may also occur for short periods and at a distance from islands such as when the Equatorial Undercurrent (EUC) and South Equatorial Current (SEC) collide over the seamounts north of Isabela Island. All productive habitats were related to topographic upwelling from the EUC into surface waters. (C) 2008 Elsevier Inc. All rights reserved. C1 [Schaeffer, Blake A.] US EPA Natl Hlth & Environm Effects Res Lab, Gulf Ecol Div, Gulf Breeze, FL 32563 USA. [Morrison, John M.] Univ N Carolina, Dept Phys & Phys Oceanog, Wilmington, NC 28401 USA. [Kamykowski, Daniel; Xie, Lian; Liu, Yanyun; Sweet, William; McCulloch, Anita] N Carolina State Univ, Dept Marine Earth & Atmospher Sci, Raleigh, NC 27695 USA. [Feldman, Gene C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Banks, Stuart] Charles Darwin Res Stn, Galapagos Isl, Ecuador. RP Schaeffer, BA (reprint author), US EPA Natl Hlth & Environm Effects Res Lab, Gulf Ecol Div, 1 Sabine Isl Dr, Gulf Breeze, FL 32563 USA. EM BlakeSchaeffer@gmail.com RI McCulloch, Anita/E-4685-2010; Liu, Yanyun/A-5785-2011 OI Liu, Yanyun/0000-0002-9754-6370 NR 40 TC 13 Z9 16 U1 3 U2 17 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD JUN 16 PY 2008 VL 112 IS 6 BP 3044 EP 3054 DI 10.1016/j.rse.2008.03.005 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 316YR UT WOS:000256986400025 ER PT J AU Giglio, L Csiszar, I Restas, A Morisette, JT Schroeder, W Morton, D Justice, CO AF Giglio, Louis Csiszar, Ivan Restas, Agoston Morisette, Jeffrey T. Schroeder, Wilfrid Morton, Douglas Justice, Christopher O. TI Active fire detection and characterization with the advanced spaceborne thermal emission and reflection radiometer (ASTER) SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE biomass burning; fire detection; fire radiative power; ASTER; MODIS ID RADIATIVE ENERGY; AVHRR DATA; MODIS; SATELLITE; TEMPERATURE; RESOLUTION; VALIDATION; PRODUCTS AB We present an automated fire detection algorithm for the Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) sensor capable of mapping actively burning fires at 30-m spatial resolution. For daytime scenes, our approach uses near infrared and short-wave infrared reflectance imagery. For nighttime scenes a simple short wave infrared radiance threshold is applied. Based on a statistical analysis of 100 ASTER scenes, we established omission and commission error rates for nine different regions. In most regions the probability of detection was between 0.8 and 0.9. Probabilities of false alarm varied between 9 x 10(-8) (India) and 2x10(-5) (USA/Canada). In most cases, the majority of false fire pixels were linked to clusters of true fire pixels, suggesting that most false fire pixels occur along ambiguous fire boundaries. We next consider fire characterization, and formulate an empirical method for estimating fire radiative power (FRP), a measure of fire intensity, using three ASTER thermal infrared channels. We performed a preliminary evaluation of our retrieval approach using four prescribed fires which were active at the time of the Terra overpass for which limited ground-truth data were collected. Retrieved FRP was accurate to within 20%, with the exception of one fire partially obscured by heavy soot. (C) 2008 Elsevier Inc. All rights reserved. C1 [Giglio, Louis] Sci Syst & Applicat Inc, Lanham, MD USA. [Giglio, Louis; Csiszar, Ivan; Schroeder, Wilfrid; Morton, Douglas; Justice, Christopher O.] Univ Maryland, Dept Geog, College Pk, MD 20742 USA. [Restas, Agoston] Szendro Fire Dept, Szendro, Hungary. [Morisette, Jeffrey T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Giglio, L (reprint author), Sci Syst & Applicat Inc, Lanham, MD USA. EM louis_giglio@ssaihq.com RI Csiszar, Ivan/D-2396-2010; Schroeder, Wilfrid/F-6738-2010; Morton, Douglas/D-5044-2012 NR 34 TC 44 Z9 45 U1 2 U2 26 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD JUN 16 PY 2008 VL 112 IS 6 BP 3055 EP 3063 DI 10.1016/j.rse.2008.03,003 PG 9 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 316YR UT WOS:000256986400026 ER PT J AU Drolet, GG Middleton, EM Huemmrich, KF Hall, FG Amiro, BD Barr, AG Black, TA McCaughey, JH Margolis, HA AF Drolet, G. G. Middleton, E. M. Huemmrich, K. F. Hall, F. G. Amiro, B. D. Barr, A. G. Black, T. A. McCaughey, J. H. Margolis, H. A. TI Regional mapping of gross light-use efficiency using MODIS spectral indices SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE photochemical reflectance index; gross light-use efficiency; MODIS; flux towers; gross ecosystem productivity; boreal forest; regional mapping; shadow fraction ID PHOTOCHEMICAL REFLECTANCE INDEX; RADIATION-USE EFFICIENCY; LEAF-AREA INDEX; NET PRIMARY PRODUCTION; CALIFORNIA CHAPARRAL ECOSYSTEM; FOREST BIOPHYSICAL STRUCTURE; CARBON-DIOXIDE EXCHANGE; BOREAL CONIFER FORESTS; ASPEN-HAZELNUT FOREST; WATER-VAPOR AB Direct estimation of photosynthetic light-use efficiency (WE) from space would be of significant benefit to LUE-based models which use inputs from remote sensing to estimate terrestrial productivity. The Photochemical Reflectance Index (PRI) has shown promise in tracking LUE at the leaf- to small canopy levels, but its use at regional to global scales still remains a challenge. In this study, we used different formulations of PRI calculated from the MODIS ocean band centered at 531 nm and a set of alternative reference bands at 488, 551, and 678 nm to explore the relationship between PRI and LUE where WE was measured at eight eddy covariance flux towers located in the boreal forest of Saskatchewan, Canada. The magnitude and variability of WE was significantly lower at the times when useful MODIS ocean band images were available (i.e. around midday under clear-sky conditions) relative to the rest of the growing season. PR1678 (reference band at 678 nm) showed the strongest relationship (r(2)=0.70) with LUE90a (i.e. 90-minute mean WE calculated using Absorbed Photosynthetically Active Radiation, APAR), but only when all sites were combined. Overall, the relationships between the MODIS PRIs and LUE90a were always stronger for observations closer to the backscatter direction and there were no significant differences in the strength of the correlations whether LUE was calculated based on incident PAR or on APAR. Predictions of ecosystem photosynthesis at the time of the MODIS overpasses were significantly improved by multiplying either PAR or APAR by MODIS PRI (r(2) improved from 0.09 to 0.44 and 0.54 depending on the PRI formulation). We used our PRI-LUE model to create a regional LUE90a map for the three cover types covering 47,500 km(2) around the flux sites. The MODIS PRI-derived LUE90a map appeared to capture more realistic spatial heterogeneity of LUE across the landscape compared to a daily WE map derived using the look-up table in the MODIS GPP (MOD17) algorithm. While our LUE map is only a snapshot of minimum regional LUE90a values, with appropriate gap-filling methods it could be used to improve regional-scale monitoring of GPR Moreover, the strong relationship between midday and daily WE on clear days (r(2)=0.93) indicates that instantaneous MODIS observations of LUE90a could be used to estimate daily WE. Finally, pixel shadow fraction from the 5-Scale geometric-optical model was closely related to both MODIS PRI and tower-derived LUE suggesting that differences in stand leaf area and in diffuse illumination among flux sites play a role in the relationship we observed between LUE and MODIS PRI. (C) 2008 Elsevier Inc. All rights reserved. C1 [Drolet, G. G.; Margolis, H. A.] Univ Laval, Fac Foresterie & Geomat, Ctr Etude Foret, Ste Foy, PQ G1K 7P4, Canada. [Middleton, E. M.; Huemmrich, K. F.; Hall, F. G.; Margolis, H. A.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. [Huemmrich, K. F.; Hall, F. G.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. [Amiro, B. D.] Univ Manitoba, Dept Soil Sci, Winnipeg, MB R3T 2N2, Canada. [Barr, A. G.] Meteorol Serv Canada, Atmospher Sci & Technol Directorate, Saskatoon, SK S7N 3H5, Canada. [Black, T. A.] Univ British Columbia, Fac Agr Sci, Vancouver, BC V6T 1Z4, Canada. [McCaughey, J. H.] Queens Univ, Dept Geog, Kingston, ON K7L 3N6, Canada. RP Margolis, HA (reprint author), Univ Laval, Fac Foresterie & Geomat, Ctr Etude Foret, Ste Foy, PQ G1K 7P4, Canada. EM hank.margolis@sbf.ulaval.ca RI Barr, Alan/H-9939-2014 NR 83 TC 87 Z9 91 U1 6 U2 41 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD JUN 16 PY 2008 VL 112 IS 6 BP 3064 EP 3078 DI 10.1016/j.rse.2008.03.002 PG 15 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 316YR UT WOS:000256986400027 ER PT J AU Roy, DP Ju, J Lewis, P Schaaf, C Gao, F Hansen, M Lindquist, E AF Roy, David P. Ju, Junchang Lewis, Philip Schaaf, Crystal Gao, Feng Hansen, Matt Lindquist, Erik TI Multi-temporal MODIS-Landsat data fusion for relative radiometric normalization, gap filling, and prediction of Landsat data SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE ETM; MODIS; data fusion; radiometric normalization; BRDF; SLC-off gap filling; image mosaicking ID REFLECTANCE DISTRIBUTION FUNCTION; BIDIRECTIONAL REFLECTANCE; ATMOSPHERIC CORRECTION; ALBEDO RETRIEVALS; SATELLITE-OBSERVATIONS; SURFACE REFLECTANCE; NADIR REFLECTANCE; SPECTRAL ALBEDO; DATA CONTINUITY; BRDF MODELS AB A semi-physical fusion approach that uses the MODIS BRDF/Albedo land surface characterization product and Landsat ETM+ data to predict ETM+ reflectance on the same, an antecedent, or subsequent date is presented. The method may be used for ETM+ cloud/cloud shadow and SLC-off gap filling and for relative radiometric normalization. It is demonstrated over three study sites, one in Africa and two in the U.S. (Oregon and Idaho) that were selected to encompass a range of land cover land use types and temporal variations in solar illumination, land cover, land use, and phenology. Specifically, the 30 m ETM+ spectral reflectance is predicted for a desired date as the product of observed ETM+ reflectance and the ratio of the 500 m surface reflectance modeled using the MODIS BRDF spectral model parameters and the sun-sensor geometry on the predicted and observed Landsat dates. The difference between the predicted and observed ETM+ reflectance (prediction residual) is compared with the difference between the ETM+ reflectance observed on the two dates (temporal residual) and with respect to the MODIS BRDF model parameter quality. For all three scenes, and all but the shortest wavelength band, the mean prediction residual is smaller than the mean temporal residual, by up to a factor of three. The accuracy is typically higher at ETM+ pixel locations where the MODIS BRDF model parameters are derived using the best quality inversions. The method is most accurate for the ETM+ near-infrared (NIR) band; mean NIR prediction residuals are 9%,12% and 14% of the mean NIR scene reflectance of the African, Oregon and Idaho sites respectively. The developed fusion approach may be applied to any high spatial resolution satellite data, does not require any tuning parameters and so may be automated, is applied on a per-pixel basis and is unaffected by the presence of missing or contaminated neighboring Landsat pixels, accommodates for temporal variations due to surface changes (e.g., phenological, land cover/land use variations) observable at the 500 m MODIS BRDF/Albedo product resolution, and allows for future improvements through BRDF model refinement and error assessment. (C) 2008 Elsevier Inc. All rights reserved. C1 [Roy, David P.; Ju, Junchang; Hansen, Matt; Lindquist, Erik] S Dakota State Univ, Geog Informat Sci Ctr Excellence, Brookings, SD 57007 USA. [Lewis, Philip] UCL, NERC Ctr Terr Carbon Dynam, London WC1E 6BT, England. [Lewis, Philip] UCL, Dept Geog, London WC1E 6BT, England. [Schaaf, Crystal] Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA. [Gao, Feng] Earth Resources Technol Inc, Annapolis Jct, MD 20701 USA. [Gao, Feng] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Roy, DP (reprint author), S Dakota State Univ, Geog Informat Sci Ctr Excellence, Brookings, SD 57007 USA. EM david.roy@sdstate.edu RI Gao, Feng/F-3944-2010; Lewis, Philip/C-1588-2008 OI Lewis, Philip/0000-0002-8562-0633 NR 75 TC 172 Z9 193 U1 9 U2 75 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD JUN 16 PY 2008 VL 112 IS 6 BP 3112 EP 3130 DI 10.1016/j.rse.2008.03.009 PG 19 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 316YR UT WOS:000256986400031 ER PT J AU Brunner, B Yu, JY Mielke, RE MacAskill, JA Madzunkov, S McGenity, TJ Coleman, M AF Brunner, Benjamin Yu, Jae-Young Mielke, Randall E. MacAskill, John A. Madzunkov, Stojan McGenity, Terry J. Coleman, Max TI Different isotope and chemical patterns of pyrite oxidation related to lag and exponential growth phases of Acidithiobacillus ferrooxidans reveal a microbial growth strategy SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Acidithiobacillus ferrooxidans; pyrite oxidation; growth phases; oxygen and sulfur isotope; composition of sulfate; degassing of sulfur dioxide from acid; solutions; sulfite ID THIOBACILLUS-THIOOXIDANS CELLS; INORGANIC SULFUR-COMPOUNDS; SULFITE OXIDATION; OXYGEN ISOTOPES; METAL SULFIDES; BISULFITE ION; ACIDIC MEDIA; FERROUS IRON; FERRIC IRON; SULFATE AB The solution chemistry during the initial (slow increase of dissolved iron and sulfate) and main stage (rapid increase of dissolved iron and sulfate) of pyrite leaching by Acidithiobacillus ferrooxidans (Af) at a starting pH of 2.05 shows significant differences. During the initial stage, ferrous iron (Fe2+) is the dominant iron species in solution and the molar ratio of produced sulfate (SO42-) and total iron (Fe-tot) is 1.1, thus does not reflect the stoichiometry of pyrite (FeS2). During the main stage, ferric iron (Fe3+) is the dominant iron species in solution and the SO42-:Fe-tot ratio is with 1.9, close to the stoichiometry of FeS2. Another difference between initial and main stage is an initial trend to slightly higher pH values followed by a drop during the main stage to pH 1.84. These observations raise the question if there are different modes of bioleaching of pyrite, and if there are, what those modes imply in terms of leaching mechanisms. Different oxygen and sulfur isotope trends of sulfate during the initial and main stages of pyrite oxidation confirm that there are two pyrite bioleaching modes. The biochemical reactions during initial stage are best explained by the net reaction FeS2+3O(2) double right arrow Fe2++SO42-+SO2(g). The clegassing of sulfur dioxide (SO2) acts as sink for sulfur depleted in S-34 compared to pyrite, and is the cause of the SO42-:Fe-tot ratio of 1.1 and the near constant pH. During the exponential phase, pyrite sulfur is almost quantitatively converted to sulfate, according to the net reaction FeS2+15/4O(2)+1/2H(2)O double right arrow Fe3++2SO(4)(2-)+H+. We hypothesize that the transition between the modes of bioleaching of pyrite is due to the impact of the accumulation of ferrous iron, which induces changes in the metabolic activity of Af and may act as an inhibitor for the oxidation of sulfur species. This transition defines a fundamental change in the growth strategy of Af A mode, where bacteria gain energy by oxidation of elemental sulfur to sulfite but show little growth is switched into a mode, where bacteria gain a smaller amount of energy by the oxidation of ferrous iron, but induce much faster pyrite leaching rates due to the production of ferric iron. (C) 2008 Elsevier B.V. All rights reserved. C1 [Brunner, Benjamin; Yu, Jae-Young; Mielke, Randall E.; Coleman, Max] CALTECH, Jet Prop Lab, Planetary Sci & Life Detect Sect, Pasadena, CA 91109 USA. [Yu, Jae-Young] Kangwon Natl Univ, Dept Geol, Chunchon 200701, Kangwon Do, South Korea. [MacAskill, John A.; Madzunkov, Stojan] CALTECH, Jet Prop Lab, Astrophys & Space Sci Sect, Pasadena, CA 91109 USA. [McGenity, Terry J.] Univ Essex, Dept Biol Sci, Colchester CO4 3SQ, Essex, England. RP Brunner, B (reprint author), Max Planck Inst Marine Microbiol, Celsiusstr 1, D-28359 Bremen, Germany. EM bbrunner@mpi-bremen.de RI McGenity, Terry/B-8661-2011; Coleman, Max/A-1303-2007; Brunner, Benjamin/F-2027-2011; OI Coleman, Max/0000-0002-5514-1826; McGenity, Terence/0000-0002-1497-8822 NR 58 TC 23 Z9 24 U1 3 U2 22 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD JUN 15 PY 2008 VL 270 IS 1-2 BP 63 EP 72 DI 10.1016/j.epsl.2008.03.019 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321HE UT WOS:000257294500006 ER PT J AU Martins, Z Botta, O Fogel, ML Sephton, MA Glavin, DP Watson, JS Dworkin, JP Schwartz, AW Ehrenfreund, P AF Martins, Zita Botta, Oliver Fogel, Marilyn L. Sephton, Mark A. Glavin, Daniel P. Watson, Jonathan S. Dworkin, Jason P. Schwartz, Alan W. Ehrenfreund, Pascale TI Extraterrestrial nucleobases in the Murchison meteorite SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE nucleobases; Murchison meteorite; carbon isotope; extraterrestrial organic molecules; origin of life ID CARBON-ISOTOPE COMPOSITION; PRIMITIVE EARTH CONDITIONS; PREBIOTIC SYNTHESIS; HYDROGEN-CYANIDE; AMINO-ACIDS; HETEROCYCLIC-COMPOUNDS; MONOCARBOXYLIC ACIDS; ORGANIC-COMPOUNDS; DICARBOXYLIC-ACIDS; CHEMICAL EVOLUTION AB Carbon-rich meteorites, carbonaceous chondrites, contain many biologically relevant organic molecules and delivered prebiotic material to the young Earth. We present compound-specific carbon isotope data indicating that measured purine and pyrimidine compounds are indigenous components of the Murchison meteorite. Carbon isotope ratios for uracil and xanthine of delta C-13 = +44.5 parts per thousand and +37.7 parts per thousand, respectively, indicate a non-terrestrial origin for these compounds. These new results demonstrate that organic compounds, which are components of the genetic code in modern biochemistry, were already present in the early solar system and may have played a key role in life's origin. (C) 2008 Elsevier B.V. All rights reserved. C1 [Martins, Zita; Sephton, Mark A.] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London SW7 2AZ, England. [Martins, Zita; Ehrenfreund, Pascale] Leiden Univ, Leiden Inst Chem, Astrobiol Lab, NL-2300 RA Leiden, Netherlands. [Botta, Oliver; Glavin, Daniel P.; Dworkin, Jason P.; Ehrenfreund, Pascale] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Botta, Oliver] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Fogel, Marilyn L.] Carnegie Inst Sci, GL, Washington, DC 20015 USA. [Watson, Jonathan S.] Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England. [Schwartz, Alan W.] Radboud Univ Nijmegen, NL-6525 ED Nijmegen, Netherlands. RP Martins, Z (reprint author), Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London SW7 2AZ, England. EM z.martins@imperial.ac.uk RI Glavin, Daniel/D-6194-2012; Martins, Zita/H-4860-2015; Dworkin, Jason/C-9417-2012; OI Glavin, Daniel/0000-0001-7779-7765; Martins, Zita/0000-0002-5420-1081; Dworkin, Jason/0000-0002-3961-8997; Sephton, Mark/0000-0002-2190-5402; Watson, Jonathan/0000-0003-0354-1729 NR 53 TC 139 Z9 140 U1 8 U2 58 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD JUN 15 PY 2008 VL 270 IS 1-2 BP 130 EP 136 DI 10.1016/j.epsl.2008.03.026 PG 7 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 321HE UT WOS:000257294500013 ER PT J AU Ferrari, R McWilliams, JC Canuto, VM Dubovikov, M AF Ferrari, Raffaele McWilliams, James C. Canuto, Vittorio M. Dubovikov, Mikhail TI Parameterization of eddy fluxes near oceanic boundaries SO JOURNAL OF CLIMATE LA English DT Article ID ANISOTROPIC HORIZONTAL VISCOSITY; MESOSCALE TRACER TRANSPORTS; EULERIAN-MEAN THEORY; MIXED-LAYER EDDIES; NORTH-ATLANTIC; CIRCULATION MODELS; PART II; BAROCLINIC INSTABILITY; NUMERICAL-SIMULATION; POTENTIAL VORTICITY AB In the stably stratified interior of the ocean, mesoscale eddies transport materials by quasi-adiabatic isopycnal stirring. Resolving or parameterizing these effects is important for modeling the oceanic general circulation and climate. Near the bottom and near the surface, however, microscale boundary layer turbulence overcomes the adiabatic, isopycnal constraints for the mesoscale transport. In this paper a formalism is presented for representing this transition from adiabatic, isopycnally oriented mesoscale fluxes in the interior to the diabatic, along-boundary mesoscale fluxes near the boundaries. A simple parameterization form is proposed that illustrates its consequences in an idealized flow. The transition is not confined to the turbulent boundary layers, but extends into the partially diabatic transition layers on their interiorward edge. A transition layer occurs because of the mesoscale variability in the boundary layer and the associated mesoscale-microscale dynamical coupling. C1 [Ferrari, Raffaele] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [McWilliams, James C.] Univ Calif Los Angeles, Los Angeles, CA USA. [Canuto, Vittorio M.] Columbia Univ, NASA Goddard Inst Space Studies, New York, NY USA. [Canuto, Vittorio M.] Columbia Univ, Dept Appl Math & Phys, New York, NY USA. RP Ferrari, R (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, 54-1420,77 Massachusetts Ave, Cambridge, MA 02139 USA. EM rferrari@mit.edu RI Ferrari, Raffaele/C-9337-2013 OI Ferrari, Raffaele/0000-0002-3736-1956 NR 71 TC 48 Z9 48 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 JUN 15 PY 2008 VL 21 IS 12 BP 2770 EP 2789 DI 10.1175/2007JCLI1510.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 320PG UT WOS:000257246700003 ER PT J AU Lin, JL Mapes, BE Weickmann, KM Kiladis, GN Schubert, SD Suarez, MJ Bacmeister, JT Lee, MI AF Lin, Jia-Lin Mapes, Brian E. Weickmann, Klaus M. Kiladis, George N. Schubert, Siegfried D. Suarez, Max J. Bacmeister, Julio T. Lee, Myong-In TI North American monsoon and convectively coupled equatorial waves simulated by IPCC AR4 coupled GCMs SO JOURNAL OF CLIMATE LA English DT Article ID GENERAL-CIRCULATION MODEL; GULF-OF-CALIFORNIA; SIMPLE MULTICLOUD PARAMETERIZATION; PACIFIC TROPICAL CYCLOGENESIS; SURFACE TEMPERATURE ANOMALIES; MADDEN-JULIAN OSCILLATION; LARGE-SCALE MODELS; EASTERLY WAVES; PART I; CUMULUS PARAMETERIZATION AB This study evaluates the fidelity of North American monsoon and associated intraseasonal variability in the Intergovernmental Panel on Climate Change (IPCC) Fourth Assessment Report (AR4) coupled general circulation models (CGCMs). Twenty years of monthly precipitation data from each of the 22 models' twentieth-century climate simulations, together with the available daily precipitation data from 12 of them, are analyzed and compared with Global Precipitation Climatology Project (GPCP) monthly and daily precipitation. The authors focus on the seasonal cycle and horizontal pattern of monsoon precipitation in conjunction with the two dominant convectively coupled equatorial wave modes: the eastward-propagating Madden-Julian oscillation (MJO) and the westward-propagating easterly waves. The results show that the IPCC AR4 CGCMs have significant problems and display a wide range of skill in simulating the North American monsoon and associated intraseasonal variability. Most of the models reproduce the monsoon rainbelt, extending from southeast to northwest, and its gradual northward shift in early summer, but overestimate the precipitation over the core monsoon region throughout the seasonal cycle and fail to reproduce the monsoon retreat in the fall. Additionally, most models simulate good westward propagation of the easterly waves, but relatively poor eastward propagation of the MJO and overly weak variances for both the easterly waves and the MJO. There is a tendency for models without undiluted updrafts in their deep convection scheme to produce better MJO propagation. C1 [Lin, Jia-Lin] Ohio State Univ, Dept Geog, Columbus, OH 43210 USA. [Lin, Jia-Lin; Weickmann, Klaus M.; Kiladis, George N.] NOAA, ESRL, Boulder, CO USA. [Lin, Jia-Lin; Weickmann, Klaus M.; Kiladis, George N.] CIRES Climate Diagnost Ctr, Boulder, CO USA. [Mapes, Brian E.] Univ Miami, RSMAS, Miami, FL USA. [Schubert, Siegfried D.; Suarez, Max J.; Bacmeister, Julio T.; Lee, Myong-In] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Bacmeister, Julio T.; Lee, Myong-In] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. RP Lin, JL (reprint author), Ohio State Univ, Dept Geog, 1105 Derby Hall,154 N Oval Mall, Columbus, OH 43210 USA. EM lin.789@osu.edu RI Mapes, Brian/A-5647-2010; OI Lee, Myong-In/0000-0001-8983-8624 NR 66 TC 26 Z9 26 U1 0 U2 6 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 J9 J CLIMATE JI J. Clim. PD JUN 15 PY 2008 VL 21 IS 12 BP 2919 EP 2937 DI 10.1175/2007JCLI1815.1 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 320PG UT WOS:000257246700012 ER PT J AU Cooper, LN Sedano, N Johansson, S May, B Brown, JD Holliday, CM Kot, BW Fish, FE AF Cooper, Lisa Noelle Sedano, Nils Johansson, Stig May, Bryan Brown, Joey D. Holliday, Casey M. Kot, Brian W. Fish, Frank E. TI Hydrodynamic performance of the minke whale (Balaenoptera acutorostrata) flipper SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE cetacea; forelimb; flipper; wind tunnel; hydrodynamics; feeding; control surface; engulfment; lunge ID CONTROL SURFACES; KINEMATICS; VORTEX; WINGS; DRAG; FISH; FLOW AB Minke whales ( Balaenoptera acutorostrata) are the smallest member of balaenopterid whales and little is known of their kinematics during feeding maneuvers. These whales have narrow and elongated flippers that are small relative to body size compared to related species such as right and gray whales. No experimental studies have addressed the hydrodynamic properties of minke whale flippers and their functional role during feeding maneuvers. This study integrated wind tunnel, locomotion and anatomical range of motion data to identify functional parameters of the cambered minke whale flipper. A full-sized cast of a minke whale flipper was used in wind tunnel testing of lift, drag and stall behavior at six speeds, corresponding to swimming speeds of 0.7-8.9 m s(-1). Flow over the model surface stalled between 10 and 14 angle of attack (alpha) depending on testing speed. When the leading edge was rotated ventrally, loss in lift occurred around - 18 degrees regardless of speed. Range of mobility in the fresh limb was approximately 40% greater than the range of positive lift-generating angles of attack predicted by wind tunnel data (+14 degrees). Video footage, photographs and observations of swimming, engulfment feeding and gulping minke whales showed limb positions corresponding to low drag in wind tunnel tests, and were therefore hydrodynamically efficient. Flippers play an important role in orienting the body during feeding maneuvers as they maintain trim of the body, an action that counters drag-induced torque of the body during water and prey intake. C1 [Cooper, Lisa Noelle] Northeastern Ohio Univ Coll Med & Pharm, Dept Anat, Rootstown, OH 44201 USA. [Cooper, Lisa Noelle] Kent State Univ, Sch Biomed Sci, Kent, OH 44242 USA. [Sedano, Nils] USAF, Res Lab, Liquid Rocket Engines Branch, Edwards AFB, CA 93524 USA. [Johansson, Stig] San Diego State Univ, Dept Aerosp Engn & Engn Mech, San Diego, CA 92182 USA. [Brown, Joey D.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Holliday, Casey M.] Joan C Edwards Sch Med, Dept Anat & Pathol, Huntington, WV 25704 USA. [Kot, Brian W.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Fish, Frank E.] W Chester Univ, Dept Biol, W Chester, PA 19383 USA. RP Cooper, LN (reprint author), Northeastern Ohio Univ Coll Med & Pharm, Dept Anat, Rootstown, OH 44201 USA. EM l.noelle.cooper@gmail.com OI Holliday, Casey/0000-0001-8210-8434 NR 34 TC 17 Z9 17 U1 0 U2 9 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 JUN 15 PY 2008 VL 211 IS 12 BP 1859 EP 1867 DI 10.1242/jeb.014134 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 307GP UT WOS:000256307700012 PM 18515715 ER PT J AU Natraj, V Boesch, H Spurr, RJD Yung, YL AF Natraj, Vijay Boesch, Hartmut Spurr, Robert J. D. Yung, Yuk L. TI Retrieval of X-CO2 from simulated Orbiting Carbon Observatory measurements using the fast linearized R-2OS radiative transfer model SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SCATTERING-ABSORBING MEDIA; PLANETARY ATMOSPHERES; MULTIPLE-SCATTERING; REFLECTED SUNLIGHT; POLARIZED LIGHT; OZONE; CLOUDS; ORDERS; ERRORS; OCEAN AB In a recent paper, we introduced a novel technique to compute the polarization in a vertically inhomogeneous, scattering-absorbing medium using a two orders of scattering (2OS) radiative transfer (RT) model. The 2OS computation is an order of magnitude faster than a full multiple scattering scalar calculation and can be implemented as an auxiliary code to compute polarization in operational retrieval algorithms. In this paper, we employ the 2OS model for polarization in conjunction with a scalar RT model (Radiant) to simulate backscatter measurements in near infrared (NIR) spectral regions by space-based instruments such as the Orbiting Carbon Observatory (OCO). Computations are performed for six different sites and two seasons, representing a variety of viewing geometries, surface and aerosol types. The aerosol extinction (at 13000 cm(-1)) was varied from 0 to 0.3. The radiance errors using the Radiant/2OS (R-2OS) RT model are an order of magnitude (or more) smaller than errors arising from the use of the scalar model alone. In addition, we perform a linear error analysis study to show that the errors in the retrieved column-averaged dry air mole fraction of CO2 (X-CO2) using the R-2OS model are much lower than the "measurement'' noise and smoothing errors appearing in the inversemodel. On the other hand, we show that use of the scalar model alone induces X-CO2 errors that could dominate the retrieval error budget. C1 [Natraj, Vijay; Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Boesch, Hartmut] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Spurr, Robert J. D.] RT Solut Inc, Cambridge, MA 02138 USA. [Boesch, Hartmut] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Natraj, V (reprint author), CALTECH, Div Geol & Planetary Sci, MC 150-21, Pasadena, CA 91125 USA. EM vijay@gps.caltech.edu RI Boesch, Hartmut/G-6021-2012 NR 40 TC 5 Z9 5 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 14 PY 2008 VL 113 IS D11 AR D11212 DI 10.1029/2007JD009017 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 314LS UT WOS:000256811500001 ER PT J AU Willis, JK Chambers, DP Nerem, RS AF Willis, Josh K. Chambers, Don P. Nerem, R. Steven TI Assessing the globally averaged sea level budget on seasonal to interannual timescales SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID GRACE; TEMPERATURE; VARIABILITY; EXPANSION; MODELS AB Analysis of ocean temperature and salinity data from profiling floats along with satellite measurements of sea surface height and the time variable gravity field are used to investigate the causes of global mean sea level rise between mid-2003 and mid-2007. The observed interannual and seasonal fluctuations in sea level can be explained as the sum of a mass component and a steric (or density related) component to within the error bounds of each observing system. During most of 2005, seasonally adjusted sea level was approximately 5 mm higher than in 2004 owing primarily to a sudden increase in ocean mass in late 2004 and early 2005, with a negligible contribution from steric variability. Despite excellent agreement of seasonal and interannual sea level variability, the 4-year trends do not agree, suggesting that systematic long-period errors remain in one or more of these observing systems. C1 [Willis, Josh K.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. [Chambers, Don P.] Univ Texas Austin, Ctr Space Res, Austin, TX 78759 USA. [Nerem, R. Steven] Univ Colorado, Dept Aerosp Engn Sci, Cooperat Inst Res Environm Sci, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA. RP Willis, JK (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr,M-S 300-323, Pasadena, CA 91109 USA. EM joshua.k.willis@jpl.nasa.gov OI Chambers, Don/0000-0002-5439-0257 NR 38 TC 136 Z9 143 U1 1 U2 26 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 EI 2169-9291 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD JUN 14 PY 2008 VL 113 IS C6 AR C06015 DI 10.1029/2007JC004517 PG 9 WC Oceanography SC Oceanography GA 314MH UT WOS:000256813000004 ER PT J AU Bonitz, RG Shiraishi, L Robinson, M Arvidson, RE Chu, PC Wilson, JJ Davis, KR Paulsen, G Kusack, AG Archer, D Smith, P AF Bonitz, Robert G. Shiraishi, Lori Robinson, Matthew Arvidson, Raymond E. Chu, P. C. Wilson, J. J. Davis, K. R. Paulsen, G. Kusack, A. G. Archer, Doug Smith, Peter TI NASA Mars 2007 Phoenix Lander Robotic Arm and Icy Soil Acquisition Device SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article AB The primary purpose of the Mars 2007 Phoenix Lander Robotic Arm (RA) and associated Icy Soil Acquisition Device (ISAD) is to acquire samples of Martian dry and icy soil (DIS) by digging, scraping, and rasping, and delivering them to the Thermal Evolved Gas Analyzer and the Microscopy, Electrochemistry, and Conductivity Analyzer. The RA will also position (1) the Thermal and Electrical Conductivity Probe (TECP) in the DIS; (2) the TECP at various heights above the surface for relative humidity measurements, and (3) the Robotic Arm Camera to take images of the surface, trench, DIS samples within the ISAD scoop, magnetic targets, and other objects of scientific interest within its workspace. The RA/ISAD will also be used to generate DIS piles for monitoring; conduct DIS scraping, penetration, rasping, and chopping experiments; perform compaction tests; and conduct trench cave-in experiments. Data from the soil mechanics experiments will yield information on Martian DIS properties such as angle of repose, cohesion, bearing strength, and grain size distribution. C1 [Bonitz, Robert G.; Shiraishi, Lori; Robinson, Matthew] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Archer, Doug; Smith, Peter] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Arvidson, Raymond E.] Washington Univ St Louis, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Chu, P. C.; Wilson, J. J.; Davis, K. R.; Paulsen, G.; Kusack, A. G.] Honeybee Robotics Spacecraft Mech Corp, New York, NY 10001 USA. RP Bonitz, RG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM arvidson@rsmail.wustl.edu NR 11 TC 20 Z9 20 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUN 14 PY 2008 VL 113 AR E00A01 DI 10.1029/2007JE003030 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 318OO UT WOS:000257101700001 ER PT J AU Austin, J Tourpali, K Rozanov, E Akiyoshi, H Bekki, S Bodeker, G Bruhl, C Butchart, N Chipperfield, M Deushi, M Fomichev, VI Giorgetta, MA Gray, L Kodera, K Lott, F Manzini, E Marsh, D Matthes, K Nagashima, T Shibata, K Stolarski, RS Struthers, H Tian, W AF Austin, J. Tourpali, K. Rozanov, E. Akiyoshi, H. Bekki, S. Bodeker, G. Bruehl, C. Butchart, N. Chipperfield, M. Deushi, M. Fomichev, V. I. Giorgetta, M. A. Gray, L. Kodera, K. Lott, F. Manzini, E. Marsh, D. Matthes, K. Nagashima, T. Shibata, K. Stolarski, R. S. Struthers, H. Tian, W. TI Coupled chemistry climate model simulations of the solar cycle in ozone and temperature SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID QUASI-BIENNIAL OSCILLATION; MIDDLE ATMOSPHERE MODEL; STRATOSPHERIC OZONE; INTERACTIVE CHEMISTRY; INTERANNUAL VARIABILITY; ART.; DEPLETION; RADIATION; TRANSPORT; IMPACT AB The 11-year solar cycles in ozone and temperature are examined using new simulations of coupled chemistry climate models. The results show a secondary maximum in stratospheric tropical ozone, in agreement with satellite observations and in contrast with most previously published simulations. The mean model response varies by up to about 2.5% in ozone and 0.8 K in temperature during a typical solar cycle, at the lower end of the observed ranges of peak responses. Neither the upper atmospheric effects of energetic particles nor the presence of the quasi biennial oscillation is necessary to simulate the lower stratospheric response in the observed low latitude ozone concentration. Comparisons are also made between model simulations and observed total column ozone. As in previous studies, the model simulations agree well with observations. For those models which cover the full temporal range 1960-2005, the ozone solar signal below 50 hPa changes substantially from the first two solar cycles to the last two solar cycles. Further investigation suggests that this difference is due to an aliasing between the sea surface temperatures and the solar cycle during the first part of the period. The relationship between these results and the overall structure in the tropical solar ozone response is discussed. Further understanding of solar processes requires improvement in the observations of the vertically varying and column integrated ozone. C1 [Austin, J.] Geophys Fluid Dynam Lab, Princeton, NJ 08542 USA. [Tourpali, K.] Aristotle Univ Thessaloniki, Lab Atmospher Phys, Thessaloniki 20006, Greece. [Rozanov, E.] PMOD WRC, CH-7260 Davos, Switzerland. [Rozanov, E.] IAC ETHZ, CH-7260 Davos, Switzerland. [Akiyoshi, H.; Nagashima, T.] Natl Inst Environm Studies, Tsukuba, Ibaraki 3050053, Japan. [Bekki, S.; Lott, F.] Univ Paris 06, CNRS, SA IPSL, F-75252 Paris, France. [Bodeker, G.; Struthers, H.] NIWA, Omakau 9352, Central Otago, New Zealand. [Bruehl, C.] Max Planck Inst Chem, D-55020 Mainz, Germany. [Butchart, N.] Met Off Climate Res Div, Exeter EX1 3PB, Devon, England. [Chipperfield, M.; Tian, W.] Univ Leeds, Inst Atmospher Sci, Leeds LS2 9JT, W Yorkshire, England. [Deushi, M.; Kodera, K.; Shibata, K.] Meteorol Res Inst, Tsukuba, Ibaraki 3050052, Japan. [Fomichev, V. I.] York Univ, Dept Earth & Space Sci & Engn, Toronto, ON M3J 1P3, Canada. [Giorgetta, M. A.] Max Planck Inst Meteorol, D-20146 Hamburg, Germany. [Gray, L.] Univ Reading, NCAS, Ctr Global Atmospher Modelling, Dept Meteorol, Reading RG6 6BB, Berks, England. [Kodera, K.] Nagoya Univ, Grad Sch Environm Studies, Nagoya, Aichi 4648601, Japan. [Manzini, E.] Inst Nazl Geofis & Vulcanol, I-40128 Bologna, Italy. [Manzini, E.] Ctr Euromediterraneo Cambiamenti Climat, I-40128 Bologna, Italy. [Marsh, D.; Matthes, K.] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA. [Matthes, K.] Free Univ Berlin, Inst Meteorol, D-12165 Berlin, Germany. [Stolarski, R. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Austin, J (reprint author), Geophys Fluid Dynam Lab, Princeton, NJ 08542 USA. EM john.austin@noaa.gov RI Chipperfield, Martyn/H-6359-2013; Stolarski, Richard/B-8499-2013; Manzini, Elisa/H-5760-2011; Rozanov, Eugene/A-9857-2012; Marsh, Daniel/A-8406-2008; Gray, Lesley/D-3610-2009; Matthes, Katja/F-7361-2014; Tourpali, Kleareti/M-5269-2014; bekki, slimane/J-7221-2015 OI Chipperfield, Martyn/0000-0002-6803-4149; Stolarski, Richard/0000-0001-8722-4012; Rozanov, Eugene/0000-0003-0479-4488; Marsh, Daniel/0000-0001-6699-494X; Matthes, Katja/0000-0003-1801-3072; bekki, slimane/0000-0002-5538-0800 NR 70 TC 83 Z9 87 U1 1 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 13 PY 2008 VL 113 IS D11 AR D11306 DI 10.1029/2007JD009391 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 314LQ UT WOS:000256811300005 ER PT J AU Rao, MN Nyquist, LE Wentworth, SJ Sutton, SR Garrison, DH AF Rao, M. N. Nyquist, L. E. Wentworth, S. J. Sutton, S. R. Garrison, D. H. TI The nature of Martian fluids based on mobile element studies in salt-assemblages from Martian meteorites SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID X-RAY SPECTROMETER; MERIDIANI-PLANUM; ISOTOPIC COMPOSITION; SNC METEORITES; NOBLE-GASES; PARENT BODY; ANTARCTIC METEORITES; WEATHERING PRODUCTS; NAKHLITE METEORITES; AQUEOUS ALTERATION AB The S, Cl, and Br abundances determined in salt assemblages in Nakhla and Lafayette olivine fracturefillings and in gas-rich impact-melt (GRIM) glasses from Shergotty and EET79001 Lithologies A & B using EMPA/EDS/APS X-ray Microprobe techniques are compared with the S and Cl abundances determined by Gooding and coworkers in similar samples using quadrupole mass-spectrometric techniques. All the analytical methods yield relatively high Cl and low SO3 abundances in Nakhla indicating a SO3/Cl ratio of similar to 0.2. The same ratio in Lafayette secondary salts seems to be similar to 2. In the case of GRIM glasses from Shergotty and EET79001 Lith A & Lith B, the SO3 abundance is found to be high whereas the Cl abundance is low yielding a SO3/Cl ratio of similar to 5-300 (large errors are associated with these ratios because of low Cl signals). The salts found in Nakhla fracturefillings are inferred to have formed from Cl-rich fluids (high pH) near nakhlite source region on Mars, whereas the secondary minerals found in shergottite GRIM glasses seem to be associated with SO3-rich fluids (low pH) near shergottite source region on Mars. The Cl-rich fluids seem to have infiltrated into the nakhlite source region similar to 600 Ma ago, whereas the SO3-rich fluids likely percolated into the shergottite source region at similar to 180 Ma (or less) suggesting the possible existence of two types of fluid sources on Mars. C1 [Rao, M. N.; Wentworth, S. J.; Garrison, D. H.] Lyndon B Johnson Space Ctr, ESCG Jacobs, Houston, TX 77058 USA. [Nyquist, L. E.] Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA. [Sutton, S. R.] Univ Chicago, Dept Geol Sci, Chicago, IL 60637 USA. RP Rao, MN (reprint author), Lyndon B Johnson Space Ctr, ESCG Jacobs, Bldg 31, Houston, TX 77058 USA. EM sitarao@sbcglobal.net NR 81 TC 7 Z9 7 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUN 13 PY 2008 VL 113 IS E6 AR E06002 DI 10.1029/2007JE002958 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 314MM UT WOS:000256813500001 ER PT J AU Son, SW Polvani, LM Waugh, DW Akiyoshi, H Garcia, R Kinnison, D Pawson, S Rozanov, E Shepherd, TG Shibata, K AF Son, S. -W. Polvani, L. M. Waugh, D. W. Akiyoshi, H. Garcia, R. Kinnison, D. Pawson, S. Rozanov, E. Shepherd, T. G. Shibata, K. TI The impact of stratospheric ozone recovery on the Southern Hemisphere westerly jet SO SCIENCE LA English DT Article ID CLIMATE-CHANGE; ANNULAR MODE; TRENDS AB In the past several decades, the tropospheric westerly winds in the Southern Hemisphere have been observed to accelerate on the poleward side of the surface wind maximum. This has been attributed to the combined anthropogenic effects of increasing greenhouse gases and decreasing stratospheric ozone and is predicted to continue by the Intergovernmental Panel on Climate Change/Fourth Assessment Report (IPCC/AR4) models. In this paper, the predictions of the Chemistry-Climate Model Validation (CCMVal) models are examined: Unlike the AR4 models, the CCMVal models have a fully interactive stratospheric chemistry. Owing to the expected disappearance of the ozone hole in the first half of the 21st century, the CCMVal models predict that the tropospheric westerlies in Southern Hemisphere summer will be decelerated, on the poleward side, in contrast with the prediction of most IPCC/AR4 models. C1 [Son, S. -W.; Polvani, L. M.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA. [Polvani, L. M.] Columbia Univ, Dept Earth & Environm Sci, New York, NY 10027 USA. [Waugh, D. W.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. [Akiyoshi, H.] Natl Inst Environm Studies, Tsukuba, Ibaraki, Japan. [Garcia, R.; Kinnison, D.] Natl Ctr Atmospher Res, Boulder, CO 80325 USA. [Pawson, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rozanov, E.] ETH, Inst Atmospher & Climate Sci, Zurich, Switzerland. [Rozanov, E.] World Radiat Ctr, Phys Meteorol Observ, Davos, Switzerland. [Shepherd, T. G.] Univ Toronto, Dept Phys, Toronto, ON, Canada. [Shibata, K.] Meteorol Res Inst, Tsukuba, Ibaraki 305, Japan. RP Son, SW (reprint author), Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA. EM sws2112@columbia.edu RI Rozanov, Eugene/A-9857-2012; Son, Seok-Woo /A-8797-2013; Pawson, Steven/I-1865-2014; Waugh, Darryn/K-3688-2016 OI Rozanov, Eugene/0000-0003-0479-4488; Pawson, Steven/0000-0003-0200-717X; Waugh, Darryn/0000-0001-7692-2798 NR 23 TC 172 Z9 176 U1 6 U2 29 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 JUN 13 PY 2008 VL 320 IS 5882 BP 1486 EP 1489 DI 10.1126/science.1155939 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 312MV UT WOS:000256676400042 PM 18556557 ER PT J AU Manney, GL Kruger, K Pawson, S Minschwaner, K Schwartz, MJ Daffer, WH Livesey, NJ Mlynczak, MG Remsberg, EE Russell, JM Waters, JW AF Manney, Gloria L. Krueger, Kirstin Pawson, Steven Minschwaner, Ken Schwartz, Michael J. Daffer, William H. Livesey, Nathaniel J. Mlynczak, Martin G. Remsberg, Ellis E. Russell, James M., III Waters, Joe W. TI The evolution of the stratopause during the 2006 major warming: Satellite data and assimilated meteorological analyses SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID STRATOSPHERIC POLAR VORTEX; COMMUNITY CLIMATE MODEL; GRAVITY-WAVE DRAG; MIDDLE-ATMOSPHERE; GENERAL-CIRCULATION; GEOPOTENTIAL HEIGHT; WINTER STRATOSPHERE; HIGH-TEMPERATURES; FEBRUARY 1979; SENSITIVITY AB Microwave Limb Sounder and Sounding of the Atmosphere with Broadband Emission Radiometry data provide the first opportunity to characterize the four-dimensional stratopause evolution throughout the life-cycle of a major stratospheric sudden warming (SSW). The polar stratopause, usually higher than that at midlatitudes, dropped by similar to 30 km and warmed during development of a major "wave 1'' SSW in January 2006, with accompanying mesospheric cooling. When the polar vortex broke down, the stratopause cooled and became ill-defined, with a nearly isothermal stratosphere. After the polar vortex started to recover in the upper stratosphere/lower mesosphere (USLM), a cool stratopause reformed above 75 km, then dropped and warmed; both the mesosphere above and the stratosphere below cooled at this time. The polar stratopause remained separated from that at midlatitudes across the core of the polar night jet. In the early stages of the SSW, the strongly tilted (westward with increasing altitude) polar vortex extended into the mesosphere, and enclosed a secondary temperature maximum extending westward and slightly equatorward from the highest altitude part of the polar stratopause over the cool stratopause near the vortex edge. The temperature evolution in the USLM resulted in strongly enhanced radiative cooling in the mesosphere during the recovery from the SSW, but significantly reduced radiative cooling in the upper stratosphere. Assimilated meteorological analyses from the European Centre for Medium-Range weather Forecasts (ECMWF) and Goddard Earth Observing System Version 5.0.1 (GEOS-5), which are not constrained by data at polar stratopause altitudes and have model tops near 80 km, could not capture the secondary temperature maximum or the high stratopause after the SSW; they also misrepresent polar temperature structure during and after the stratopause breakdown, leading to large biases in their radiative heating rates. ECMWF analyses represent the stratospheric temperature structure more accurately, suggesting a better representation of vertical motion; GEOS-5 analyses more faithfully describe stratopause level wind and wave amplitudes. The high-quality satellite temperature data used here provide the first daily, global, multiannual data sets suitable for assessing and, eventually, improving representation of the USLM in models and assimilation systems. C1 [Manney, Gloria L.; Schwartz, Michael J.; Daffer, William H.; Livesey, Nathaniel J.; Waters, Joe W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Krueger, Kirstin] Univ Kiel, Leibniz Inst Marine Sci, IFM, GEOMAR, D-24105 Kiel, Germany. [Manney, Gloria L.; Minschwaner, Ken] New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA. [Mlynczak, Martin G.; Remsberg, Ellis E.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. [Pawson, Steven] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Russell, James M., III] Hampton Univ, Dept Phys, Hampton, VA 23668 USA. RP Manney, GL (reprint author), CALTECH, Jet Prop Lab, Mail Stop 183-701,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM gloria.l.manney@jpl.nasa.gov RI Mlynczak, Martin/K-3396-2012; Schwartz, Michael/F-5172-2016; Pawson, Steven/I-1865-2014 OI Schwartz, Michael/0000-0001-6169-5094; Pawson, Steven/0000-0003-0200-717X NR 66 TC 131 Z9 131 U1 4 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 12 PY 2008 VL 113 IS D11 AR D11115 DI 10.1029/2007JD009097 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 314LN UT WOS:000256811000001 ER PT J AU Zhang, Y Fu, R Yu, HB Dickinson, RE Juarez, RN Chin, M Wang, H AF Zhang, Yan Fu, Rong Yu, Hongbin Dickinson, Robert E. Juarez, Robinson Negron Chin, Mian Wang, Hui TI A regional climate model study of how biomass burning aerosol impacts land-atmosphere interactions over the Amazon SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OPTICAL-PROPERTIES; MODIS RETRIEVALS; SOLAR-RADIATION; BOUNDARY-LAYER; SOUTH-AMERICA; GOCART MODEL; SMOKE; VARIABILITY; CLOUDS; FOREST AB Ensemble simulations of a regional climate model assuming smoke aerosol in the Amazon suggest that dynamic changes of cloud cover contributes to the radiative effect of the smoke on the diurnal cycles of surface fluxes and the depth and structure of planetary boundary layer (PBL). In addition to their local effects, the aerosol radiative forcing also appears to weaken or delay the circulation transition from dry to wet season, leading to a weaker moisture transport into the smoke area where the aerosols optical depth, AOD, exceeds 0.3 and a stronger moisture transport and increase of cloudiness in the region upwind to the smoke area. The land surface scheme is modified to improve the regional climate model simulation of the daily mean and diurnal cycle of the surface sensible and latent heat fluxes over the Amazon rain forest. The aerosol radiative forcing is applied to the model during a dry to wet transition season (August-October) in that region. Cloudiness decreases in early afternoon due to the absorption of solar radiation by smoke aerosols partially compensate for the reduction of surface solar flux by aerosol scattering, shifting the strongest changes of surface flux and the PBL to late morning. The reduction of net solar radiation at the surface by smoke is locally largely compensated by reduction of surface sensible flux, with reduction of latent flux only about 30% as large. The strong aerosol absorption in the top 1 km of the aerosol layer stabilizes the 2 to 3 km layer immediately above the daytime PBL and consequently cloudiness decreases. This reduced surface solar flux and more stable lapse rate at the top of the PBL stabilize the lower troposphere. These changes lead to anomalous wind divergence in the southern Amazon and anomalous wind convergence over the equatorial western Amazon in the upwind direction of the smoke area. C1 [Zhang, Yan; Fu, Rong; Dickinson, Robert E.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. [Chin, Mian] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Juarez, Robinson Negron] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. [Wang, Hui] NOAA, Climate Predict Ctr, Wyle Informat Syst, Camp Springs, MD 20746 USA. [Yu, Hongbin] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. RP Zhang, Y (reprint author), Georgia Inst Technol, Sch Earth & Atmospher Sci, 311 Ferst Dr, Atlanta, GA 30332 USA. EM yan.zhang@gatech.edu RI Wang, Hui/B-6516-2008; Zhang, Yan/C-4792-2012; Fu, Rong/B-4922-2011; Chin, Mian/J-8354-2012; Yu, Hongbin/C-6485-2008 OI Yu, Hongbin/0000-0003-4706-1575 NR 48 TC 22 Z9 22 U1 1 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 12 PY 2008 VL 113 IS D14 AR D14S15 DI 10.1029/2007JD009449 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 314LT UT WOS:000256811600001 ER PT J AU Garrigues, S Lacaze, R Baret, F Morisette, JT Weiss, M Nickeson, JE Fernandes, R Plummer, S Shabanov, NV Myneni, RB Knyazikhin, Y Yang, W AF Garrigues, S. Lacaze, R. Baret, F. Morisette, J. T. Weiss, M. Nickeson, J. E. Fernandes, R. Plummer, S. Shabanov, N. V. Myneni, R. B. Knyazikhin, Y. Yang, W. TI Validation and intercomparison of global Leaf Area Index products derived from remote sensing data SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Review ID SPECTRAL VEGETATION INDEXES; NET PRIMARY PRODUCTION; LAND-COVER; SATELLITE DATA; RADIATIVE-TRANSFER; SPATIAL HETEROGENEITY; ACCURACY ASSESSMENT; CANOPY REFLECTANCE; CLIMATE MODELS; LAI PRODUCTS AB This study investigates the performances of four major global Leaf Area Index (LAI) products at 1/11.2 degrees spatial sampling and a monthly time step: ECOCLIMAP climatology, GLOBCARBON (from SPOT/VEGETATION and ATSR/AATSR), CYCLOPES (from SPOT/VEGETATION) and MODIS Collection 4 (main algorithm, from MODIS/TERRA). These products were intercompared during the 2001 - 2003 period over the BELMANIP network of sites. Their uncertainty was assessed by comparison with 56 LAI reference maps derived from ground measurements. CYCLOPES and MODIS depict realistic spatial variations at continental scale, while ECOCLIMAP poorly captures surface spatial heterogeneity, and GLOBCARBON tends to display erratic variations. ECOCLIMAP and GLOBCARBON show the highest frequency of successful retrievals while MODIS and CYCLOPES retrievals are frequently missing in winter over northern latitudes and over the equatorial belt. CYCLOPES and MODIS describe consistent temporal profiles over most vegetation types, while ECOCLIMAP does not show any interannual variations, and GLOBCARBON can exhibit temporal instability during the growing season over forests. The CYCLOPES, MODIS, and GLOBCARBON LAI values agree better over croplands and grasslands than over forests, where differences in vegetation structure representation between algorithms and surface reflectance uncertainties lead to substantial discrepancies between products. CYCLOPES does not reach high enough LAI values to properly characterize forests. In contrast, the other products have sufficient dynamic range of LAI to describe the global variability of LAI. Overall, CYCLOPES is the most similar product to the LAI reference maps. However, more accurate ground measurements and better representation of the global and seasonal variability of vegetation are required to refine this result. C1 [Garrigues, S.] Univ Maryland, NASA, Goddard Space Flight Ctr, Earth Syst Sci Interdisciplinary Ctr, Greenbelt, MD 20770 USA. [Lacaze, R.] MEDIAS France, POSTEL Serv Ctr, F-31401 Toulouse 9, France. [Baret, F.; Weiss, M.] INRA, EMMAH, UMR 1114, F-84914 Avignon 9, France. [Morisette, J. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Nickeson, J. E.] NASA, Goddard Space Flight Ctr, INOVIM, Greenbelt, MD 20771 USA. [Fernandes, R.] Canada Ctr Remote Sensing, Ottawa, ON K1A 0Y7, Canada. [Plummer, S.] IGBP European Space Agcy, I-00044 Frascati, Italy. [Shabanov, N. V.; Myneni, R. B.; Knyazikhin, Y.; Yang, W.] Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA. RP Garrigues, S (reprint author), Univ Maryland, NASA, Goddard Space Flight Ctr, Earth Syst Sci Interdisciplinary Ctr, Greenbelt, MD 20770 USA. EM sebastien.garrigues@gsfc.nasa.gov RI Yang, Wenze/B-8356-2012; Myneni, Ranga/F-5129-2012; Baret, Fred/C-4135-2011; OI Yang, Wenze/0000-0001-8514-2742; Baret, Fred/0000-0002-7655-8997; Weiss, Marie/0000-0002-2341-667X NR 102 TC 166 Z9 177 U1 8 U2 67 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-8953 EI 2169-8961 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD JUN 11 PY 2008 VL 113 IS G2 AR G02028 DI 10.1029/2007JG000635 PG 20 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 314LY UT WOS:000256812100002 ER PT J AU Rubin, RH Simpson, JP Colgan, SWJ Dufour, RJ Brunner, G McNabb, IA Pauldrach, AWA Erickson, EF Haas, MR Citron, RI AF Rubin, Robert H. Simpson, Janet P. Colgan, Sean W. J. Dufour, Reginald J. Brunner, Gregory McNabb, Ian A. Pauldrach, Adalbert W. A. Erickson, Edwin F. Haas, Michael R. Citron, Robert I. TI Spitzer observations of M33 and the hot star, HII region connection SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars : atmospheres; ISM : abundances; HII regions; galaxies : individual; M33 ID H-II REGIONS; FINE-STRUCTURE LINES; EFFECTIVE COLLISION STRENGTHS; ABUNDANCE GRADIENTS; IRON PROJECT; ATOMIC DATA; CHEMICAL EVOLUTION; INFRARED SPECTROGRAPH; ELEMENTAL ABUNDANCES; METALLICITY GRADIENT AB We have observed emission lines of [SIV] 10.51, H(7-6) 12.37, [NeII] 12.81, [NeIII] 15.56 and [SIII] 18.71 mu m in a number of extragalactic HII regions with the Spitzer Space Telescope. A previous paper presented our data and analysis for the substantially face-on spiral galaxy M83. Here we report our results for the Local Group spiral galaxy M33. The nebulae selected cover a wide range of galactocentric radii (R(G)). The observations were made with the Infrared Spectrograph with the short wavelength, high-resolution module. The above set of five lines is observed cospatially, thus permitting a reliable comparison of the fluxes. From the measured fluxes, we determine the ionic abundance ratios including Ne(++)/Ne(+), S(3+)/S(++), and S(++)/Ne(+) and find that there is a correlation of increasingly higher ionization with larger R(G). By sampling the dominant ionization states of Ne (Ne(+), Ne(++)) and S (S(++), S(3+)) for HII regions, we can estimate the Ne/H, S/H and Ne/S ratios. We find from linear least-squares fits that there is a decrease in metallicity with increasing R(G): d log (Ne/H)/dR(G) = -0.058 +/- 0.014 and d log (S/H)/dR(G)=-0.052 +/- 0.021 dex kpc(-1). There is no apparent variation in the Ne/S ratio with R(G). Unlike our previous similar study of M83, where we conjectured that this ratio was an upper limit, for M33 the derived ratios are likely a robust indication of Ne/S. This occurs because the HII regions have lower metallicity and higher ionization than those in M83. Both Ne and S are primary elements produced in alpha-chain reactions, following C and O burning in stars, making their yields depend very little on the stellar metallicity. Thus, it is expected that the Ne/S ratio remains relatively constant throughout a galaxy. The median (average) Ne/S ratio derived for HII regions in M33 is 16.3 (16.9), just slightly higher than the Orion Nebula value of 14.3. The same methodology is applied to Spitzer observations recently published for three massive HII regions: NGC 3603 (Milky Way), 30 Dor (LMC) and N 66 (SMC) as well as for a group of blue compact dwarf galaxies. We find median Ne/S values of 14.6, 11.4, 10.1, and 14.0, respectively. All of these values are in sharp contrast with the much lower 'canonical', but controversial, solar value of similar to 5. A recent nucleosynthesis, galactic chemical evolution model predicts an Ne/S abundance of similar to 9. Our observations may also be used to test the predicted ionizing spectral energy distribution of various stellar atmosphere models. We compare the ratio of fractional ionizations < Ne(++)>/< S(++)>, < Ne(++)>/< S(3+)>,and < Ne(++)>/< Ne(+)> versus < S(3+)>/< S(++)> with predictions made from our photoionization models using several of the state-of-the-art stellar atmosphere model grids. The trends of the ionic ratios established from the prior M83 study are remarkably similar, but continued to higher ionization with the present M33 objects. C1 [Rubin, Robert H.; Simpson, Janet P.; Colgan, Sean W. J.; McNabb, Ian A.; Erickson, Edwin F.; Haas, Michael R.; Citron, Robert I.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rubin, Robert H.] Orion Enterprises, Moffett Field, CA 94035 USA. [Simpson, Janet P.] SETI Inst, Mountain View, CA 94043 USA. [Dufour, Reginald J.; Brunner, Gregory] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA. [Pauldrach, Adalbert W. A.] Univ Munich, D-81679 Munich, Germany. RP Rubin, RH (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM rubin@cygnus.arc.nasa.gov RI Colgan, Sean/M-4742-2014 NR 67 TC 30 Z9 30 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 11 PY 2008 VL 387 IS 1 BP 45 EP 62 DI 10.1111/j.1365-2966.2008.13225.x PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 308HH UT WOS:000256378700004 ER PT J AU Clements, DL Vaccari, M Babbedge, T Oliver, S Rowan-Robinson, M Davoodi, P Ivison, R Farrah, D Dunlop, J Shupe, D Waddington, I Simpson, C Furusawa, H Serjeant, S Afonso-Luis, A Alexander, DM Aretxaga, I Blain, A Borys, C Chapman, S Coppin, K Dunne, L Dye, S Eales, SA Evans, T Fang, F Frayer, D Fox, M Gear, WK Greve, TR Halpern, M Hughes, DH Jenness, T Lonsdale, CJ Mortier, AMJ Page, MJ Pope, A Priddey, RS Rawlings, S Savage, RS Scott, D Scott, SE Sekiguchi, K Smail, I Smith, HE Stevens, JA Surace, J Takagi, T van Kampen, E AF Clements, D. L. Vaccari, M. Babbedge, T. Oliver, S. Rowan-Robinson, M. Davoodi, P. Ivison, R. Farrah, D. Dunlop, J. Shupe, Dave Waddington, I. Simpson, C. Furusawa, H. Serjeant, S. Afonso-Luis, A. Alexander, D. M. Aretxaga, I. Blain, A. Borys, C. Chapman, S. Coppin, K. Dunne, L. Dye, S. Eales, S. A. Evans, T. Fang, F. Frayer, D. Fox, M. Gear, W. K. Greve, T. R. Halpern, M. Hughes, D. H. Jenness, T. Lonsdale, C. J. Mortier, A. M. J. Page, M. J. Pope, A. Priddey, R. S. Rawlings, S. Savage, R. S. Scott, D. Scott, S. E. Sekiguchi, K. Smail, I. Smith, H. E. Stevens, J. A. Surace, J. Takagi, T. van Kampen, E. TI The SCUBA Half-Degree Extragalactic Survey (SHADES) - VIII. The nature of faint submillimetre galaxies in SHADES, SWIRE and SXDF surveys SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : high-redshift; infrared : galaxies; submillimetre ID SPITZER-SPACE-TELESCOPE; STAR-FORMATION HISTORY; INFRARED ARRAY CAMERA; SUPERNOVA HOST GALAXIES; DEEP-FIELD; PHOTOMETRIC REDSHIFTS; NUMBER COUNTS; LEGACY SURVEY; LOCKMAN HOLE; DARK-MATTER AB We present the optical-to-submillimetre spectral energy distributions (SEDs) for 33 radio and mid-infrared (mid-IR) identified submillimetre galaxies discovered via the SHADES 850-mu m SCUBA imaging in the Subaru-XMM Deep Field (SXDF). Optical data for the sources come from the SXDF and mid- and far-IR fluxes from SWIRE. We obtain photometric redshift estimates for our sources using optical and IRAC 3.6- and 4.5-mu m fluxes. We then fit SED templates to the longer wavelength data to determine the nature of the far-IR emission that dominates the bolometric luminosity of these sources. The IR template fits are also used to resolve ambiguous identifications and cases of redshift aliasing. The redshift distribution obtained broadly matches previous results for submillimetre sources and on the SHADES SXDF field. Our template fitting finds that active galactic nuclei, while present in about 10 per cent of our sources, do not contribute significantly to their bolometric luminosity. Dust heating by starbursts, with either Arp220 or M82 type SEDs, appears to be responsible for the luminosity in most sources (23/33 are fitted by Arp220 templates, 2/33 by the warmer M82 templates). 8/33 sources, in contrast, are fitted by a cooler cirrus dust template, suggesting that cold dust has a role in some of these highly luminous objects. Three of our sources appear to have multiple identifications or components at the same redshift, but we find no statistical evidence that close associations are common among our SHADES sources. Examination of rest-frame K-band luminosity suggests that 'downsizing' is underway in the submillimetre galaxy population, with lower redshift systems lying in lower mass host galaxies. Of our 33 identifications six are found to be of lower reliability but their exclusion would not significantly alter our conclusions. C1 [Clements, D. L.; Vaccari, M.; Babbedge, T.; Rowan-Robinson, M.; Fox, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BW, England. [Oliver, S.; Davoodi, P.; Waddington, I.; Savage, R. S.] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Ivison, R.; Dunlop, J.; Dunne, L.; Mortier, A. M. J.; Scott, S. E.] Univ Edinburgh, Royal Observ, SUPA, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R.] Royal Observ, UK ATC, Edinburgh EH9 3HJ, Midlothian, Scotland. [Farrah, D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Shupe, Dave; Fang, F.] CALTECH, Jet Prop Lab, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Simpson, C.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Furusawa, H.] Natl Opt Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Serjeant, S.] Open Univ, CEPSR, Milton Keynes MK7 6AA, Bucks, England. [Afonso-Luis, A.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain. [Alexander, D. M.; Coppin, K.; Smail, I.] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England. [Alexander, D. M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Aretxaga, I.; Hughes, D. H.] Inst Nacl Astrofis Opt & Electr, Puebla 72000, Mexico. [Dunne, L.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Dye, S.; Eales, S. A.; Gear, W. K.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3YB, Wales. [Evans, T.; Frayer, D.] CALTECH, IPAC, JPL, Pasadena, CA 91125 USA. [Halpern, M.; Pope, A.; Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Jenness, T.] Joint Astron Ctr, Hilo, HI 96720 USA. [Lonsdale, C. J.; Smith, H. E.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92063 USA. [Page, M. J.] UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Priddey, R. S.; Stevens, J. A.] Univ Hertfordshire, Ctr Astrophys Res, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England. [Rawlings, S.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Sekiguchi, K.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Takagi, T.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [van Kampen, E.] Univ Innsbruck, Inst Astro & Particle Phys, A-6020 Innsbruck, Austria. RP Clements, DL (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Prince Consort Rd, London SW7 2BW, England. EM d.clements@imperial.ac.uk RI Smail, Ian/M-5161-2013; Ivison, R./G-4450-2011; Vaccari, Mattia/R-3431-2016; OI Smail, Ian/0000-0003-3037-257X; Ivison, R./0000-0001-5118-1313; Vaccari, Mattia/0000-0002-6748-0577; Jenness, Tim/0000-0001-5982-167X; Scott, Douglas/0000-0002-6878-9840; Dye, Simon/0000-0002-1318-8343; Alexander, David/0000-0002-5896-6313 NR 81 TC 53 Z9 53 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 11 PY 2008 VL 387 IS 1 BP 247 EP 267 DI 10.1111/j.1365-2966.2008.13172.x PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 308HH UT WOS:000256378700023 ER PT J AU Arevalo, P McHardy, IM Markowitz, A Papadakis, IE Turner, TJ Miller, L Reeves, J AF Arevalo, P. McHardy, I. M. Markowitz, A. Papadakis, I. E. Turner, T. J. Miller, L. Reeves, J. TI Fourier-resolved energy spectra of the Narrow-Line Seyfert 1 Mkn 766 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : active ID ACTIVE GALACTIC NUCLEI; X-RAY-SPECTRUM; XMM-NEWTON; BLACK-HOLE; TIMING PROPERTIES; POWER SPECTRUM; VARIABILITY; MARKARIAN-766; SPECTROSCOPY; GALAXIES AB We compute Fourier-resolved X-ray spectra of the Seyfert 1 Markarian 766 to study the shape of the variable components contributing to the 0.3-10 keV energy spectrum and their time-scale dependence. The fractional variability spectra peak at 1-3 keV, as in other Seyfert 1 galaxies, consistent with either a constant contribution from a soft excess component below 1 keV and Compton reflection component above 2 keV or variable warm absorption enhancing the variability in the 1-3 keV range. The rms spectra, which show the shape of the variable components only, are well described by a single power law with an absorption feature around 0.7 keV, which gives it an apparent soft excess. This spectral shape can be produced by a power law varying in normalization, affected by an approximately constant (within each orbit) warm absorber, with parameters similar to those found by Turner et al. for the warm-absorber layer covering all spectral components in their scattering scenario [N(H) similar to 3 x 10(21) cm(-2), log(xi) similar to 1]. The total soft excess in the average spectrum can therefore be produced by a combination of constant warm absorption on the power-law plus an additional less variable component. On shorter time-scales, the rms spectrum hardens and this evolution is well described by a change in power-law slope, while the absorption parameters remain the same. The frequency dependence of the rms spectra can be interpreted as variability arising from propagating fluctuations through an extended emitting region, whose emitted spectrum is a power law that hardens towards the centre. This scenario reduces the short time-scale variability of lower energy bands making the variable spectrum harder on shorter time-scales and at the same time explains the hard lags found in these data by Markowitz et al. C1 [Arevalo, P.; McHardy, I. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Markowitz, A.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Papadakis, I. E.] Univ Crete, Dept Phys, Iraklion 71003, Greece. [Papadakis, I. E.] Fdn Res & Technol, IESL, Iraklion 71110, Greece. [Turner, T. J.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Turner, T. J.] NASA, Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA. [Miller, L.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Reeves, J.] Univ Keele, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England. RP Arevalo, P (reprint author), Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. EM patricia@astro.soton.ac.uk RI Papadakis, Iossif/C-3235-2011 NR 28 TC 11 Z9 11 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 11 PY 2008 VL 387 IS 1 BP 279 EP 288 DI 10.1111/j.1365-2966.2008.13216.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 308HH UT WOS:000256378700026 ER PT J AU Green, DA Reynolds, SP Borkowski, KJ Hwang, U Harrus, I Petre, R AF Green, D. A. Reynolds, S. P. Borkowski, K. J. Hwang, U. Harrus, I. Petre, R. TI The radio expansion and brightening of the very young supernova remnant G1.9+0.3 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ISM: individual: G1.9+0.3; supernova remnants; radio continuum: ISM ID GALACTIC-CENTER REGION; NRAO PMN SURVEYS; SOURCE CATALOG; VLA OBSERVATIONS; SEARCH; PLANE; MHZ; EVOLUTION; EMISSION; LATITUDES AB Recent radio observations of the small Galactic supernova remnant G1.6+0.3 made at 4.86 GHz which have a comparable resolution (10 x 4 arcsec(2)). These show that the radio emission from this remnant has expanded significantly, by about 15 per cent over 23 yr, with a current outer diameter of approximate to 92 arcsec. This expansion confirms that G1.9+0.3 is the youngest Galactic remnant yet identified, only about 150 yr old at most. Recent, lower resolution, 1.43-GHz observations are also discussed, and the intergrated flux densities from these and the 4.86-GHz observations are compared with earlier results. This shows that the integrated flux density of G1.9+0.3 has been increasing recently. C1 [Green, D. A.] Cavevdish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Reynolds, S. P.; Borkowski, K. J.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. [Hwang, U.; Harrus, I.; Petre, R.] NASA, GSFC, Greenbelt, MD USA. RP Green, DA (reprint author), Cavevdish Lab, Astrophys Grp, 19 JJ Thomson Ave, Cambridge CB3 0HE, England. EM dag@mrao.cam.ac.uk RI Green, David/E-9609-2010 OI Green, David/0000-0003-3189-9998 NR 41 TC 24 Z9 24 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 11 PY 2008 VL 387 IS 1 BP L54 EP L58 DI 10.1111/j.1745-3933.2008.00484.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 308HH UT WOS:000256378700058 ER PT J AU Rykoff, ES Evrard, AE McKay, TA Becker, MR Johnston, DE Koester, BP Nord, B Rozo, E Sheldon, ES Stanek, R Wechsler, RH AF Rykoff, E. S. Evrard, A. E. McKay, T. A. Becker, M. R. Johnston, D. E. Koester, B. P. Nord, B. Rozo, E. Sheldon, E. S. Stanek, R. Wechsler, R. H. TI The L-X-M relation of clusters of galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: general; X-rays: galaxies: clusters ID OPTICAL RICHNESS RELATION; MASS-TEMPERATURE RELATION; DIGITAL SKY SURVEY; RAY-CLUSTERS; MAXBCG; EVOLUTION; CATALOG; SAMPLE; SIMULATIONS; SCATTER AB We present a new measurement of the scaling relation between X-ray luminosity and total mass for 17000 galaxy clusters in the maxBCG cluster sample. Stacking subsamples within fixed ranges of optical richness. N-200, we measure the mean 0.1-2.4 keV X-ray luminosity, (L-X), from the ROSAT All-Sky Survey. The mean mass, (M-200), is measured from weak gravitational lensing of SDSS background galaxies. For 9 <= N-200 < 200, the data are well fitted by a power law, (L-X)/10(42) h(-2) erg s(-1) = [12.6(-1.3)(+1.4) (stat) +/- 1.6 (sys)]((M-200)/10(14)h(-1) M-circle dot)(1.65 +/- 0.13). The slope agrees to within 10 per cent with previous estimates based on X-ray selected catalogues, implying that the covariance in L-X and N-200 at a fixed halo mass is not large. The luminosity intercept is 30 per cent, or 2 nu, lower than that determined from the X-ray flux-limited sample of Reiprich & Bohringer, assuming hydrostatic equilibrium. This slight difference could arise from a combination of Malmquist bias and/or systematic error in hydrostatic mass estimates, both of which are expected. The intercept agrees with that dervied by Stanek et al. using a model for the statistical correspondence between clusters and haloes in a WMAP3 cosmology with power spectrum normalization nu(8) = 0.85. Similar exercises applied to future data sets will allow constraints on the covariance among optical and hot gas properties of clusters at a fixed mass. C1 [Rykoff, E. S.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Evrard, A. E.; McKay, T. A.; Becker, M. R.; Nord, B.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Evrard, A. E.; McKay, T. A.; Stanek, R.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Evrard, A. E.; McKay, T. A.] Michigan Ctr Theoret Phys, Ann Arbor, MI 48109 USA. [Becker, M. R.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Johnston, D. E.] Jet Propuls Lab, Pasadena, CA 91109 USA. [Koester, B. P.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Koester, B. P.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Rozo, E.] Ohio State Univ, Columbus, OH 43210 USA. [Sheldon, E. S.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Wechsler, R. H.] Stanford Univ, Dept Phys, KIPAC, Stanford, CA 94305 USA. Stanford Univ, SLAC, Stanford, CA 94305 USA. RP Rykoff, ES (reprint author), Univ Calif Santa Barbara, Dept Phys, 2233B Broida Hall, Santa Barbara, CA 93106 USA. EM erykoff@physics.ucsb.edu RI McKay, Timothy/C-1501-2009; OI McKay, Timothy/0000-0001-9036-6150; Becker, Matthew/0000-0001-7774-2246; Evrard, August/0000-0002-4876-956X FU NSF [AST-0206277, AST-0407061, AST-0708150]; TABASGO foundation FX ESR and TAMcK are pleased to acknowledge financial support from NSF AST-0206277 and AST-0407061, and the hospitality of the MCTP.ESR also thanks the TABASGO foundation. AEE acknowledges support from NSF AST-0708150. We thank A. Finoguenov, T. Reiprich and H. Boehringer for helpful feedback. NR 30 TC 77 Z9 78 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 11 PY 2008 VL 387 IS 1 BP L28 EP L32 DI 10.1111/j.1745-3933.2008.00476.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 308HH UT WOS:000256378700052 ER PT J AU Wolfire, MG Tielens, AGGM Hollenbach, D Kaufman, MJ AF Wolfire, Mark G. Tielens, A. G. G. M. Hollenbach, David Kaufman, M. J. TI Chemical rates on small grains and PAHs: C+ recombination and H-2 formation SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM : clouds; ISM : general; ISM : molecules ID DIFFUSE INTERSTELLAR CLOUDS; POLYCYCLIC AROMATIC-HYDROCARBONS; ABSORPTION PROFILE SPECTROGRAPH; MOLECULAR-HYDROGEN FORMATION; ELECTRON-ION RECOMBINATION; NEUTRAL ATOMIC PHASES; PHYSICAL CONDITIONS; PHOTODISSOCIATION REGIONS; CARBON ABUNDANCES; RATE COEFFICIENTS AB We use observations of the C I, C II, H I, and H-2 column densities along lines of sight in the Galactic plane to determine the formation rate of H-2 on grains and to determine chemical reaction rates with polycyclic aromatic hydrocarbons (PAHs). Photodissociation region models are used to find the best-fit parameters to the observed columns. We find the H-2 formation rate on grains has a low rate (R similar to 1 x 10(-17) cm(3) s(-1)) along lines of sight with low column density (A(V) less than or similar to 0.25) and low molecular fraction (f(H2) less than or similar to 10(-4)). At higher column densities (0.25 <= A(V) <= 2.13), we find a rate of R similar to 3.5 x 10(-17) cm(3) s(-1). The lower rate at low column densities could be the result of grain processing by interstellar shocks, which may deplete the grain surface area or process the sites of H + H formation, thereby inhibiting H-2 production. Alternatively, the formation rate may be normal, and the low molecular fraction may be the result of lines of sight that graze larger clouds. Such lines of sight would have a reduced H-2 self-shielding compared to the line-of-sight column. We find the reaction C+ + PAH(-) -> C + PAH(0) is best fit with a rate 2.4 x 10(-7) Phi(PAH) T-2(-0.5) cm(3) s(-1) with T-2 = T/100 K, and the reaction C+ + PAH(-) -> C + PAH(0) is best fit with a rate 8.8 x 10(-9) Phi(PAH) cm(3) s(-1). In high-column-density gas, we find Phi(PAH) similar to 0.4. In low-column-density gas, Phi(PAH) is less well constrained, with Phi(PAH) similar to 0.2-0.4. C1 [Wolfire, Mark G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Tielens, A. G. G. M.; Hollenbach, David] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Kaufman, M. J.] San Jose State Univ, Dept Phys, San Jose, CA 95192 USA. RP Wolfire, MG (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM mwolfire@astro.umd.edu; atielens@mail.arc.nasa.gov; hollenbach@ism.arc.nasa.gov; mkaufman@email.sjsu.edu NR 61 TC 61 Z9 61 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 JUN 10 PY 2008 VL 680 IS 1 BP 384 EP 397 DI 10.1086/587688 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 310AH UT WOS:000256500800031 ER PT J AU Goldsmith, PF Heyer, M Narayanan, G Snell, R Li, D Brunt, C AF Goldsmith, Paul F. Heyer, Mark Narayanan, Gopal Snell, Ronald Li, Di Brunt, Chris TI Large-scale structure of the molecular gas in Taurus revealed by high linear dynamic range spectral line mapping SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : evolution; ISM : individual (Taurus); ISM : molecules; radio lines : ISM; stars : formation ID DENSE CLOUD CORES; CARBON-MONOXIDE ABUNDANCE; NARROW SELF-ABSORPTION; STAR-FORMATION; DARK CLOUDS; MAGNETIC-FIELD; INTERSTELLAR-MEDIUM; (CO)-O-18 SURVEY; T-TAURI; RATIO AB We report the results of a 100 deg(2) survey of the Taurus molecular cloud region in (CO)-C-12 and (CO)-C-13 J = 1 -> 0. The image of the cloud in each velocity channel includes similar or equal to 3 x 10(6) Nyquist-sampled pixels on a 20 '' grid. The high sensitivity and large spatial dynamic range of the maps reveal a very complex, highly structured cloud morphology, including filaments, cavities, and rings. The axes of the striations seen in the (CO)-C-12 emission from relatively diffuse gas are aligned with the direction of the magnetic field. We have developed a statistical method for analyzing the pixels in which (CO)-C-12 but not (CO)-C-13 is detected, which allows us to determine the CO column in the diffuse portion of the cloud, as well as in the denser regions in which we detect both isotopologues. Using a column-density-dependent model for the CO fractional abundance, we derive the mass of the region mapped to be 2.4 x 10(4) M-circle dot, more than twice as large as would be obtained using a canonical fixed fractional abundance of (CO)-C-13, and a factor of 3 greater than would be obtained considering only the high column density regions. We determine that half the mass of the cloud is in regions having column density below 2.1 x 10(21) cm(-2). The distribution of young stars in the region covered is highly nonuniform, with the probability offinding a star in a pixel with a specified column density rising sharply for N(H-2) = 6 x 10(21) cm(-2). We determine a relatively low star formation efficiency (mass of young stars/mass of molecular gas), between 0.3% and 1.2%, and an average star formation rate during the past 3 Myr of 8; 10(-5) stars yr(-1). C1 [Goldsmith, Paul F.; Li, Di] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Heyer, Mark; Narayanan, Gopal; Snell, Ronald] Univ Massachusetts, Dept Astron, FCRAO, Amherst, MA 01003 USA. [Brunt, Chris] Univ Exeter, Exeter EX4 4QJ, Devon, England. RP Goldsmith, PF (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA USA. EM Paul.F.Goldsmith@jpl.nasa.gov RI Goldsmith, Paul/H-3159-2016 NR 68 TC 204 Z9 204 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2008 VL 680 IS 1 BP 428 EP 445 DI 10.1086/587166 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 310AH UT WOS:000256500800034 ER PT J AU Sahai, R Claussen, M Contreras, CS Morris, M Sarkar, G AF Sahai, Raghvendra Claussen, Mark Contreras, Carmen Sanchez Morris, Mark Sarkar, Geetanjali TI High-velocity interstellar bullets in IRAS 05506+2414: A very young protostar SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : clouds; ISM : individual (IRAS 05506+2414); radio lines : ISM; stars : formation; stars : mass loss; stars : pre-main-sequence ID STELLAR OBJECTS; MOLECULAR CLOUD; STAR-FORMATION; IRAS SOURCES; AMMONIA; MASS; NEBULA; CLASSIFICATION; EMISSION; OUTFLOWS AB We have made a serendipitous discovery of an enigmatic outflow source, IRAS 05506+2414 (hereafter IRAS 05506), as part of a multiwavelength survey of pre-planetary nebulae (PPNs). The HST optical and near-infrared images show a bright compact central source with a jetlike extension, and a fanlike spray of high-velocity (with radial velocities up to 350 km s(-1)) elongated knots which appear to emanate from it. These structures are possibly analogous to the near-IR "bullets'' seen in the Orion Nebula. Interferometric observations at 2.6 mm show the presence of a continuum source and a high-velocity CO outflow, which is aligned with the optical jet structure. IRAS 05506 is most likely not a PPN. We find extended NH(3) (1,1) emission toward IRAS 05506; these data, together with the combined presence of far-IR emission, H(2)O and OH masers, and CO and CS J = 2-1 emission, strongly argue for a dense, dusty star-forming core associated with IRAS 05506. IRAS 05506 is probably an intermediate-mass or massive protostar, and the very short timescale (200 yr) of its outflows indicates that it is very young. If IRAS 05506 is a massive star, then the lack of radio continuum and the late G to early K spectral type we find from our optical spectra imply that in this object we are witnessing the earliest stages of its life, while its temperature is still too low to provide sufficient UV flux for ionization. C1 [Sahai, Raghvendra] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Claussen, Mark] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Contreras, Carmen Sanchez] CSIC, Inst Estructura Mat, Dept Astrofis Mol & Infraroja, E-28006 Madrid, Spain. [Morris, Mark] Univ Calif Los Angeles, Div Astron & Astrophys, Los Angeles, CA 90095 USA. [Sarkar, Geetanjali] Indian Inst Technol, Dept Phys, Kanpur 208016, Uttar Pradesh, India. RP Sahai, R (reprint author), CALTECH, Jet Prop Lab, MS 183-900, Pasadena, CA 91109 USA. NR 42 TC 9 Z9 9 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 JUN 10 PY 2008 VL 680 IS 1 BP 483 EP 494 DI 10.1086/587638 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 310AH UT WOS:000256500800039 ER PT J AU Mazets, EP Aptekar, RL Cline, TL Frederiks, DD Goldsten, JO Golenetskii, SV Hurley, K von Kienlin, A Pal'shin, VD AF Mazets, E. P. Aptekar, R. L. Cline, T. L. Frederiks, D. D. Goldsten, J. O. Golenetskii, S. V. Hurley, K. von Kienlin, A. Pal'shin, V. D. TI A giant flare from a soft gamma repeater in the Andromeda galaxy (M31) SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts; stars : neutron ID HIGH-ENERGY TRANSIENT; SGR 1627-41; RAY BURST; SGR-1806-20; LOCALIZATION; EMISSION; OUTBURST; SPECTRA; EVENT AB The light curve, energy spectra, energetics, and IPN localization of an exceedingly intense, short-duration, hard-spectrum burst, GRB 070201, obtained from Konus-Wind, INTEGRAL (SPI-ACS), and MESSENGER data are presented. The total fluence of the burst and the peak flux are S = 2.00(-0.26)(+0.10) x 10(-5) erg cm(-2) and F(max) = 1.61(-0.50)(+0.29) x 10(-3) erg cm(-2) s(-1). The IPN error box has an area of 446 arcmin(2) and covers the peripheral part of the M31 galaxy. Assuming that the source of the burst is indeed in M31 at a distance of 0.78 Mpc, the measured values of the fluence S and maximum flux F(max) correspond to a total energy of Q = 1.5 x 10(45) erg and a maximum luminosity L = 1.2 x 10(47) erg s(-1). These data are in good agreement with the corresponding characteristics of the previously observed giant flares from other soft gamma repeaters. The evidence for the identification of this event as a giant flare from a soft gamma repeater in the M31 galaxy is presented. C1 [Mazets, E. P.; Aptekar, R. L.; Frederiks, D. D.; Golenetskii, S. V.; Pal'shin, V. D.] Russian Acad Sci, AF Ioffe Physicotech Inst, St Petersburg 194021, Russia. [Cline, T. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Goldsten, J. O.] Johns Hopkins Univ, Appl Phys Lab, Baltimore, MD 20723 USA. [Hurley, K.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. RP Mazets, EP (reprint author), Russian Acad Sci, AF Ioffe Physicotech Inst, St Petersburg 194021, Russia. RI Frederiks, Dmitry/C-7612-2014; Pal'shin, Valentin/F-3973-2014; Aptekar, Raphail/B-3456-2015; Golenetskii, Sergey/B-3818-2015; OI Frederiks, Dmitry/0000-0002-1153-6340 NR 44 TC 37 Z9 38 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 JUN 10 PY 2008 VL 680 IS 1 BP 545 EP 549 DI 10.1086/587955 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 310AH UT WOS:000256500800044 ER PT J AU Farinelli, R Titarchuk, L Paizis, A Frontera, F AF Farinelli, Ruben Titarchuk, Lev Paizis, Ada Frontera, Filippo TI A new comptonization model for weakly magnetized, accreting neutron stars in low-mass X-ray binaries SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars : individual (Scorpius X-1, GX 17+2, Cygnus X-2, GX 340+0, GX 3+1, GX 354-0); stars : neutron; X-rays : binaries ID ENERGY CONCENTRATOR SPECTROMETER; QUASI-PERIODIC OSCILLATIONS; MONTE-CARLO SIMULATIONS; CONVERGING FLUID-FLOW; COLOR-COLOR DIAGRAM; BLACK-HOLES; OBSERVATIONAL EVIDENCE; TIMING-EXPLORER; BOUNDARY-LAYER; GX 17+2 AB We have developed a new model for the X-ray spectral fitting package XSPEC that takes into account the effects of both thermal and dynamical (i.e., bulk) Comptonization. The model consists of two components: one is the direct blackbody-like emission due to seed photons that are not subjected to effective Compton scattering, while the other is a convolution of the Green's function of the energy operator with a blackbody-like seed photon spectrum. When combined thermal and bulk effects are considered, the analytical form of the Green's function may be obtained as a solution of the diffusion equation describing Comptonization. Using data from the BeppoSAX, INTEGRAL, and RXTE satellites, we test our model on the spectra of a sample of six bright neutron star low-mass X-ray binaries with low magnetic fields, covering three different spectral states. Particular attention is given to the transient power-law-like hard X-ray (greater than or similar to 30 keV) tails, which we interpret in the framework of the bulk motion Comptonization process. We show that the values of the best-fit delta-parameter, which represents the importance of bulk with respect to thermal Comptonization, can be physically meaningful and can at least qualitatively describe the physical conditions of the environment in the innermost part of the system. Moreover, we show that in fitting the thermal Comptonization spectra to the X-ray spectra of these systems, the best-fit parameters of our model are in excellent agreement with those from compTT, a broadly used and well-established XSPEC model. C1 [Farinelli, Ruben] Univ Ferrara, Dipartimento Fis, I-44100 Ferrara, Italy. [Titarchuk, Lev] George Mason Univ, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Titarchuk, Lev] USN, Res Lab, High Energy Space Environm Branch, Washington, DC 20375 USA. [Titarchuk, Lev] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA. [Paizis, Ada] INAF, Sez Milano, Ist Astrofis Spaziale & Fis Cosm, I-20100 Milan, Italy. [Frontera, Filippo] INAF, Sez Bologna, Ist Astrofis Spaziale & Fis Cosm, I-40100 Bologna, Italy. RP Farinelli, R (reprint author), Univ Ferrara, Dipartimento Fis, I-44100 Ferrara, Italy. EM farinelli@fe.infn.it; Lev.Titarchuk@nrl.navy.mil; ada@iasf-milano.inaf.it; frontera@fe.infn.it OI Paizis, Adamantia/0000-0001-5067-0377 NR 55 TC 39 Z9 39 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 JUN 10 PY 2008 VL 680 IS 1 BP 602 EP 614 DI 10.1086/587162 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 310AH UT WOS:000256500800049 ER PT J AU Henley, DB Corcoran, MF Pittard, JM Stevens, IR Hamaguchi, K Gull, TR AF Henley, D. B. Corcoran, M. F. Pittard, J. M. Stevens, I. R. Hamaguchi, K. Gull, T. R. TI Chandra X-ray grating spectrometry of eta carinae near X-ray minimum. I. Variability of the sulfur and silicon emission lines SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : early-type; stars : individual (eta Car); X-rays : stars ID WIND-WIND COLLISION; HELIUM-LIKE IONS; ATOMIC DATABASE; CROSS-SECTIONS; BINARY-SYSTEMS; LIGHT-CURVE; COMPANION; SPECTROSCOPY; PARAMETERS; STAR AB We report on variations in important X-ray emission lines in a series of Chandra grating spectra of the supermassive colliding wind binary star eta Car, including key phases around the X-ray minimum/periastron passage in 2003.5. The X-rays arise from the collision of the slow, dense wind of eta Car with the fast, low-density wind of an otherwise hidden companion star. The X-ray emission lines provide the only direct measure of the flow dynamics of the companion's wind along the wind-wind collision zone. We concentrate here on the silicon and sulfur lines, which are the strongest and best-resolved lines in the X-ray spectra. Most of the line profiles can be adequately fit with symmetric Gaussians with little significant skewness. Both the silicon and sulfur lines show significant velocity shifts and correlated increases in line widths through the observations. The R = forbidden-to-intercombination ratio from the Si XIII and S XV triplets is near or above the low-density limit in all observations, suggesting that the line-forming region is > 1.6 stellar radii from the companion star. We show that simple geometrical models cannot simultaneously fit both the observed centroid variations and changes in line width as a function of phase. We show that the observed profiles can be fitted with synthetic profiles with a reasonable model of the emissivity along the wind-wind collision boundary. We use this analysis to help constrain the line formation region as a function of orbital phase, and the orbital geometry. C1 [Henley, D. B.] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. [Corcoran, M. F.; Hamaguchi, K.] NASA, Goddard Space Flight Ctr, CRESST, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Corcoran, M. F.; Hamaguchi, K.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Pittard, J. M.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Stevens, I. R.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. RP Henley, DB (reprint author), Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. EM dbh@physast.uga.edu RI Gull, Theodore/D-2753-2012 OI Gull, Theodore/0000-0002-6851-5380 NR 60 TC 28 Z9 28 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 JUN 10 PY 2008 VL 680 IS 1 BP 705 EP 727 DI 10.1086/587472 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 310AH UT WOS:000256500800059 ER PT J AU Ji, HS Wang, HM Liu, C Dennis, BR AF Ji, Haisheng Wang, Haimin Liu, Chang Dennis, Brian R. TI A hard X-ray sigmoidal structure during the initial phase of the 2003 october 29x10 flare SO ASTROPHYSICAL JOURNAL LA English DT Article DE sun : flares; sun : magnetic fields; sun : X-rays, gamma rays ID CORONAL MASS EJECTIONS; SOLAR-FLARES; MAGNETIC RECONNECTION; X10 FLARE; CURRENT SHEET; FLUX ROPES; RHESSI; RELAXATION; SHRINKAGE; ERUPTIONS AB We find a hard X-ray (HXR) sigmoidal ( S-shaped) structure observed by RHESSI between 6 and 150 keV during the initial phase of the X10 flare of 2003 October 29. Its counterparts are seen with the Solar X-Ray Imager and TRACE. The flare evolves from a sigmoid to an arcade phase as observed in TRACE 195 8 images. According to the spatial structure of HXR emission, the flare process can be divided into two different phases. During the first phase, HXR emission in different energy ranges shares a similar sigmoidal evolving structure. The structure appears to contract initially as shown by the time profile of the separation between the two footpoints ( FPs) at the ends of the HXR sigmoid. During the second phase, HXR emission in the lower energy range (less than or similar to 30 keV) evolves into two sources located along the neutral line. Meanwhile, the FPs in the higher energies (greater than or similar to 30 keV) move apart as usual. During the whole flaring process, the value of the flare shear, defined as the angle between the line connecting two FPs and the line perpendicular to the neutral line, decreases steadily. We conclude that the flare was triggered by magnetic reconnection near the center of the sigmoid. The converging and unshearing motion during the sigmoid period is explained by continuing magnetic reconnection driven by the erupting sigmoidal flux rope. The reconnection progresses from highly sheared magnetic field lines to less sheared field lines surrounding the flux rope. C1 [Ji, Haisheng] Purple Mt Observ, Nanjing 210008, Peoples R China. [Ji, Haisheng; Wang, Haimin; Liu, Chang] New Jersey Inst Technol, Big Bear Solar Observ, Big Bear City, CA 92314 USA. [Dennis, Brian R.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA. RP Ji, HS (reprint author), Purple Mt Observ, 2 Beijing Xi Lu, Nanjing 210008, Peoples R China. EM jihs@pmo.ac.cn RI Dennis, Brian/C-9511-2012; OI Liu, Chang/0000-0002-6178-7471 NR 44 TC 29 Z9 30 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2008 VL 680 IS 1 BP 734 EP 739 DI 10.1086/587138 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 310AH UT WOS:000256500800061 ER PT J AU Liu, YCM Opher, M Cohen, O Liewer, PC Gombosi, TI AF Liu, Y. C. -M. Opher, M. Cohen, O. Liewer, P. C. Gombosi, T. I. TI A simulation of a coronal mass ejection propagation and shock evolution in the lower solar corona SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; MHD; shock waves; Sun : coronal mass ejections (CMEs); Sun : evolution; Sun : magnetic fields ID PARTICLE-ACCELERATION; MAGNETOHYDRODYNAMIC MODEL; WIND; CMES; SUN; HELIOSPHERE; TOPOLOGY; SPACE AB We present a detailed simulation of the evolution of a moderately slow coronal mass ejection (CME; 800 km s(-1) at 5 R circle dot, where R circle dot is solar radii) in the lower solar corona (2-5 R circle dot). The configuration of the Sun's magnetic field is based on the MDI data for the solar surface during Carrington rotation 1922. The pre-CME background solar wind is generated using the Wang-Sheeley-Arge (WSA) model. To initiate a CME, we inserted a modified Titov-Demoulin flux rope in an active region near the solar equator using the Space Weather Modeling Framework (SWMF). After the initiation stage ( within 2.5 R circle dot), the CME evolves at a nearly constant and slow acceleration of the order of 100 m s(-2), which corresponds to an intermediate-acceleration CME. Detailed analysis of the pressures shows that the thermal pressure accounts for most of the acceleration of the CME. The magnetic pressure contributes to the acceleration early in the evolution and becomes negligible when the CME moves beyond similar to 3 R circle dot. We also present the evolution of the shock geometry near the nose of the CME, which shows that the shock is quasi parallel most of the time. C1 [Liu, Y. C. -M.; Opher, M.] George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA. [Cohen, O.; Gombosi, T. I.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Liewer, P. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RI Gombosi, Tamas/G-4238-2011; Yong, Liu/H-5333-2011; OI Gombosi, Tamas/0000-0001-9360-4951; Cohen, Ofer/0000-0003-3721-0215 NR 36 TC 15 Z9 15 U1 0 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 JUN 10 PY 2008 VL 680 IS 1 BP 757 EP 763 DI 10.1086/587867 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 310AH UT WOS:000256500800063 ER PT J AU Bonev, BP Mumma, MJ Radeva, YL DiSanti, MA Gibb, EL Villanueva, GL AF Bonev, Boncho P. Mumma, Michael J. Radeva, Yana L. DiSanti, Michael A. Gibb, Erika L. Villanueva, Geronimo L. TI The peculiar volatile composition of comet 8P/Tuttle: A contact binary of chemically distinct cometesimals? SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE comets : general; comets : individual (8P/Tuttle); infrared : solar system ID ORGANIC COMPOSITION; ORIGIN; SPECTROSCOPY; EMISSION; SYSTEM; DISK AB We report measurements of eight native (i.e., released directly from the comet nucleus) volatiles (H2O, HCN, CH4, C2H2, C2H6, CO, H2CO, and CH3OH) in comet 8P/Tuttle using NIRSPEC at Keck 2. Comet Tuttle reveals a truly unusual composition, distinct from that of any comet observed to date at infrared wavelengths. The prominent enrichment of methanol relative to water contrasts with the depletions of other molecules, especially C2H2, HCN, and H2CO. We suggest that the nucleus of 8P/Tuttle may contain two cometesimals characterized by distinct volatile composition. The relative abundances C-2/CN, C-2/OH, and CN/OH in 8P/Tuttle (measured at optical/near-UV wavelengths) differ substantially from the mixing ratios of their potential parents (C2H2/HCN, C2H2/H2O, and HCN/H2O) found in this work. Based on this comparison, our results do not support C2H2 and HCN being the principal precursors for respectively C-2 and CN in Tuttle. The peculiar native composition observed in 8P/Tuttle (compared to other comets) provides new strong evidence for chemical diversity in the volatile materials stored in comet nuclei. We discuss the implications of this diversity for expected variations in the deuterium enrichment of water among comets. C1 [Bonev, Boncho P.; Mumma, Michael J.; Radeva, Yana L.; DiSanti, Michael A.; Villanueva, Geronimo L.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Bonev, Boncho P.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Radeva, Yana L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Gibb, Erika L.] Univ Missouri, Dept Phys & Astron, St Louis, MO 63121 USA. RP Bonev, BP (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, MS 693, Greenbelt, MD 20771 USA. EM bonev@cua.edu RI mumma, michael/I-2764-2013 NR 32 TC 29 Z9 29 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 10 PY 2008 VL 680 IS 1 BP L61 EP L64 DI 10.1086/589649 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 313DX UT WOS:000256722400016 ER PT J AU Patsourakos, S Pariat, E Vourlidas, A Antiochos, SK Wuelser, JP AF Patsourakos, S. Pariat, E. Vourlidas, A. Antiochos, S. K. Wuelser, J. P. TI STEREO SECCHI stereoscopic observations constraining the initiation of polar coronal jets SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun : corona; Sun : magnetic fields ID X-RAY JETS; H-ALPHA SURGES; TRANSITION REGION; SOLAR; HINODE; WAVES; EUV; HOLES AB We report on the first stereoscopic observations of polar coronal jets made by the EUVI/SECCHI imagers on board the twin STEREO spacecraft. The significantly separated viewpoints (similar to 11 degrees) allowed us to infer the 3D dynamics and morphology of a well-defined EUV coronal jet for the first time. Triangulations of the jet's location in simultaneous image pairs led to the true 3D position and thereby its kinematics. Initially the jet ascends slowly at approximate to 10-20 km s(-1) and then, after an apparent "jump" takes place, it accelerates impulsively to velocities exceeding 300 km s(-1) with accelerations exceeding the solar gravity. Helical structure is the most important geometrical feature of the jet which shows evidence of untwisting. The jet structure appears strikingly different from each of the two STEREO viewpoints: face-on in one viewpoint and edge-on in the other. This provides conclusive evidence that the observed helical structure is real and does not result from possible projection effects of single-viewpoint observations. The clear demonstration of twisted structure in polar jets compares favorably with synthetic images from a recent MHD simulation of jets invoking magnetic untwisting as their driving mechanism. Therefore, the latter can be considered as a viable mechanism for the initiation of polar jets. C1 [Patsourakos, S.; Pariat, E.; Vourlidas, A.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Pariat, E.] George Mason Univ, Ctr Earth Observing & Space Res, Inst Computat Sci, Coll Sci, Fairfax, VA 22030 USA. [Pariat, E.; Antiochos, S. K.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20774 USA. [Wuelser, J. P.] Lockheed Martin ATC, Solar & Astrophys Lab, Palo Alto, CA 94304 USA. RP Patsourakos, S (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. RI Vourlidas, Angelos/C-8231-2009; Antiochos, Spiro/D-4668-2012 OI Vourlidas, Angelos/0000-0002-8164-5948; Antiochos, Spiro/0000-0003-0176-4312 NR 24 TC 92 Z9 93 U1 1 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 10 PY 2008 VL 680 IS 1 BP L73 EP L76 DI 10.1086/589769 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 313DX UT WOS:000256722400019 ER PT J AU Pitman, KM Buratti, BJ Mosher, JA Bauer, JM Momary, TW Brown, RH Nicholson, PD Hedman, MM AF Pitman, K. M. Buratti, B. J. Mosher, J. A. Bauer, J. M. Momary, T. W. Brown, R. H. Nicholson, P. D. Hedman, M. M. TI First high solar phase angle observations of Rhea using Cassini VIMS: Upper limits on water vapor and geologic activity SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planets and satellites : individual (Rhea); solar system : general; techniques : spectroscopic ID SATURNS MAGNETOSPHERE; E-RING; ENCELADUS; PLASMA; DIONE; SPECTROMETER; ATMOSPHERE; SURFACE; TETHYS; RADAR AB Using radiances acquired with Cassini's Visual and Infrared Mapping Spectrometer (VIMS), we construct high solar phase angle curves for Saturn's second largest moon, Rhea. Ground-based studies of Rhea and Saturnian icy satellites are focussing on low phase angles; to our knowledge, these are the first solar phase curve data for Rhea on phase angles > 70 degrees. We compare these data to similar phase curves for Enceladus at near-infrared wavelengths to estimate the amount of water vapor that could possibly be generated and thus set an upper limit on the amount of geologic activity that may be occurring on Rhea. We find that Enceladus's plume manifests itself in the VIMS solar phase curve at a phase angle near 160 degrees and peaks most strongly for lambda = 2.017810 mu m. No such peak can be found in the Rhea VIMS phase curve. Absence of a forward scattering peak supports the recent determination that particles in Rhea's surrounding ring are not small. We calculate that the maximum water vapor column density that could be supplied from Rhea ranges from 1.52 x 10(14) to 1.91 x 10(15) cm(-2), 2 orders of magnitude less than what is calculated by Cassini UVIS for Enceladus. This implies that for Rhea, the level of active internal (endogenic) processes is exceedingly small, if any. C1 [Pitman, K. M.; Buratti, B. J.; Mosher, J. A.; Bauer, J. M.; Momary, T. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Brown, R. H.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Nicholson, P. D.; Hedman, M. M.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Pitman, KM (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM karly.m.pitman@jpl.nasa.gov NR 42 TC 7 Z9 7 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 10 PY 2008 VL 680 IS 1 BP L65 EP L68 DI 10.1086/589745 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 313DX UT WOS:000256722400017 ER PT J AU Reynolds, SP Borkowski, KJ Green, DA Hwang, U Harrus, I Petre, R AF Reynolds, Stephen P. Borkowski, Kazimierz J. Green, David A. Hwang, Una Harrus, Ilana Petre, Robert TI The youngest Galactic supernova remnant: G1.9+0.3 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE acceleration of particles; ISM : individual (G1.9+0.3); supernova remnants; supernovae : general; X-rays : ISM ID SHOCK ACCELERATION; IA SUPERNOVAE; CENTER REGION; X-RAYS; CAS-A; SHELL; MODELS; EXTINCTION; ELECTRONS; TI-44 AB Our 50 ks Chandra observation of the small radio supernova remnant (SNR) G1.9+0.3 shows a complete shell structure with strong bilateral symmetry, about 100 '' in diameter. The radio morphology is also shell-like, but only about 84 '' in diameter, based on observations made in 1985. We attribute the size difference to expansion between 1985 and our Chandra observations of 2007. Expansion is confirmed in comparing radio images from 1985 and 2008. We deduce that G1.9+0.3 is of order 100 years old-the youngest supernova remnant in the Galaxy. Based on a very high absorbing column density of 5.5 x 10(22) cm(-2), we place G1.9+0.3 near the Galactic center, at a distance of about 8.5 kpc, where the mean remnant radius would be about 2 pc, and the required expansion speed about 14,000 km s(-1). The X-ray spectrum is featureless and well described by the exponentially cut off synchrotron model srcut. With the radio flux at 1 GHz fixed at 0.9 Jy, we find a spectral index of 0.65 and a rolloff frequency of 1.4 x 10(18) Hz. The implied characteristic rolloff electron energy of about 94(B/10 mu G)(-1/2) TeV is the highest ever reported for a shell supernova remnant. It can easily be reached by standard diffusive shock acceleration, given the very high shock velocities; it can be well described by either age-limited or synchrotron-loss-limited acceleration. Not only is G1.9+0.3 the youngest known Galactic remnant, it is also only the fourth Galactic X-ray-synchrotron-dominated shell supernova remnant. C1 [Reynolds, Stephen P.; Borkowski, Kazimierz J.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. [Green, David A.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Hwang, Una; Harrus, Ilana; Petre, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Reynolds, SP (reprint author), N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. EM stephen_reynolds@ncsu.edu RI Green, David/E-9609-2010 OI Green, David/0000-0003-3189-9998 NR 29 TC 63 Z9 63 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 10 PY 2008 VL 680 IS 1 BP L41 EP L44 DI 10.1086/589570 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 313DX UT WOS:000256722400011 ER PT J AU Dubinin, E Modolo, R Fraenz, M Woch, J Duru, F Akalin, F Gurnett, D Lundin, R Barabash, S Plaut, JJ Picardi, G AF Dubinin, E. Modolo, R. Fraenz, M. Woch, J. Duru, F. Akalin, F. Gurnett, D. Lundin, R. Barabash, S. Plaut, J. J. Picardi, G. TI Structure and dynamics of the solar wind/ionosphere interface on Mars: MEX-ASPERA-3 and MEX-MARSIS observations SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MAGNETIC-FIELD; ASPERA-3; IONOSPHERE; BOUNDARY; MISSION; EXPRESS; WIND AB The measurements of the local plasma parameters of the ionospheric and solar wind plasmas and the magnetic field strength carried out by the ASPERA-3 and MARSIS experiments onboard Mars Express (MEX) in the subsolar region of the induced Martian magnetosphere provide us with a first test of the pressure balance across the solar wind/ionosphere interface. The structure of this transition is very dynamic and is controlled by the solar wind. For a broad range of the solar wind dynamic pressures, the magnetic field in the boundary layer raises to the values just sufficient to balance the solar wind pressure. The magnetic field frozen into the electrons is transported across the magnetospheric boundary (MB) where solar wind terminates and the planetary plasma begins to prevail. The dense ionospheric plasma has a sharp outer boundary the position of which is usually a little closer to the planet than the MB. Although the number density reaches on this boundary similar to 10(3) cm(-3) the contribution of the ionospheric thermal pressure is rather small and the ionosphere is magnetized. There are also cases when the magnetic field almost does not vary across both boundaries. C1 [Dubinin, E.; Fraenz, M.; Woch, J.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [Modolo, R.; Duru, F.; Akalin, F.; Gurnett, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Plaut, J. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lundin, R.; Barabash, S.] Swedish Inst Space Phys, SE-90187 Kiruna, Sweden. [Picardi, G.] Univ Roma La Sapienza, Dept Info Com, I-00184 Rome, Italy. RP Dubinin, E (reprint author), Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. EM dubinin@mps.mpg.de; ronan-modolo@uiowa.edu; rickard@irf.se; stas@irf.se NR 19 TC 33 Z9 33 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUN 10 PY 2008 VL 35 IS 11 AR L11103 DI 10.1029/2008GL033730 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 314KS UT WOS:000256808900003 ER PT J AU Eldering, A Kulawik, SS Worden, J Bowman, K Osterman, G AF Eldering, Annmarie Kulawik, Susan S. Worden, John Bowman, Kevin Osterman, Greg TI Implementation of cloud retrievals for TES atmospheric retrievals: 2. Characterization of cloud top pressure and effective optical depth retrievals SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SATELLITE SOUNDERS 3I; SCATTERING ATMOSPHERES; RADIATIVE PROPERTIES; IMAGERS ISCCP; WATER-VAPOR; MODIS; PARAMETERIZATION; AIRS/AMSU/HSB; TEMPERATURE; WAVELENGTHS AB We characterize and validate the cloud products from the Tropospheric Emission Spectrometer (TES) by comparing TES estimates of effective cloud optical depth and cloud top height to those from the Moderate Resolution Imaging Spectroradiometer (on EOS) (MODIS), the Atmospheric Infrared Sounder (AIRS), and to simulated data. TES measures in the infrared spectral region (650-2260 cm(-1)), where clouds have a ubiquitous impact on measured radiances and therefore on trace gas profile retrievals. The radiance contribution of clouds is parameterized in TES retrievals in terms of a set of frequency-dependent nonscattering effective optical depths and a cloud height. This unique approach jointly retrieves cloud parameters with surface temperature, emissivity, atmospheric temperature, and trace gases such as ozone from TES spectral radiances. We calculate the relationship between the true optical depth and the TES effective optical depth for a range of single-scatter albedo and phase functions to show how this varies with cloud type. We estimate the errors on retrieved cloud parameters using a simulated data set covering a wide range of cloud cases. For simulations with no noise on the radiances, cloud height errors are less than 30 hPa, and effective optical depth follows expected behavior for input optical depths of less than 3. When random noise is included on the radiances, and atmospheric variables are included in the retrieval, cloud height errors are approximately 200 hPa, and the estimated effective optical depth has sensitivity between optical depths of 0.3 and 10. The estimated errors from simulation are consistent with differences between TES and cloud top heights and optical depth from MODIS and AIRS. C1 [Eldering, Annmarie; Kulawik, Susan S.; Worden, John; Bowman, Kevin; Osterman, Greg] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Eldering, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM annmarie.eldering@jpl.nasa.gov NR 34 TC 27 Z9 27 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 10 PY 2008 VL 113 IS D16 AR D16S37 DI 10.1029/2007JD008858 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 314LW UT WOS:000256811900004 ER PT J AU Nardi, B Gille, JC Barnett, JJ Randall, CE Harvey, VL Waterfall, A Reburn, WJ Leblanc, T Mcgee, TJ Twigg, LW Thompson, AM Godin-Beekmann, S Bernath, PF Bojkov, BR Boone, CD Cavanaugh, C Coffey, MT Craft, J Craig, C Dean, V Eden, TD Francis, G Froidevaux, L Halvorson, C Hannigan, JW Hepplewhite, CL Kinnison, DE Khosravi, R Krinsky, C Lambert, A Lee, H Loh, J Massie, ST McDermid, IS Packman, D Torpy, B Valverde-Canossa, J Walker, KA Whiteman, DN Witte, JC Young, G AF Nardi, Bruno Gille, John C. Barnett, John J. Randall, Cora E. Harvey, V. Lynn Waterfall, Alison Reburn, W. Jolyon Leblanc, Thierry McGee, Tom J. Twigg, Laurence W. Thompson, Anne M. Godin-Beekmann, Sophie Bernath, Peter F. Bojkov, Bojan R. Boone, Chris D. Cavanaugh, Charles Coffey, Michael T. Craft, James Craig, Cheryl Dean, Vincil Eden, Thomas D. Francis, Gene Froidevaux, Lucien Halvorson, Chris Hannigan, James W. Hepplewhite, Christopher L. Kinnison, Douglas E. Khosravi, Rashid Krinsky, Charlie Lambert, Alyn Lee, Hyunah Loh, Joanne Massie, Steven T. McDermid, I. Stuart Packman, Daniel Torpy, Brendan Valverde-Canossa, Jessica Walker, Kaley A. Whiteman, David N. Witte, Jacquelyn C. Young, Greg TI Initial validation of ozone measurements from the High Resolution Dynamics Limb Sounder SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID STRATOSPHERIC OZONE; VERTICAL-DISTRIBUTION; AURA SATELLITE; EOS MLS; LIDAR; CLIMATOLOGY; SYSTEM; DESIGN AB Comparisons of the latest High Resolution Dynamics Limb Sounder (HIRDLS) ozone retrievals (v2.04.09) are made with ozonesondes, ground-based lidars, airborne lidar measurements made during the Intercontinental Chemical Transport Experiment-B, and satellite observations. A large visual obstruction blocking over 80% of the HIRDLS field of view presents significant challenges to the data analysis methods and implementation, to the extent that the radiative properties of the obstruction must be accurately characterized in order to adequately correct measured radiances. The radiance correction algorithms updated as of August 2007 are used in the HIRDLS v2.04.09 data presented here. Comparisons indicate that HIRDLS ozone is recoverable between 1 and 100 hPa at middle and high latitudes and between 1 and 50 hPa at low latitudes. Accuracy of better than 10% is indicated between 1 and 30 hPa (HIRDLS generally low) by the majority of the comparisons with coincident measurements, and 5% is indicated between 2 and 10 hPa when compared with some lidars. Between 50 and 100 hPa, at middle and high latitudes, accuracy is 10-20%. The ozone precision is estimated to be generally 5-10% between 1 and 50 hPa. Comparisons with ozonesondes and lidars give strong indication that HIRDLS is capable of resolving fine vertical ozone features (1-2 km) in the region between 1 and 50 hPa. Development is continuing on the radiance correction and the cloud detection and filtering algorithms, and it is hoped that it will be possible to achieve a further reduction in the systematic bias and an increase in the measurement range downward to lower heights (at pressures greater than 50-100 hPa). C1 [Nardi, Bruno; Gille, John C.; Cavanaugh, Charles; Coffey, Michael T.; Craig, Cheryl; Eden, Thomas D.; Francis, Gene; Halvorson, Chris; Hannigan, James W.; Kinnison, Douglas E.; Khosravi, Rashid; Lee, Hyunah; Massie, Steven T.; Packman, Daniel] Natl Ctr Atmospher Res, Boulder, CO 80301 USA. [Barnett, John J.; Hepplewhite, Christopher L.] Univ Oxford, Dept Phys, Oxford OX1 2JD, England. [Bernath, Peter F.; Boone, Chris D.; Walker, Kaley A.] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. [McGee, Tom J.; Twigg, Laurence W.; Bojkov, Bojan R.; Whiteman, David N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Gille, John C.; Craft, James; Dean, Vincil; Krinsky, Charlie; Loh, Joanne; Torpy, Brendan; Young, Greg] Univ Colorado, Ctr Limb Atomspher Sounding, Boulder, CO 80309 USA. [Froidevaux, Lucien; Lambert, Alyn] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Godin-Beekmann, Sophie] Univ Paris 06, CNRS, IPSL, Serv Aeron,UMR 7620, F-75005 Paris, France. [Randall, Cora E.; Harvey, V. Lynn] Atmospher & Space Phys Lab, Boulder, CO 80303 USA. [Leblanc, Thierry; McDermid, I. Stuart] CALTECH, Jet Prop Lab, Table Mt Facil, Wrightwood, CA 92397 USA. [Waterfall, Alison; Reburn, W. Jolyon] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Thompson, Anne M.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. [Valverde-Canossa, Jessica] Univ Nacl, Lab Quim Atmosfera, Heredia 3000, Costa Rica. [Witte, Jacquelyn C.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Bernath, Peter F.] Univ York, Dept Chem, Heslington, Yorks, England. [Walker, Kaley A.] Univ Toronto, Dept Phys, Toronto, ON, Canada. RP Nardi, B (reprint author), Natl Ctr Atmospher Res, Boulder, CO 80301 USA. EM nardi@ucar.edu RI Bernath, Peter/B-6567-2012; McGee, Thomas/G-4951-2013; Randall, Cora/L-8760-2014; Thompson, Anne /C-3649-2014 OI Bernath, Peter/0000-0002-1255-396X; Randall, Cora/0000-0002-4313-4397; Thompson, Anne /0000-0002-7829-0920 NR 34 TC 26 Z9 26 U1 2 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 10 PY 2008 VL 113 IS D16 AR D16S36 DI 10.1029/2007JD008837 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 314LW UT WOS:000256811900003 ER PT J AU Schoeberl, MR Douglass, AR Joiner, J AF Schoeberl, M. R. Douglass, A. R. Joiner, J. TI Introduction to special section on Aura Validation SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Editorial Material ID OZONE MONITORING INSTRUMENT; MISSION AB Aura, the last of the large EOS observatories, was launched on 15 July 2004 and has now been operating for several years. Aura is designed to make comprehensive stratospheric, mesospheric, and tropospheric constituent measurements from its four instruments HIRDLS, MLS, OMI, and TES. All of the instruments are performing well and observations of stratospheric and tropospheric trace gases and aerosols are revolutionizing our understanding of stratospheric chemistry and transport processes, ozone depletion, air quality, and the hydrological cycle. In this special section, the instrument teams and collaborators report on the validation of the released Aura data products. C1 [Schoeberl, M. R.; Douglass, A. R.; Joiner, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Schoeberl, MR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM mark.r.schoeberl@nasa.gov RI Joiner, Joanna/D-6264-2012; Douglass, Anne/D-4655-2012 NR 73 TC 4 Z9 4 U1 2 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 10 PY 2008 VL 113 IS D15 AR D15S01 DI 10.1029/2007JD009602 PG 6 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 314LU UT WOS:000256811700001 ER PT J AU Vaughan, RG Kervyn, M Realmuto, V Abrams, M Hook, SJ AF Vaughan, R. Greg Kervyn, Matthieu Realmuto, Vince Abrams, Michael Hook, Simon J. TI Satellite measurements of recent volcanic activity at Oldoinyo Lengai, Tanzania SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH LA English DT Article DE Oldoinyo Lengai; thermal infrared remote sensing; ASTER; MODIS; volcanic ash plume ID SPACEBORNE THERMAL EMISSION; REFLECTION RADIOMETER ASTER; OL DOINYO LENGAI; CARBONATITE LAVA; LASCAR VOLCANO; INFRARED DATA; MOUNT-ETNA; ERUPTION; TEMPERATURE; SILICATE AB Oldoinyo Lengai (OL) is the only active volcano in the world that produces natrocarbonatite lava. These carbonate-rich lavas are unique in that they have relatively low temperatures (495-590 degrees C) and very low viscosity. OL has been erupting intermittently since 1983, mostly with small lava flows, pools and spatter cones (hornitos) confined to the summit crater. Explosive, ash-producing eruptions are rare, however, on September 4, 2007 the Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) captured the first satellite image of an ash plume erupting from OL, which may be indicative of a new phase of more silica-rich products and explosive activity that has not occurred since 1966-1967. In the months prior to the eruption, thermal infrared (TIR) satellite monitoring detected an increasing number of thermal anomalies around OL. Data from the Moderate Resolution Imaging Spectroradiometer (MODIS) sensor analyzed with the MODLEN algorithm detected more than 30 hot spots in the last week of August and first week of September 2007, some of which were from bush fires ignited by lava flows or spatter around the volcano. Higher-resolution ASTER data confirmed the location of these burn scars associated with lava flows. ASTER also detected the appearance of an anomalous hot spot at the summit of OL in mid-June with temperatures similar to 440 degrees C, the presence of several new lava flows in the crater in July and August, and on September 4 measured higher temperatures (similar to 550 degrees C) possibly suggesting a more silicate-rich eruption. ASTER spectral emissivity data were interpreted to indicate a mixture of carbonate and silicate ash in the eruption plume from September 4. Based on the analysis of both ASTER and MODIS data combined with occasional field observations, there appear to have been 2 distinct eruptive events so far in 2007: a typical natrocarbonatite eruption confined to the summit crater in June-July, and a more intense eruption in August-September consisting of natrocarbonatite lava overflowing the crater and explosive events forming ash plumes up to similar to 5 km high, apparently consisting of a mixture of silicate and carbonate ash. OL is one of the many volcanoes in the world, and especially Africa, that is not regularly monitored with in situ instruments. Continued satellite monitoring along with studies of past thermal activity will help determine how future eruptions and ensuing hazards may be forecasted. (C) 2008 Elsevier B.V. All rights reserved. C1 [Vaughan, R. Greg; Realmuto, Vince; Abrams, Michael; Hook, Simon J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kervyn, Matthieu] Univ Ghent, Dept Soil Sci & Geol, Mercator & Ortelius Res Ctr Erupt Dynam, B-9000 Ghent, Belgium. RP Vaughan, RG (reprint author), CALTECH, Jet Prop Lab, MS 183-501,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM vaughanrg@gmail.com RI Kervyn, Matthieu/I-6512-2015 OI Kervyn, Matthieu/0000-0002-4966-3468 NR 51 TC 29 Z9 29 U1 1 U2 18 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 JUN 10 PY 2008 VL 173 IS 3-4 BP 196 EP 206 DI 10.1016/j.jvolgeores.2008.01.028 PG 11 WC Geosciences, Multidisciplinary SC Geology GA 322CN UT WOS:000257352900004 ER PT J AU Cantrell, JH AF Cantrell, John H. TI Effects of diffraction and dispersion on acoustic radiation-induced static pulses SO APPLIED PHYSICS LETTERS LA English DT Article ID SOLIDS; STRESS AB It is shown that the shapes of acoustic radiation-induced static strain and displacement pulses are defined locally by the energy density of the generating waveform and that diffraction and attenuation produce dramatic changes in the shape of static displacement pulses when using laser detection. The effects of dispersion on static pulses are obtained by including a dispersive term in the phase of the particle velocity solution to the nonlinear wave equation. The dispersion causes an evolutionary change in the shape of the energy density profile that leads to the generation of solitons experimentally observed in fused silica. (C) 2008 American Institute of Physics. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Cantrell, JH (reprint author), NASA, Langley Res Ctr, Mail Stop 231, Hampton, VA 23681 USA. EM john.h.cantrell@nasa.gov NR 14 TC 9 Z9 9 U1 1 U2 1 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD JUN 9 PY 2008 VL 92 IS 23 AR 231914 DI 10.1063/1.2937474 PG 3 WC Physics, Applied SC Physics GA 312XP UT WOS:000256706000023 ER PT J AU Mouroulis, P Green, RO Wilson, DW AF Mouroulis, Pantazis Green, Robert O. Wilson, Daniel W. TI Optical design of a coastal ocean imaging spectrometer SO OPTICS EXPRESS LA English DT Article ID GRATING FABRICATION; AIRBORNE; LITHOGRAPHY; CALIBRATION; SYSTEM AB We present an optical design for an airborne imaging spectrometer that addresses the unique constraints imposed by imaging the coastal ocean region. A fast (F/1.8) wide field system (36 degrees) with minimum polarization dependence and high response uniformity is required, that covers the spectral range 350-1050 nm with 3 nm sampling. We show how these requirements can be achieved with a two-mirror telescope and a compact Dyson spectrometer utilizing a polarization-insensitive diffraction grating. (c) 2008 Optical Society of America. C1 [Mouroulis, Pantazis; Green, Robert O.; Wilson, Daniel W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mouroulis, P (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM pantazis.mouroulis@jpl.nasa.gov NR 22 TC 34 Z9 39 U1 3 U2 14 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD JUN 9 PY 2008 VL 16 IS 12 BP 9087 EP 9096 DI 10.1364/OE.16.009087 PG 10 WC Optics SC Optics GA 315ED UT WOS:000256859900075 PM 18545620 ER PT J AU Bargmann, S Steinmann, P Jordan, PM AF Bargmann, S. Steinmann, P. Jordan, P. M. TI On the propagation of second-sound in linear and nonlinear media: Results from Green-Naghditheory SO PHYSICS LETTERS A LA English DT Article DE Green-Naghdi theory; second-sound; temperature rate waves; traveling wave solution; Lambert W-function ID LAMBERT-W-FUNCTION; DISCONTINUITY WAVES; ENERGY-DISSIPATION; HEAT-CONDUCTION; VISCOUS FLUID; THERMOELASTICITY AB We investigate thermal wave propagation in one-dimensional media according to Green-Naghdi's heat conduction theory. Under the linearized theory, the dynamic propagation of a Heaviside input signal in h half-space is examined. Exact analytical solutions are derived for the three cases (i.e., types I-III) of this theory. We then numerically compare the evolution of the linear and nonlinear type-II temperature profiles, and track the finite-time blow-up of the latter's temperature rate wave, in the setting of an initial-boundary value problem involving a sudden sinusoidal input signal. Lastly, an exact traveling wave solution of a lossless, nonlinear equation, which arises under type-II theory, is determined and analyzed. Published by Elsevier B.V. C1 [Jordan, P. M.] Stennis Space Ctr, Naval Res Lab, Stennis Space Ctr, MS 39529 USA. [Bargmann, S.] Univ Kaiserslautern, Chair Appl Mech, D-67653 Kaiserslautern, Germany. [Steinmann, P.] Univ Erlangen Nurnberg, Chair Appl Mech, D-91058 Erlangen, Germany. RP Jordan, PM (reprint author), Stennis Space Ctr, Naval Res Lab, Code 7181, Stennis Space Ctr, MS 39529 USA. EM pjordan@nrlssc.navy.mil OI Steinmann, Paul/0000-0003-1490-947X NR 32 TC 23 Z9 23 U1 1 U2 3 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 JUN 9 PY 2008 VL 372 IS 24 BP 4418 EP 4424 DI 10.1016/j.physleta.2008.04.010 PG 7 WC Physics, Multidisciplinary SC Physics GA 319ZO UT WOS:000257203700017 ER PT J AU Abbott, B Abbott, R Adhikari, R Ajith, P Allen, B Allen, G Amin, R Anderson, SB Anderson, WG Arain, MA Araya, M Armandula, H Armor, P Aso, Y Aston, S Aufmuth, P Aulbert, C Babak, S Ballmer, S Bantilan, H Barish, BC Barker, C Barker, D Barr, B Barriga, P Barton, MA Bastarrika, M Bayer, K Betzwieser, J Beyersdorf, PT Bilenko, IA Billingsley, G Biswas, R Black, E Blackburn, K Blackburn, L Blair, D Bland, B Bodiya, TP Bogue, L Bork, R Boschi, V Bose, S Brady, PR Braginsky, VB Brau, JE Brinkmann, M Brooks, A Brown, DA Brunet, G Bullington, A Buonanno, A Burmeister, O Byer, RL Cadonati, L Cagnoli, G Camp, JB Cannizzo, J Cannon, K Cao, J Cardenas, L Casebolt, T Castaldi, G Cepeda, C Chalkley, E Charlton, P Chatterji, S Chelkowski, S Chen, Y Christensen, N Clark, D Clark, J Cokelaer, T Conte, R Cook, D Corbitt, T Coyne, D Creighton, JDE Cumming, A Cunningham, L Cutler, RM Dalrymple, J Danzmann, K Davies, G DeBra, D Degallaix, J Degree, M Dergachev, V Desai, S DeSalvo, R Dhurandhar, S Diaz, M Dickson, J Dietz, A Donovan, F Dooley, KL Doomes, EE Drever, RWP Duke, I Dumas, JC Dupuis, RJ Dwyer, JG Echols, C Effler, A Ehrens, P Espinoza, E Etzel, T Evans, T Fairhurst, S Fan, Y Fazi, D Fehrmann, H Fejer, MM Finn, LS Flasch, K Fotopoulos, N Freise, A Frey, R Fricke, T Fritschel, P Frolov, VV Fyffe, M Garofoli, J Gholami, I Giaime, JA Giampanis, S Giardina, KD Goda, K Goetz, E Goggin, L Gonzalez, G Gossler, S Gouaty, R Grant, A Gras, S Gray, C Gray, M Greenhalgh, RJS Gretarsson, AM Grimaldi, F Grosso, R Grote, H Grunewald, S Guenther, M Gustafson, EK Gustafson, R Hage, B Hallam, JM Hammer, D Hanna, C Hanson, J Harms, J Harry, G Harstad, E Hayama, K Hayler, T Heefner, J Heng, IS Hennessy, M Heptonstall, A Hewitson, M Hild, S Hirose, E Hoak, D Hosken, D Hough, J Huttner, SH Ingram, D Ito, M Ivanov, A Johnson, B Johnson, WW Jones, DI Jones, G Jones, R Ju, L Kalmus, P Kalogera, V Kamat, S Kanner, J Kasprzyk, D Katsavounidis, E Kawabe, K Kawamura, S Kawazoe, F Kells, W Keppel, DG Khalili, FY Khan, R Khazanov, E Kim, C King, P Kissel, JS Klimenko, S Kokeyama, K Kondrashov, V Kopparapu, RK Kozak, D Kozhevatov, I Krishnan, B Kwee, P Lam, PK Landry, M Lang, MM Lantz, B Lazzarini, A Lei, M Leindecker, N Leonhardt, V Leonor, I Libbrecht, K Lin, H Lindquist, P Lockerbie, NA Lodhia, D Lormand, M Lu, P Lubinski, M Lucianetti, A Luck, H Machenschalk, B MacInnis, M Mageswaran, M Mailand, K Mandic, V Marka, S Marka, Z Markosyan, A Markowitz, J Maros, E Martin, I Martin, RM Marx, JN Mason, K Matichard, F Matone, L Matzner, R Mavalvala, N McCarthy, R McClelland, DE McGuire, SC McHugh, M McIntyre, G McIvor, G McKechan, D McKenzie, K Meier, T Melissinos, A Mendell, G Mercer, RA Meshkov, S Messenger, CJ Meyers, D Miller, J Minelli, J Mitra, S Mitrofanov, VP Mitselmakher, G Mittleman, R Miyakawa, O Moe, B Mohanty, S Moreno, G Mossavi, K MowLowry, C Mueller, G Mukherjee, S Mukhopadhyay, H Muller-Ebhardt, H Munch, J Murray, P Myers, E Myers, J Nash, T Nelson, J Newton, G Nishizawa, A Numata, K O'Dell, J Ogin, G O'Reilly, B O'Shaughnessy, R Ottaway, DJ Ottens, RS Overmier, H Owen, BJ Pan, Y Pankow, C Papa, MA Parameshwaraiah, V Patel, P Pedraza, M Penn, S Perreca, A Petrie, T Pinto, IM Pitkin, M Pletsch, HJ Plissi, MV Postiglione, F Principe, M Prix, R Quetschke, V Raab, F Rabeling, DS Radkins, H Rainer, N Rakhmanov, M Ramsunder, M Rehbein, H Reid, S Reitze, DH Riesen, R Riles, K Rivera, B Robertson, NA Robinson, C Robinson, EL Roddy, S Rodriguez, A Rogan, AM Rollins, J Romano, JD Romie, J Route, R Rowan, S Rudiger, A Ruet, L Russell, P Ryan, K Sakata, S Samidi, M de la Jordana, LS Sandberg, V Sannibale, V Saraf, S Sarin, P Sathyaprakash, BS Sato, S Saulson, PR Savage, R Savov, P WSchediwy, S Schilling, R Schnabel, R Schofield, R Schutz, BF Schwinberg, P Scott, SM Searle, AC Sears, B Seifert, F Sellers, D Sengupta, AS Shawhan, P Shoemaker, DH Sibley, A Siemens, X Sigg, D Sinha, S Sintes, AM Slagmolen, BJJ Slutsky, J Smith, JR Smith, MR Smith, ND Somiya, K Sorazu, B Stein, LC Stochino, A Stone, R Strain, KA Strom, DM Stuver, A Summerscales, TZ Sun, KX Sung, M Sutton, PJ Takahashi, H Tanner, DB Taylor, R Taylor, R Thacker, J Thorne, KA Thorne, KS Thuring, A Tokmakov, KV Torres, C Torrie, C Traylor, G Trias, M Tyler, W Ugolini, D Ulmen, J Urbanek, K Vahlbruch, H Van Den Broeck, C van der Sluys, M Vass, S Vaulin, R Vecchio, A Veitch, J Veitch, P Villar, A Vorvick, C Vyachanin, SP Waldman, SJ Wallace, L Ward, H Ward, R Weinert, M Weinstein, A Weiss, R Wen, S Wette, K Whelan, J Whitcomb, SE Whiting, B Wilkinson, C Willems, PA Williams, HR Williams, L Willke, B Wilmut, I Winkler, W Wipf, CC Wiseman, AG Woan, G Wooley, R Worden, J Wu, W Yakushin, I Yamamoto, H Yan, Z Yoshida, S Zanolin, M Zhang, J Zhang, L Zhao, C Zotov, N Zucker, M Zweizig, J Acernese, F Alshourbagy, M Amico, P Antonucci, F Aoudia, S Astone, P Avino, S Baggio, L Ballardin, G Barone, F Barsotti, L Barsuglia, M Bauer, TS Bigotta, S Birindelli, S Bizouard, MA Boccara, C Bondu, F Bosi, L Braccini, S Bradaschia, C Brillet, A Brisson, V Buskulic, D Cagnoli, G Calloni, E Campagna, E Carbognani, F Cavalier, F Cavalieri, R Cella, G Cesarini, E Chassande-Mottin, E Clapson, AC Cleva, F Coccia, E Corda, C Corsi, A Cottone, F Coulon, JP Cuoco, E D'Antonio, S Dari, A Dattilo, V Davier, M De Rosa, R Del Prete, M Di Fiore, L Di Lieto, A Emilio, MDP Di Virgilio, A Evans, M Fafone, V Ferrante, I Fidecaro, F Fiori, I Flaminio, R Fournier, JD Frasca, S Frasconi, F Gammaitoni, L Garufi, F Genin, E Gennai, A Giazotto, A Giordano, L Granata, V Greverie, C Grosjean, D Guidi, G Hamdani, S Hebri, S Heitmann, H Hello, P Huet, D Kreckelbergh, S La Penna, P Laval, M Leroy, N Letendre, N Lopez, B Lorenzini, M Loriette, V Losurdo, G Mackowski, JM Majorana, E Man, CN Mantovani, M Marchesoni, F Marion, F Marque, J Martelli, F Masserot, A Menzinger, F Milano, L Minenkov, Y Moins, C Moreau, J Morgado, N Mosca, S Mours, B Neri, I Nocera, F Pagliaroli, G Palomba, C Paoletti, F Pardi, S Pasqualetti, A Passaquieti, R Passuello, D Piergiovanni, F Pinard, L Poggiani, R Punturo, M Puppo, P Rapagnani, P Regimbau, T Remillieux, A Ricci, F Ricciardi, I Rocchi, A Rolland, L Romano, R Ruggi, P Russo, G Solimeno, S Spallicci, A Swinkels, BL Tarallo, M Terenzi, R Toncelli, A Tonelli, M Tournefier, E Travasso, F Vajente, G van den Brand, JFJ van der Putten, S Verkindt, D Vetrano, F Vicere, A Vinet, JY Vocca, H Yvert, M AF Abbott, B. 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Hough, J. Huttner, S. H. Ingram, D. Ito, M. Ivanov, A. Johnson, B. Johnson, W. W. Jones, D. I. Jones, G. Jones, R. Ju, L. Kalmus, P. Kalogera, V. Kamat, S. Kanner, J. Kasprzyk, D. Katsavounidis, E. Kawabe, K. Kawamura, S. Kawazoe, F. Kells, W. Keppel, D. G. Khalili, F. Ya Khan, R. Khazanov, E. Kim, C. King, P. Kissel, J. S. Klimenko, S. Kokeyama, K. Kondrashov, V. Kopparapu, R. K. Kozak, D. Kozhevatov, I. Krishnan, B. Kwee, P. Lam, P. K. Landry, M. Lang, M. M. Lantz, B. Lazzarini, A. Lei, M. Leindecker, N. Leonhardt, V. Leonor, I. Libbrecht, K. Lin, H. Lindquist, P. Lockerbie, N. A. Lodhia, D. Lormand, M. Lu, P. Lubinski, M. Lucianetti, A. Lueck, H. Machenschalk, B. MacInnis, M. Mageswaran, M. Mailand, K. Mandic, V. Marka, S. Marka, Z. Markosyan, A. Markowitz, J. Maros, E. Martin, I. Martin, R. M. Marx, J. N. Mason, K. Matichard, F. Matone, L. Matzner, R. Mavalvala, N. McCarthy, R. McClelland, D. E. McGuire, S. C. McHugh, M. McIntyre, G. McIvor, G. McKechan, D. McKenzie, K. Meier, T. Melissinos, A. Mendell, G. Mercer, R. A. Meshkov, S. Messenger, C. J. Meyers, D. Miller, J. Minelli, J. Mitra, S. Mitrofanov, V. P. Mitselmakher, G. Mittleman, R. Miyakawa, O. Moe, B. Mohanty, S. Moreno, G. Mossavi, K. MowLowry, C. Mueller, G. Mukherjee, S. Mukhopadhyay, H. Mueller-Ebhardt, H. Munch, J. Murray, P. Myers, E. Myers, J. Nash, T. Nelson, J. Newton, G. Nishizawa, A. Numata, K. O'Dell, J. Ogin, G. O'Reilly, B. O'Shaughnessy, R. Ottaway, D. J. Ottens, R. S. Overmier, H. Owen, B. J. Pan, Y. Pankow, C. Papa, M. A. Parameshwaraiah, V. Patel, P. Pedraza, M. Penn, S. Perreca, A. Petrie, T. Pinto, I. M. Pitkin, M. Pletsch, H. J. Plissi, M. V. Postiglione, F. Principe, M. Prix, R. Quetschke, V. Raab, F. Rabeling, D. S. Radkins, H. Rainer, N. Rakhmanov, M. Ramsunder, M. Rehbein, H. Reid, S. Reitze, D. H. Riesen, R. Riles, K. Rivera, B. Robertson, N. A. Robinson, C. Robinson, E. L. Roddy, S. Rodriguez, A. Rogan, A. M. Rollins, J. Romano, J. D. Romie, J. Route, R. Rowan, S. 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Davier, M. De Rosa, R. Del Prete, M. Di Fiore, L. Di Lieto, A. Emilio, M. Di Paolo Di Virgilio, A. Evans, M. Fafone, V. Ferrante, I. Fidecaro, F. Fiori, I. Flaminio, R. Fournier, J-D Frasca, S. Frasconi, F. Gammaitoni, L. Garufi, F. Genin, E. Gennai, A. Giazotto, A. Giordano, L. Granata, V. Greverie, C. Grosjean, D. Guidi, G. Hamdani, S. Hebri, S. Heitmann, H. Hello, P. Huet, D. Kreckelbergh, S. La Penna, P. Laval, M. Leroy, N. Letendre, N. Lopez, B. Lorenzini, M. Loriette, V. Losurdo, G. Mackowski, J-M Majorana, E. Man, C. N. Mantovani, M. Marchesoni, F. Marion, F. Marque, J. Martelli, F. Masserot, A. Menzinger, F. Milano, L. Minenkov, Y. Moins, C. Moreau, J. Morgado, N. Mosca, S. Mours, B. Neri, I. Nocera, F. Pagliaroli, G. Palomba, C. Paoletti, F. Pardi, S. Pasqualetti, A. Passaquieti, R. Passuello, D. Piergiovanni, F. Pinard, L. Poggiani, R. Punturo, M. Puppo, P. Rapagnani, P. Regimbau, T. Remillieux, A. Ricci, F. Ricciardi, I. Rocchi, A. Rolland, L. Romano, R. Ruggi, P. Russo, G. Solimeno, S. Spallicci, A. Swinkels, B. L. Tarallo, M. Terenzi, R. Toncelli, A. Tonelli, M. Tournefier, E. Travasso, F. Vajente, G. van den Brand, J. F. J. van der Putten, S. Verkindt, D. Vetrano, F. Vicere, A. Vinet, J-Y Vocca, H. Yvert, M. CA LIGO Sci Collaboration Virgo Collaboration TI Astrophysically triggered searches for gravitational waves: status and prospects SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article; Proceedings Paper CT 18th International Conference on General Relativity and Gravitation/7th Edoardo Amaldi Conference on Gravitational Waves CY JUL, 2007 CL Sydney, AUSTRALIA ID GAMMA-RAY BURSTS; ACCRETING NEUTRON-STARS; SGR 1806-20; ENERGY NEUTRINOS; 2004 HYPERFLARE; GIANT FLARE; DISCOVERY; OSCILLATIONS; SENSITIVITY; DETECTOR AB In gravitational-wave detection, special emphasis is put onto searches that focus on cosmic events detected by other types of astrophysical observatories. The astrophysical triggers, e. g. from gamma-ray and x-ray satellites, optical telescopes and neutrino observatories, provide a trigger time for analyzing gravitational-wave data coincident with the event. In certain cases the expected frequency range, source energetics, directional and progenitor information are also available. Beyond allowing the recognition of gravitational waveforms with amplitudes closer to the noise floor of the detector, these triggered searches should also lead to rich science results even before the onset of Advanced LIGO. In this paper we provide a broad review of LIGO's astrophysically triggered searches and the sources they target. C1 [Abbott, B.; Abbott, R.; Adhikari, R.; Anderson, S. B.; Araya, M.; Armandula, H.; Ballmer, S.; Barish, B. C.; Betzwieser, J.; Billingsley, G.; Black, E.; Blackburn, K.; Bork, R.; Boschi, V.; Brooks, A.; Cannon, K.; Cardenas, L.; Cepeda, C.; Chatterji, S.; Coyne, D.; DeSalvo, R.; Dupuis, R. 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J.] Vrije Univ Amsterdam, NL-1081 HV Amsterdam, Netherlands. RP Abbott, B (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA. RI Marchesoni, Fabio/A-1920-2008; Kawabe, Keita/G-9840-2011; Bondu, Francois/A-2071-2012; Toncelli, Alessandra/A-5352-2012; Vocca, Helios/F-1444-2010; Finn, Lee Samuel/A-3452-2009; Punturo, Michele/I-3995-2012; Cuoco, Elena/I-8789-2012; Vicere, Andrea/J-1742-2012; Mitrofanov, Valery/D-8501-2012; Puppo, Paola/J-4250-2012; Rapagnani, Piero/J-4783-2012; Bilenko, Igor/D-5172-2012; Lam, Ping Koy/A-5276-2008; Gammaitoni, Luca/B-5375-2009; Bigotta, Stefano/F-8652-2011; Freise, Andreas/F-8892-2011; Neri, Igor/F-1482-2010; McClelland, David/E-6765-2010; Martin, Iain/A-2445-2010; Hild, Stefan/A-3864-2010; Rowan, Sheila/E-3032-2010; Strain, Kenneth/D-5236-2011; Acernese, Fausto/E-4989-2010; Raab, Frederick/E-2222-2011; Lueck, Harald/F-7100-2011; Kawazoe, Fumiko/F-7700-2011; Cella, Giancarlo/A-9946-2012; Travasso, Flavio/J-9595-2016; Cesarini, Elisabetta/C-4507-2017; Frey, Raymond/E-2830-2016; ricciardi, iolanda/D-5527-2009; Di Virgilio, Angela Dora Vittoria/E-9078-2015; Ward, Robert/I-8032-2014; Khan, Rubab/F-9455-2015; Ottaway, David/J-5908-2015; Garufi, Fabio/K-3263-2015; Postiglione, Fabio/O-4744-2015; Rocchi, Alessio/O-9499-2015; Martelli, Filippo/P-4041-2015; Biswas, Rahul/H-7474-2016; Tarallo, Marco/B-2096-2012; mosca, simona/I-7116-2012; Frasconi, Franco/K-1068-2016; Sigg, Daniel/I-4308-2015; Pinto, Innocenzo/L-3520-2016; Harms, Jan/J-4359-2012; Ferrante, Isidoro/F-1017-2012; Allen, Bruce/K-2327-2012; Chen, Yanbei/A-2604-2013; Barker, David/A-5671-2013; Zhao, Chunnong/C-2403-2013; Ju, Li/C-2623-2013; Pitkin, Matthew/I-3802-2013; Vyatchanin, Sergey/J-2238-2012; Khazanov, Efim/B-6643-2014; Lucianetti, Antonio/G-7383-2014; Losurdo, Giovanni/K-1241-2014; Khalili, Farit/D-8113-2012; Vecchio, Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015 OI Zweizig, John/0000-0002-1521-3397; O'Shaughnessy, Richard/0000-0001-5832-8517; Aulbert, Carsten/0000-0002-1481-8319; Di Paolo Emilio, Maurizio/0000-0002-9558-3610; Freise, Andreas/0000-0001-6586-9901; Marchesoni, Fabio/0000-0001-9240-6793; Bondu, Francois/0000-0001-6487-5197; Toncelli, Alessandra/0000-0003-4400-8808; Vocca, Helios/0000-0002-1200-3917; Finn, Lee Samuel/0000-0002-3937-0688; Punturo, Michele/0000-0001-8722-4485; Vicere, Andrea/0000-0003-0624-6231; Puppo, Paola/0000-0003-4677-5015; Lam, Ping Koy/0000-0002-4421-601X; Gammaitoni, Luca/0000-0002-4972-7062; Neri, Igor/0000-0002-9047-9822; McClelland, David/0000-0001-6210-5842; Strain, Kenneth/0000-0002-2066-5355; Acernese, Fausto/0000-0003-3103-3473; Lueck, Harald/0000-0001-9350-4846; Hallam, Jonathan Mark/0000-0002-7087-0461; Vetrano, Flavio/0000-0002-7523-4296; calloni, enrico/0000-0003-4819-3297; Sorazu, Borja/0000-0002-6178-3198; Nishizawa, Atsushi/0000-0003-3562-0990; Fairhurst, Stephen/0000-0001-8480-1961; Boschi, Valerio/0000-0001-8665-2293; Matichard, Fabrice/0000-0001-8982-8418; Pinto, Innocenzo M./0000-0002-2679-4457; Swinkels, Bas/0000-0002-3066-3601; Guidi, Gianluca/0000-0002-3061-9870; Minelli, Jeff/0000-0002-5330-912X; Coccia, Eugenio/0000-0002-6669-5787; Cella, Giancarlo/0000-0002-0752-0338; Travasso, Flavio/0000-0002-4653-6156; Cesarini, Elisabetta/0000-0001-9127-3167; Frey, Raymond/0000-0003-0341-2636; ricciardi, iolanda/0000-0002-1804-6782; Di Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; Stein, Leo/0000-0001-7559-9597; Ward, Robert/0000-0001-5503-5241; Ricci, Fulvio/0000-0001-5475-4447; Whelan, John/0000-0001-5710-6576; Avino, Saverio/0000-0001-6623-9784; Khan, Rubab/0000-0001-5100-5168; Garufi, Fabio/0000-0003-1391-6168; Postiglione, Fabio/0000-0003-0628-3796; Rocchi, Alessio/0000-0002-1382-9016; Martelli, Filippo/0000-0003-3761-8616; Biswas, Rahul/0000-0002-0774-8906; Tarallo, Marco/0000-0001-5169-4987; mosca, simona/0000-0001-7869-8275; Frasconi, Franco/0000-0003-4204-6587; Sigg, Daniel/0000-0003-4606-6526; Ferrante, Isidoro/0000-0002-0083-7228; Whiting, Bernard F/0000-0002-8501-8669; Veitch, John/0000-0002-6508-0713; Principe, Maria/0000-0002-6327-0628; Papa, M.Alessandra/0000-0002-1007-5298; Kanner, Jonah/0000-0001-8115-0577; Allen, Bruce/0000-0003-4285-6256; Zhao, Chunnong/0000-0001-5825-2401; Pitkin, Matthew/0000-0003-4548-526X; Losurdo, Giovanni/0000-0003-0452-746X; Vecchio, Alberto/0000-0002-6254-1617; NR 68 TC 16 Z9 16 U1 3 U2 22 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD JUN 7 PY 2008 VL 25 IS 11 AR 114051 DI 10.1088/0264-9381/25/11/114051 PG 12 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 301LH UT WOS:000255897200052 ER PT J AU Babak, S Baker, JG Benacquista, MJ Cornish, NJ Crowder, J Cutler, C Larson, SL Littenberg, TB Porter, EK Vallisneri, M Vecchio, A Auger, G Barack, L Blaut, A Bloomer, E Brown, DA Christensen, N Clark, J Fairhurst, S Gair, JR Halloin, H Hendry, M Jimenez, A Krolak, A Mandel, I Messenger, C Meyer, R Mohanty, S Nayak, R Petiteau, A Pitkin, M Plagnol, E Prix, R Robinson, EL Roever, C Savov, P Stroeer, A Toher, J Veitch, J Vinet, JY Wen, LQ Whelan, JT Woan, G AF Babak, Stanislav Baker, John G. Benacquista, Matthew J. Cornish, Neil J. Crowder, Jeff Cutler, Curt Larson, Shane L. Littenberg, Tyson B. Porter, Edward K. Vallisneri, Michele Vecchio, Alberto Auger, Gerard Barack, Leor Blaut, Arkadiusz Bloomer, Ed Brown, Duncan A. Christensen, Nelson Clark, James Fairhurst, Stephen Gair, Jonathan R. Halloin, Hubert Hendry, Martin Jimenez, Arturo Krolak, Andrzej Mandel, Ilya Messenger, Chris Meyer, Renate Mohanty, Soumya Nayak, Rajesh Petiteau, Antoine Pitkin, Matt Plagnol, Eric Prix, Reinhard Robinson, Emma L. Roever, Christian Savov, Pavlin Stroeer, Alexander Toher, Jennifer Veitch, John Vinet, Jean-Yves Wen, Linqing Whelan, John T. Woan, Graham CA Mock Lisa Data Challenge Task Forc Challenge-2 Participants TI Report on the second Mock LISA data challenge SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article; Proceedings Paper CT 18th International Conference on General Relativity and Gravitation/7th Edoardo Amaldi Conference on Gravitational Waves CY JUL, 2007 CL Sydney, AUSTRALIA ID BLACK-HOLE BINARIES; SEARCH AB The Mock LISA data challenges are a program to demonstrate LISA data-analysis capabilities and to encourage their development. Each round of challenges consists of several data sets containing simulated instrument noise and gravitational waves from sources of undisclosed parameters. Participants are asked to analyze the data sets and report the maximum information about the source parameters. The challenges are being released in rounds of increasing complexity and realism: here we present the results of Challenge 2, issued in Jan 2007, which successfully demonstrated the recovery of signals from nonspinning supermassive-black-hole binaries with optimal SNRs between similar to 10 and 2000, from similar to 20 000 overlapping galactic white-dwarf binaries (among a realistically distributed population of 26 million), and from the extreme-mass-ratio inspirals of compact objects into central galactic black holes with optimal SNRs similar to 100. C1 [Babak, Stanislav; Porter, Edward K.; Prix, Reinhard; Wen, Linqing; Whelan, John T.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany. [Baker, John G.] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA. [Benacquista, Matthew J.; Jimenez, Arturo; Mohanty, Soumya; Nayak, Rajesh] Univ Texas Brownsville, Ctr Gravitat Wave Astron, Brownsville, TX 78520 USA. [Cornish, Neil J.; Littenberg, Tyson B.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Crowder, Jeff; Cutler, Curt; Vallisneri, Michele] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cutler, Curt; Vallisneri, Michele; Brown, Duncan A.; Fairhurst, Stephen; Mandel, Ilya; Savov, Pavlin] CALTECH, Pasadena, CA 91125 USA. [Larson, Shane L.] Weber State Univ, Dept Phys, Ogden, UT 84408 USA. [Vecchio, Alberto; Robinson, Emma L.; Stroeer, Alexander; Veitch, John] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Vecchio, Alberto; Mandel, Ilya; Stroeer, Alexander] Northwestern Univ, Dept Phys & Astron, Evanston, IL USA. [Auger, Gerard; Halloin, Hubert; Petiteau, Antoine; Plagnol, Eric] Univ Paris 07, APC, UMR 7164, F-75025 Paris 13, France. [Barack, Leor] Univ Southampton, Sch Math, Southampton SO17 1BJ, Hants, England. [Blaut, Arkadiusz] Univ Wroclaw, Inst Theoret Phys, PL-50138 Wroclaw, Poland. [Bloomer, Ed; Clark, James; Hendry, Martin; Messenger, Chris; Pitkin, Matt; Toher, Jennifer; Woan, Graham] Univ Glasgow, Dept Phys & Astron, Glasgow, Lanark, Scotland. [Brown, Duncan A.] Syracuse Univ, Dept Phys, Syracuse, NY 13244 USA. [Brown, Duncan A.; Fairhurst, Stephen] CALTECH, LIGO Lab, Pasadena, CA 91125 USA. [Christensen, Nelson] Carleton Coll, Northfield, MN 55057 USA. [Fairhurst, Stephen] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3YB, Wales. [Gair, Jonathan R.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Krolak, Andrzej] Polish Acad Sci, Inst Math, Warsaw, Poland. [Meyer, Renate; Roever, Christian] Univ Auckland, Dept Stat, Auckland 1, New Zealand. [Vinet, Jean-Yves] CNRS, Observ Cote Dazur, ARTEMIS, F-06304 Nice, France. RP Babak, S (reprint author), Max Planck Inst Gravitat Phys, Albert Einstein Inst, Muhlenberg 1, D-14476 Golm, Germany. EM Michele.Vallisneri@jpl.nasa.gov RI Larson, Shane/E-8576-2010; Pitkin, Matthew/I-3802-2013; Vecchio, Alberto/F-8310-2015; OI Pitkin, Matthew/0000-0003-4548-526X; Vecchio, Alberto/0000-0002-6254-1617; Rover, Christian/0000-0002-6911-698X; Whelan, John/0000-0001-5710-6576; Fairhurst, Stephen/0000-0001-8480-1961; Mandel, Ilya/0000-0002-6134-8946; Veitch, John/0000-0002-6508-0713 NR 13 TC 33 Z9 33 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD JUN 7 PY 2008 VL 25 IS 11 AR 114037 DI 10.1088/0264-9381/25/11/114037 PG 8 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 301LH UT WOS:000255897200038 ER PT J AU Berti, E Cardoso, V Gonzalez, JA Sperhake, U Brugmann, B AF Berti, E. Cardoso, V. Gonzalez, J. A. Sperhake, U. Bruegmann, B. TI Multipolar analysis of spinning binaries SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article; Proceedings Paper CT 18th International Conference on General Relativity and Gravitation/7th Edoardo Amaldi Conference on Gravitational Waves CY JUL, 2007 CL Sydney, AUSTRALIA ID INSPIRALLING COMPACT BINARIES; GRAVITATIONAL WAVE-FORMS; NUMERICAL RELATIVITY; ORDER AB We present a preliminary study of the multipolar structure of gravitational radiation from spinning black hole binary mergers. We consider three different spinning binary configurations: (1) one 'hang-up' run, where the black holes have equal masses and large spins initially aligned with the orbital angular momentum; (2) seven 'spin-flip' runs, where the holes have a mass ratio q = M-1/M-2 = 4, the spins are anti-aligned with the orbital angular momentum, and the initial Kerr parameters of the holes j(1) = j(2) = j(i) (where j = J/M-2) are fine-tuned to produce a Schwarzschild remnant after merger; (3) three 'superkick' runs where the mass ratio q = 1, 2, 4 and the spins of the two holes are initially located on the orbital plane, pointing in opposite directions. For all of these simulations we compute the multipolar energy distribution and the Kerr parameter of the final hole. For the hang-up run, we show that including leading-order spin-orbit and spin-spin terms in a multipolar decomposition of the post-Newtonian waveforms improves agreement with the numerical simulation. C1 [Berti, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Berti, E.] Washington Univ, Dept Phys, McDonnell Ctr Space Sci, St Louis, MO 63130 USA. [Cardoso, V.] Univ Mississippi, Dept Phys & Astron, University, MS 38677 USA. [Cardoso, V.] Inst Super Tecn, Ctr Multidisciplinar Astrofis CENTRA, Dept Fis, P-1049001 Lisbon, Portugal. [Gonzalez, J. A.; Sperhake, U.; Bruegmann, B.] Univ Jena, Inst Theoret Phys, D-07743 Jena, Germany. [Gonzalez, J. A.] Univ Michoacana, Inst Fis & Matemat, Morelia 58040, Michoacan, Mexico. RP Berti, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM berti@wugrav.wustl.edu RI Berti, Emanuele/C-9331-2016; Cardoso, Vitor/K-1877-2015 OI Berti, Emanuele/0000-0003-0751-5130; Cardoso, Vitor/0000-0003-0553-0433 NR 37 TC 38 Z9 38 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD JUN 7 PY 2008 VL 25 IS 11 AR 114035 DI 10.1088/0264-9381/25/11/114035 PG 9 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 301LH UT WOS:000255897200036 ER PT J AU Everitt, CWF Adams, M Bencze, W Buchman, S Clarke, B Conklin, J Debra, DB Dolphin, M Heifetz, M Hipkins, D Holmes, T Keiser, GM Kolodziejczak, J Li, J Lockhart, JM Muhlfelder, B Parkinson, BW Salomon, M Silbergleit, A Solomonik, V Stahl, K Turneaure, JP Worden, PW AF Everitt, C. W. F. Adams, M. Bencze, W. Buchman, S. Clarke, B. Conklin, J. Debra, D. B. Dolphin, M. Heifetz, M. Hipkins, D. Holmes, T. Keiser, G. M. Kolodziejczak, J. Li, J. Lockhart, J. M. Muhlfelder, B. Parkinson, B. W. Salomon, M. Silbergleit, A. Solomonik, V. Stahl, K. Turneaure, J. P. Worden, P. W., Jr. TI Gravity Probe B data analysis status and potential for improved accuracy of scientific results SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article; Proceedings Paper CT 18th International Conference on General Relativity and Gravitation/7th Edoardo Amaldi Conference on Gravitational Waves CY JUL, 2007 CL Sydney, AUSTRALIA AB Gravity Probe B (GP-B) is a landmark physics experiment in space designed to yield precise tests of two fundamental predictions of Einstein's theory of general relativity, the geodetic and frame-dragging effects, by means of cryogenic gyroscopes in Earth orbit. Launched on 20 April 2004, data collection began on 28 August 2004 and science operations were completed on 29 September 2005 upon liquid helium depletion. During the course of the experiment, two unexpected and mutually-reinforcing complications were discovered: (1) larger than expected 'misalignment' torques on the gyroscopes producing classical drifts larger than the relativity effects under study and (2) a damped polhode oscillation that complicated the calibration of the instrument's scale factor against the aberration of starlight. Steady progress through 2006 and 2007 established the methods for treating both problems; in particular, an extended effort from January 2007 on 'trapped flux mapping' led in August 2007 to a dramatic breakthrough, resulting in a factor of similar to 20 reduction in data scatter. This paper reports results up to November 2007. Detailed investigation of a central 85-day segment of the data has yielded robust measurements of both relativity effects. Expansion to the complete science data set, along with anticipated improvements in modeling and in the treatment of systematic errors may be expected to yield a 3-6% determination of the frame-dragging effect. C1 [Everitt, C. W. F.; Adams, M.; Bencze, W.; Buchman, S.; Clarke, B.; Conklin, J.; Debra, D. B.; Dolphin, M.; Heifetz, M.; Hipkins, D.; Holmes, T.; Keiser, G. M.; Li, J.; Lockhart, J. M.; Muhlfelder, B.; Parkinson, B. W.; Salomon, M.; Silbergleit, A.; Solomonik, V.; Stahl, K.; Turneaure, J. P.; Worden, P. W., Jr.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Kolodziejczak, J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Everitt, CWF (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. NR 0 TC 7 Z9 7 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD JUN 7 PY 2008 VL 25 IS 11 AR 114002 DI 10.1088/0264-9381/25/11/114002 PG 11 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 301LH UT WOS:000255897200003 ER PT J AU Searle, AC Sutton, PJ Tinto, M Woan, G AF Searle, Antony C. Sutton, Patrick J. Tinto, Massimo Woan, Graham TI Robust Bayesian detection of unmodelled bursts SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article; Proceedings Paper CT 18th International Conference on General Relativity and Gravitation/7th Edoardo Amaldi Conference on Gravitational Waves CY JUL, 2007 CL Sydney, AUSTRALIA ID GRAVITATIONAL-WAVE BURSTS; INVERSE PROBLEM AB We develop a Bayesian treatment of the problem of detecting unmodelled gravitational wave bursts using the new global network of interferometric detectors. We also compare this Bayesian treatment with existing coherent methods, and demonstrate that the existing methods make implicit assumptions on the distribution of signals that make them sub-optimal for realistic signal populations. C1 [Searle, Antony C.] Australian Natl Univ, Ctr Gravitat Phys, Dept Phys, Fac Sci, Canberra, ACT 0200, Australia. [Sutton, Patrick J.] CALTECH, LIGO, Pasadena, CA 91125 USA. [Sutton, Patrick J.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, Wales. [Tinto, Massimo] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Woan, Graham] Univ Glasgow, Dept Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland. RP Searle, AC (reprint author), Australian Natl Univ, Ctr Gravitat Phys, Dept Phys, Fac Sci, GPO Box 4, Canberra, ACT 0200, Australia. EM antony.searle@anu.edu.au; psutton@ligo.caltech.edu; mtinto@mail1.jpl.nasa.gov; graham@astro.gla.ac.uk NR 8 TC 21 Z9 21 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD JUN 7 PY 2008 VL 25 IS 11 AR 114038 DI 10.1088/0264-9381/25/11/114038 PG 9 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 301LH UT WOS:000255897200039 ER PT J AU Shaddock, DA AF Shaddock, D. A. TI Space-based gravitational wave detection with LISA SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article; Proceedings Paper CT 18th International Conference on General Relativity and Gravitation/7th Edoardo Amaldi Conference on Gravitational Waves CY JUL, 2007 CL Sydney, AUSTRALIA ID LASER FREQUENCY STABILIZATION; TIME-DELAY INTERFEROMETRY; LOCKING; PHASE; ARM; PATHFINDER; TRACKING AB The laser interferometer space antenna will be the first space-based laser interferometric gravitational wave detector. This paper provides a brief introduction to the LISA mission and science goals, highlighting the differences from ground-based detectors. A tutorial of the LISA measurement concept is presented focusing on the LISA interferometry with a summary of laser frequency noise cancellation and clock noise removal schemes. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Shaddock, DA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM Daniel.Shaddock@jpl.nasa.gov RI Shaddock, Daniel/A-7534-2011 OI Shaddock, Daniel/0000-0002-6885-3494 NR 43 TC 19 Z9 19 U1 2 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD JUN 7 PY 2008 VL 25 IS 11 AR 114012 DI 10.1088/0264-9381/25/11/114012 PG 11 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 301LH UT WOS:000255897200013 ER PT J AU Stebbins, RT AF Stebbins, R. T. TI Recent progress at NASA in LISA formulation and technology development SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article; Proceedings Paper CT 18th International Conference on General Relativity and Gravitation/7th Edoardo Amaldi Conference on Gravitational Waves CY JUL, 2007 CL Sydney, AUSTRALIA AB Over the last year, the NASA half of the joint LISA project has focused its efforts on responding to a major review, and advancing the formulation and technology development of the mission. The NAS/NRC Beyond Einstein program assessment review will be described, including the outcome. The basis of the LISA science requirements has changed from detection determined by integrated signal-to-noise ratio to observation determined by uncertainty in the estimation of astrophysical source parameters. The NASA team has further defined the spacecraft bus design, participated in many design trade studies and advanced the requirements flow down and the associated current best estimates of performance. Recent progress in technology development is also summarized. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Stebbins, RT (reprint author), NASA, Goddard Space Flight Ctr, Code 663, Greenbelt, MD 20771 USA. EM Robin.T.Stebbins@nasa.gov RI Stebbins, Robin/G-5009-2013 NR 6 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD JUN 7 PY 2008 VL 25 IS 11 AR 114050 DI 10.1088/0264-9381/25/11/114050 PG 9 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 301LH UT WOS:000255897200051 ER PT J AU Leventis, N Sotiriou-Leventis, C Mulik, S Dass, A Schnobrich, J Hobbs, A Fabrizio, EF Luo, H Churu, G Zhang, Y Lu, H AF Leventis, N. Sotiriou-Leventis, C. Mulik, S. Dass, A. Schnobrich, J. Hobbs, A. Fabrizio, E. F. Luo, H. Churu, G. Zhang, Y. Lu, H. TI Polymer nanoencapsulated mesoporous vanadia with unusual ductility at cryogenic temperatures SO JOURNAL OF MATERIALS CHEMISTRY LA English DT Article ID AMINE-MODIFIED SILICA; CORE-SHELL SUPERSTRUCTURES; THIN-FILMS; MECHANICAL-PROPERTIES; BRITTLE TRANSITION; FRACTURE-BEHAVIOR; AEROGEL MONOLITHS; OXIDE AEROGELS; V2O5; MODEL AB An aerogel-like composite material was synthesized by casting a conformal 4-6 nm diisocyanate-derived polymer coating on the bird-nest like skeletal framework of mesoporous vanadia consisting of entangled 100-200 nm long, 30-40 nm thick worm-like objects. The new material does not fail even under high strain compression (> 90%) and maintains a highly unusual ductility at cryogenic temperatures (-196 degrees C). By comparison, nanoparticulate silica crosslinked with the same polymer at the same bulk density (similar to 0.45 g cm(-1)) behaves as a typical polymer and metal, showing brittle behavior as the temperature decreases. The high strength of nanoencapsulated vanadia is attributed to interlocking of the skeletal nanoworms, and the high ductility at cryogenic temperatures to sintering-like melting and fusion of their polymer coating under compression. C1 [Leventis, N.; Sotiriou-Leventis, C.; Mulik, S.; Dass, A.] Univ Missouri Sci & Technol, Dept Chem, Rolla, MO 65409 USA. [Leventis, N.; Schnobrich, J.; Hobbs, A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Fabrizio, E. F.] Ohio Aerosp Inst, Cleveland, OH 44142 USA. [Luo, H.; Churu, G.; Zhang, Y.; Lu, H.] Oklahoma State Univ, Sch Mech & Aerosp Engn, Stillwater, OK 74078 USA. RP Leventis, N (reprint author), Univ Missouri Sci & Technol, Dept Chem, Rolla, MO 65409 USA. EM leventis@mst.edu; cslevent@mst.edu; hongbing.lu@okstate.edu RI Lu, Hongbing/A-1312-2011; Dass, Amal/A-2520-2011; Dass, Amala/H-4729-2012 OI Dass, Amala/0000-0001-6942-5451 NR 48 TC 26 Z9 26 U1 1 U2 13 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 0959-9428 J9 J MATER CHEM JI J. Mater. Chem. PD JUN 7 PY 2008 VL 18 IS 21 BP 2475 EP 2482 DI 10.1039/b801770k PG 8 WC Chemistry, Physical; Materials Science, Multidisciplinary SC Chemistry; Materials Science GA 308QK UT WOS:000256404900012 ER PT J AU Shindell, DT Levy, H Schwarzkopf, MD Horowitz, LW Lamarque, JF Faluvegi, G AF Shindell, Drew T. Levy, Hiram, II Schwarzkopf, M. Daniel Horowitz, Larry W. Lamarque, Jean-Francois Faluvegi, Greg TI Multimodel projections of climate change from short-lived emissions due to human activities SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID CHEMICAL-TRANSPORT MODEL; TROPOSPHERIC OZONE; GISS MODELE; AEROSOL; SIMULATIONS; METHANE; PREINDUSTRIAL; SENSITIVITY; FORMULATION; SATELLITE AB We use the GISS ( Goddard Institute for Space Studies), GFDL ( Geophysical Fluid Dynamics Laboratory) and NCAR ( National Center for Atmospheric Research) climate models to study the climate impact of the future evolution of short-lived radiatively active species ( ozone and aerosols). The models used mid-range A1B emission scenarios, independently calculated the resulting composition change, and then performed transient simulations to 2050 examining the response to projected changes in short-lived species and to changes in both long-lived and short-lived species together. By 2050, two models show that the global mean annual average warming due to long-lived GHGs ( greenhouse gases) is enhanced by 20-25% due to the radiatively active short-lived species. One model shows virtually no effect from short-lived species. Intermodel differences are largely related to differences in emissions projections for short-lived species, which are substantial even for a particular storyline. For aerosols, these uncertainties are usually dominant, though for sulfate uncertainties in aerosol physics are also substantial. For tropospheric ozone, uncertainties in physical processes are more important than uncertainties in precursor emissions. Differences in future atmospheric burdens and radiative forcing for aerosols are dominated by divergent assumptions about emissions from South and East Asia. In all three models, the spatial distribution of radiative forcing is less important than that of climate sensitivity in predicting climate impact. Both short-lived and long-lived species appear to cause enhanced climate responses in the same regions of high sensitivity rather than short-lived species having an enhanced effect primarily near polluted areas. Since short-lived species can significantly influence climate, regional air quality emission control strategies for short-lived pollutants may substantially impact climate over large ( e. g., hemispheric) scales. C1 [Shindell, Drew T.; Faluvegi, Greg] Columbia Univ, NASA, Goddard Inst Space Studies, Ctr Climate Syst Res, New York, NY 10025 USA. [Levy, Hiram, II; Schwarzkopf, M. Daniel; Horowitz, Larry W.] Princeton Univ, NOAA, Geophys Fluid Dynam Lab, Princeton, NJ 08542 USA. [Lamarque, Jean-Francois] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA. RP Shindell, DT (reprint author), Columbia Univ, NASA, Goddard Inst Space Studies, Ctr Climate Syst Res, 2880 Broadway, New York, NY 10025 USA. EM dshindell@giss.nasa.gov RI Shindell, Drew/D-4636-2012; Horowitz, Larry/D-8048-2014; Lamarque, Jean-Francois/L-2313-2014 OI Horowitz, Larry/0000-0002-5886-3314; Lamarque, Jean-Francois/0000-0002-4225-5074 NR 48 TC 52 Z9 53 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 6 PY 2008 VL 113 IS D11 AR D11109 DI 10.1029/2007JD009152 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 310WH UT WOS:000256561000001 ER PT J AU Champion, DJ Ransom, SM Lazarus, P Camilo, F Bassa, C Kaspi, VM Nice, DJ Freire, PCC Stairs, IH van Leeuwen, J Stappers, BW Cordes, JM Hessels, JWT Lorimer, DR Arzoumanian, Z Backer, DC Bhat, NDR Chatterjee, S Cognard, I Deneva, JS Faucher-Giguere, CA Gaensler, BM Han, JL Jenet, FA Kasian, L Kondratiev, VI Kramer, M Lazio, J McLaughlin, MA Venkataraman, A Vlemmings, W AF Champion, David J. Ransom, Scott M. Lazarus, Patrick Camilo, Fernando Bassa, Cees Kaspi, Victoria M. Nice, David J. Freire, Paulo C. C. Stairs, Ingrid H. van Leeuwen, Joeri Stappers, Ben W. Cordes, James M. Hessels, Jason W. T. Lorimer, Duncan R. Arzoumanian, Zaven Backer, Don C. Bhat, N. D. Ramesh Chatterjee, Shami Cognard, Ismael Deneva, Julia S. Faucher-Giguere, Claude-Andre Gaensler, Bryan M. Han, JinLin Jenet, Fredrick A. Kasian, Laura Kondratiev, Vlad I. Kramer, Michael Lazio, Joseph McLaughlin, Maura A. Venkataraman, Arun Vlemmings, Wouter TI An eccentric binary millisecond pulsar in the galactic plane SO SCIENCE LA English DT Article ID RADIO PULSARS; NEUTRON-STAR; EVOLUTION; SYSTEMS; 2MASS; MASS AB Binary pulsar systems are superb probes of stellar and binary evolution and the physics of extreme environments. In a survey with the Arecibo telescope, we have found PSR J1903+ 0327, a radio pulsar with a rotational period of 2.15 milliseconds in a highly eccentric ( e = 0.44) 95- day orbit around a solar mass ( M.) companion. Infrared observations identify a possible main- sequence companion star. Conventional binary stellar evolution models predict neither large orbital eccentricities nor main- sequence companions around millisecond pulsars. Alternative formation scenarios involve recycling a neutron star in a globular cluster, then ejecting it into the Galactic disk, or membership in a hierarchical triple system. A relativistic analysis of timing observations of the pulsar finds its mass to be 1.74 +/- 0.04 M. an unusually high value. C1 [Champion, David J.; Lazarus, Patrick; Bassa, Cees; Kaspi, Victoria M.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Champion, David J.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Ransom, Scott M.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Camilo, Fernando] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Nice, David J.] Bryn Mawr Coll, Dept Phys, Bryn Mawr, PA 19010 USA. [Freire, Paulo C. C.; Venkataraman, Arun] Natl Astron & Ionosphere Ctr, Arecibo Observ, Arecibo, PR 00612 USA. [Stairs, Ingrid H.; Kasian, Laura] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [van Leeuwen, Joeri; Backer, Don C.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Stappers, Ben W.; Kramer, Michael] Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. [Cordes, James M.; Deneva, Julia S.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Hessels, Jason W. T.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Lorimer, Duncan R.; Kondratiev, Vlad I.; McLaughlin, Maura A.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. [Arzoumanian, Zaven] NASA, Ctr Res & Explorat Space Sci & Technol, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Arzoumanian, Zaven] NASA, Xray Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bhat, N. D. Ramesh] Swinburne Univ Technol, Hawthorn, Vic 3122, Australia. [Chatterjee, Shami; Gaensler, Bryan M.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. [Cognard, Ismael] CNRS, Lab Phys & Chim Environm, UMR 6115, F-45071 Orleans 2, France. [Faucher-Giguere, Claude-Andre] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Han, JinLin] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Jenet, Fredrick A.] Univ Texas Brownsville, Ctr Gravitat Wave Astron, Brownsville, TX 78520 USA. [Lazio, Joseph] USN, Res Lab, Washington, DC 20375 USA. [Vlemmings, Wouter] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. RP Champion, DJ (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada. EM David.Champion@atnf.csiro.au RI Gaensler, Bryan/F-8655-2010; Bhat, Ramesh/B-7396-2013; Kondratiev, Vladislav/N-1105-2015; OI Kondratiev, Vladislav/0000-0001-8864-7471; Champion, David/0000-0003-1361-7723; Nice, David/0000-0002-6709-2566; Ransom, Scott/0000-0001-5799-9714; /0000-0002-2700-9916; Gaensler, Bryan/0000-0002-3382-9558 NR 27 TC 110 Z9 110 U1 0 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 JUN 6 PY 2008 VL 320 IS 5881 BP 1309 EP 1312 DI 10.1126/science.1157580 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 309DO UT WOS:000256441100036 PM 18483399 ER PT J AU Fuselier, SA Claflin, ES Moore, TE AF Fuselier, S. A. Claflin, E. S. Moore, T. E. TI Magnetic local time extent of ion outflow during substorm recovery SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ENERGIZATION MECHANISMS; CONIC DISTRIBUTIONS; AURORAL REGION; HIGH-LATITUDE; IMAGE-FUV; FIELD; CUSP; IONOSPHERE AB Ions from the Earth's ionosphere are an important component of the coupled magnetosphere-ionosphere system. These ions are accelerated out of the ionosphere in the auroral zone. As they gain altitude, a fraction of them are charge exchanged, producing energetic neutrals. These neutrals (in the energy range from similar to 10 to similar to 300 eV) are imaged by the Low Energy Neutral Atom (LENA) imager on the Imager for Magnetopause to Aurora Global Exploration spacecraft. From these images, the instantaneous local time extent of the ion outflow is determined. These data show that, during times of substorm recovery, the local time extent of the outflow is large and variable, typically centered on the dayside, but often extending over nearly the entire auroral oval. The local time extent appears to encompass the ionospheric footprint of the cusp. C1 [Fuselier, S. A.; Claflin, E. S.] Lockheed Martin Adv Technol Ctr, Space Phys Lab, Dept ADCS, Palo Alto, CA 94304 USA. [Moore, T. E.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. RP Fuselier, SA (reprint author), Lockheed Martin Adv Technol Ctr, Space Phys Lab, Dept ADCS, Bldg 255,3251 Hanover St, Palo Alto, CA 94304 USA. EM fuselier@spasci.com; thomas.e.moore@gsfc.nasa.gov RI Moore, Thomas/D-4675-2012 OI Moore, Thomas/0000-0002-3150-1137 NR 25 TC 3 Z9 3 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 JUN 5 PY 2008 VL 113 IS A6 AR A06204 DI 10.1029/2007JA012811 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 310YV UT WOS:000256567900003 ER PT J AU Purewal, J Hwang, SJ Bowman, RC Ronnebro, E Fultz, B Ahn, C AF Purewal, Justin Hwang, Son-Jong Bowman, Robert C. Ronnebro, Ewa Fultz, Brent Ahn, Channing TI Hydrogen sorption behavior of the ScH(2)-LiBH(4) system: Experimental assesment of chemical destabilization effects SO JOURNAL OF PHYSICAL CHEMISTRY C LA English DT Article ID STORAGE PROPERTIES; METAL-HYDRIDES; LIBH4; MGH2 AB The hydrogen storage reaction ScH(2) + 2LiBH(4) -> ScB(2) + 2LiH + 4H(2) (8-91 wt %), based on the thermodynamic destabilization of LiBH(4), is predicted to have a reaction enthalpy of Delta H(300K) = 34.1 kJ/mol H(2). The isothermal kinetic desorption behavior in this system was measured. At temperatures up to 450 degrees C, less than 5 wt % H(2) is released, which is only half of the theoretical capacity. Powder X-ray diffraction data indicate that LiBH(4) has decomposed into LiH in the final desorption product, but the data provide no evidence that ScH(2) has participated in the reaction. Magic angle spinning NMR (MAS NMR) results do not show that the expected ScB2 equilibrium product phase has formed during desorption. While the addition of 2 mol % TiCl(3) catalyst does improve desorption kinetics at 280 degrees C, it does not otherwise assist the destabilization reaction. The calculated reaction enthalpy suggests that this system should be of interest at moderate temperatures, but the large heats of formation of the reactant phases in this system appear to play a critical role in determining overall kinetics. Furthermore, the formation of a Li(2)B(12)H(12) intermediate phase was determined by MAS NMR, which is an undesirable stable product if reaction reversibility is to be accomplished. C1 [Purewal, Justin; Fultz, Brent; Ahn, Channing] CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA. [Hwang, Son-Jong] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA. [Ronnebro, Ewa] Sandia Natl Labs, Energy Syst Dept, Livermore, CA 94551 USA. [Bowman, Robert C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Purewal, J (reprint author), CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA. EM purewal@caltech.edu OI Bowman, Robert/0000-0002-2114-1713 NR 21 TC 55 Z9 56 U1 1 U2 11 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1932-7447 J9 J PHYS CHEM C JI J. Phys. Chem. C PD JUN 5 PY 2008 VL 112 IS 22 BP 8481 EP 8485 DI 10.1021/jp800486n PG 5 WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Chemistry; Science & Technology - Other Topics; Materials Science GA 306RI UT WOS:000256265100059 ER PT J AU Park, C Kang, JH Harrison, JS Costen, RC Lowther, SE AF Park, Cheol Kang, Jin Ho Harrison, Joycelyn S. Costen, Robert C. Lowther, Sharon E. TI Actuating single wall carbon nanotube-polymer composites: Intrinsic unimorphs SO ADVANCED MATERIALS LA English DT Article ID ELECTROSTRICTIVE RESPONSE; POLYURETHANES; DISPERSION; FILMS AB A novel actuating single wall carbon nanotube (SWNT)/polymer composite is reported. It exhibits a large strain (2.6%) at a low driving voltage (<1 MV m(-1)) while possessing excellent mechanical and thermal properties. The strain energy density is at least an order of magnitude greater than any state-of-the-art polymeric materials eported. The actuating characteristic rmainly originates from the electrostrictive contribution, presumably due to interfacial polarization. C1 [Park, Cheol; Kang, Jin Ho] Natl Inst Aerosp, Hampton, VA 23681 USA. [Harrison, Joycelyn S.; Costen, Robert C.; Lowther, Sharon E.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA. RP Park, C (reprint author), Natl Inst Aerosp, MS-226, Hampton, VA 23681 USA. EM cheol.park-1@nasa.gov NR 27 TC 43 Z9 43 U1 5 U2 21 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0935-9648 EI 1521-4095 J9 ADV MATER JI Adv. Mater. PD JUN 4 PY 2008 VL 20 IS 11 BP 2074 EP + DI 10.1002/adma.200702566 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 317UC UT WOS:000257044600008 ER PT J AU Han, SC Rowlands, DD Luthcke, SB Lemoine, FG AF Han, Shin-Chan Rowlands, David D. Luthcke, Scott B. Lemoine, Frank G. TI Localized analysis of satellite tracking data for studying time-variable Earth's gravity fields SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID GRAVITATIONAL-FIELD; GRACE; VARIABILITY; MODEL; TIDES AB We present a method to analyze the observations of relative distance change between two low Earth orbiting satellites of the Gravity Recovery And Climate Experiment (GRACE) mission after removing the effects caused by the mean gravity field and better-known temporal mass redistribution. The gravitational acceleration exerted by the block mean mass within a region on the Earth surface is formulated by point mass approximation and by spherical harmonic expansion. In addition to the regional mass parameters, the arc-dependent parameters (initial relative state vectors) is simultaneously modeled to remove the signals not associated with the mass variation within the focus area. While a certain level of approximation, that is committed when locally formulating the gravitational acceleration vector for numerical integration, causes model error, we benefit from regionally estimating time-variable mass with improved spatial and temporal resolutions. In addition, various temporal parameterizations depending on geographical areas and expected signals can be applied for the regional analysis in a straightforward manner and it helps to retrieve even sub-daily time-variable signals such as tides from many years of GRACE data. We present the results of hydrology and ocean tide recovery in South America, Africa, North America, and Antarctica from the analysis of 3.5 years of GRACE tracking data and compare them with the traditional global harmonic approach. The algorithm development thoroughly described here will be helpful for the science community to exploit fundamental data (range rate) of the GRACE mission in addition to monthly gravity products. C1 [Han, Shin-Chan; Rowlands, David D.; Luthcke, Scott B.; Lemoine, Frank G.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Han, Shin-Chan] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. RP Han, SC (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Code 698,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM schan@puuoo.gsfc.nasa.gov RI Rowlands, David/D-2751-2012; Luthcke, Scott/D-6283-2012; Lemoine, Frank/D-1215-2013; Han, Shin-Chan/A-2022-2009 NR 36 TC 17 Z9 18 U1 0 U2 3 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 JUN 4 PY 2008 VL 113 IS B6 AR B06401 DI 10.1029/2007JB005218 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 310YG UT WOS:000256566300001 ER PT J AU Jalbout, AF Trzaskowski, B Xia, Y Li, Y Hu, X Li, H El-Nahas, A Adamowicz, L AF Jalbout, Abraham F. Trzaskowski, B. Xia, Y. Li, Y. Hu, X. Li, H. El-Nahas, A. Adamowicz, Ludwik TI Structures, stabilities and tautomerizations of uracil and diphosphouracil tautomers (vol 332, pg 152, 2007) SO CHEMICAL PHYSICS LA English DT Correction C1 [Jalbout, Abraham F.] Univ Nacl Autonoma Mexico, Inst Chem, Mexico City 04510, DF, Mexico. [Trzaskowski, B.; Xia, Y.; Li, Y.; Hu, X.; Li, H.; Adamowicz, Ludwik] Univ Arizona, Dept Chem, NASA, Astrobiol Inst, Tucson, AZ 85721 USA. [El-Nahas, A.] Menoufia Univ, Dept Chem, Fac Sci, Shibin Al Kawm, Egypt. RP Jalbout, AF (reprint author), Univ Nacl Autonoma Mexico, Inst Chem, Mexico City 04510, DF, Mexico. EM amelnahas@hotmail.com RI Trzaskowski, Bartosz/B-1881-2008 OI Trzaskowski, Bartosz/0000-0003-2385-1476 NR 1 TC 0 Z9 0 U1 0 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0301-0104 J9 CHEM PHYS JI Chem. Phys. PD JUN 2 PY 2008 VL 348 IS 1-3 BP 254 EP 254 DI 10.1016/j.chemphys.2008.02.012 PG 1 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 313JP UT WOS:000256737200034 ER PT J AU Sietzen, F Gilbrech, R AF Sietzen, Frank Gilbrech, Richard TI With Richard Gilbrech SO AEROSPACE AMERICA LA English DT Editorial Material C1 [Gilbrech, Richard] NASA, ESMD, Washington, DC USA. [Gilbrech, Richard] NASA Stennis, Stennis Space Ctr, MS USA. [Gilbrech, Richard] NASA Langley, Hampton, VA USA. RP Sietzen, F (reprint author), NASA, ESMD, Washington, DC 20546 USA. NR 0 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 0740-722X J9 AEROSPACE AM JI Aerosp. Am. PD JUN PY 2008 VL 46 IS 6 BP 12 EP 13 PG 2 WC Engineering, Aerospace SC Engineering GA 309LG UT WOS:000256461300005 ER PT J AU Lohn, JD Hornby, GS Linden, DS AF Lohn, Jason D. Hornby, Gregory S. Linden, Derek S. TI Human-competitive evolved antennas SO AI EDAM-ARTIFICIAL INTELLIGENCE FOR ENGINEERING DESIGN ANALYSIS AND MANUFACTURING LA English DT Article DE antenna; computational design; design; evolutionary computation; genetic programming; spacecraft; wire antenna ID GENETIC ALGORITHMS; DESIGN AB We present a case study,showing a human-competitive design of an evolved antenna that was deployed on a NASA spacecraft in 2006. We were fortunate to develop our antennas in parallel with another group using traditional design methodologies. This allowed us to demonstrate that our techniques were human-competitive because our automatically designed antenna could be directly compared to a human-designed antenna. The antennas described below were evolved to meet a challenging set of mission requirements, most notably the combination of wide beamwidth for a circularly polarized wave and wide bandwidth. Two evolutionary algorithms were used in the development process: one used a genetic algorithm style representation that did not allow branching in the antenna arms; the second used a genetic programming style tree-structured representation that allowed branching in the antenna arms. The highest performance antennas from both algorithms were fabricated and tested, and both yielded very similar performance. Both antennas were comparable in performance to a hand-designed antenna produced by the antenna contractor for the mission, and so we consider them examples of human-competitive performance by evolutionary algorithms. Our design was approved for flight, and three copies of it were successfully flown on NASA's Space Technology 5 mission between March 22 and June 30, 2006. These evolved antennas represent the first evolved hardware in space and the first evolved antennas to be deployed. C1 [Lohn, Jason D.] Carnegie Mellon Univ, Computat Sci Div, NASA Ames Res Ctr, Moffett Field, CA 94035 USA. [Hornby, Gregory S.] Univ Calif Santa Cruz, NASA Ames Res Ctr, Santa Cruz, CA 95064 USA. [Linden, Derek S.] JEM Engn, Laurel, MD USA. RP Lohn, JD (reprint author), Carnegie Mellon Univ, Computat Sci Div, NASA Ames Res Ctr, MS 269-1, Moffett Field, CA 94035 USA. EM jlohn@email.arc.nasa.gov NR 15 TC 10 Z9 10 U1 0 U2 2 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0890-0604 J9 AI EDAM JI AI EDAM-Artif. Intell. Eng. Des. Anal. Manuf. PD SUM PY 2008 VL 22 IS 3 BP 235 EP 247 DI 10.1017/S0890060408000164 PG 13 WC Computer Science, Artificial Intelligence; Computer Science, Interdisciplinary Applications; Engineering, Multidisciplinary; Engineering, Manufacturing SC Computer Science; Engineering GA 318NM UT WOS:000257098700006 ER PT J AU Schoppers, M AF Schoppers, Marcel TI Moving Walls SO AI MAGAZINE LA English DT Editorial Material C1 NASA, Jet Prop Lab, Sect 316, Pasadena, CA USA. RP Schoppers, M (reprint author), NASA, Jet Prop Lab, Sect 316, Pasadena, CA USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC ARTIFICIAL INTELL PI MENLO PK PA 445 BURGESS DRIVE, MENLO PK, CA 94025-3496 USA SN 0738-4602 J9 AI MAG JI AI Mag. PD SUM PY 2008 VL 29 IS 2 BP 28 EP 28 PG 1 WC Computer Science, Artificial Intelligence SC Computer Science GA 364XF UT WOS:000260368200006 ER PT J AU Crawford, J AF Crawford, James TI Lessons Learned Delivering Optimized Supply-Chain Planning to the Business World SO AI MAGAZINE LA English DT Article AB The late 1990s saw a huge upswing in the demand for supply-chain management software. The rapid commercial adoption of these tools brought into sharp relief the complexity of automating supply-chain planning and optimization. This article summarizes four years of real-world experience in combining AI and operations research (OR) techniques, balancing representational power against planning complexity, and understanding the practical implications of nondeterministic polynomial time (NP)-completeness. C1 [Crawford, James] NASA, Ames Res Ctr, Washington, DC USA. [Crawford, James] Univ Oregon, CIRL, Eugene, OR 97403 USA. NR 5 TC 1 Z9 1 U1 0 U2 0 PU AMER ASSOC ARTIFICIAL INTELL PI MENLO PK PA 445 BURGESS DRIVE, MENLO PK, CA 94025-3496 USA SN 0738-4602 J9 AI MAG JI AI Mag. PD SUM PY 2008 VL 29 IS 2 BP 51 EP 56 PG 6 WC Computer Science, Artificial Intelligence SC Computer Science GA 364XF UT WOS:000260368200012 ER PT J AU Isaac, KM Rolwes, J Colozza, A AF Isaac, K. M. Rolwes, Jessica Colozza, Anthony TI Aerodynamics of a flapping and pitching wing using Simulations and experiments SO AIAA JOURNAL LA English DT Article; Proceedings Paper CT AIAA 44th Aerospace Sciences Meeting and Exhibit CY JAN 09-12, 2006 CL Reno, NV SP AIAA ID INSECT FLIGHT; HEAVING AIRFOIL; FLOW; EFFICIENCY; VEHICLES; MODEL AB Computational fluid dynamics simulation results for a thin cambered plate airfoil, and How visualization and force measurements from experiments conducted in water on a flapping-and-pitching thin flat-plate wing of semi-elliptic planform at low Reynolds numbers are reported. Time-varying force data, measured using a force transducer, provide a means to understand the mechanisms that lead to enhanced performance observed in insect flight compared with fixed-wing aerodynamics. Experimental uncertainties associated with low-level (similar to 1 N) fluid dynamic force measurements on flapping-and-pitching wings, including inertia effects, are addressed. A previously proposed pitching mode in which the leading-edge and trailing-edge switch roles to allow using cambered airfoils is shown to be feasible. A vortex-trapping model is proposed to explain the aerodynamic advantages of switching. The present results also support the authors' proposed idea that an optimum reduced flapping frequency might exist. The study has applications in micro air vehicle development. C1 [Isaac, K. M.; Rolwes, Jessica] Missouri Univ Sci & Technol, Rolla, MO 65409 USA. [Colozza, Anthony] NASA, John H Glenn Res Ctr, Lewis Field, Cleveland, OH 44135 USA. RP Isaac, KM (reprint author), Missouri Univ Sci & Technol, 1870 Miner Circle, Rolla, MO 65409 USA. NR 33 TC 7 Z9 7 U1 0 U2 12 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD JUN PY 2008 VL 46 IS 6 BP 1505 EP 1515 DI 10.2514/1.32846 PG 11 WC Engineering, Aerospace SC Engineering GA 315SR UT WOS:000256900500020 ER PT J AU Kwon, O Tranter, M Jones, WK Sankovic, JM Banerjee, RK AF Kwon, Ohwon Tranter, Michael Jones, W. Keith Sankovic, John M. Banerjee, Rupak K. TI Enhanced nuclear translocation of nuclear factor-kappa B in micro-G stimulated cardiomyocyte cells SO ARTERIOSCLEROSIS THROMBOSIS AND VASCULAR BIOLOGY LA English DT Meeting Abstract CT 9th Annual Conference on Arteriosclerosis, Thrombosis and Vascular Biology CY APR 16-18, 2008 CL Atlanta, GA C1 [Kwon, Ohwon; Tranter, Michael; Jones, W. Keith; Banerjee, Rupak K.] Univ Cincinnati, Cincinnati, OH USA. [Sankovic, John M.] NASA, Glenn Rsch Cntr, Cleveland, OH USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU LIPPINCOTT WILLIAMS & WILKINS PI PHILADELPHIA PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA SN 1079-5642 J9 ARTERIOSCL THROM VAS JI Arterioscler. Thromb. Vasc. Biol. PD JUN PY 2008 VL 28 IS 6 MA P414 BP E108 EP E109 PG 2 WC Hematology; Peripheral Vascular Disease SC Hematology; Cardiovascular System & Cardiology GA 303PS UT WOS:000256053400420 ER PT J AU Marais, DJD Borg, LE Beaty, DW AF Marais, David J. Des Borg, Lars E. Beaty, David W. TI Science priorities for Mars Sample Return SO ASTROBIOLOGY LA English DT Editorial Material ID MARTIAN METEORITE ALH84001; MERIDIANI-PLANUM; GUSEV CRATER; DIFFERENTIATION HISTORY; ISOTOPIC COMPOSITION; IONIZING-RADIATION; AQUEOUS ALTERATION; SPECTRAL EVIDENCE; SNC METEORITES; MINERALOGY C1 [Marais, David J. Des] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Borg, Lars E.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Beaty, David W.] Jet Prop Lab, Pasadena, CA 91109 USA. RP Marais, DJD (reprint author), NASA, Ames Res Ctr, Mail Stop 239-4, Moffett Field, CA 94035 USA. EM David.J.DesMarais@nasa.gov; borg5@llnl.gov; David.Beaty@jpl.nasa.gov RI Eigenbrode, Jennifer/D-4651-2012; OI Grady, Monica/0000-0002-4055-533X NR 172 TC 14 Z9 14 U1 2 U2 9 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD JUN PY 2008 VL 8 IS 3 BP 489 EP 535 PG 47 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 336SO UT WOS:000258385100001 ER PT J AU Horikawa, DD Kunieda, T Abe, W Watanabe, M Nakahara, Y Yukuhiro, F Sakashita, T Hamada, N Wada, S Funayama, T Katagiri, C Kobayashi, Y Higashi, S Okuda, T AF Horikawa, Daiki D. Kunieda, Takekazu Abe, Wataru Watanabe, Masahiko Nakahara, Yuichi Yukuhiro, Fumiko Sakashita, Tetsuya Hamada, Nobuyuki Wada, Seiichi Funayama, Tomoo Katagiri, Chihiro Kobayashi, Yasuhiko Higashi, Seigo Okuda, Takashi TI Establishment of a rearing system of the extremotolerant tardigrade Ramazzottius varieornatus: A new model animal for astrobiology SO ASTROBIOLOGY LA English DT Article DE tardigrades; Ramazzottius varieornatus; tolerance; anhydrobiosis; extremophiles; extreme environments ID MILNESIUM-TARDIGRADUM; RICHTERSIUS-CORONIFER; RADIATION TOLERANCE; BACILLUS-SUBTILIS; HEAVY-IONS; SURVIVAL; LIFE; PRESSURE; SPACE; WATER AB Studies on the ability of multicellular organisms to tolerate specific environmental extremes are relatively rare compared to those of unicellular microorganisms in extreme environments. Tardigrades are extremotolerant animals that can enter an ametabolic dry state called anhydrobiosis and have high tolerance to a variety of extreme environmental conditions, particularly while in anhydrobiosis. Although tardigrades have been expected to be a potential model animal for astrobiological studies due to their excellent anhydrobiotic and extremotolerant abilities, few studies of tolerance with cultured tardigrades have been reported, possibly due to the absence of a model species that can be easily maintained under rearing conditions. We report the successful rearing of the herbivorous tardigrade, Ramazzottius varieornatus, by supplying the green alga Chlorella vulgaris as food. The life span was 35 +/- 16.4 d, deposited eggs required 5.7 +/- 1.1 d to hatch, and animals began to deposit eggs 9 d after hatching. The reared individuals of this species had an anhydrobiotic capacity throughout their life cycle in egg, juvenile, and adult stages. Furthermore, the reared adults in an anhydrobiotic state were tolerant of temperatures of 90 degrees C and - 196 degrees C, and exposure to 99.8% acetonitrile or irradiation with 4000 Gy (4)He ions. Based on their life history traits and tolerance to extreme stresses, R. varieornatus may be a suitable model for astrobiological studies of multicellular organisms. C1 [Horikawa, Daiki D.; Higashi, Seigo] Hokkaido Univ, Grad Sch Environm Earth Sci, Sapporo, Hokkaido 060, Japan. [Horikawa, Daiki D.; Kunieda, Takekazu; Abe, Wataru] Univ Tokyo, Grad Sch Sci, Tokyo 113, Japan. [Horikawa, Daiki D.; Watanabe, Masahiko; Nakahara, Yuichi; Okuda, Takashi] Natl Inst Agrobiol Sci, Anhydrobiosis Res Unit, Tsukuba, Ibaraki, Japan. [Yukuhiro, Fumiko] Natl Inst Agrobiol Sci, Insect Microbe Res Unit, Tsukuba, Ibaraki, Japan. [Sakashita, Tetsuya; Hamada, Nobuyuki; Wada, Seiichi; Funayama, Tomoo; Kobayashi, Yasuhiko] Japan Atom Energy Agcy, Microbeam Radiat Biol Grp, Takasaki, Japan. [Hamada, Nobuyuki; Wada, Seiichi; Kobayashi, Yasuhiko] Gunma Univ, Grad Sch Med, Dept Quantum Biol, Maebashi, Gumma, Japan. [Katagiri, Chihiro] Hokkaido Univ, Inst Low Temp Sci, Sapporo, Hokkaido 060, Japan. RP Horikawa, DD (reprint author), NASA Ames Res Ctr, Mail Stop 239-20,Bldg N239,Rm 371, Moffett Field, CA 94035 USA. EM horikawa@biol.s.u-tokyo.ac.jp RI Kunieda, Takekazu/G-4946-2014 NR 32 TC 36 Z9 39 U1 9 U2 47 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD JUN PY 2008 VL 8 IS 3 BP 549 EP 556 DI 10.1089/ast.2007.0139 PG 8 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 336SO UT WOS:000258385100003 PM 18554084 ER PT J AU Coleman, M Grunthaner, F AF Coleman, Max Grunthaner, Frank TI Astrobiology special collection: Instruments for in situ exploration of planets - Introduction SO ASTROBIOLOGY LA English DT Editorial Material ID MARS C1 [Coleman, Max; Grunthaner, Frank] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Coleman, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Max.Coleman@jpl.nasa.gov; Frank.J.Grunthaner@jpl.nasa.gov NR 11 TC 6 Z9 6 U1 0 U2 6 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD JUN PY 2008 VL 8 IS 3 BP 569 EP 570 DI 10.1089/ast.2008.1625 PG 2 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 336SO UT WOS:000258385100005 PM 18680408 ER PT J AU ten Kate, IL Canham, JS Conrad, PG Errigo, T Katz, I Mahaffy, PR AF ten Kate, Inge L. Canham, John S. Conrad, Pamela G. Errigo, Therese Katz, Ira Mahaffy, Paul R. TI Mitigation of the impact of terrestrial contamination on organic measurements from the Mars Science Laboratory SO ASTROBIOLOGY LA English DT Article; Proceedings Paper CT Fall Meeting of the American-Geophysical-Union CY DEC, 2006 CL San Francisco, CA SP Amer Geophys Union DE Mars; organics; instrumentation; contamination; in situ measurements AB The objective of the 2009 Mars Science Laboratory (MSL), which is planned to follow the Mars Exploration Rovers and the Phoenix lander to the surface of Mars, is to explore and assess quantitatively a site on Mars as a potential habitat for present or past life. Specific goals include an assessment of the past or present biological potential of the target environment and a characterization of its geology and geochemistry. Included in the 10 investigations of the MSL rover is the Sample Analysis at Mars (SAM) instrument suite, which is designed to obtain trace organic measurements, measure water and other volatiles, and measure several light isotopes with experiment sequences designed for both atmospheric and solid-phase samples. SAM integrates a gas chromatograph, a mass spectrometer, and a tunable laser spectrometer supported by sample manipulation tools both within and external to the suite. The sub-part-per-billion sensitivity of the suite for trace species, particularly organic molecules, along with a mobile platform that will contain many kilograms of organic materials, presents a considerable challenge due to the potential for terrestrial contamination to mask the signal of martian organics. We describe the effort presently underway to understand and mitigate, wherever possible within the resource constraints of the mission, terrestrial contamination in MSL and SAM measurements. C1 [ten Kate, Inge L.; Errigo, Therese; Mahaffy, Paul R.] NASA Goddard Space Flight Ctr, Atmospher Expt Lab, Greenbelt, MD 20771 USA. [ten Kate, Inge L.] Goddard Earth Sci & Technol Ctr, Baltimore, MD USA. [Canham, John S.] ATK Space, Beltsville, MD USA. [Conrad, Pamela G.; Katz, Ira] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP ten Kate, IL (reprint author), NASA Goddard Space Flight Ctr, Atmospher Expt Lab, Code 699, Greenbelt, MD 20771 USA. EM inge.l.tenkate@nasa.gov RI Mahaffy, Paul/E-4609-2012 NR 28 TC 8 Z9 8 U1 0 U2 6 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD JUN PY 2008 VL 8 IS 3 BP 571 EP 582 DI 10.1089/ast.2007.0160 PG 12 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 336SO UT WOS:000258385100006 PM 18558810 ER PT J AU Aubrey, AD Chalmers, JH Bada, JL Grunthaner, FJ Amashukeli, X Willis, P Skelley, AM Mathies, RA Quinn, RC Zent, AP Ehrenfreund, P Amundson, R Glavin, DP Botta, O Barron, L Blaney, DL Clark, BC Coleman, M Hofmann, BA Josset, JL Rettberg, P Ride, S Robert, F Sephton, MA Yen, A AF Aubrey, Andrew D. Chalmers, John H. Bada, Jeffrey L. Grunthaner, Frank J. Amashukeli, Xenia Willis, Peter Skelley, Alison M. Mathies, Richard A. Quinn, Richard C. Zent, Aaron P. Ehrenfreund, Pascale Amundson, Ron Glavin, Daniel P. Botta, Oliver Barron, Laurence Blaney, Diana L. Clark, Benton C. Coleman, Max Hofmann, Beda A. Josset, Jean-Luc Rettberg, Petra Ride, Sally Robert, Francois Sephton, Mark A. Yen, Albert TI The Urey instrument: An advanced in situ organic and oxidant detector for Mars exploration SO ASTROBIOLOGY LA English DT Article; Proceedings Paper CT Fall Meeting of the American-Geophysical-Union CY DEC, 2006 CL San Francisco, CA SP Amer Geophys Union DE in situ measurement-Mars-extraterrestrial life; biosignatures; atacama desert ID POLYCYCLIC AROMATIC-HYDROCARBONS; AMINO-ACIDS; CAPILLARY-ELECTROPHORESIS; BIOMARKER DETECTION; WATER EXTRACTION; MARTIAN SOIL; LIFE; MOLECULES; PRESERVATION; SUBLIMATION AB The Urey organic and oxidant detector consists of a suite of instruments designed to search for several classes of organic molecules in the martian regolith and ascertain whether these compounds were produced by biotic or abiotic processes using chirality measurements. These experiments will also determine the chemical stability of organic molecules within the host regolith based on the presence and chemical reactivity of surface and atmospheric oxidants. Urey has been selected for the Pasteur payload on the European Space Agency's (ESA's) upcoming 2013 ExoMars rover mission. The diverse and effective capabilities of Urey make it an integral part of the payload and will help to achieve a large portion of the mission's primary scientific objective: "to search for signs of past and present life on Mars." This instrument is named in honor of Harold Urey for his seminal contributions to the fields of cosmochemistry and the origin of life. C1 [Aubrey, Andrew D.; Grunthaner, Frank J.; Amashukeli, Xenia; Willis, Peter; Blaney, Diana L.; Coleman, Max; Yen, Albert] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. [Chalmers, John H.; Bada, Jeffrey L.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Mathies, Richard A.; Amundson, Ron] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Quinn, Richard C.] SETI Inst, Mountain View, CA USA. [Zent, Aaron P.] NASA Ames Res Ctr, Moffett Field, CA USA. [Ehrenfreund, Pascale] Leiden Univ, Leiden Inst Chem, NL-2300 RA Leiden, Netherlands. [Glavin, Daniel P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Botta, Oliver] Int Space Sci Inst, Bern, Switzerland. [Barron, Laurence] Univ Glasgow, Glasgow G12 8QQ, Lanark, Scotland. [Clark, Benton C.] Lockheed Martin Space Syst Co, Denver, CO USA. [Hofmann, Beda A.] Nat Hist Museum, Bern, Switzerland. [Josset, Jean-Luc] SPACE X Explorat Inst, Neuchatel, Switzerland. [Rettberg, Petra] Inst Aerospace Med, Cologne, Germany. [Ride, Sally] Imaginary Lines, San Diego, CA USA. [Robert, Francois] Musee Natl Hist Nat, Paris, France. [Sephton, Mark A.] Univ London Imperial Coll Sci Technol & Med, London, England. RP Aubrey, AD (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr,MS 302-306, Pasadena, CA 91109 USA. EM Andrew.D.Aubrey@jpl.nasa.gov RI Glavin, Daniel/D-6194-2012; Amundson, Ronald /E-2654-2015; Willis, Peter/I-6621-2012; Rettberg, Petra/K-2378-2015; OI Glavin, Daniel/0000-0001-7779-7765; Rettberg, Petra/0000-0003-4439-2395; Sephton, Mark/0000-0002-2190-5402 NR 57 TC 24 Z9 25 U1 4 U2 33 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD JUN PY 2008 VL 8 IS 3 BP 583 EP 595 DI 10.1089/ast.2007.0169 PG 13 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 336SO UT WOS:000258385100007 PM 18680409 ER PT J AU Amashukeli, X Grunthaner, FJ Patrick, SB Yung, PT AF Amashukeli, Xenia Grunthaner, Frank J. Patrick, Steven B. Yung, Pun To TI Subcritical water extractor for Mars analog soil analysis SO ASTROBIOLOGY LA English DT Article; Proceedings Paper CT Fall Meeting of the American-Geophysical-Union CY DEC, 2006 CL San Francisco, CA SP Amer Geophys Union DE planetary science; instruments and techniques; in situ instrument; astrobiology and extraterrestrial materials; Mars; subcritical water extraction; Atacama Desert ID VIKING BIOLOGY EXPERIMENTS; ATACAMA DESERT; LIFE AB Technologies that enable rapid and efficient extraction of biomarker compounds from various solid matrices are a critical requirement for the successful implementation of in situ chemical analysis of the martian regolith. Here, we describe a portable subcritical water extractor that mimics multiple organic solvent polarities by tuning the dielectric constant of liquid water through adjustment of temperature and pressure. Soil samples, collected from the Yungay region of the Atacama Desert ( martian regolith analogue) in the summer of 2005, were used to test the instrument's performance. The total organic carbon was extracted from the samples at concentrations of 0.2-55.4 parts per million. The extraction data were compared to the total organic carbon content in the bulk soil, which was determined via a standard analytical procedure. The instrument's performance was examined over the temperature range of 25-250 degrees C at a fixed pressure of 20.7 MPa. Under these conditions, water remains in a subcritical fluid state with a dielectric constant varying between similar to 80 ( at 25 degrees C) and similar to 30 (at 250 degrees C). C1 [Amashukeli, Xenia] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Amashukeli, X (reprint author), MS 302-231,4800 Oak Grove Dr, Pasadena, CA 91001 USA. EM Xenia.Amashukeli@jpl.nasa.gov NR 31 TC 14 Z9 14 U1 1 U2 16 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD JUN PY 2008 VL 8 IS 3 BP 597 EP U10 DI 10.1089/ast.2007.0154 PG 9 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 336SO UT WOS:000258385100008 PM 18680410 ER PT J AU Litvak, ML Mitrofanov, IG Barmakov, YN Behar, A Bitulev, A Bobrovnitsky, Y Bogolubov, EP Boynton, WV Bragin, SI Churin, S Grebennikov, AS Konovalov, A Kozyrev, AS Kurdumov, IG Krylov, A Kuznetsov, YP Malakhov, AV Mokrousov, MI Ryzhkov, VI Sanin, AB Shvetsov, VN Smirnov, GA Sholeninov, S Timoshenko, GN Tomilina, TM Tuvakin, DV Tretyakov, VI Troshin, VS Uvarov, VN Varenikov, A Vostrukhin, A AF Litvak, M. L. Mitrofanov, I. G. Barmakov, Yu. N. Behar, A. Bitulev, A. Bobrovnitsky, Yu. Bogolubov, E. P. Boynton, W. V. Bragin, S. I. Churin, S. Grebennikov, A. S. Konovalov, A. Kozyrev, A. S. Kurdumov, I. G. Krylov, A. Kuznetsov, Yu. P. Malakhov, A. V. Mokrousov, M. I. Ryzhkov, V. I. Sanin, A. B. Shvetsov, V. N. Smirnov, G. A. Sholeninov, S. Timoshenko, G. N. Tomilina, T. M. Tuvakin, D. V. Tretyakov, V. I. Troshin, V. S. Uvarov, V. N. Varenikov, A. Vostrukhin, A. TI The Dynamic Albedo of Neutrons (DAN) experiment for NASA's 2009 Mars Science Laboratory SO ASTROBIOLOGY LA English DT Article; Proceedings Paper CT Fall Meeting of the American-Geophysical-Union CY DEC, 2006 CL San Francisco, CA SP Amer Geophys Union DE Mars exploration; neutron spectroscopy; neutron activation analysis; neutron logging ID HEND INSTRUMENT ONBOARD; GAMMA-RAY; ODYSSEY SPACECRAFT; WATER; HYDROGEN; SURFACE; ICE AB We present a summary of the physical principles and design of the Dynamic Albedo of Neutrons (DAN) instrument onboard NASA's 2009 Mars Science Laboratory (MSL) mission. The DAN instrument will use the method of neutron-neutron activation analysis in a space application to study the abundance and depth distribution of water in the martian subsurface along the path of the MSL rover. C1 [Litvak, M. L.; Mitrofanov, I. G.; Kozyrev, A. S.; Malakhov, A. V.; Mokrousov, M. I.; Sanin, A. B.; Tretyakov, V. I.; Troshin, V. S.; Uvarov, V. N.; Varenikov, A.; Vostrukhin, A.] Space Res Inst, Moscow 117997, Russia. [Barmakov, Yu. N.; Bitulev, A.; Bogolubov, E. P.; Bragin, S. I.; Churin, S.; Kurdumov, I. G.; Kuznetsov, Yu. P.; Ryzhkov, V. I.; Smirnov, G. A.; Sholeninov, S.; Tuvakin, D. V.] NL Dukhov All Russian Inst Automat, Moscow, Russia. [Behar, A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Bobrovnitsky, Yu.; Grebennikov, A. S.] AA Blagonravov Mech Engn Inst, Moscow, Russia. [Boynton, W. V.] Univ Arizona, Tucson, AZ USA. [Krylov, A.; Shvetsov, V. N.; Timoshenko, G. N.] Joint Inst Nucl Res, Dubna, Russia. RP Litvak, ML (reprint author), Space Res Inst, Profsojuznaya St 84-32, Moscow 117997, Russia. EM Litvak@mx.iki.rssi.ru NR 21 TC 21 Z9 21 U1 1 U2 14 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD JUN PY 2008 VL 8 IS 3 BP 605 EP U11 DI 10.1089/ast.2007.0157 PG 9 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 336SO UT WOS:000258385100009 PM 18598140 ER PT J AU Pfiffner, SM Onstott, TC Ruskeeniemi, T Talikka, M Bakermans, C McGown, D Chan, E Johnson, A Phelps, TJ Le Puil, M Difurio, SA Pratt, LM Stotler, R Frape, S Telling, J Lollar, BS Neill, I Zerbin, B AF Pfiffner, S. M. Onstott, T. C. Ruskeeniemi, T. Talikka, M. Bakermans, C. McGown, D. Chan, E. Johnson, A. Phelps, T. J. Le Puil, M. Difurio, S. A. Pratt, L. M. Stotler, R. Frape, S. Telling, J. Lollar, B. Sherwood Neill, I. Zerbin, B. TI Challenges for coring deep permafrost on Earth and Mars SO ASTROBIOLOGY LA English DT Article; Proceedings Paper CT Fall Meeting of the American-Geophysical-Union CY DEC, 2006 CL San Francisco, CA SP Amer Geophys Union DE Mars; deep subsurface biosphere; planetary protection; planetary instrumentation; microbial ecology ID SUBSURFACE MICROBIAL COMMUNITIES; PHOSPHOLIPID FATTY-ACIDS; PERFLUOROCARBON TRACERS; MASS-SPECTROMETRY; SEDIMENTS; BIOMASS; MICROORGANISMS; AQUIFER; SAMPLES; BASIN AB A scientific drilling expedition to the High Lake region of Nunavut, Canada, was recently completed with the goals of collecting samples and delineating gradients in salinity, gas composition, pH, pe, and microbial abundance in a 400 m thick permafrost zone and accessing the underlying pristine subpermafrost brine. With a triple-barrel wireline tool and the use of stringent quality assurance and quality control (QA/QC) protocols, 200 m of frozen, Archean, mafic volcanic rock was collected from the lower boundary that separates the permafrost layer and subpermafrost saline water. Hot water was used to remove cuttings and prevent the drill rods from freezing in place. No cryopegs were detected during penetration through the permafrost. Coring stopped at the 535 m depth, and the drill water was bailed from the hole while saline water replaced it. Within 24 hours, the borehole iced closed at 125 m depth due to vapor condensation from atmospheric moisture and, initially, warm water leaking through the casing, which blocked further access. Preliminary data suggest that the recovered cores contain viable anaerobic microorganisms that are not contaminants even though isotopic analyses of the saline borehole water suggests that it is a residue of the drilling brine used to remove the ice from the upper, older portion of the borehole. Any proposed coring mission to Mars that seeks to access subpermafrost brine will not only require borehole stability but also a means by which to generate substantial heating along the borehole string to prevent closure of the borehole from condensation of water vapor generated by drilling. C1 [Pfiffner, S. M.; Le Puil, M.; Difurio, S. A.] Univ Tennessee, Ctr Environm Biotechnol, Knoxville, TN 37932 USA. [Onstott, T. C.; McGown, D.; Chan, E.] Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA. [Ruskeeniemi, T.; Talikka, M.] Geol Survey Finland GTK, Espoo, Finland. [Bakermans, C.] Michigan State Univ, Ctr Microbial Ecol, E Lansing, MI 48824 USA. [Johnson, A.; Pratt, L. M.] Indiana Univ, NASA Astrobiol Inst, IPTAI, Bloomington, IN USA. [Phelps, T. J.] Oak Ridge Natl Lab, Oak Ridge, TN USA. [Frape, S.] Univ Waterloo, Dept Earth Sci, Waterloo, ON N2L 3G1, Canada. [Telling, J.; Lollar, B. Sherwood] Univ Toronto, Dept Geol, Toronto, ON, Canada. [Neill, I.] Wolfden Resources Inc, Thunder Bay, ON, Canada. [Zerbin, B.] Major Drilling Grp Int Inc, Winnipeg, MB, Canada. RP Pfiffner, SM (reprint author), Univ Tennessee, Ctr Environm Biotechnol, 10515 Res Dr,Suite 300, Knoxville, TN 37932 USA. EM pfiffner@utk.edu RI phelps, tommy/A-5244-2011; Stotler, Randy/C-9782-2011; Telling, Jon/M-7643-2013; OI Stotler, Randy/0000-0001-9893-9259; Telling, Jon/0000-0002-8180-0979 NR 60 TC 9 Z9 9 U1 0 U2 14 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD JUN PY 2008 VL 8 IS 3 BP 623 EP 638 DI 10.1089/ast.2007.0159 PG 16 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 336SO UT WOS:000258385100011 PM 18680412 ER PT J AU Elphic, RC Chu, P Hahn, S James, MR Lawrence, DJ Prettyman, TH Johnson, JB Podgorney, RK AF Elphic, R. C. Chu, P. Hahn, S. James, M. R. Lawrence, D. J. Prettyman, T. H. Johnson, J. B. Podgorney, R. K. TI Surface and downhole prospecting tools for planetary exploration: Tests of neutron and gamma ray probes SO ASTROBIOLOGY LA English DT Article; Proceedings Paper CT Fall Meeting of the American-Geophysical-Union CY DEC, 2006 CL San Francisco, CA SP Amer Geophys Union DE neutron; gamma ray; prospecting; water; hydrogen; habitat ID LUNAR SOUTH-POLE; MARS ODYSSEY; ICE DEPOSITS; NEAR-SURFACE; GROUND ICE; WATER ICE; HYDROGEN; SPECTROMETER; MISSION; PAYLOAD AB The ability to locate and characterize icy deposits and other hydrogenous materials on the Moon and Mars will help us understand the distribution of water and, therefore, possible habitats at Mars, and may help us locate primitive prebiotic compounds at the Moon's poles. We have developed a rover-borne neutron probe that localizes a near-surface icy deposit and provides information about its burial depth and abundance. We have also developed a borehole neutron probe to determine the stratigraphy of hydrogenous subsurface layers while operating within a drill string segment. In our field tests, we have used a neutron source to "illuminate" surrounding materials and gauge the instruments' efficacy, and we can simulate accurately the observed instrument responses using a Monte Carlo nuclear transport code (MCNPX). An active neutron source would not be needed for lunar or martian near-surface exploration: cosmic-ray interactions provide sufficient neutron flux to depths of several meters and yield better depth and abundance sensitivity than an active source. However, for deep drilling (>= 10 m depth), a source is required. We also present initial tests of a borehole gamma ray lithodensity tool and demonstrate its utility in determining soil or rock densities and composition. C1 [Elphic, R. C.] NASA Ames Res Ctr, Planetary Syst Branch, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Chu, P.] Honeybee Robot Spacecraft Mech Corp, Houston, TX USA. [Hahn, S.] Los Alamos Natl Lab, Space Instrumentat & Syst Engn Grp, Los Alamos, NM USA. [James, M. R.] Los Alamos Natl Lab, Nucl Design & Risk Anal, Los Alamos, NM USA. [Lawrence, D. J.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Planetary Explorat Grp, Laurel, MD USA. [Prettyman, T. H.] Planetary Sci Inst, Tucson, AZ USA. [Johnson, J. B.] USA, Corps Engineers, ERDC Cold Reg & Engn Lab, Ft Wainwright, AR USA. [Podgorney, R. K.] Idaho Natl Lab, Modeling & Measurement Dept, Idaho Falls, ID USA. RP Elphic, RC (reprint author), NASA Ames Res Ctr, Planetary Syst Branch, Space Sci & Astrobiol Div, Mail Stop 245-3, Moffett Field, CA 94035 USA. EM richard.c.elphic@nasa.gov RI Lawrence, David/E-7463-2015; OI Lawrence, David/0000-0002-7696-6667; Prettyman, Thomas/0000-0003-0072-2831 NR 37 TC 8 Z9 8 U1 0 U2 7 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD JUN PY 2008 VL 8 IS 3 BP 639 EP U15 DI 10.1089/ast.2007.0163 PG 15 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 336SO UT WOS:000258385100012 PM 18554085 ER PT J AU Glass, B Cannon, H Branson, M Hanagud, S Paulsen, G AF Glass, B. Cannon, H. Branson, M. Hanagud, S. Paulsen, G. TI DAME: Planetary-prototype drilling automation SO ASTROBIOLOGY LA English DT Article; Proceedings Paper CT Fall Meeting of the American-Geophysical-Union CY DEC, 2006 CL San Francisco, CA SP Amer Geophys Union DE robotics; drilling; subsurface; automation; artificial intelligence; structural dynamics; sampling; NASA AB We describe results from the Drilling Automation for Mars Exploration ( DAME) project, including those of the summer 2006 tests from an Arctic analog site. The drill hardware is a hardened, evolved version of the Advanced Deep Drill by Honeybee Robotics. DAME has developed diagnostic and executive software for hands-off surface operations of the evolved version of this drill. The DAME drill automation tested from 2004 through 2006 included adaptively controlled drilling operations and the downhole diagnosis of drilling faults. It also included dynamic recovery capabilities when unexpected failures or drilling conditions were discovered. DAME has developed and tested drill automation software and hardware under stressful operating conditions during its Arctic field testing campaigns at a Mars analog site. C1 [Glass, B.] NASA Ames Res Ctr, Explorat Syst Div, Moffett Field, CA 94035 USA. [Hanagud, S.] Georgia Inst Technol, Atlanta, GA 30332 USA. [Paulsen, G.] Honeybee Robot, New York, NY USA. RP Glass, B (reprint author), NASA Ames Res Ctr, Explorat Syst Div, Mail Stop 269-4, Moffett Field, CA 94035 USA. EM brian.glass@nasa.gov NR 18 TC 19 Z9 21 U1 0 U2 10 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD JUN PY 2008 VL 8 IS 3 BP 653 EP U20 DI 10.1089/ast.2007.0148 PG 13 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 336SO UT WOS:000258385100013 PM 18597659 ER PT J AU Zacny, K Bar-Cohen, Y Brennan, M Briggs, G Cooper, G Davis, K Dolgin, B Glaser, D Glass, B Gorevan, S Guerrero, J Mckay, C Paulsen, G Stanley, S Stoker, C AF Zacny, K. Bar-Cohen, Y. Brennan, M. Briggs, G. Cooper, G. Davis, K. Dolgin, B. Glaser, D. Glass, B. Gorevan, S. Guerrero, J. Mckay, C. Paulsen, G. Stanley, S. Stoker, C. TI Drilling systems for extraterrestrial subsurface exploration SO ASTROBIOLOGY LA English DT Article; Proceedings Paper CT Fall Meeting of the American-Geophysical-Union CY DEC, 2006 CL San Francisco, CA SP Amer Geophys Union DE drilling; coring; sampling; subsurface exploration; drill bits ID GROUND ICE; MARS; SEARCH; LIFE; CONSTRAINTS; SIMULATION; BEHAVIOR; MODEL; SOIL AB Drilling consists of 2 processes: breaking the formation with a bit and removing the drilled cuttings. In rotary drilling, rotational speed and weight on bit are used to control drilling, and the optimization of these parameters can markedly improve drilling performance. Although fluids are used for cuttings removal in terrestrial drilling, most planetary drilling systems conduct dry drilling with an auger. Chip removal via water-ice sublimation ( when excavating water-ice-bound formations at pressure below the triple point of water) and pneumatic systems are also possible. Pneumatic systems use the gas or vaporization products of a high-density liquid brought from Earth, gas provided by an in situ compressor, or combustion products of a monopropellant. Drill bits can be divided into coring bits, which excavate an annular shaped hole, and full-faced bits. While cylindrical cores are generally superior as scientific samples, and coring drills have better performance characteristics, full-faced bits are simpler systems because the handling of a core requires a very complex robotic mechanism. The greatest constraints to extraterrestrial drilling are ( 1) the extreme environmental conditions, such as temperature, dust, and pressure; ( 2) the light-time communications delay, which necessitates highly autonomous systems; and ( 3) the mission and science constraints, such as mass and power budgets and the types of drilled samples needed for scientific analysis. A classification scheme based on drilling depth is proposed. Each of the 4 depth categories ( surface drills, 1-meter class drills, 10-meter class drills, and deep drills) has distinct technological profiles and scientific ramifications. C1 [Zacny, K.; Davis, K.; Glaser, D.; Gorevan, S.; Paulsen, G.] Honeybee Robot Spacecraft Mech Corp, New York, NY 10001 USA. [Bar-Cohen, Y.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA USA. [Brennan, M.] Raytheon UTD, Springfield, VA USA. [Briggs, G.; Glass, B.; Stoker, C.] NASA Ames Res Ctr, Moffett Field, CA USA. [Cooper, G.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Guerrero, J.] ATK Space Syst Inc, Pasadena, CA USA. [Stanley, S.] Alliance Spacesyst LLC, Pasadena, CA USA. RP Zacny, K (reprint author), Honeybee Robot Spacecraft Mech Corp, 460 W 34th St, New York, NY 10001 USA. EM zacny@honeybeerobotics.com NR 87 TC 35 Z9 37 U1 2 U2 20 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD JUN PY 2008 VL 8 IS 3 BP 665 EP U148 DI 10.1089/ast.2007.0179 PG 43 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 336SO UT WOS:000258385100014 PM 18598141 ER PT J AU Persi, P Gomez, M Tapia, M Roth, M De Buizer, JM Marenzi, AR AF Persi, P. Gomez, M. Tapia, M. Roth, M. De Buizer, J. M. Marenzi, A. R. TI Star formation in the southern dark cloud DC 296.2-3.6 SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared : ISM; ISM : clouds; stars : formation; stars : individual (DC 296.2-3.6) ID YOUNG STELLAR OBJECTS; VELOCITY-FIELD; OUTER GALAXY AB We report near-and mid-infrared (IR) images of the southern hemisphere dark cloud DC 296.2-3.6 associated with IRAS 11431-6516. The K(s) and L' images show the presence of an IR nebulosity at the center of the dark cloud (DC). From the analysis of the near-IR color-color diagrams we have identified a young stellar population in the region. Five of these young stellar objects, here named A, B, C, D, and E, were also detected in the mid-IR. Sources B, D, and E are Class I-II T Tauri as suggested by the analysis of their spectral energy distributions. In addition, source E shows a long-term near-IR variability. The near-IR color color diagrams indicate the presence of circumstellar dust envelope in sources A, B, D, and E, while the fit of SEDs of the intermediate-and low-mass objects A and B with a radiation transfer model including infalling envelope+disk+central source suggests circumstellar disks around these two objects. These results indicate that DC 296.2-3.6, located in the far Carina arm, is associated with an embedded cluster of low-mass young stellar objects. C1 [Persi, P.; Marenzi, A. R.] INAF IASF Roma, I-00133 Rome, Italy. [Gomez, M.] Astron Observ, Cordoba, Argentina. [Tapia, M.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada, Baja California, Mexico. [Roth, M.] Carnegie Inst Washington, Las Campanas Observ, La Serena, Chile. [De Buizer, J. M.] Gemini Observ, La Serena, Chile. [De Buizer, J. M.] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA. RP Persi, P (reprint author), INAF IASF Roma, Via Foss Cavaliere 100, I-00133 Rome, Italy. EM paolo.persi@iasf-roma.inaf.it OI Tapia, Mauricio/0000-0002-0506-9854 NR 17 TC 0 Z9 0 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2008 VL 135 IS 6 BP 2279 EP 2286 DI 10.1088/0004-6256/135/6/2279 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 309IK UT WOS:000256453700028 ER PT J AU Vokrouhlicky, D Chesley, SR Matson, RD AF Vokrouhlicky, D. Chesley, S. R. Matson, R. D. TI Orbital identification for asteroid 152563 (1992 BF) through the Yarkovsky effect SO ASTRONOMICAL JOURNAL LA English DT Article DE minor planets; asteroids ID NEAR-EARTH ASTEROIDS; DETECTION OPPORTUNITIES; FRAGMENTS; OBJECTS AB Often a newly discovered near-Earth asteroid is linked to old observations of a formerly lost object. This orbital identification is done using a standard dynamical model that accounts for gravitational perturbations from planets and relativistic effects. Here we report the first case where such an identification requires consideration of the Yarkovsky effect, a tiny non-gravitational perturbation due to the recoil of thermal radiation from the body. Moreover, this implies that the Yarkovsky force is revealed in the orbital motion of the body, asteroid 152563 (1992 bf), only the second case so far. Orbital fits indicate a drift in the orbital semi-major axis of -(10.7 +/- 0.7) x 10(-4) AU Myr(-1), which we ascribe to Yarkovsky forces. This yields a correlated constraint of physical parameters such as the obliquity, rotation rate, surface thermal inertial, and bulk density. The magnitude and direction of drift point to an obliquity in excess of 120 degrees. Observations taken during 2011 and subsequent close encounters with the Earth might help establish rotation parameters and thereby constrain thermal inertia of 1992 bf, thus making the Yarkovsky strength a measure of this asteroid's bulk density. C1 [Vokrouhlicky, D.] Charles Univ Prague, Inst Astron, CZ-18000 Prague 8, Czech Republic. [Chesley, S. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Matson, R. D.] Sci Applicat Int Corp, Seal Beach, CA 90740 USA. RP Vokrouhlicky, D (reprint author), Charles Univ Prague, Inst Astron, Holesovickach 2, CZ-18000 Prague 8, Czech Republic. EM vokrouhl@cesnet.cz; steve.chesley@jpl.nasa.gov; robert.d.matson@saic.com NR 33 TC 19 Z9 19 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2008 VL 135 IS 6 BP 2336 EP 2340 DI 10.1088/0004-6256/135/6/2336 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 309IK UT WOS:000256453700033 ER PT J AU Smith, BJ Struck, C Hancock, M Giroux, ML Appleton, PN Charmandaris, V Reach, W Hurlock, S Hwang, JS AF Smith, Beverly J. Struck, Curtis Hancock, Mark Giroux, Mark L. Appleton, Philip N. Charmandaris, Vassilis Reach, William Hurlock, Sabrina Hwang, Jeong-Sun TI Stochastic "beads on a string" in the accretion tail of Arp 285 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : individual (Arp 285); galaxies : interactions; galaxies : starburst ID SPITZER-SPACE-TELESCOPE; HIERARCHICAL STAR-FORMATION; DWARF IRREGULAR GALAXIES; YOUNG GLOBULAR-CLUSTERS; DIGITAL SKY SURVEY; INTERACTING GALAXIES; SURFACE PHOTOMETRY; ANTENNAE GALAXIES; STELLAR CLUSTERS; ALPHA ABSORPTION AB We present Spitzer infrared, Galaxy Evolution Explorer UV, and Sloan Digitized Sky Survey and Southeastern Association for Research in Astronomy optical images of the peculiar interacting galaxy pair Arp 285 (NGC 2856/4), and compare with a new numerical model of the interaction. We estimate the ages of clumps of star formation in these galaxies using population synthesis models, carefully considering the uncertainties on these ages. This system contains a striking example of "beads on a string": a series of star-formation complexes similar to 1 kpc apart. These "beads" are found in a tail-like feature that is perpendicular to the disk of NGC 2856, which implies that it was formed from material accreted from the companion NGC 2854. The extreme blueness of the optical/UV colors and redness of the mid-infrared colors implies very young stellar ages (similar to 4-20 Myr) for these star-forming regions. Spectral decomposition of these "beads" shows excess emission above the modeled stellar continuum in the 3.6 mu m and 4.5 mu m bands, indicating either contributions from interstellar matter to these fluxes or a second older stellar population. These clumps have -12.0 < M(B) < -10.6, thus they are less luminous than most dwarf galaxies. Our model suggests that bridge material falling into the potential of the companion overshoots the companion. The gas then piles up at apogalacticon before falling back onto the companion, and star formation occurs in the pile-up. There was a time delay of similar to 500 Myr between the point of closest approach between the two galaxies and the initiation of star formation in this feature. A luminous (M(B) similar to -13.6) extended (FWHM similar to 1.3 kpc) "bright spot" is visible at the northwestern edge of the NGC 2856 disk, with an intermediate stellar population (400-1500 Myr). Our model suggests that this feature is part of a expanding ripple-like "arc" created by an off-center ring-galaxy-like collision between the two disks. C1 [Smith, Beverly J.; Hancock, Mark; Giroux, Mark L.; Hurlock, Sabrina] E Tennessee State Univ, Dept Phys Astron & Geol, Johnson City, TN 37614 USA. [Struck, Curtis; Hwang, Jeong-Sun] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Appleton, Philip N.] CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. [Charmandaris, Vassilis] Univ Crete, Dept Phys, Iraklion 71003, Greece. [Reach, William] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RP Smith, BJ (reprint author), E Tennessee State Univ, Dept Phys Astron & Geol, Johnson City, TN 37614 USA. EM smithbj@etsu.edu; curt@iastate.edu; hancockm@etsu.edu; girouxm@etsu.edu; apple@ipac.caltech.edu; vassilis@physics.uoc.gr; reach@ipac.caltech.edu; zshh7@imail.etsu.edu; jshwang@iastate.edu RI Charmandaris, Vassilis/A-7196-2008; OI Charmandaris, Vassilis/0000-0002-2688-1956; Struck, Curtis/0000-0002-6490-2156; Appleton, Philip/0000-0002-7607-8766; Reach, William/0000-0001-8362-4094 NR 68 TC 31 Z9 31 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2008 VL 135 IS 6 BP 2406 EP 2423 DI 10.1088/0004-6256/135/6/2406 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 309IK UT WOS:000256453700040 ER PT J AU Cheng, AF Simon-Miller, AA Weaver, HA Baines, KH Orton, GS Yanamandra-Fisher, PA Mousis, O Pantin, E Vanzi, L Fletcher, LN Spencer, JR Stern, SA Clarke, JT Mutchler, MJ Noll, KS AF Cheng, A. F. Simon-Miller, A. A. Weaver, H. A. Baines, K. H. Orton, G. S. Yanamandra-Fisher, P. A. Mousis, O. Pantin, E. Vanzi, L. Fletcher, L. N. Spencer, J. R. Stern, S. A. Clarke, J. T. Mutchler, M. J. Noll, K. S. TI Changing characteristics of Jupiter's little red spot SO ASTRONOMICAL JOURNAL LA English DT Article DE atmospheric effects; convection; hydrodynamics; planets and satellites : individual (Jupiter) ID WHITE OVALS; ATMOSPHERE; BC AB The Little Red Spot (LRS) in Jupiter's atmosphere was investigated in unprecedented detail by the New Horizons spacecraft together with the Hubble Space Telescope (HST) and the Very Large Telescope (VLT). The LRS and the larger Great Red Spot (GRS) of Jupiter are the largest known atmospheric storms in the solar system. Originally a white oval, the LRS formed from the mergers of three smaller storms in 1998 and 2000, and became as red as the GRS between 2005 and 2006. Here we show that circulation and wind speeds in the LRS have increased substantially since the Voyager and Galileo eras when the oval was white. The maximum tangential velocity of the LRS is now 172 +/- 18 m s(-1), close to the highest values ever seen in the GRS, which has also evolved both in size and maximum wind speed. The cloud-top altitudes of the GRS and LRS are similar, both storms extending much higher in the atmosphere than other Jovian anti-cyclonic systems. The similarities in wind speeds, cloud morphology, and coloring suggest a common dynamical mechanism explaining the reddening of the two largest anticyclonic systems on Jupiter. These storms will not be observed again from close range until at least 2016. C1 [Cheng, A. F.; Weaver, H. A.] Johns Hopkins Appl Phys Lab, Laurel, MD 20723 USA. [Simon-Miller, A. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Baines, K. H.; Orton, G. S.; Yanamandra-Fisher, P. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Mousis, O.] Univ Franche Comte, CNRS, Inst UTINAM, UMR 6213, F-25030 Besancon, France. [Pantin, E.] CEA SAp, Ctr Etud Atom, F-91190 Gif Sur Yvette, France. [Vanzi, L.] European So Observ, Santiago 19, Chile. [Fletcher, L. N.] Univ Oxford, Dept Phys, Clarendon Lab, Oxford OX1 3PU, England. [Spencer, J. R.] SW Res Inst, Boulder, CO 80302 USA. [Cheng, A. F.; Stern, S. A.] NASA Headquarters, Washington, DC 20546 USA. [Clarke, J. T.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Clarke, J. T.] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA. [Mutchler, M. J.; Noll, K. S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Cheng, AF (reprint author), Johns Hopkins Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM andrew.cheng@jhuapl.edu; Amy.Simon@nasa.gov; Hal.Weaver@jhuapl.edu; kbaines@mail.jpl.nasa.gov; go@scn.jpl.nasa.gov; padma@scn.jpl.nasa.gov; olivier.mousis@obs-besancon.fr; epantin@cea.fr; lvanzi@eso.org; fletcher@atm.ox.ac.uk; spencer@boulder.swri.edu; alan.stern@nasa.gov RI Fletcher, Leigh/D-6093-2011; Simon, Amy/C-8020-2012; Noll, Keith/C-8447-2012; Clarke, John/C-8644-2013; Vanzi, Leonardo/D-1381-2014; Weaver, Harold/D-9188-2016 OI Fletcher, Leigh/0000-0001-5834-9588; Simon, Amy/0000-0003-4641-6186; NR 24 TC 24 Z9 24 U1 3 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2008 VL 135 IS 6 BP 2446 EP 2452 DI 10.1088/0004-6256/135/6/2446 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 309IK UT WOS:000256453700042 ER PT J AU Connelley, MS Reipurth, B Tokunaga, AT AF Connelley, Michael S. y Reipurth, Bo Tokunaga, Alan T. TI The evolution of the multiplicity of embedded protostars. I. Sample properties and binary detections SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : general; infrared : stars; stars : formation; stars : statistics ID BRIGHT-RIMMED CLOUDS; HARO ENERGY-SOURCES; IRAS POINT SOURCES; RADIATION-DRIVEN IMPLOSION; NEARBY MOLECULAR CLOUDS; YOUNG STELLAR OBJECTS; INFRARED FILTER SET; STAR-FORMATION; DARK CLOUDS; MAUNA-KEA AB We present the observational results of a near-infrared survey of a large sample of Class I protostars designed to determine the Class I binary separation distribution from similar to 100 AU to similar to 5000 AU. We have selected targets from a new sample of 267 nearby candidate Class I objects. This sample is well understood, consists of mostly Class I young stellar objects (YSOs) within 1 kpc, has targets selected from the whole sky, and is not biased by previous studies of star formation. We have observed 189 Class I YSOs north of delta = -40 degrees. at the H, K, and L' bands, with a median angular resolution of 0 ''.33 at L'. We determine our detection limit for close binary companions by observing artificial binaries. We choose a contrast limit and an outer detection limit to minimize contamination and to ensure that a candidate companion is gravitationally bound. Our survey uses observations at the L' rather than the K band for the detection of binary companions since there is less scattered light and better seeing at L'. This paper presents the positions of our targets, the near-IR photometry of sources detected in our fields at L', as well as the observed properties of the 89 detected companions (73 of which are newly discovered). Although we have chosen contrast and separation limits to minimize contamination, we expect that there are about six stars identified as binary companions that are due to contamination. Finder charts at L' for each field are shown to facilitate future studies of these objects. C1 [Connelley, Michael S. y] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Reipurth, Bo] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. [Reipurth, Bo] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Connelley, MS (reprint author), NASA, Ames Res Ctr, MS 246-6, Moffett Field, CA 94035 USA. EM michael.s.connelley@nasa.gov; reipurth@ifa.hawaii.edu; tokunaga@ifa.hawaii.edu NR 91 TC 40 Z9 40 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 JUN PY 2008 VL 135 IS 6 BP 2496 EP 2525 DI 10.1088/0004-6256/135/6/2496 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 309IK UT WOS:000256453700045 ER PT J AU Connelley, MS Reipurth, B Tokunaga, AT AF Connelley, Michael S. Reipurth, Bo Tokunaga, Alan T. TI The evolution of the multiplicity of embedded protostars. II. Binary separation distribution and analysis SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : general; infrared : stars; stars : formation; stars : statistics ID STAR-FORMING REGIONS; YOUNG STELLAR OBJECTS; MAIN-SEQUENCE STARS; T-TAURI STARS; MOLECULAR CLOUDS; IMAGING SURVEY; SYSTEMS; MASS; OPHIUCHUS; SPECTRUM AB We present the Class I protostellar binary separation distribution based on the data tabulated in a companion paper. We verify the excess of Class I binary stars over solar-type main-sequence stars in the separation range from 500 AU to 4500 AU. Although our sources are in nearby star-forming regions distributed across the entire sky (including Orion), none of our objects are in a high stellar density environment. A log-normal function, used by previous authors to fit the main-sequence and T Tauri binary separation distributions, poorly fits our data, and we determine that a log-uniform function is a better fit. Our observations show that the binary separation distribution changes significantly during the Class I phase, and that the binary frequency at separations greater than 1000 AU declines steadily with respect to spectral index. Despite these changes, the binary frequency remains constant until the end of the Class I phase, when it drops sharply. We propose a scenario to account for the changes in the Class I binary separation distribution. This scenario postulates that a large number of companions with a separation greater than similar to 1000 AU were ejected during the Class 0 phase, but remain gravitationally bound due to the significant mass of the Class I envelope. As the envelope dissipates, these companions become unbound and the binary frequency at wide separations declines. Circumstellar and circumbinary disks are expected to play an important role in the orbital evolution at closer separations. This scenario predicts that a large number of Class 0 objects should be non-hierarchical multiple systems, and that many Class I young stellar objects (YSOs) with a widely separated companion should also have a very close companion. We also find that Class I protostars are not dynamically pristine, but have experienced dynamical evolution before they are visible as Class I objects. Our analysis shows that the Class I binary frequency and the binary separation distribution strongly depend on the star-forming environment. C1 [Connelley, Michael S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Reipurth, Bo] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. [Tokunaga, Alan T.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Connelley, MS (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA. EM michael.s.connelly@nasa.gov; reipurth@ifa.hawaii.edu; tokunaga@ifa.hawaii.edu NR 49 TC 42 Z9 42 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2008 VL 135 IS 6 BP 2526 EP 2536 DI 10.1088/0004-6256/135/6/2526 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 309IK UT WOS:000256453700046 ER PT J AU Martin-Zaidi, C Deleuil, M Le Bourlot, J Bouret, JC Roberge, A Dullemond, CP Testi, L Feldman, PD Des Etangs, AL Vidal-Madjar, A AF Martin-Zaidi, C. Deleuil, M. Le Bourlot, J. Bouret, J. -C. Roberge, A. Dullemond, C. P. Testi, L. Feldman, P. D. des Etangs, A. Lecavelier Vidal-Madjar, A. TI Molecular hydrogen in the circumstellar environments of Herbig Ae/Be stars probed by FUSE SO ASTRONOMY & ASTROPHYSICS LA English DT Review DE stars : circumstellar matter; stars : formation; stars : pre-main sequence; ISM : molecules ID INTERMEDIATE-MASS STARS; MAIN-SEQUENCE STARS; YOUNG STELLAR OBJECTS; ULTRAVIOLET-SPECTROSCOPIC-EXPLORER; LOCAL INTERSTELLAR-MEDIUM; ROTATIONAL H-2 EMISSION; AB-AURIGAE SYSTEM; AE STAR; BETA-PICTORIS; HIGH-RESOLUTION AB Context. Molecular hydrogen ( H(2)) gas is the most abundant molecule in the circumstellar ( CS) environments of young stars. It is thus a key element in our understanding of the evolution of pre-main sequence stars and their environments towards the main sequence. Aims. At the present time, little is known about the gas as compared to the dust in the environments of young stars. We thus observed molecular hydrogen around a sample of pre-main sequence stars in order to better characterize their gaseous CS environments. Methods. The FUSE ( Far Ultraviolet Spectroscopic Explorer) spectral range offers access to electronic transitions of H(2). We analyzed the FUSE spectra of a sample of Herbig Ae/Be stars (HAeBes) covering a broad spectral range ( from F4 to B2), including the main-sequence A5 star beta Pictoris. To better diagnose the origin of the detected molecular gas and its excitation conditions, we used a model of a photodissociation region. Results. Our analysis demonstrates that the excitation of H2 is clearly different around most of the HAeBes compared to the interstellar medium. Moreover, the characteristics of H2 around Herbig Ae and Be stars give evidence for different excitation mechanisms. For the most massive stars of our sample ( B8 to B2 type), the excitation diagrams are reproduced well by a model of photodissociation regions ( PDR). Our results favor an interpretation in terms of large CS envelopes, remnants of the molecular clouds in which the stars were formed. On the other hand, the group of Ae stars ( later than B9 type) known to possess disks is more inhomogeneous. In most cases, when CS H2 is detected, the lines of sight do not pass through the disks. The excitation conditions of H2 around Ae stars cannot be reproduced by PDR models and correspond to warm and/or hot excited media very close to the stars. In addition, no clear correlation has been found between the ages of the stars and the amount of circumstellar H2. Our results suggest structural differences between Herbig Ae and Be star environments. Herbig Be stars do evolve faster than Ae stars, and consequently, most Herbig Be stars are younger than Ae ones at the time we observe them. It is thus more likely to find remnants of their parent cloud around them. C1 [Martin-Zaidi, C.] Univ Grenoble 1, CNRS, Lab Astrophys Grenoble, UMR 5571, Grenoble, France. [Deleuil, M.; Bouret, J. -C.] Astrophys Lab, F-13376 Marseille 12, France. [Le Bourlot, J.] Univ Paris 07, Observ Paris, LUTH, F-92195 Meudon, France. [Roberge, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dullemond, C. P.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Testi, L.] Osserv Astrofis Arcetri, I-50125 Florence, Italy. [Feldman, P. D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [des Etangs, A. Lecavelier; Vidal-Madjar, A.] CNRS, Inst Astrophys Paris, F-75014 Paris, France. RP Martin-Zaidi, C (reprint author), Univ Grenoble 1, CNRS, Lab Astrophys Grenoble, UMR 5571, Grenoble, France. EM claire.martin-zaidi@obs.ujf-grenoble.fr RI Roberge, Aki/D-2782-2012; OI Roberge, Aki/0000-0002-2989-3725; Dullemond, Cornelis/0000-0002-7078-5910 NR 115 TC 31 Z9 31 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 JUN PY 2008 VL 484 IS 1 BP 225 EP U79 DI 10.1051/0004-6361:20079325 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 307HG UT WOS:000256309400021 ER PT J AU Boersma, C Bouwman, J Lahuis, F van Kerckhoven, C Tielens, AGGM Waters, LBFM Henning, T AF Boersma, C. Bouwman, J. Lahuis, F. van Kerckhoven, C. Tielens, A. G. G. M. Waters, L. B. F. M. Henning, T. TI The characteristics of the IR emission features in the spectra of Herbig Ae stars: evidence for chemical evolution SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : planetary systems : formation; infrared : stars; line : profiles; ISM : molecules ID POLYCYCLIC AROMATIC-HYDROCARBONS; SPITZER-SPACE-TELESCOPE; T-TAURI STARS; AE/BE STARS; CIRCUMSTELLAR DISKS; INFRARED-EMISSION; PAH EMISSION; ISO SPECTROSCOPY; MICRON REGION; HD 163296 AB Context. Infrared ( IR) spectra provide a prime tool to study the characteristics of polycyclic aromatic hydrocarbon ( PAH) molecules in regions of star formation. Herbig Ae/Be stars are a class of young pre-main sequence stellar objects of intermediate mass. They are known to have varying amounts of natal cloud material still present in their direct vicinity. Aims. We characterise the IR emission bands, due to fluorescence by PAH molecules, in the spectra of Herbig Ae/Be stars and link observed variations to spatial aspects of the mid-IR emission. Methods. We analysed two PAH dominated spectra from a sample of 15 Herbig Ae/Be stars observed with the Spitzer Space Telescope. Results. We derived profiles of the major PAH bands by subtracting appropriate continua. The shape and the measured band characteristics show pronounced variations between the two Spitzer spectra investigated. Those variations parallel those found between three infrared space observatory (ISO) spectra of other, well-studied, Herbig Ae/Be stars. The derived profiles are compared to those from a broad sample of sources, including reflection nebulae, planetary nebulae, H II regions, young stellar objects, evolved stars and galaxies. The Spitzer and ISO spectra exhibit characteristics commonly interpreted respectively as interstellar matter-like ( ISM), non-ISM-like, or a combination of the two. Conclusions. We argue that the PAH emission detected from the sources exhibiting a combination of ISM-like and non-ISM-like characteristics indicates the presence of two dissimilar, spatially separated, PAH families. As the shape of the individual PAH band profiles reflects the composition of the PAH molecules involved, this demonstrates that PAHs in subsequent, evolutionary linked stages of star formation are different from those in the general ISM, implying active chemistry. None of the detected PAH emission can be associated with the ( unresolved) disk and is thus associated with the circumstellar ( natal) cloud. This implies that chemical changes may already occur in the ( collapsing?) natal cloud and not necessarily in the disk. C1 [Boersma, C.; Tielens, A. G. G. M.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Bouwman, J.; Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Lahuis, F.] Space Res Org Netherlands, NL-9700 AV Groningen, Netherlands. [Lahuis, F.] Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Kerckhoven, C.] Katholieke Univ Leuven, Inst Sterrekunde, B-3001 Heverlee, Belgium. [Tielens, A. G. G. M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Waters, L. B. F. M.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. RP Boersma, C (reprint author), Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands. EM boersma@astro.rug.nl RI Boersma, Christiaan/L-7696-2014 OI Boersma, Christiaan/0000-0002-4836-217X NR 52 TC 31 Z9 31 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 JUN PY 2008 VL 484 IS 1 BP 241 EP 249 DI 10.1051/0004-6361:20078001 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 307HG UT WOS:000256309400022 ER PT J AU Shanmugaraju, A Moon, YJ Cho, KS Gopalswamy, N Umapathy, S AF Shanmugaraju, A. Moon, Y. -J. Cho, K. -S. Gopalswamy, N. Umapathy, S. TI Investigation of CME dynamics in the LASCO field of view SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun : flares; Sun : coronal mass ID CORONAL MASS EJECTIONS; II RADIO-BURSTS AB Context. The speed-distance profile of CMEs is important for understanding the propagation of CMEs. Aims. Our main aim is to study the initial speed of CMEs in the LASCO field of view and its role in subsequent CME propagation using the acceleration-speed profile. The secondary aim is to obtain the speed growth rate. Methods. We considered the height-time data of 307 CMEs observed by SOHO/LASCO during January-March 2005. To study the CME speed profile, we used only 116 events for which there were at least 10 height-time measurements in the LASCO field of view. Using this data, we obtained their initial speed, extrapolated initial speed, and growth rate. Results. The following results were found from this analysis. (i) The initial speed obtained from the first two data points is in the range 24-1208 km s(-1), which is nearly similar to the range of linear speed (67-920 km s(-1)) obtained from a least squares fit through the entire h-t data set for each CME. (ii) However, the initial speed or extrapolated initial speed is much better correlated with acceleration and growth rate than the linear speed. (iii) Nearly two thirds of the events (74/116) are found to be accelerating. (iv) The speed growth rate is within the range -0.058 to 0.061 x 10(-3) s(-1), and it decreases with the distance. (v) The final observed distance in the LASCO field of view depends very weakly upon the initial speed, or extrapolated initial speed whereas it depends strongly on the linear speed. The above results demonstrate the role played by the initial speed of the CMEs. C1 [Shanmugaraju, A.] Arul Anandar Coll, Dept Phys, Karumathur 625514, India. [Moon, Y. -J.] Kyung Hee Univ, Dept Astron & Space Sci, Yongin 446701, South Korea. [Cho, K. -S.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Gopalswamy, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Umapathy, S.] Madurai Kamaraj Univ, Sch Phys, Madurai 625021, Tamil Nadu, India. RP Shanmugaraju, A (reprint author), Arul Anandar Coll, Dept Phys, Karumathur 625514, India. EM shanmugaraju_a@yahoo.com RI Gopalswamy, Nat/D-3659-2012; Moon, Yong-Jae/E-1711-2013 NR 19 TC 2 Z9 2 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 JUN PY 2008 VL 484 IS 2 BP 511 EP 516 DI 10.1051/0004-6361:20078978 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 307HJ UT WOS:000256309700028 ER PT J AU Goossens, M Arregui, I Ballester, JL Wang, TJ AF Goossens, M. Arregui, I. Ballester, J. L. Wang, T. J. TI Analytic approximate seismology of transversely oscillating coronal loops SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE magnetohydrodynamics (MHD); methods : analytical; Sun : corona; Sun : magnetic fields; Sun : oscillations ID MAGNETIC-FLUX TUBES; MODE KINK OSCILLATIONS; RESONANT ABSORPTION; MHD WAVES; MAGNETOHYDRODYNAMIC WAVES; CONNECTION FORMULAS; SUMER; SURFACES; BEHAVIOR; PLASMA AB Aims. We present an analytic approximate seismic inversion scheme for damped transverse coronal loop oscillations based on the thin tube and thin boundary approximation for computing the period and the damping time. Methods. Asymptotic expressions for the period and damping rate are used to illustrate the process of seismological inversion in a simple and easy to follow manner. The inversion procedure is formulated in terms of two simple functions, which are given by simple closed expressions. Results. The analytic seismic inversion shows that an infinite amount of 1-dimensional equilibrium models can reproduce the observed periods and damping times. It predicts a specific range of allowable values for the Alfven travel time and lower bounds for the density contrast and the inhomogeneity length scale. When the results of the present analytic seismic inversion are compared with those of a previous numerical inversion, excellent agreement is found up to the point that the analytic seismic inversion emerges as a tool for validating results of numerical inversions. Actually it helped us to identify and correct inaccuracies in a previous numerical investigation. C1 [Goossens, M.] Katholieke Univ Leuven, Ctr Plasma Astrophys, B-3001 Louvain, Belgium. [Arregui, I.; Ballester, J. L.] Univ Illes Balears, Dept Fis, Palma de Mallorca 07122, Spain. [Wang, T. J.] Catholic Univ Amer, Dept Phys, Greenbelt, MD 20771 USA. [Wang, T. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Goossens, M (reprint author), Katholieke Univ Leuven, Ctr Plasma Astrophys, B-3001 Louvain, Belgium. EM marcel.goossens@wis.kuleuven.be; inigo.arregui@uib.es; dfsjlb0@uib.es; wangtj@helio.gsfc.nasa.gov RI Arregui, Inigo/A-9992-2008; Ballester, Jose /A-2637-2011 OI Arregui, Inigo/0000-0002-7008-7661; Ballester, Jose /0000-0001-8921-9225 NR 28 TC 60 Z9 60 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 JUN PY 2008 VL 484 IS 3 BP 851 EP 857 DI 10.1051/0004-6361:200809728 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 310EG UT WOS:000256511100028 ER PT J AU Foschini, L Treves, A Tavecchio, F Impiombato, D Ghisellini, G Covino, S Tosti, G Gliozzi, M Bianchin, V Di Cocco, G Malaguti, G Maraschi, L Pian, E Raiteri, CM Sambruna, RM Tagliaferri, G Villata, M AF Foschini, L. Treves, A. Tavecchio, F. Impiombato, D. Ghisellini, G. Covino, S. Tosti, G. Gliozzi, M. Bianchin, V. Di Cocco, G. Malaguti, G. Maraschi, L. Pian, E. Raiteri, C. M. Sambruna, R. M. Tagliaferri, G. Villata, M. TI Infrared to X-ray observations of PKS 2155-304 in a low state SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : BL Lacertae objects : individual : PKS 2155-30; galaxies : BL Lacertae objects : general ID EXTRAGALACTIC BACKGROUND LIGHT; ACTIVE GALACTIC NUCLEI; PHOTON IMAGING CAMERA; BL LACERTAE OBJECT; XMM-NEWTON; SPECTRAL EVOLUTION; PKS 2155-304; TEV BLAZARS; BEPPOSAX; RADIATION AB Aims. Our goal is to understand the nature of blazars and the mechanisms for the generation of high-energy gamma-rays, through the investigation of the prototypical blazar PKS 2155-304, which shows complex behaviour. Methods. We analyze simultaneous infrared-to-X-ray observations obtained with XMM-Newton and REM on November 7, 2006, when the source was in a low X-ray state. We perform a comparative analysis of these results with those obtained from previous observations in different brightness states. Results. We found that the peak of the synchrotron emission moved from ultraviolet to optical wavelengths and the X-ray spectrum is best fit with a broken power law model with Gamma(2) similar to 2.4 harder than Gamma(1) similar to 2.6 and a break at about 3.5 keV. This suggests that the soft X-rays (E < 3.5 keV) are related to the high-energy tail of the synchrotron emission, while the hard X-rays (E > 3.5 keV) are from the energy region between the synchrotron and inverse-Compton humps. The different variability at energies below and above the break strengthens this hypothesis. Our results also stress the importance of monitoring this source at both low and high energies to better characterize its variability behaviour. C1 [Foschini, L.; Bianchin, V.; Di Cocco, G.; Malaguti, G.] IASF Bologna, INAF, I-40129 Bologna, Italy. [Treves, A.] Univ Insubria, Dipartimento Sci, I-22100 Como, Italy. [Tavecchio, F.; Ghisellini, G.; Covino, S.; Maraschi, L.; Tagliaferri, G.] Osserv Astron Brera, INAF, I-23807 Merate, Italy. [Impiombato, D.; Tosti, G.] Univ Perugia, Osservatorio Astron, I-06126 Perugia, Italy. [Gliozzi, M.] George Mason Univ, Fairfax, VA 22030 USA. [Pian, E.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. [Raiteri, C. M.; Villata, M.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy. [Sambruna, R. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Foschini, L (reprint author), IASF Bologna, INAF, Via Gobetti 101, I-40129 Bologna, Italy. EM foschini@iasfbo.inaf.it RI Foschini, Luigi/H-3833-2012; Tosti, Gino/E-9976-2013; OI Foschini, Luigi/0000-0001-8678-0324; Covino, Stefano/0000-0001-9078-5507; Tagliaferri, Gianpiero/0000-0003-0121-0723; Pian, Elena/0000-0001-8646-4858; Villata, Massimo/0000-0003-1743-6946; Malaguti, Giuseppe/0000-0001-9872-3378; Ghisellini, Gabriele/0000-0002-0037-1974; Raiteri, Claudia Maria/0000-0003-1784-2784 NR 35 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 JUN PY 2008 VL 484 IS 3 BP L35 EP L38 DI 10.1051/0004-6361:200809973 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 310EG UT WOS:000256511100005 ER PT J AU Gorjian, V Brodwin, M Kochanek, CS Murray, S Stern, D Brand, K Eisenhardt, PR Ashby, MLN Barmby, P Brown, MJI Dey, A Forman, W Jannuzi, BT Jones, C Kenter, AT Pahre, MA Shields, JC Werner, MW Willner, SP AF Gorjian, V. Brodwin, M. Kochanek, C. S. Murray, S. Stern, D. Brand, K. Eisenhardt, P. R. Ashby, M. L. N. Barmby, P. Brown, M. J. I. Dey, A. Forman, W. Jannuzi, B. T. Jones, C. Kenter, A. T. Pahre, M. A. Shields, J. C. Werner, M. W. Willner, S. P. TI The mid-infrared properties of X-ray sources SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : nuclei; galaxies : Seyfert; infrared : galaxies; X-rays : galaxies ID SPITZER-SPACE-TELESCOPE; SPECTRAL ENERGY-DISTRIBUTIONS; ACTIVE GALACTIC NUCLEI; INFRARED ARRAY CAMERA; LUMINOSITY FUNCTION; STAR POPULATIONS; SOURCE CATALOG; BOOTES FIELD; GALAXIES; COUNTERPARTS AB We combine the results of the Spitzer IRAC Shallow Survey and the Chandra XBootes Survey of the 8.5 deg(2) Bootes field of the NOAO Deep Wide- Field Survey to produce the largest comparison of mid-IR and X-ray sources to date. The comparison is limited to sources with X-ray fluxes > 8 x 10(-15) ergs cm(-2) s(-1) in the 0.5-7.0 keV range and mid-IR sources with 3.6 mu m fluxes brighter than 18.4 mag (12.3 mu Jy). In this most sensitive IRAC band, 85% of the 3086 X-ray sources have mid-IR counterparts at an 80% confidence level based on a Bayesian matching technique. Only 2.5% of the sample have no IRAC counterpart at all based on visual inspection. Even for a smaller but a significantly deeper Chandra survey in the same field, the IRAC Shallow Survey recovers most of the X-ray sources. A majority (65%) of the Chandra sources detected in all four IRAC bands occupy a well-defined region of IRAC [3.6] - [4.5] versus [5.8] - [8.0] color-color space. These X-ray sources are likely infrared-luminous, unobscured type I AGNs with little mid-infrared flux contributed by the AGN host galaxy. Of the remaining Chandra sources, most are lower luminosity type I and type II AGNs whose mid-IR emission is dominated by the host galaxy, while approximately 5% are either Galactic stars or very local galaxies. C1 [Gorjian, V.; Brodwin, M.; Stern, D.; Eisenhardt, P. R.; Werner, M. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kochanek, C. S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Murray, S.; Ashby, M. L. N.; Barmby, P.; Forman, W.; Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brand, K.; Dey, A.; Jannuzi, B. T.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Brown, M. J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Shields, J. C.] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. RP Gorjian, V (reprint author), CALTECH, Jet Prop Lab, MS 169-327,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM varoujan.gorjian@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 31 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 JUN 1 PY 2008 VL 679 IS 2 BP 1040 EP 1046 DI 10.1086/587431 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 307JP UT WOS:000256315500010 ER PT J AU Kraemer, SB Schmitt, HR Crenshaw, DM AF Kraemer, S. B. Schmitt, H. R. Crenshaw, D. M. TI Probing the ionization structure of the narrow-line region in the Seyfert 1 galaxy NGC 4151 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 4151); galaxies : Seyfert; line : formation ID ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; X-RAY-ABSORPTION; HOPKINS-ULTRAVIOLET-TELESCOPE; LONG-SLIT SPECTROSCOPY; NGC 4151; PHYSICAL CONDITIONS; RESOLVED SPECTROSCOPY; UV ABSORBERS; EMISSION AB We present a study of the distribution of [O III] lambda 5007 and [O II] lambda 3727 emission in the narrow-line region (NLR) of the Seyfert 1 galaxy NGC 4151. While the NLR of NGC 4151 exhibits an overall structure consistent with the unified model of Seyfert galaxies, narrowband [O III] and [O II] images obtained with the Wide Field and Planetary Camera 2 aboard the Hubble Space Telescope reveal significant emission from outside the emission-line bicone. The [O III]/[O II] ratios are lower in these regions, consistent with a weaker ionizing flux. We performed a photo-ionization modeling analysis of the emission-line gas within a series of annuli, centered on the central continuum source, with inner radii from 13 to 90 pc. The gas is ionized by radiation that has been attenuated by a relatively highly ionized absorber (HABS), which completely covers the central source, and a lower ionization absorber (LABS), which has a covering factor ranging from 0 to 1. We found that the [O III]/[O II] ratios are well fit by assuming that, within each segment of an annulus, some fraction of the NLR gas is completely within the shadow of LABS, while the rest is irradiated by the continuum filtered only by HABS. This suggests that the structure of the NLR is due to filtering of the ionizing radiation by ionized gas, consistent with disk-wind models. One possible scenario is that the low-ionization absorbers are dense knots of gas swept up by a wind. C1 [Kraemer, S. B.] Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Kraemer, S. B.] NASA, Goddard Space Flight Ctr, Div Sci, Greenbelt, MD 20771 USA. [Schmitt, H. R.] Naval Res Lab, Remote Sensing Div, Washington, DC 20375 USA. [Schmitt, H. R.] Interferometr Inc, Herndon, VA 20171 USA. [Crenshaw, D. M.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. RP Kraemer, SB (reprint author), Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. EM kraemer@yancey.gsfc.nasa.gov; henrique.schmitt@nrl.navy.mil; crenshaw@chara.gsu.edu NR 50 TC 26 Z9 26 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2008 VL 679 IS 2 BP 1128 EP 1143 DI 10.1086/587802 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 307JP UT WOS:000256315500013 ER PT J AU Desai, V Soifer, BT Dey, A Jannuzi, BT Le Floc'h, E Bian, C Brand, K Brown, MJI Armus, L Weedman, DW Cool, R Stern, D Brodwin, M AF Desai, Vandana Soifer, B. T. Dey, Arjun Jannuzi, Buell T. Le Floc'h, Emeric Bian, Chao Brand, Kate Brown, Michael J. I. Armus, Lee Weedman, Dan W. Cool, Richard Stern, Daniel Brodwin, Mark TI Redshift distribution of extragalactic 24 mu m sources SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : distances and redshifts; galaxies : evolution; galaxies : formation; infrared : galaxies ID ULTRALUMINOUS INFRARED GALAXIES; SPITZER-SPACE-TELESCOPE; STAR-FORMATION HISTORY; ACTIVE GALACTIC NUCLEI; HUBBLE DEEP FIELD; ULTRAVIOLET LUMINOSITY DENSITY; POLYCYCLIC AROMATIC-HYDROCARBON; BACKGROUND EXPERIMENT SEARCH; IRAC SHALLOW SURVEY; ARRAY CAMERA IRAC AB We present the redshift distribution of a complete, unbiased sample of 24 mu m sources down to f(nu)(24 mu m) 300 mu Jy ( 5 sigma). The sample consists of 591 sources detected in the Bootes field of the NOAO Deep Wide-Field Survey. We have obtained optical spectroscopic redshifts for 421 sources (71%). These have a redshift distribution peaking at z similar to 0: 3, with a possible additional peak at z similar to 0.9, and objects detected out to z = 4.5. The spectra of the remaining 170 (29%) exhibit no strong emission lines from which to determine a redshift. We develop an algorithm to estimate the redshift distribution of these sources, based on the assumption that they have emission lines but that these lines are not observable due to the limited wavelength coverage of our spectroscopic observations. The redshift distribution derived from all 591 sources exhibits an additional peak of extremely luminous (L8-1000 mu m > 3 x 10(12) L-circle dot) objects at z similar to 2, consisting primarily of sources without observable emission lines. We use optical line diagnostics and IRAC colors to estimate that 55% of the sources within this peak are AGN-dominated. We compare our results to published models of the evolution of infrared-luminous galaxies. The models which best reproduce our observations predict a large population of star-formation-dominated ULIRGs at z > 1.5 rather than the AGN-dominated sources we observe. C1 [Desai, Vandana] CALTECH, Div Phys Math & Astron, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Dey, Arjun; Jannuzi, Buell T.; Brand, Kate; Brodwin, Mark] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Le Floc'h, Emeric; Cool, Richard] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Le Floc'h, Emeric] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Brand, Kate] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Brown, Michael J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Weedman, Dan W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Desai, V (reprint author), CALTECH, Div Phys Math & Astron, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RI Brown, Michael/B-1181-2015 OI Brown, Michael/0000-0002-1207-9137 NR 100 TC 31 Z9 31 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2008 VL 679 IS 2 BP 1204 EP 1217 DI 10.1086/587637 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 307JP UT WOS:000256315500019 ER PT J AU Fukumura, K Kazanas, D AF Fukumura, Keigo Kazanas, Demosthenes TI Light echoes in Kerr geometry: A source of high-frequency QPOs from random X-ray bursts SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; stars : oscillations; X-rays : galaxies ID QUASI-PERIODIC OSCILLATIONS; ACCRETING BLACK-HOLES; MAGNETIC FLARES; GRO J1655-40; DISK; VARIABILITY; BINARIES; GRS-1915+105; DISCOVERY; MODEL AB We propose that high-frequency quasi-periodic oscillations (HFQPOs) can be produced from randomly formed X-ray bursts (flashes) by plasma interior to the ergosphere of a rapidly rotating black hole. We show by direct computation of their orbits that the photons comprising the observed X-ray light curves, if due to a multitude of such flashes, are significantly affected by the black hole's dragging of inertial frames; the photons of each such burst arrive to an observer at infinity in multiple (double or triple), distinct "bunches'' separated by a roughly constant time lag of Delta t(lag)/ M similar or equal to 14, regardless of the bursts' azimuthal position. We argue that every other such "bunch'' represents photons that follow trajectories with an additional orbit around the black hole at the photon circular orbit radius (a photon "echo''). The presence of this constant lag in the response function of the system leads to a QPO feature in its power density spectra, even though the corresponding light curve consists of a totally stochastic signal. This effect is by and large due to the black hole spin and is shown to gradually diminish as the spin parameter a decreases or the radial position of the burst moves outside the static limit surface (ergosphere). Our calculations indicate that for a black hole with Kerr parameter of a/M 0: 99 and mass of M 10 M-circle dot, the QPO is expected at a frequency of nu(QPO) similar to 1:3-1:4 kHz. We discuss the plausibility and observational implications of our model results, as well as its limitations. C1 [Fukumura, Keigo; Kazanas, Demosthenes] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Fukumura, K (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 663, Greenbelt, MD 20771 USA. EM Keigo.Fukumura@nasa.gov; Demos.Kazanas@nasa.gov NR 32 TC 8 Z9 8 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 JUN 1 PY 2008 VL 679 IS 2 BP 1413 EP 1421 DI 10.1086/587159 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 307JP UT WOS:000256315500035 ER PT J AU Ormel, CW Cuzzi, JN Tielens, AGGM AF Ormel, C. W. Cuzzi, J. N. Tielens, A. G. G. M. TI Co-accretion of chondrules and dust in the solar nebula SO ASTROPHYSICAL JOURNAL LA English DT Review DE planetary systems : formation; planetary systems : protoplanetary disks; solar system : formation ID UNEQUILIBRATED ORDINARY CHONDRITES; TURBULENT PROTOPLANETARY NEBULA; WEAKLY MAGNETIZED DISKS; LOCAL SHEAR INSTABILITY; FINE-GRAINED RIMS; PLANETESIMAL FORMATION; PREPLANETARY DUST; SIZED PARTICLES; AGGREGATE COLLISIONS; COMET 81P/WILD-2 AB We present a mechanism for chondrules to stick together by means of compaction of a porous dust rim they sweep up as they move through the dusty nebula gas. It is shown that dust aggregates formed out of micron-size grains stick to chondrules, forming a porous dust rim. When chondrules collide, this dust can be compacted by means of rolling motions within the porous dust layer. This mechanism dissipates the collisional energy, compacting the rim and allowing chondrules to stick. The structure of the obtained chondrule-dust agglomerates ( referred to as compounds) then consists of three phases: chondrules, porous dust, and dust that has been compacted by collisions. Subsequently, these compounds accrete their own dust and collide with other compounds. The evolution of the compound size distribution and the relative importance of the phases is calculated by a Monte Carlo code. Growth ends, and a simulation is terminated when all the dust in the compounds has been compacted. Numerous runs are performed, reflecting the uncertainty in the physical conditions at the chondrule formation time. It is found that compounds can grow by 1-2 orders of magnitudes in radius, up to dm sizes when turbulence levels are low. However, relative velocities associated with radial drift form a barrier for further growth. Earlier findings that the dust sweep-up by chondrules is proportional to their sizes are confirmed. We contrast two scenarios regarding how this dust evolved further toward the densely packed rims seen in chondrites. C1 [Ormel, C. W.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Cuzzi, J. N.; Tielens, A. G. G. M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Ormel, CW (reprint author), Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands. EM ormel@astro.rug.nl; jcuzzi@mail.arc.nasa.gov; atielens@mail.arc.nasa.gov NR 126 TC 36 Z9 36 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 JUN 1 PY 2008 VL 679 IS 2 BP 1588 EP 1610 DI 10.1086/587836 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 307JP UT WOS:000256315500053 ER PT J AU Djuric, N Smith, SJ Simcic, J Chutjian, A AF Djuric, N. Smith, S. J. Simcic, J. Chutjian, A. TI Absolute single and multiple charge exchange cross sections for highly charged C, N, and O ions colliding with CH4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic data; comets : general; solar wind ID X-RAY-EMISSION; ELECTRON-CAPTURE; COMET 9P/TEMPEL-1; DEEP IMPACT; COLLISIONS; ENCELADUS; SPECTRA; SYSTEM; ATOMS AB Absolute charge exchange (CE) cross sections have been measured for single and multiple exchanges between the highly charged ions (HCIs) Cq+ (q = 3-6), Nq+ (q = 4-7) and Oq+ (q = 5-7) colliding with the target methane (CH4) present in comet and planetary atmospheres. Measurements were made at collision energies of 7 x q keV (1.8-3.5 keV amu(-1)), representative of the fast component of the solar wind. The HCIs are produced in a 14 GHz electron cyclotron resonance ion source. Absolute cross sections are measured using the retarding potential analyzer method, with knowledge of the target length, density, and projectile currents. Comparison is made with results of the classical trajectory Monte Carlo method, and the classical overbarrier model. C1 [Djuric, N.; Smith, S. J.; Simcic, J.; Chutjian, A.] CALTECH, Jet Prop Lab, Atom & Mol Phys Grp, Pasadena, CA 91109 USA. RP Djuric, N (reprint author), CALTECH, Jet Prop Lab, Atom & Mol Phys Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 33 TC 9 Z9 9 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2008 VL 679 IS 2 BP 1661 EP 1664 DI 10.1086/587782 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 307JP UT WOS:000256315500059 ER PT J AU Leamon, RJ McIntosh, SW AF Leamon, Robert J. McIntosh, Scott W. TI Could we have forecast "The Day the Solar Wind Died"? SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE solar wind; Sun : magnetic fields ID MAGNETIC-FIELDS; CHROMOSPHERE; HELIOSPHERE; DISSIPATION AB In 1999 May an interval of unusually slow (< 300 km s(-1)) and rarefied (< 1 cm(-3))solar wind was observed upstream of Earth by the ACE spacecraft. The event has been dubbed "The Day the Solar Wind Died." We apply our solar wind forecast model to the interval in question, to ask whether we could have predicted the phenomenon. The model fails, but by the manner in which it fails, we support the conclusion that the rarefaction was caused by a suppression of coronal outflow from a region that earlier provided fast wind flow, possibly caused by a rapid restructuring of solar magnetic fields. C1 [Leamon, Robert J.] NASA, Goddard Space Flight Ctr, Adnet Syst Inc, Greenbelt, MD 20771 USA. [McIntosh, Scott W.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. RP Leamon, RJ (reprint author), NASA, Goddard Space Flight Ctr, Adnet Syst Inc, Code 6711, Greenbelt, MD 20771 USA. EM robert.j.leamon@nasa.gov NR 15 TC 0 Z9 0 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 1 PY 2008 VL 679 IS 2 BP L147 EP L150 DI 10.1086/589329 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 313DU UT WOS:000256722100022 ER PT J AU Strohmayer, TE AF Strohmayer, Tod E. TI High-resolution X-ray spectroscopy of RX J0806.3+1527 with Chandra SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries : close; gravitational waves; stars : individual (RX J0806.3+1527, V407 Vulpeculae); white dwarfs; X-rays : binaries ID SHORTEST PERIOD BINARY; AM CVN BINARIES; MASS-TRANSFER; SPIN-UP; RX-J0806.3+1527; V407-VUL; MODEL AB RX J0806.3+1527 is a candidate double-degenerate binary with possibly the shortest known orbital period. The source shows an approximate to 100% X-ray intensity modulation at the putative orbital period of 321.5 s, but there still is no direct detection of orbital motion at this period. Here we report the results of high-resolution X-ray spectroscopic observations of the source, obtained with the Chandra Low Energy Transmission Grating (LETG) spectrometer. We obtained a total of approximate to 80 ks of exposure in two pointings separated by about 5 months. We detect the source in both the zeroth-order image and the dispersed spectrum. Detection of the 321.5 s pulsations in the zeroth-order image allows us to extract dispersed spectra as a function of the pulse phase of the X-ray modulation. The bulk of the source flux appears in the 20-60 angstrom band. We find evidence for emission features in the 25-50 angstrom range. The strongest feature (detected at better than 3 sigma confidence) is an approximate to 0.6 angstrom-wide FWHM) emission line centered at 27 angstrom. Weaker features at 31.6 and 46.4 angstrom are also suggested, but they require confirmation with deeper exposures. The continuum is adequately A described by an absorbed blackbody model with a temperature of 65 +/- 5 eV and column depth of (2 +/- 0.5) x 10(20) cm(-2). Interestingly, the spectrum does not show strong emission lines of typically abundant elements such as carbon, nitrogen, oxygen, and neon. We briefly discuss possible identifications for the emission features. C1 NASAs Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Strohmayer, TE (reprint author), NASAs Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. EM stroh@clarence.gsfc.nasa.gov NR 22 TC 8 Z9 8 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 1 PY 2008 VL 679 IS 2 BP L109 EP L112 DI 10.1086/589439 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 313DU UT WOS:000256722100013 ER PT J AU Su, KYL Rieke, GH Stapelfeldt, KR Smith, PS Bryden, G Chen, CH Trilling, DE AF Su, K. Y. L. Rieke, G. H. Stapelfeldt, K. R. Smith, P. S. Bryden, G. Chen, C. H. Trilling, D. E. TI The exceptionally large debris disk around gamma Ophiuchi SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE circumstellar matter; infrared : stars; planetary systems; stars : individual (gamma Ophiuchi) ID MULTIBAND IMAGING PHOTOMETER; VEGA-LIKE STARS; SUN-LIKE STARS; ABSOLUTE CALIBRATION; SPITZER; DUST; EVOLUTION AB Spitzer images resolve the debris disk around gamma Ophiuchi at both 24 and 70 mu m. The resolved images suggest a disk radius of similar to 520 AU at 70 mu m and greater than or similar to 260 AU at 24 mu m. The images, along with a consistent fit to the spectral energy distribution of the disk from 20 to 350 mu m, show that the primary disk structure is inclined by similar to 50 degrees from the plane of the sky at a position angle of 55 +/- 2 degrees. Among a group of 12 debris disks that have similar host star spectral types, ages, and infrared fractional luminosities, the observed sizes in the infrared and color temperatures indicate that evolution of the debris disks is influenced by multiple parameters in addition to the protoplanetary disk initial mass. C1 [Su, K. Y. L.; Rieke, G. H.; Smith, P. S.; Trilling, D. E.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Stapelfeldt, K. R.; Bryden, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 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 NR 23 TC 20 Z9 20 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 1 PY 2008 VL 679 IS 2 BP L125 EP L129 DI 10.1086/589508 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 313DU UT WOS:000256722100017 ER PT J AU Turner, NJ Sano, T AF Turner, N. J. Sano, T. TI Dead zone accretion flows in protostellar disks SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE circumstellar matter; instabilities; MHD; solar system : formation; stars : formation ID 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS; WEAKLY MAGNETIZED DISKS; PRIMORDIAL SOLAR NEBULA; T-TAURI DISKS; PROTOPLANETARY DISKS; IONIZATION FRACTION; LAYERED ACCRETION; DUST COAGULATION; MIGRATION; FIELDS AB Planets form inside protostellar disks in a dead zone where the electrical resistivity of the gas is too high for magnetic forces to drive turbulence. We show that much of the dead zone nevertheless is active and flows toward the star while smooth, large-scale magnetic fields transfer the orbital angular momentum radially outward. Stellar X-ray and radionuclide ionization sustain a weak coupling of the dead zone gas to the magnetic fields, despite the rapid recombination of free charges on dust grains. Net radial magnetic fields are generated in the magneto-rotational turbulence in the electrically conducting top and bottom surface layers of the disk, and reach the midplane by ohmic diffusion. A toroidal component to the fields is produced near the midplane by the orbital shear. The process is similar to the magnetization of the solar tachocline. The result is a laminar, magnetically driven accretion flow in the region where the planets form. C1 [Turner, N. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Sano, T.] Osaka Univ, Inst Laser Engn, Suita, Osaka 5650871, Japan. RP Turner, NJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM neal.turner@jpl.nasa.gov; sano@ile.osaka-u.ac.jp RI Sano, Takayoshi/E-7860-2010; OI Turner, Neal/0000-0001-8292-1943 NR 37 TC 85 Z9 85 U1 1 U2 8 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 1 PY 2008 VL 679 IS 2 BP L131 EP L134 DI 10.1086/589540 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 313DU UT WOS:000256722100018 ER PT J AU Horner, DJ Perlman, ES Ebeling, H Jones, LR Scharf, CA Wegner, G Malkan, M Maughan, B AF Horner, Donald J. Perlman, Eric S. Ebeling, Harald Jones, Laurence R. Scharf, Caleb A. Wegner, Gary Malkan, Matthew Maughan, Ben TI The warps survey. VII. The warps-II cluster catalog SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; galaxies : clusters : general; surveys; X-rays : galaxies : clusters; X-rays : general ID LUMINOUS GALAXY CLUSTER; XMM-NEWTON OBSERVATION; HIGH-REDSHIFT CLUSTERS; ROSAT POINTED SURVEY; X-RAY-CLUSTERS; TEMPERATURE RELATION; CL J0152.7-1357; SHARC SURVEY; EVOLUTION; CHANDRA AB We present the galaxy cluster catalog from the second, larger phase of the Wide Angle ROSAT Pointed Survey ( WARPS), an X-ray selected survey for high-redshift galaxy clusters. WARPS is among the largest deep X-ray cluster surveys and is being used to study the properties and evolution of galaxy clusters. The WARPS-II sample contains 125 clusters serendipitously detected in a survey of 301 ROSAT PSPC pointed observations and covers a sky area of 56.7 deg(2). Of these 125 clusters, 53 have not been previously reported in the literature. We have nearly complete spectroscopic follow-up of the clusters, which range in redshift from z = 0.029 to z = 0.92 with a median redshift of z = 0.29 and find 59 clusters with z >= 0.3 (29 not previously reported in the literature) and 11 clusters with z >= 0.6 (6 not previously reported). We also define a statistically complete subsample of 102 clusters above a uniform flux limit of 6: 5 x 10(-14) ergs cm(-2) s(-1) (0.5-2.0 keV). Here we provide the cluster catalog and finder charts consisting of X-ray overlays on optical CCD images. We also compare our redshifts, fluxes, and detection methods to other similar published cluster surveys and find no serious issues with our measurements or completeness. C1 [Horner, Donald J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Perlman, Eric S.] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA. [Ebeling, Harald] Inst Astron, Honolulu, HI 96822 USA. [Jones, Laurence R.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Scharf, Caleb A.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Wegner, Gary] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. [Malkan, Matthew] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90024 USA. RP Horner, DJ (reprint author), NASA, Goddard Space Flight Ctr, Code 660-1, Greenbelt, MD 20771 USA. OI Perlman, Eric/0000-0002-3099-1664 NR 46 TC 23 Z9 23 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUN PY 2008 VL 176 IS 2 BP 374 EP 413 DI 10.1086/529494 PG 40 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 326PU UT WOS:000257672200004 ER PT J AU Carter, D Goudfrooij, P Mobasher, B Ferguson, HC Puzia, TH Aguerri, AL Balcells, M Batcheldor, D Bridges, TJ Davies, JI Erwin, P Graham, AW Guzman, R Hammer, D Hornschemeier, A Hoyos, C Hudson, MJ Huxor, A Jogee, S Komiyama, Y Lotz, J Lucey, JR Marzke, RO Merritt, D Miller, BW Miller, NA Mouhcine, M Okamura, S Peletier, RF Phillipps, S Poggianti, BM Sharples, RM Smith, RJ Trentham, N Tully, RB Valentijn, E Kleijn, GV AF Carter, David Goudfrooij, Paul Mobasher, Bahram Ferguson, Henry C. Puzia, Thomas H. Aguerri, Alfonso L. Balcells, Marc Batcheldor, Dan Bridges, Terry J. Davies, Jonathan I. Erwin, Peter Graham, Alister W. Guzman, Rafael Hammer, Derek Hornschemeier, Ann Hoyos, Carlos Hudson, Michael J. Huxor, Avon Jogee, Shardha Komiyama, Yutaka Lotz, Jennifer Lucey, John R. Marzke, Ronald O. Merritt, David Miller, Bryan W. Miller, Neal A. Mouhcine, Mustapha Okamura, Sadanori Peletier, Reynier F. Phillipps, Steven Poggianti, Bianca M. Sharples, Ray M. Smith, Russell J. Trentham, Neil Tully, R. Brent Valentijn, Edwin Kleijn, Gijs Verdoes TI The Hubble Space Telescope advanced camera for surveys coma cluster survey. I. Survey objectives and design SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Review DE galaxies : clusters : individual (Abell 1656); galaxies : fundamental parameters; galaxies : luminosity function, mass function; galaxies : photometry; galaxies : stellar content; galaxies : structure ID EARLY-TYPE GALAXIES; DWARF ELLIPTIC GALAXIES; SUPERMASSIVE BLACK-HOLES; FUNDAMENTAL-PLANE-SURVEY; EXTREME-ULTRAVIOLET EMISSION; SURFACE-BRIGHTNESS PROFILES; BRIGHTEST SPIRAL GALAXIES; COLOR MAGNITUDE RELATION; STELLAR MASS DENSITIES; DIGITAL SKY SURVEY AB We describe the HST ACS Coma Cluster Treasury survey, a deep two-passband imaging survey of one of the nearest rich clusters of galaxies, the Coma Cluster (Abell 1656). The survey was designed to cover an area of 740 arcmin(2) in regions of different density of both galaxies and intergalactic medium within the cluster. The ACS failure of 2007 January 27 leaves the survey 28% complete, with 21 ACS pointings (230 arcmin(2)) complete, and partial data for a further four pointings (44 arcmin(2)). The predicted survey depth for 10 sigma detections for optimal photometry of point sources is g' = 27.6 in the F475W filter and I-C = 26.8 mag in F814 (AB magnitudes). Initial simulations with artificially injected point sources show 90% recovered at magnitude limits of g' = 27.55 and I-C = 26.65. For extended sources, the predicted 10 sigma limits for a 1 arcsec(2) region are g' = 25.8 mag arcsec(-2) and I-C = 25.0 mag arcsec(-2). We highlight several motivating science goals of the survey, including study of the faint end of the cluster galaxy luminosity function, structural parameters of dwarf galaxies, stellar populations and their effect on colors and color gradients, evolution of morphological components in a dense environment, the nature of ultracompact dwarf galaxies, and globular cluster populations of cluster galaxies of a range of luminosities and types. This survey will also provide a local rich cluster benchmark for various well-known global scaling relations and explore new relations pertaining to the nuclear properties of galaxies. C1 [Carter, David; Mouhcine, Mustapha] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Goudfrooij, Paul; Mobasher, Bahram; Ferguson, Henry C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Puzia, Thomas H.] Natl Res Council Canada, Herzberg Inst Astrophys, Dominion Astrophys Observ, Victoria, BC V9E 2E7, Canada. [Aguerri, Alfonso L.; Balcells, Marc] Inst Astrofis Canarias, Tenerife 38200, Spain. [Batcheldor, Dan; Merritt, David] Rochester Inst Technol, Dept Phys, Rochester, NY 14623 USA. [Bridges, Terry J.] Queens Univ, Dept Phys Engn Phys & Astron, Kingston, ON K7L 3N6, Canada. [Davies, Jonathan I.] Cardiff Univ, Sch Phys & Astron, The Parade, Cardiff CF24 3YB, S Glam, Wales. [Erwin, Peter] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Erwin, Peter] Univ Sternwarte, D-81679 Munich, Germany. [Graham, Alister W.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, VIC 3122, Australia. [Guzman, Rafael; Hoyos, Carlos] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Hammer, Derek; Miller, Neal A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Hornschemeier, Ann] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA. [Hoyos, Carlos] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain. [Hudson, Michael J.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Huxor, Avon; Phillipps, Steven] Univ Bristol, Astrophys Grp, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Jogee, Shardha] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Komiyama, Yutaka] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Lotz, Jennifer] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Lucey, John R.; Sharples, Ray M.; Smith, Russell J.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Marzke, Ronald O.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. [Miller, Bryan W.] Gemini Observ, La Serena, Chile. [Okamura, Sadanori] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Peletier, Reynier F.; Valentijn, Edwin; Kleijn, Gijs Verdoes] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Poggianti, Bianca M.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy. [Trentham, Neil] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Tully, R. Brent] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Carter, D (reprint author), Liverpool John Moores Univ, Astrophys Res Inst, Twelve Quays House, Birkenhead CH41 1LD, Merseyside, England. RI Peletier, Reynier/B-9633-2012; Hudson, Michael/H-3238-2012; Graham, Alister/G-1217-2013; Sharples, Ray/N-7309-2013; OI Hudson, Michael/0000-0002-1437-3786; Graham, Alister/0000-0002-6496-9414; Sharples, Ray/0000-0003-3449-8583; Batcheldor, Daniel/0000-0002-8588-5682; De Hoyos Fernandez De Cordova, Carlos/0000-0003-3120-6856; Erwin, Peter/0000-0003-4588-9555 NR 208 TC 53 Z9 54 U1 0 U2 5 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 JUN PY 2008 VL 176 IS 2 BP 424 EP 437 DI 10.1086/533439 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 326PU UT WOS:000257672200006 ER EF