FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Wong, T Hughes, A Fukui, Y Kawamura, A Mizuno, N Ott, J Muller, E Pineda, JL Welty, DE Kim, S Mizuno, Y Murai, M Onishi, T AF Wong, T. Hughes, A. Fukui, Y. Kawamura, A. Mizuno, N. Ott, J. Muller, E. Pineda, J. L. Welty, D. E. Kim, S. Mizuno, Y. Murai, M. Onishi, T. TI MOLECULAR AND ATOMIC GAS IN THE LARGE MAGELLANIC CLOUD. I. CONDITIONS FOR CO DETECTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: ISM; ISM: molecules; Magellanic Clouds ID STAR-FORMATION; H-I; INTERSTELLAR CLOUDS; SPIRAL GALAXIES; GRAVITATIONAL-INSTABILITY; APERTURE SYNTHESIS; RAPID FORMATION; SPITZER SURVEY; HYDROGEN; LMC AB We analyze the conditions for detection of CO(1-0) emission in the Large Magellanic Cloud, using the recently completed second NANTEN CO survey. In particular, we investigate correlations between CO integrated intensity and H I integrated intensity, peak brightness temperature, and line width at a resolution of 2'.6 (similar to 40 pc). We find that significant H I column density (exceeding similar to 10(21) cm(-2)) and peak brightness temperature (exceeding similar to 20 K) are necessary but not sufficient conditions for CO detection, with many regions of strong H I emission not associated with molecular clouds. The large scatter in CO intensities for a given H I intensity persists even when averaging on scales of > 200 pc, indicating that the scatter is not solely due to local conversion of H I into H(2) near GMCs. We focus on two possibilities to account for this scatter: either there exist spatial variations in the I(CO) to N(H(2)) conversion factor, or a significant fraction of the atomic gas is not involved in molecular cloud formation. A weak tendency for CO emission to be suppressed for large H I linewidths supports the second hypothesis, insofar as large linewidths may be indicative of warm H I, and calls into question the likelihood of forming molecular clouds from colliding H I flows. We also find that the ratio of molecular to atomic gas shows no significant correlation (or anticorrelation) with the stellar surface density, though a correlation with midplane hydrostatic pressure P(h) is found when the data are binned in P(h). The latter correlation largely reflects the increasing likelihood of CO detection at high H I column density. C1 [Wong, T.; Welty, D. E.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Wong, T.; Hughes, A.; Muller, E.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Hughes, A.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Fukui, Y.; Kawamura, A.; Mizuno, N.; Muller, E.; Mizuno, Y.; Murai, M.; Onishi, T.] Nagoya Univ, Dept Phys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Mizuno, N.] Natl Astron Observ Japan, ALMA J Project Off, Tokyo 1818588, Japan. [Ott, J.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Ott, J.] CALTECH, Caltech Astron, Pasadena, CA 91125 USA. [Pineda, J. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kim, S.] Sejong Univ, Dept Astron & Space Sci, Seoul 143747, South Korea. RP Wong, T (reprint author), Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. EM wongt@astro.uiuc.edu FU ATNF; Nagoya University; University of Illinois; NRAO; NASA; Korea Science and Engineering Foundation (KOSEF); Astrophysical Research Center of the Structure and Evolution of the Cosmos (ARCSEC) FX We thank Robert Gruendl for providing the stellar surface density image and Lister Staveley-Smith for providing the Hi data cube for analysis. The survival analysis used in this study was performed with the ASURV software provided by the Penn State Center for Astrostatistics. T.W. acknowledges support from the ATNF and Nagoya University during the early stages of this project, and support from the University of Illinois during its completion. J.O. acknowledges support from NRAO, which is operated by Associated Universities, Inc., under cooperative agreement with the National Science Foundation. J.L.P. was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. S.K. was supported in part by the Korea Science and Engineering Foundation (KOSEF) under a cooperative agreement with the Astrophysical Research Center of the Structure and Evolution of the Cosmos (ARCSEC). We thank the referee for a detailed report which led to significant improvement and clarification of the text and figures. NR 67 TC 26 Z9 26 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2009 VL 696 IS 1 BP 370 EP 384 DI 10.1088/0004-637X/696/1/370 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 435NH UT WOS:000265350100033 ER PT J AU Hildebrand, RH Kirby, L Dotson, JL Houde, M Vaillancourt, JE AF Hildebrand, Roger H. Kirby, Larry Dotson, Jessie L. Houde, Martin Vaillancourt, John E. TI DISPERSION OF MAGNETIC FIELDS IN MOLECULAR CLOUDS. I SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: magnetic fields; polarization; turbulence ID STAR-FORMING REGIONS; LARGE-SCALE STRUCTURE; POLARIZATION; POLARIMETRY; TURBULENCE; CORES; FLUCTUATIONS; STRENGTHS; VELOCITY; DENSITY AB We describe a method for determining the dispersion of magnetic field vectors about large-scale fields in turbulent molecular clouds. The method is designed to avoid inaccurate estimates of magnetohydrodynamic or turbulent dispersion-and help avoiding inaccurate estimates of field strengths-due to a large-scale, nonturbulent field structure when using the well known method of Chandrasekhar and Fermi. Our method also provides accurate, independent estimates of the turbulent to large-scale magnetic field strength ratio. We discuss applications to the molecular clouds OMC-1, M17, and DR21(Main). C1 [Hildebrand, Roger H.; Kirby, Larry] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Hildebrand, Roger H.; Kirby, Larry] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Hildebrand, Roger H.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Dotson, Jessie L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Houde, Martin] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Vaillancourt, John E.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. RP Hildebrand, RH (reprint author), Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. FU NSF [AST 05-05230, AST 02-41356, AST 05-05124]; Department of Astronomy; Astrophysics of the University of Chicago; NSERC; Canada Research Chair; Canada Foundation for Innovation; Ontario Innovation Trust; Western's Academic Development Fund; CSO [AST 05-40882] FX We thank Shantanu Basu for helpful discussions. This work has been supported in part by NSF grants AST 05-05230, AST 02-41356, and AST 05-05124. L. K. acknowledges support from the Department of Astronomy and Astrophysics of the University of Chicago. M.H.' s research is funded through the NSERC Discovery Grant, Canada Research Chair, Canada Foundation for Innovation, Ontario Innovation Trust, and Western's Academic Development Fund programs. J.E.V. acknowledges support from the CSO, which is funded through NSF AST 05-40882. NR 33 TC 77 Z9 77 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2009 VL 696 IS 1 BP 567 EP 573 DI 10.1088/0004-637X/696/1/567 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 435NH UT WOS:000265350100045 ER PT J AU Stritzinger, M Mazzali, P Phillips, MM Immler, S Soderberg, A Sollerman, J Boldt, L Braithwaite, J Brown, P Burns, CR Contreras, C Covarrubias, R Folatelli, G Freedman, WL Gonzalez, S Hamuy, M Krzeminski, W Madore, BF Milne, P Morrell, N Persson, SE Roth, M Smith, M Suntzeff, NB AF Stritzinger, Maximilian Mazzali, Paolo Phillips, Mark M. Immler, Stefan Soderberg, Alicia Sollerman, Jesper Boldt, Luis Braithwaite, Jonathan Brown, Peter Burns, Christopher R. Contreras, Carlos Covarrubias, Ricardo Folatelli, Gaston Freedman, Wendy L. Gonzalez, Sergio Hamuy, Mario Krzeminski, Wojtek Madore, Barry F. Milne, Peter Morrell, Nidia Persson, S. E. Roth, Miguel Smith, Mathew Suntzeff, Nicholas B. TI THE HE-RICH CORE-COLLAPSE SUPERNOVA 2007Y: OBSERVATIONS FROM X-RAY TO RADIO WAVELENGTHS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 1187); supernovae: general; supernovae: individual (SN 2007Y) ID 25 APRIL 1998; IB SUPERNOVA; LIGHT CURVES; CIRCUMSTELLAR INTERACTION; STANDARD STARS; NEUTRON-STAR; SN 1993J; PHOTOMETRIC CALIBRATION; OPTICAL SPECTROSCOPY; UBVRI PHOTOMETRY AB A detailed study spanning approximately a year has been conducted on the Type Ib supernova (SN) 2007Y. Imaging was obtained from X-ray to radio wavelengths, and a comprehensive set of multi-band (w2m2w1u'g'r'i'UBVYJHK(s)) light curves and optical spectroscopy is presented. A virtually complete bolometric light curve is derived, from which we infer a (56)Ni mass of 0.06 M(circle dot). The early spectrum strongly resembles SN 2005bf and exhibits high- velocity features of Ca II and H alpha; during late epochs the spectrum shows evidence of an ejecta-wind interaction. Nebular emission lines have similar widths and exhibit profiles that indicate a lack of major asymmetry in the ejecta. Late phase spectra are modeled with a non-LTE code, from which we find (56)Ni, O, and total-ejecta masses (excluding He) to be 0.06, 0.2, and 0.42 M(circle dot), respectively, below 4500 km s(-1). The (56)Ni mass confirms results obtained from the bolometric light curve. The oxygen abundance suggests that the progenitor was most likely a approximate to 3.3 M(circle dot) He core star that evolved from a zero-age-main-sequence mass of 10-13 M(circle dot). The explosion energy is determined to be approximate to 10(50) erg, and the mass-loss rate of the progenitor is constrained from X-ray and radio observations to be less than or similar to 10(-6) M(circle dot) yr(-1). SN 2007Y is among the least energetic normal Type Ib SNe ever studied. C1 [Stritzinger, Maximilian; Phillips, Mark M.; Boldt, Luis; Contreras, Carlos; Covarrubias, Ricardo; Gonzalez, Sergio; Krzeminski, Wojtek; Morrell, Nidia; Roth, Miguel] Carnegie Observ, Las Campanas Observ, La Serena, Chile. [Stritzinger, Maximilian; Sollerman, Jesper] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [Mazzali, Paolo] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Mazzali, Paolo] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Immler, Stefan] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, XrayAstrophys Lab, Greenbelt, MD 20771 USA. [Immler, Stefan] Univ Space Res Assoc, Columbia, MD 21044 USA. [Soderberg, Alicia] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Soderberg, Alicia] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sollerman, Jesper] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Braithwaite, Jonathan] Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Brown, Peter] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Burns, Christopher R.; Freedman, Wendy L.; Madore, Barry F.; Persson, S. E.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Folatelli, Gaston; Hamuy, Mario] Univ Chile, Dept Astron, Santiago, Chile. [Madore, Barry F.] CALTECH, Jet Prop Lab, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Milne, Peter] Univ Arizona, Dept Astron & Steward Observ, Tucson, AZ 85721 USA. [Smith, Mathew] Univ Cape Town, Cosmol & Grav Grp, Dept Math & Appl Math, ZA-7700 Rondebosch, South Africa. [Suntzeff, Nicholas B.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. RP Stritzinger, M (reprint author), Carnegie Observ, Las Campanas Observ, Casilla 601, La Serena, Chile. EM mstritzinger@lco.cl; mazzali@mpa-garching.mpg.de; mmp@lco.cl; stefan.m.immler@nasa.gov; alicia@astro.princeton.edu; jesper@dark-cosmology.dk; lboldt@lco.cl; jon@cita.utoronto.ca; pbrown@astro.psu.edu; cburns@ociw.edu; ccontreras@lco.cl; ricardo@lco.cl; gaston@das.uchile.cl; wendy@ociw.edu; sgonzalez@lco.cl; mhamuy@das.uchile.cl; wojtek@lco.cl; barry@ociw.edu; pmilne@as.asrizona.edu; nmorrell@lco.cl; persson@ociw.edu; miguel@lco.cl; mathew.smith@uct.ac.za; nsuntzeff@tamu.edu RI Folatelli, Gaston/A-4484-2011; Hamuy, Mario/G-7541-2016; OI Sollerman, Jesper/0000-0003-1546-6615; stritzinger, maximilian/0000-0002-5571-1833 NR 97 TC 54 Z9 54 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2009 VL 696 IS 1 BP 713 EP 728 DI 10.1088/0004-637X/696/1/713 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 435NH UT WOS:000265350100061 ER PT J AU Patsourakos, S Klimchuk, JA AF Patsourakos, S. Klimchuk, J. A. TI SPECTROSCOPIC OBSERVATIONS OF HOT LINES CONSTRAINING CORONAL HEATING IN SOLAR ACTIVE REGIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona ID EUV IMAGING SPECTROMETER; X-RAY; EMISSION-LINES; LOOP OBSERVATIONS; ATOMIC DATABASE; HINODE; PLASMA; DIAGNOSTICS; FIELD; TEMPERATURE AB Extreme-ultraviolet observations of warm coronal loops suggest that they are bundles of unresolved strands that are heated impulsively to high temperatures by nanoflares. The plasma would then have the observed properties ( e. g., excess density compared with static equilibrium) when it cools into the 1-2MK range. If this interpretation is correct, then very hot emission should be present outside of proper flares. It is predicted to be very faint, however. A critical element for proving or refuting this hypothesis is the existence of hot, yet faint plasmas which should be at amounts predicted by impulsive heating models. We report on the first comprehensive spectroscopic study of hot plasmas in active regions (ARs). Data from the Extreme- ultraviolet Imaging Spectrometer on Hinode were used to construct emission measure (EM) distributions in quiescent ARs in the 1-5MK temperature range. The distributions are flat or slowly increasing up to approximately 3MK and then fall off rapidly at higher temperatures. We show that AR models based on impulsive heating can reproduce the observed EM distributions relatively well. Our results provide strong new evidence that coronal heating is impulsive in nature. C1 [Patsourakos, S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Patsourakos, S.] George Mason Univ, Ctr Earth Observing & Space Res, Inst Computat Sci, Coll Sci, Fairfax, VA 22030 USA. [Klimchuk, J. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Patsourakos, S (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. RI Klimchuk, James/D-1041-2012 OI Klimchuk, James/0000-0003-2255-0305 FU NASA Hinode and LWS programs FX Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with ESA and NSC ( Norway). This work was supported by the NASA Hinode and LWS programs. We wish to thank H. Warren, I. Ugarte Urra, U. Feldman, C. Brown, E. Robbrecht, G. Doscheck J.-F. Hochedez, and J. Mariska for helpful discussions. We acknowledge useful discussions with the members of the ISSI team "The Role of Spectroscopic and Imaging Data in Understanding Coronal Heating" ( team Parenti). NR 41 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 MAY 1 PY 2009 VL 696 IS 1 BP 760 EP 765 DI 10.1088/0004-637X/696/1/760 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 435NH UT WOS:000265350100065 ER PT J AU Hickox, RC Jones, C Forman, WR Murray, SS Kochanek, CS Eisenstein, D Jannuzi, BT Dey, A Brown, MJI Stern, D Eisenhardt, PR Gorjian, V Brodwin, M Narayan, R Cool, RJ Kenter, A Caldwell, N Anderson, ME AF Hickox, Ryan C. Jones, Christine Forman, William R. Murray, Stephen S. Kochanek, Christopher S. Eisenstein, Daniel Jannuzi, Buell T. Dey, Arjun Brown, Michael J. I. Stern, Daniel Eisenhardt, Peter R. Gorjian, Varoujan Brodwin, Mark Narayan, Ramesh Cool, Richard J. Kenter, Almus Caldwell, Nelson Anderson, Michael E. TI HOST GALAXIES, CLUSTERING, EDDINGTON RATIOS, AND EVOLUTION OF RADIO, X-RAY, AND INFRARED-SELECTED AGNs SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies: active; large-scale structure of universe; quasars: general; radio continuum: galaxies; surveys; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; SUPERMASSIVE BLACK-HOLES; DEEP FIELD-SOUTH; QUASAR LUMINOSITY FUNCTION; STAR-FORMATION HISTORY; DARK-MATTER HALOES; ADVECTION-DOMINATED ACCRETION; COLOR-MAGNITUDE RELATION; IRAC SHALLOW SURVEY AB We explore the connection between different classes of active galactic nuclei (AGNs) and the evolution of their host galaxies, by deriving host galaxy properties, clustering, and Eddington ratios of AGNs selected in the radio, Xray, and infrared (IR) wavebands. We study a sample of 585 AGNs at 0.25 < z < 0.8 using redshifts from the AGN and Galaxy Evolution Survey ( AGES). We select AGNs with observations in the radio at 1.4 GHz from the Westerbork Synthesis Radio Telescope, X-rays from the Chandra XBootes Survey, and mid-IR from the Spitzer IRAC Shallow Survey. The radio, X-ray, and IR AGN samples show only modest overlap, indicating that to the flux limits of the survey, they represent largely distinct classes of AGNs. We derive host galaxy colors and luminosities, as well as Eddington ratios, for obscured or optically faint AGNs. We also measure the two-point cross-correlation between AGNs and galaxies on scales of 0.3-10 h(-1) Mpc, and derive typical dark matter halo masses. We find that: (1) radio AGNs are mainly found in luminous red sequence galaxies, are strongly clustered (with M(halo) similar to 3 x 10(13) h(-1) M(circle dot)), and have very low Eddington ratios lambda less than or similar to 10(-3); (2) X-ray-selected AGNs are preferentially found in galaxies that lie in the "green valley" of color-magnitude space and are clustered similar to the typical AGES galaxies (M(halo) similar to 10(13) h(-1) M(circle dot)), with 10(-3) less than or similar to lambda less than or similar to 1; (3) IR AGNs reside in slightly bluer, slightly less luminous galaxies than X-ray AGNs, are weakly clustered (M(halo) less than or similar to 10(12)h(-1) M(circle dot)), and have lambda > 10(-2). We interpret these results in terms of a simple model of AGN and galaxy evolution, whereby a "quasar" phase and the growth of the stellar bulge occurs when a galaxy's dark matter halo reaches a critical mass between similar to 10(12) and 10(13) M(circle dot). After this event, star formation ceases and AGN accretion shifts from radiatively efficient (optical- and IR-bright) to radiatively inefficient ( optically faint, radio-bright) modes. C1 [Hickox, Ryan C.; Jones, Christine; Forman, William R.; Murray, Stephen S.; Brodwin, Mark; Narayan, Ramesh; Kenter, Almus; Caldwell, Nelson; Anderson, Michael E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kochanek, Christopher S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Kochanek, Christopher S.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Eisenstein, Daniel] Steward Observ, Tucson, AZ 85721 USA. [Jannuzi, Buell T.; Dey, Arjun; Brodwin, Mark] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Brown, Michael J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Stern, Daniel; Eisenhardt, Peter R.; Gorjian, Varoujan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cool, Richard J.] Princeton Univ Observ, Princeton, NJ 08544 USA. [Anderson, Michael E.] CALTECH, Dept Astron, Pasadena, CA 91109 USA. RP Hickox, RC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rhickox@cfa.harvard.edu RI Brown, Michael/B-1181-2015; OI Brown, Michael/0000-0002-1207-9137; Narayan, Ramesh/0000-0002-1919-2730 NR 209 TC 227 Z9 227 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2009 VL 696 IS 1 BP 891 EP 919 DI 10.1088/0004-637X/696/1/891 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 435NH UT WOS:000265350100075 ER PT J AU Cieza, LA Padgett, DL Allen, LE McCabe, CE Brooke, TY Carey, SJ Chapman, NL Fukagawa, M Huard, TL Noriga-Crespo, A Peterson, DE Rebull, LM AF Cieza, Lucas A. Padgett, Deborah L. Allen, Lori E. McCabe, Caer E. Brooke, Timothy Y. Carey, Sean J. Chapman, Nicholas L. Fukagawa, Misato Huard, Tracy L. Noriga-Crespo, Alberto Peterson, Dawn E. Rebull, Luisa M. TI PRIMORDIAL CIRCUMSTELLAR DISKS IN BINARY SYSTEMS: EVIDENCE FOR REDUCED LIFETIMES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries: general; circumstellar matter; infrared: stars; planetary systems: protoplanetary disks; stars: pre-main sequence ID T-TAURI STARS; GIANT PLANET FORMATION; SPITZER C2D SURVEY; FORMING REGIONS; YOUNG STARS; PROTOPLANETARY DISKS; CORONAE-AUSTRALIS; IMAGING SURVEY; CHAMELEON-I; MULTIPLICITY AB We combine the results from several multiplicity surveys of pre-main-sequence stars located in four nearby star-forming regions with Spitzer data from three different Legacy Projects. This allows us to construct a sample of 349 targets, including 125 binaries, which we use to to investigate the effect of companions on the evolution of circumstellar disks. We find that the distribution of projected separations of systems with Spitzer excesses is significantly different (P similar to 2.4e-5, according to the K-S test for binaries with separations less than 400AU) from that of systems lacking evidence for a disk. As expected, systems with projected separations less than 40AU are half as likely to retain at least one disk than are systems with projected separations in the 40-400 AU range. These results represent the first statistically significant evidence for a correlation between binary separation and the presence of an inner disk (r similar to 1AU). Several factors (e. g., the incompleteness of the census of close binaries, the use of unresolved disk indicators, and projection effects) have previously masked this correlation in smaller samples. We discuss the implications of our findings for circumstellar disk lifetimes and the formation of planets in multiple systems. C1 [Cieza, Lucas A.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Padgett, Deborah L.; McCabe, Caer E.; Brooke, Timothy Y.; Carey, Sean J.; Noriga-Crespo, Alberto; Rebull, Luisa M.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Allen, Lori E.; Peterson, Dawn E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chapman, Nicholas L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Fukagawa, Misato] Osaka Univ, Osaka 5600043, Japan. [Huard, Tracy L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Cieza, LA (reprint author), Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. EM lcieza@ifa.hawaii.edu OI Rebull, Luisa/0000-0001-6381-515X FU NASA through the Spitzer Fellowship Program FX We thank Jonathan Williams, Jonathan Swift, Michael Liu, and the anonymous referee for their valuable comments. Support for this work was provided by NASA through the Spitzer Fellowship Program under an award from Caltech. This work makes use of data obtained with the Spitzer Space Telescope, which is operated by JPL/Caltech, under a contract with NASA. NR 45 TC 63 Z9 63 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAY 1 PY 2009 VL 696 IS 1 BP L84 EP L88 DI 10.1088/0004-637X/696/1/L84 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 434CP UT WOS:000265253100020 ER PT J AU Kovalev, YY Aller, HD Aller, MF Homan, DC Kadler, M Kellermann, KI Kovalev, YA Lister, ML McCormick, MJ Pushkarev, AB Ros, E Zensus, JA AF Kovalev, Y. Y. Aller, H. D. Aller, M. F. Homan, D. C. Kadler, M. Kellermann, K. I. Kovalev, Yu. A. Lister, M. L. McCormick, M. J. Pushkarev, A. B. Ros, E. Zensus, J. A. TI THE RELATION BETWEEN AGN GAMMA-RAY EMISSION AND PARSEC-SCALE RADIO JETS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: jets; radio continuum: galaxies ID ACTIVE GALACTIC NUCLEI; BLAZARS; QUASARS; OBJECTS; MOJAVE; IMAGES; MODEL AB We have compared the radio emission from a sample of parsec-scale active galactic nucleus (AGN) jets as measured by the VLBA at 15 GHz, with their associated. gamma-ray properties that are reported in the Fermi Large Area Telescope (LAT) three month bright source list. We find in our radio-selected sample that the. gamma-ray photon flux correlates well with the quasi-simultaneously measured compact radio flux density. The LAT-detected jets in our radio-selected complete sample generally have higher compact radio flux densities, and their parsec-scale cores are brighter (i.e., have higher brightness temperature) than the jets in the LAT nondetected objects. This suggests that the jets of bright. gamma-ray AGN have preferentially higher Doppler-boosting factors. In addition, AGN jets tend to be found in a more active radio state within several months from LAT-detection of their strong. gamma-ray emission. This result becomes more pronounced for confirmed. gamma-ray flaring sources. We identify the parsec-scale radio core as a likely location for both the. gamma-ray and radio flares, which appear within typical timescales of up to a few months of each other. C1 [Kovalev, Y. Y.; Pushkarev, A. B.; Ros, E.; Zensus, J. A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Kovalev, Y. Y.; Kovalev, Yu. A.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [Aller, H. D.; Aller, M. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Homan, D. C.; McCormick, M. J.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Kadler, M.] Univ Erlangen Nurnberg, Dr Remeis Sternwarte Bamberg, D-96049 Bamberg, Germany. [Kadler, M.] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany. [Kadler, M.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Kadler, M.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Kellermann, K. I.; Zensus, J. A.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Lister, M. L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Pushkarev, A. B.] Pulkovo Observ, St Petersburg 196140, Russia. [Pushkarev, A. B.] Crimean Astrophys Observ, UA-98409 Nauchnyi, Crimea, Ukraine. [Ros, E.] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain. RP Kovalev, YY (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM ykovalev@mpifr.de; haller@umich.edu; mfa@umich.edu; homand@denison.edu; matthias.kadler@sternwarte.uni-erlangen.de; kkellerm@nrao.edu; mlister@purdue.edu; mccorm_m@denison.edu; apushkar@mpifr.de; ros@mpifr.de; azensus@mpifr.de RI Kovalev, Yuri/J-5671-2013; Kovalev, Yuri/N-1053-2015; Pushkarev, Alexander/M-9997-2015; OI Kovalev, Yuri/0000-0001-9303-3263; Ros, Eduardo/0000-0001-9503-4892; Kadler, Matthias/0000-0001-5606-6154 NR 28 TC 101 Z9 102 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAY 1 PY 2009 VL 696 IS 1 BP L17 EP L21 DI 10.1088/0004-637X/696/1/L17 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 434CP UT WOS:000265253100005 ER PT J AU Lister, ML Homan, DC Kadler, M Kellermann, KI Kovalev, YY Ros, E Savolainen, T Zensus, JA AF Lister, M. L. Homan, D. C. Kadler, M. Kellermann, K. I. Kovalev, Y. Y. Ros, E. Savolainen, T. Zensus, J. A. TI A CONNECTION BETWEEN APPARENT VLBA JET SPEEDS AND INITIAL ACTIVE GALACTIC NUCLEUS DETECTIONS MADE BY THE FERMI GAMMA-RAY OBSERVATORY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE BL Lacertae objects: general; galaxies: active; galaxies: jets; gamma rays: observations; quasars: general; radio continuum: galaxies ID LINE ARRAY OBSERVATIONS; FLUX-LIMITED SAMPLES; BL LACERTAE OBJECTS; EGRET CATALOG; QUASARS; BLAZARS; VARIABILITY; MULTIEPOCH; MOJAVE; IMAGES AB In its first three months of operations, the Fermi Gamma-Ray Observatory has detected approximately one quarter of the radio-flux-limited MOJAVE sample of bright flat-spectrum active galactic nuclei (AGNs) at energies above 100 MeV. We have investigated the apparent parsec-scale jet speeds of 26 MOJAVE AGNs measured by the Very Long Baseline Array (VLBA) that are in the LAT bright AGN sample ( LBAS). We find that the. gamma-ray bright quasars have faster jets on average than the non-LBAS quasars, with a median of 15c, and values ranging up to 34c. The LBAS AGNs in which the LAT has detected significant. gamma-ray flux variability generally have faster jets than the nonvariable ones. These findings are in overall agreement with earlier results based on nonuniform EGRET data which suggested that. gamma-ray bright AGNs have preferentially higher Doppler boosting factors than other blazar jets. However, the relatively low LAT detection rates for the full MOJAVE sample (24%) and previously known MOJAVE EGRET-detected blazars (43%) imply that Doppler boosting is not the sole factor that determines whether a particular AGN is bright at. gamma-ray energies. The slower apparent jet speeds of LBAS BL Lac objects and their higher overall LAT detection rate as compared to quasars suggest that the former are being detected by Fermi because of their higher intrinsic (unbeamed). gamma-ray to radio luminosity ratios. C1 [Lister, M. L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Homan, D. C.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Kadler, M.] Univ Erlangen Nurnberg, Dr Remeis Sternwarte Bamberg, D-96049 Bamberg, Germany. [Kadler, M.] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany. [Kadler, M.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Kadler, M.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Kellermann, K. I.; Zensus, J. A.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Kovalev, Y. Y.; Ros, E.; Savolainen, T.; Zensus, J. A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Kovalev, Y. Y.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [Ros, E.] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain. RP Lister, ML (reprint author), Purdue Univ, Dept Phys, 525 NW Ave, W Lafayette, IN 47907 USA. EM mlister@purdue.edu; homand@denison.edu; matthias.kadler@sternwarte.uni-erlangen.de; kkellerm@nrao.edu; ykovalev@mpifr.de; ros@mpifr.de; tsavolainen@mpifr.de; azensus@mpifr.de RI Kovalev, Yuri/J-5671-2013; OI Kovalev, Yuri/0000-0001-9303-3263; Ros, Eduardo/0000-0001-9503-4892; Savolainen, Tuomas/0000-0001-6214-1085; Kadler, Matthias/0000-0001-5606-6154 NR 24 TC 65 Z9 66 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAY 1 PY 2009 VL 696 IS 1 BP L22 EP L26 DI 10.1088/0004-637X/696/1/L22 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 434CP UT WOS:000265253100006 ER PT J AU Stothers, RB AF Stothers, Richard B. TI ON THE PERIOD AND AMPLITUDE CHANGES IN POLARIS AND OTHER SHORT-PERIOD CEPHEIDS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE stars: interiors; stars: magnetic fields; stars: oscillations; stars: variables: other; turbulence ID RR-LYRAE STARS; VARIABLE AMPLITUDE; CONVECTIVE MODEL; PULSATING STARS; HR-7308; PARALLAXES AB The observed modulation of the period and amplitude of Polaris, the short-period classical Cepheid, may be cyclical, though irregular, and superimposed on the continuing evolutionary changes of this star. If so, it curiously resembles the Blazhko effect seen in RR Lyrae stars, as Evans and her colleagues have noted. The present author's recent theory of the Blazhko effect based on a solar-like magnetoconvective cycle in the stellar envelope is here applied to Polaris, with some limited success. The theory may also explain the slow cycle seen in another short-period Cepheid, V473 Lyr. It is therefore possible to predict, tentatively, an entire new class of short-period "Blazhko Cepheids." C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Stothers, RB (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. NR 31 TC 6 Z9 6 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAY 1 PY 2009 VL 696 IS 1 BP L37 EP L39 DI 10.1088/0004-637X/696/1/L37 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 434CP UT WOS:000265253100009 ER PT J AU Norbury, JW AF Norbury, John W. TI PARAMETERIZATIONS OF INCLUSIVE CROSS SECTIONS FOR KAON, PROTON, AND ANTIPROTON PRODUCTION IN PROTON-PROTON COLLISIONS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE elementary particles; methods: analytical; methods: data analysis; methods: miscellaneous; radiation mechanisms: general ID GAMMA-RAY EMISSION; SPECTRUM; NUCLEUS; PHYSICS; MODELS AB Inclusive kaon, proton, and antiproton production from high-energy proton-proton collisions is studied. Various available parameterizations of Lorentz-invariant, differential cross sections, as a function of transverse momentum and rapidity, are compared with experimental data. This paper shows that the Badhwar parameterization provides the best fit for charged kaon production. For proton production, the Alper parameterization is best and for antiproton production the Carey parameterization works best. The formulae for these cross sections are suitable for use in high-energy cosmic ray transport codes. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Norbury, JW (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM john.w.norbury@nasa.gov NR 22 TC 1 Z9 1 U1 0 U2 1 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 MAY PY 2009 VL 182 IS 1 BP 120 EP 126 DI 10.1088/0067-0049/182/1/120 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 442BX UT WOS:000265815900007 ER PT J AU Witthoeft, MC Bautista, MA Mendoza, C Kallman, TR Palmeri, P Quinet, P AF Witthoeft, M. C. Bautista, M. A. Mendoza, C. Kallman, T. R. Palmeri, P. Quinet, P. TI K-SHELL PHOTOIONIZATION AND PHOTOABSORPTION OF Ne, Mg, Si, S, Ar, AND Ca SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE atomic data; atomic processes; methods: numerical; X-rays: general ID R-MATRIX METHOD; GENERAL PROGRAM; VACANCY STATES; ELECTRON-SCATTERING; CROSS-SECTIONS; AUGER DECAY; ATOMIC DATA; FE-XVII; IONS; IRON AB We present extensive computations of photoabsorption and photoionization cross sections across the K-edge of Ne, Mg, Si, S, Ar, and Ca ions with less than 11 electrons. The calculations are performed using the Breit-Pauli R-matrix method and include the effects of radiative and Auger damping by means of an optical potential. The wave functions are constructed from single-electron orbital bases obtained using a Thomas-Fermi-Dirac statistical model potential. Configuration interaction is considered among all fine-structure levels within the n = 2 complex. The damping processes affect the resonances converging to the K thresholds causing them to display symmetric profiles of constant width that smear the otherwise sharp edge at the photoionization thresholds. C1 [Witthoeft, M. C.; Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bautista, M. A.] Virginia Polytech & State Univ, Dept Phys, Blacksburg, VA 24061 USA. [Mendoza, C.] Inst Venezolano Invest Cient, Ctr Fis, Caracas 1020A, Venezuela. [Palmeri, P.; Quinet, P.] Univ Mons Hainaut, B-7000 Mons, Belgium. RP Witthoeft, MC (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. EM bautista@vt.edu FU NASA Astrophysics Theory Program; FNRS FX Support for this research was provided in part by a grant from the NASA Astrophysics Theory Program. M. C. W. is grateful to Nigel Badnell for many helpful discussions. P. P. and P. Q. are respectively Research Associate and Senior Research Associate of the Belgian F. R. S.- FNRS. Financial support from this organization is acknowledged. NR 31 TC 24 Z9 24 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAY PY 2009 VL 182 IS 1 BP 127 EP 130 DI 10.1088/0067-0049/182/1/127 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 442BX UT WOS:000265815900008 ER PT J AU Hogrefe, C Lynn, B Goldberg, R Rosenzweig, C Zalewsky, E Hao, W Doraiswamy, P Civerolo, K Ku, JY Sistla, G Kinney, PL AF Hogrefe, Christian Lynn, Barry Goldberg, Richard Rosenzweig, Cynthia Zalewsky, Eric Hao, Winston Doraiswamy, Prakash Civerolo, Kevin Ku, Jia-Yeong Sistla, Gopal Kinney, P. L. TI A combined model-observation approach to estimate historic gridded fields of PM2.5 mass and species concentrations SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Long-term air quality modeling; Aerosol model evaluation; Air quality characterization; Data integration; Community Multiscale; Air Quality (CMAQ) model ID COMMUNITY-MULTISCALE-AIR; SOUTHEASTERN UNITED-STATES; PARTICULATE MATTER; PERFORMANCE EVALUATION; QUALITY MODELS; PART II; OZONE; CMAQ; MORTALITY; EXPOSURE AB This paper introduces a methodology for estimating gridded fields of total and speciated fine particulate matter (PM2.5) concentrations for time periods and regions not covered by observational data. The methodology is based on performing long-term regional scale meteorological and air quality simulations and then integrating these simulations with available observational data. To illustrate this methodology, we present an application in which year-round simulations with a meteorological model (the National Center for Atmospheric Research/Penn State Mesoscale Model, hereafter referred to as MM5) and a photochemical air quality model (the Community Multiscale Air Quality Model, hereafter referred to as CMAQ) have been performed over the northeastern United States for 1988-2005. Model evaluation results for total PM2.5 mass and individual species for the time period from 2000 to 2005 show that model performance varies by species, season, and location. Therefore, an approach is developed to adjust CMAQ output with factors based on these three variables. The adjusted model values for total PM2.5 mass for 2000-2005 are compared against independent measurements not utilized for the adjustment approach. This comparison reveals that the adjusted model values have a lower root mean square error (RMSE) and higher correlation coefficients than the original model values. Furthermore, the PM2.5 estimates from these adjusted model values are compared against an alternate method for estimating historic PM2.5 values that is based on PM2.5/PM10 ratios calculated at co-located monitors. Results reveal that both methods yield estimates of historic PM2.5 mass that are broadly consistent; however, the adjusted CMAQ values provide greater spatial coverage and information for PM2.5 species in addition to total PM2.5 mass. Finally, strengths and limitations of the proposed approach are discussed in the context of potential uses of this method. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Hogrefe, Christian; Zalewsky, Eric; Hao, Winston; Ku, Jia-Yeong; Sistla, Gopal] Bur Air Qual Anal & Res, New York State Dept Environm Conservat, Albany, NY 12233 USA. [Hogrefe, Christian; Doraiswamy, Prakash] SUNY Albany, Atmospher Sci Res Ctr, Albany, NY 12203 USA. [Lynn, Barry] Weather It Is LTD, Efrat, Israel. [Goldberg, Richard; Rosenzweig, Cynthia] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Kinney, P. L.] Columbia Univ, Mailman Sch Publ Hlth, New York, NY 10032 USA. RP Hogrefe, C (reprint author), Bur Air Qual Anal & Res, New York State Dept Environm Conservat, 625 Broadway, Albany, NY 12233 USA. EM chogrefe@dec.state.ny.us RI Kinney, Patrick/H-7914-2012; OI Civerolo, Kevin/0000-0003-1536-2664 FU National Oceanic and Atmospheric Administration [NAO40AR4310185185]; Oak Ridge Institute for Science and Education (ORISE) FX The work presented here was supported by the National Oceanic and Atmospheric Administration under award NAO40AR4310185185, but it has not been subjected to its required peer and policy review. Therefore, the statements, findings, conclusions, and recommendations are those of the authors and do not necessarily reflect the views of the sponsoring agency and no official endorsement should be inferred. Additionally, part of the work presented in this paper was performed by the New York State Department of Environmental Conservation, but the views expressed in this paper do not necessarily reflect the views or policies of the New York State Department of Environmental Conservation. Finally, Christian Hogrefe also gratefully acknowledges partial support for this work through a research fellowship from the Oak Ridge Institute for Science and Education (ORISE). NR 30 TC 27 Z9 28 U1 0 U2 11 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 J9 ATMOS ENVIRON JI Atmos. Environ. PD MAY PY 2009 VL 43 IS 16 BP 2561 EP 2570 DI 10.1016/j.atmosenv.2009.02.031 PG 10 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 448PA UT WOS:000266273300006 ER PT J AU Platts, SH Tuxhorn, JA Ribeiro, LC Stenger, MB Lee, SMC Meck, JV AF Platts, Steven H. Tuxhorn, Jennifer A. Ribeiro, L. Christine Stenger, Michael B. Lee, Stuart M. C. Meck, Janice V. TI Compression Garments as Countermeasures to Orthostatic Intolerance SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE hypovolemia; kentavr; anti-gravity suit; spaceflight; tilt test; hypotension ID SPACE-SHUTTLE REENTRY; SPACEFLIGHT; ASTRONAUTS; BLOOD; HYPOTENSION; VOLUME; SUIT; MASS AB Introduction: All astronauts experience some degree of orthostatic intolerance following spaceflight, ranging from tachycardia to orthostatic hypotension and syncope. The purpose of this study was to evaluate the ability of two compression garments, the National Aeronautics and Space Administration's inflatable antigravity suit (AGS) and the Russian Federal Space Agency's non-inflatable compression garment (Kentavr), to prevent hypovolemia-related orthostatic intolerance. Methods: To mimic the plasma Volume loss experience(] by astronauts during spaceflight 19 healthy Subjects received an intravenous close of a dliueretic, furosemide (0.5 mg . kg(-1)), and then consumed a low-salt diet for 36 h. Thereafter, subjects participated in a 15-min 80 degrees head-up tilt test wearing either the AGS (N = 9) or Kentavr (N = 10). Compression garments were used in the fashion recommended by the respective agencies, delivering similar to 78 mmHg and similar to 30 mmHg of compression in the AGS and Kentavr, respectively. Incidence of presyncope and hemodynamic responses during upright tilt were compared to a separate group of hypovolemic control subjects (N = 16). Results: Subjects wearing the AGS or Kentavr completed the full 15 min of upright tilt without incidence of orthostatic hypotension or presyncope. In contrast, only 9 control subject (56%) were able to complete the tilt test. in addition, both types of compression garments maintained systolic blood pressure and significantly reduced tilt-induced tachycardia and reductions in stroke volume. Conclusions: Although both garments Successfully countered hypovolemia-induced orthostatic intolerance, the Kentavr provided protection by using lower levels of compression. Determining the optimal compression level required for protection of intolerance may improve crewmember comfort and decrease restrictions on physical activities after spaceflight. C1 [Platts, Steven H.; Meck, Janice V.] NASA, Lyndon B Johnson Space Ctr, Human Adaptat & Countermeasures Div, Houston, TX 77058 USA. [Tuxhorn, Jennifer A.; Ribeiro, L. Christine; Stenger, Michael B.; Lee, Stuart M. C.] Integrated Sci & Engn Grp, Houston, TX USA. RP Platts, SH (reprint author), NASA, Lyndon B Johnson Space Ctr, Human Adaptat & Countermeasures Div, 2101 NASA Pkwy,Mail Code SK, Houston, TX 77058 USA. EM steven.platts-1@nasa.gov FU NASA 3 FX The authors wish to thank the subjects for their participation in this investigation, the staff of the JSC Cardiovascular Laboratory for the collection and reduction of these data, Angela Brown for her assistance with manuscript preparation, and NASA for financial Support of this work. NR 21 TC 16 Z9 19 U1 0 U2 5 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 MAY PY 2009 VL 80 IS 5 BP 437 EP 442 DI 10.3357/ASEM.2473.2009 PG 6 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 438JD UT WOS:000265550800001 PM 19456003 ER PT J AU Crucian, BE Stowe, RP Mehta, SK Yetman, DL Leal, MJ Quiriarte, HD Pierson, DL Sams, CF AF Crucian, Brian E. Stowe, Raymond P. Mehta, Satish K. Yetman, Deborah L. Leal, Melanie J. Quiriarte, Heather D. Pierson, Duane L. Sams, Clarence F. TI Immune Status, Latent Viral Reactivation, and Stress During Long-Duration Head-Down Bed Rest SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE immune function; cytokines; viral reactivation; microgravity ID EPSTEIN-BARR-VIRUS; TIME PCR ASSAY; SPACE-FLIGHT; QUANTITATIVE-ANALYSIS; PERIPHERAL-BLOOD; SYSTEM CHANGES; SPACEFLIGHT; ASTRONAUTS; RESPONSES; MICROGRAVITY AB Introduction: As logistical access for space research becomes more limited and NASA prepares for exploration-class missions, ground-based spaceflight analogs will increase in importance for biomedical countermeasures development. A monitoring of immune parameters was performed during the NASA Flight Analogs Project bed rest study (without countermeasure); to establish 'control' data against Which future studies (with countermeasure) will he evaluated. Some of the countermeasures planned to be evaluated in future studies may impact immune function. Methods: The immune assessment consisted of leukocyte subset distribution, early T cell activation, intracellular cytokine profiles, latent viral reactivation, virus specific T cell levels and function, stress hormone levels and a behavioral assessment using stress questionnaires. Results: in general, subjects did riot display altered peripheral leukocyte subsets, constitutive immune activation, altered T cell function, or significant latent viral reactivation (EBV, VZV). Levels of constitutively activated T cells (CD8+/CD69+) and virus-specific T cells (CMV and EBV) decreased during the study. Cortisol levels (plasma and saliva) did not vary significantly during 90-d bed rest. Conclusions: These data demonstrate the absence of significant immune system alteration and physiological stress during 90-d bed rest, and establish control data against which future Studies (including countermeasures) may be compared. C1 [Pierson, Duane L.; Sams, Clarence F.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Crucian, Brian E.] Wyle, Houston, TX USA. [Stowe, Raymond P.; Yetman, Deborah L.] Microgen Labs, Lamarque, TX USA. [Mehta, Satish K.; Leal, Melanie J.] Enterprise Advisory Serv Inc, Houston, TX USA. [Quiriarte, Heather D.] JES Tech, Houston, TX USA. RP Sams, CF (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy,Mail Code SK3, Houston, TX 77058 USA. EM csams@nasa.gov FU NASA Flight Analogs Project [M01 RR 0073] FX Sponsored by the NASA Flight Analogs Project and conducted at the NIH-funded (M01 RR 0073) General Clinical Research Center at the University of Texas Medical Branch, Galveston, TX. NR 31 TC 19 Z9 20 U1 0 U2 6 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 MAY PY 2009 VL 80 IS 5 BP A37 EP A44 DI 10.3357/ASEM.BR05.2009 PG 8 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 438JE UT WOS:000265550900006 PM 19476168 ER PT J AU Inniss, AM Rice, BL Smith, SM AF Inniss, Astrid M. Rice, Barbara L. Smith, Scott M. TI Dietary Support of Long-Duration Head-Down Bed Rest SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE nutrition; food support; menu planning; bed rest ID MASS AB Introduction: Dietary control and nutrient intake are critical aspects of any metabolic study, but this is especially true in the case of bed rest studies. We Sought to define nutritional requirements, develop menus, and implement them during long-duration head-down bed rest studies. Methods: The dietary goals were to provide 100%, of subjects' nutrient requirements and to maintain subjects' bodyweight to within 3% of their weight on the third clay of head-down bed rest. The research dietitian and metabolic kitchen staff are an important part of the multidisciplinary team required to implement a bed rest study. Results. We report herein the planning steps and nutrient intake results from 13 subjects. We also provide insight into some of the dietary challenges that arise during long-duration bed rest studies. Discussion: Regardless of the overall objective of the bed rest study to be performed, nutrition must be carefully planned, implemented, and monitored to prevent results from being compromised. C1 [Inniss, Astrid M.] Univ Texas Med Branch, Gen Clin Res Ctr, Galveston, TX USA. [Rice, Barbara L.] Enterprise Advisory Serv Inc, Houston, TX USA. [Smith, Scott M.] NASA, Lyndon B Johnson Space Ctr, Human Adaptat & Countermeasures Div, Houston, TX USA. EM aminniss@utmb.edu FU NCATS NIH HHS [UL1 TR000071]; NCRR NIH HHS [UL1 RR029876] NR 15 TC 19 Z9 19 U1 0 U2 1 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 MAY PY 2009 VL 80 IS 5 SU S BP A9 EP A14 DI 10.3357/ASEM.BR04.2009 PG 6 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 438JE UT WOS:000265550900002 PM 19476164 ER PT J AU Meck, JV Dreyer, SA Warren, LE AF Meck, Janice V. Dreyer, Sherlene A. Warren, L. Elisabeth TI Long-Duration Head-Down Bed Rest: Project Overview, Vital Signs, and Fluid Balance SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE fluid balance; blood pressure; heart rate AB Introduction: Spaceflight has profound effects on the human body. Many of these effects can be induced with head-clown bed rest, which has been a Useful ground-based analog. With limited resources aboard the International Space Station for human research, the bed rest analog will be a primary platform On Which countermeasures will be developed and tested for lunar and Mars mission scenarios. Methods: NASA Johnson Space Center, in conjunction with the University of Texas Medical Branch (UTMB), has created the NASA Flight Analogs Project (FAP), a research program with the overall objective Of using head-clown bed rest to evaluate, compare, and refine candidate countermeasures to space-flight deconditioning. This paper serves as an overview and describes the standard conditions, the standard set of subject screening criteria, and the standard set of measurements for all FAP bed rest Subjects. Results: Heart rate and diastolic pressures decreased transiently at the onset of bed rest. Fluid balance showed an early diuresis, which stabilized within 3 d. In this supplement, detailed results from Multiple disciplines are presented in a series of reports. Discussion: The following reports describe multi-disciplinary results from the standard measurements by which the responses to bed rest will be assessed and by which countermeasures will be evaluated. The data presented in this overview are meant to serve as a context in which to view the data presented in the discipline specific manuscripts. The dietary support and behavioral health papers provide additional information regarding those aspects of implementing bed rest studies successfully. C1 [Meck, Janice V.] NASA, Lyndon B Johnson Space Ctr, Human Adaptat & Countermeasures Div, Houston, TX 77058 USA. [Dreyer, Sherlene A.; Warren, L. Elisabeth] Univ Space Res Assoc, Houston, TX USA. RP Meck, JV (reprint author), NASA, Lyndon B Johnson Space Ctr, Human Adaptat & Countermeasures Div, Mail Code SK3,2101 NASA Pkwy, Houston, TX 77058 USA. EM janice.v.meck@nasa.gov FU NASA Flight Analogs Project [M01 RR 0073] FX No project of this magnitude and complexity could succeed without tremendous Support. We are indebted to the UTMB GCRC staff; David Ware, M.D., our attending physician; the Johnson Space Center research laboratories; Wvle Laboratories Integration Coordinators; and, most of all, Our Subjects. Sponsored by the NASA Flight Analogs Project; conducted at the NIH-funded (M01 RR 0073) General Clinical Research Center at the University of Texas Medical Branch, Galveston, TX. NR 12 TC 37 Z9 40 U1 1 U2 2 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD MAY PY 2009 VL 80 IS 5 BP A1 EP A8 DI 10.3357/ASEM.BR01.2009 PG 8 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 438JE UT WOS:000265550900001 PM 19476163 ER PT J AU Platts, SH Martin, DS Stenger, MB Perez, SA Ribeiro, LC Summers, R Meck, JV AF Platts, Steven H. Martin, David S. Stenger, Michael B. Perez, Sondra A. Ribeiro, L. Christine Summers, Richard Meck, Janice V. TI Cardiovascular Adaptations to Long-Duration Head-Down Bed Rest SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE spaceflight; orthostatic intolerance; hypotension; fluid-shift; plasma volume ID POSTSPACEFLIGHT ORTHOSTATIC HYPOTENSION; CARDIAC-OUTPUT; SPACEFLIGHT; MICROGRAVITY; ASTRONAUTS; INTOLERANCE; ARTERIOLES; MECHANISMS; EXPRESSION; EXERCISE AB Introduction: Orthostatic hypotension is a serious risk for crewmembers returning from spaceflight. Numerous cardiovascular mechanisms have been proposed to account for this problem, including vascular and cardiac dysfunction, which we studied during bed rest, Methods: Thirteen subjects were studied before and during bed rest. Statistical analysis was limited to the first 49-60 d of bed rest and compared to pre-bed rest data. Ultrasound data were collected on Vascular and cardiac structure and function. Tilt testing was conducted for 30 min or until presyncopal symptoms intervened. Results: Plasma volume was significantly reduced (151%) by day 7 of bed rest. Flow-mediated dilation in the leg was significantly increased at bed rest clay 49 (6% from pre-bed rest). Arterial responses to nitroglycerin differed in the arm and leg, but did not change as a result of bed rest. Anterior tibial artery intimal-medial thickness markedly decreased at bed rest days 21 (21%), 35 (22%), and 49 (19%). Several cardiac functional parameters, including isovolumic relaxation time (73 ms to 85 ms at clay 7) and myocardial performance index, were significantly increased (0.41 to 0.49 by day 7 of bed rest; indicating a decrease in cardiac function) during bed rest. There was a trend for decreased orthostatic tolerance following 60 d of bed rest (P = 0.1). Discussion: Our data Suggest that bed rest altered cardiovascular structure and function in a pattern similar to short-duration spaceflight. Additionally, the vascular alterations were primarily seen in the lower body, while vessels of the upper body were unaffected. C1 [Platts, Steven H.; Meck, Janice V.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Martin, David S.; Stenger, Michael B.; Perez, Sondra A.; Ribeiro, L. Christine] Wyle Integrated Sci & Engn, Houston, TX USA. [Summers, Richard] Univ Mississippi, University, MS 38677 USA. RP Platts, SH (reprint author), NASA, Lyndon B Johnson Space Ctr, Mail Code SK,2101 NASA Pkwy, Houston, TX 77058 USA. EM steven.platts-1@nasa.gov FU NASA Flight Analogs Project [M01 RR 0073]; NASA [NAS9-97005] FX Sponsored by the NASA Flight Analogs Project; conducted at the NEH-funded (M01 RR 0073) GCRC at the University of Texas Medical Branch, Galveston, TX, and NASA grant NAS9-97005 to JVM. NR 30 TC 30 Z9 32 U1 0 U2 6 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 MAY PY 2009 VL 80 IS 5 BP A29 EP A36 DI 10.3357/ASEM.BR03.2009 PG 8 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 438JE UT WOS:000265550900005 PM 19476167 ER PT J AU Reschke, MF Bloomberg, JJ Paloski, WH Mulavara, AP Feiveson, AH Harm, DL AF Reschke, Millard F. Bloomberg, Jacob J. Paloski, William H. Mulavara, Ajitkumar P. Feiveson, Alan H. Harm, Deborah L. TI Postural Reflexes, Balance Control, and Functional Mobility with Long-Duration Head-Down Bed Rest SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE spaceflight; stretch reflex; functional reflex; exclusionary hypothesis; microgravity; flight analog; posturography; sensorimotor ID INPUT; WEIGHTLESSNESS; MICROGRAVITY; SENSORIMOTOR; LOCOMOTION; GAIT AB Introduction: Spaceflight has functionally significant effects oil sensorimotor behavior, but it is difficult to separate the effects of ascending somatosensory changes caused 1)), postural muscle and plantar surface unloading from descending visual-vestibular neural changes. To differentiate somatosensory changes from graviceptor changes in post-spaceflight sensorimotor behavior, bed rest may serve as an exclusionary analog to spaceflight. Methods: Four separate tests were used to measure changes in sensorimotor performance: 1) the monosynaptic stretch reflex (MSR); 2) the functional stretch reflex (FSR); 3) balance control parameters associated with computerized dynamic posturography (CDP); and 4) a functional mobility test (FMT). Results: A mixed model regression analysis showed significant increases in median MSR start and peak latencies, while the median FSR latency showed no significant increase. Median MSR peak magnitude showed a significant increase during the middle bed rest period (19-60 d). There were no significant effects of bed rest on balance control, but some indication that dynamic head movements may affect posture after bed rest. Time to complete the course for the FMT increased significantly with bed rest. Discussion: The four primary tests indicate that long-duration head-clown bed rest, through unloading and modification of the body's support surface, serves as an exclusionary analog for sensorimotor responses to spaceflight. Furthermore, the data Suggest that procedures designed to alleviate modifications to the sensory substrate serving the soles of the feet may provide a countermeasure to hell) maintain support afferentation of the postural muscles. C1 [Reschke, Millard F.; Bloomberg, Jacob J.; Paloski, William H.; Harm, Deborah L.] NASA, Lyndon B Johnson Space Ctr, Neurosci Labs, Houston, TX 77058 USA. [Feiveson, Alan H.] NASA, Lyndon B Johnson Space Ctr, Human Adaptat & Countermeasures Div, Houston, TX 77058 USA. [Mulavara, Ajitkumar P.] Univ Space Res Assoc, Houston, TX USA. RP Reschke, MF (reprint author), NASA, Lyndon B Johnson Space Ctr, Neurosci Labs, Mail Code SK272,2101 NASA Pkwy, Houston, TX 77058 USA. EM millard.f.reschke@nasa.gov FU NASA Flight Analogs Project [M01 RR 0073] FX The USO of our sensorimotor test paradigms as standard measures for head-down bed rest would not have been possible Without the support of NASA's Flight Analogs Project Team. We would also like to thank the Subjects who persisted throughout the bed rest, and the staff of the UTMB General Clinical Research Center for their Support and assistance. Sponsored by the NASA Flight Analogs Project; conducted at the NTH-funded (M01 RR 0073) General Clinical Research Center at the University of Texas Medical Branch, Galveston, TX. Lastly and most importantly, we are greatly indebted to Danielle L. Blau v; Rachel A. Brady; Elizabeth A. Fisher; George A. Ford; Jody M. Krnavek; Jeffrey T. Somers; and Laura C. Taylor. Without the service and long hours these individuals dedicated to this research project, the software, hardware, and data presented in this paper would net have been possible. NR 32 TC 16 Z9 19 U1 0 U2 3 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD MAY PY 2009 VL 80 IS 5 BP A45 EP A54 DI 10.3357/ASEM.BR06.2009 PG 10 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 438JE UT WOS:000265550900007 PM 19476169 ER PT J AU Seaton, KA Bowie, KE Sipes, WA AF Seaton, Kimberly A. Bowie, Kendra E. Sipes, Walter A. TI Behavioral and Psychological Issues in Long-Duration Head-Down Bed Rest SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE spaceflight; emotional support ID GROUP-DYNAMICS; CONFINEMENT; EXEMSI; SPACE AB Introduction: This report is one of a series on the Flight Analogs Project, which is designed to lay the groundwork for a standard bed rest protocol. Behavioral health services, similar to those offered to the U.S. astronauts who undertake 6-mo missions onboard the international Space Station, were provided to 13 long-duration head-down bed rest participants. Long-duration missions pose unique challenges and stressors, including separation from primary Support group, monotonous environment, and loss of privacy and autonomy. Methods: The psychological services team, consisting of a psychiatrist, a psychologist, and a master's level psychological support scientist, provided behavioral health services throughout all phases of the Flight Analogs Project (FAP) long-duration head-down bed rest study. During the initial screening phase, potential candidates completed 4 h of psychological testing and a 1.5-h clinical interview with a psychologist to assess their psychological fitness and ability to complete the Study Successfully. Additionally, the psychological services team provided pre-admission trainings on time management, stress management, and communication skills and conflict resolution. Throughout their stay on the research unit, study participants received regular individual and group visits from the psychological services team. Training was also provided to study personnel to address personality and behavioral management challenges. Results: Psychological support and training provided to both subjects and Study personnel have successfully improved the well being Of Study participants. Discussion: Behavioral health services are indispensable to long-duration head-down bed rest studies. C1 [Seaton, Kimberly A.; Bowie, Kendra E.] Wyle, Houston, TX 77058 USA. [Seaton, Kimberly A.] Univ Texas Med Branch, Galveston, TX USA. [Sipes, Walter A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Seaton, KA (reprint author), Wyle, 1290 Hercules Blvd, Houston, TX 77058 USA. EM kseaton@wylehou.com FU NASA Flight Analogs Project [M01 RR 0073] FX Sponsored by the NASA Flight Analogs Project; conducted at the NIH-funded (M01 RR 0073) General Clinical Research Center at the University of Texas Medical Branch, Galveston, TX. NR 19 TC 5 Z9 6 U1 1 U2 1 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 MAY PY 2009 VL 80 IS 5 BP A55 EP A61 DI 10.3357/ASEM.BR08.2009 PG 7 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 438JE UT WOS:000265550900008 PM 19476170 ER PT J AU Seaton, KA Slack, KJ Sipes, WA Bowie, KE AF Seaton, Kimberly A. Slack, Kelley J. Sipes, Walter A. Bowie, Kendra E. TI Cognitive Functioning In Long-Duration Head-Down Bed Rest SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE WinSCAT; spaceflight; cognitive function assessment tool AB Introduction: This report is one of a series on the Flight Analog Project, which is designed to lay the groundwork for a standard bed rest protocol. The Spaceflight Cognitive Assessment Tool for Windows (WinSCAT) is a self-administered battery of tests used on the International Space Station for evaluating cognitive functioning. Here, WinSCAT was used to assess cognitive functioning during extended head-down bed rest. Methods: There were 13 subjects who participated in 60 or 90 d of head-down bed rest and took WinSCAT during the pre-bed rest phase, the in-bed rest phase, and the post-bed rest (reconditioning) phase of study participation. Results: After adjusting for individual baseline performance, 12 off-nominal scores were observed out of 351 total observations during bed rest and 7 of 180 during reconditioning. No evidence was found for systematic changes in off-nominal incidence as time in bed rest progressed, or during the reconditioning period. Discussion: Cognitive functioning does not appear to be adversely affected by long-duration head-clown bed rest. individual differences in underlying cognitive ability and motivation level are likely explanations for the current findings. C1 [Seaton, Kimberly A.; Bowie, Kendra E.] Wyle, Houston, TX 77058 USA. [Seaton, Kimberly A.] Univ Texas Med Branch, Galveston, TX USA. [Slack, Kelley J.] LZ Technol, Alvin, TX USA. [Sipes, Walter A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Seaton, KA (reprint author), Wyle, 1290 Hercules Blvd, Houston, TX 77058 USA. EM kseaton@wylehou.com FU NASA Flight Analogs Project [M01 RR 0073] FX Sponsored by the NASA Flight Analogs Project; conducted at the NIFI-funded (M01 RR 0073) General Clinical Research Center at the University of Texas Medical Branch, Galveston, TX. NR 5 TC 12 Z9 16 U1 0 U2 3 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD MAY PY 2009 VL 80 IS 5 BP A62 EP A65 DI 10.3357/ASEM.BR09.2009 PG 4 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 438JE UT WOS:000265550900009 PM 19476171 ER PT J AU Spector, ER Smith, SM Sibonga, JD AF Spector, Elisabeth R. Smith, Scott M. Sibonga, Jean D. TI Skeletal Effects of Long-Duration Head-Down Red Rest SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE microgravity; disuse; bone mineral density; BMD recovery; bone resorption; bone formation ID BONE-MINERAL DENSITY; BIOCHEMICAL MARKERS; BED REST; SPACEFLIGHT; RECOVERY; TURNOVER AB Introduction: Skeletal unloading during spaceflight causes regional loss of bone mineral density (BMD), primarily in the spine and lower body regions. This loss of skeletal mass could adversely affect crew health during and after spaceflight and jeopardize mission success. Bed rest has long been used as a spaceflight analog to study the effects of disuse oil many body systems, including the skeleton. This study was undertaken by the NASA Flight Analogs Project (FAP) to collect control data for up-coming Countermeasure studies. Methods: There were 13 subjects who participated in 42, 44, 49, 52, 60, or 90 d of continuous, head-clown bed rest. DXA scans (dual-energy X-ray absorptiometry) were obtained before and after bed rest to measure changes in BMD of the whole body, lumbar spine, hip, heel, and wrist; the 90-d subjects were also scanned at the 60-d time point. Follow-up DXA scans were performed after 6 mo and 12 mo of reambulation to assess BMD recovery. Results: BMD changes were consistent with earlier bed rest and spaceflight studies, with statistically significant losses averaging 1% per month in the hip, pelvis, and heel. Recovery data were also consistent with data obtained after spaceflight. Bone biomarker data are described, and support the findings of previous studies. Specifically, the process of normal bone remodeling is uncoupled: increased bone resorption with no concomitant change in bone formation. Conclusion: The FAP appears to be a valid test bed for skeletal disuse studies, and should provide a useful research platform for evaluating countermeasures to spaceflight-induced bone loss. C1 [Sibonga, Jean D.] NASA, Lyndon B Johnson Space Ctr, Bone & Mineral Lab, Human Adaptat & Countermeasures Div, Houston, TX 77058 USA. [Spector, Elisabeth R.] Wyle, Houston, TX USA. [Sibonga, Jean D.] Univ Space Res Assoc, Houston, TX USA. RP Sibonga, JD (reprint author), NASA, Lyndon B Johnson Space Ctr, Bone & Mineral Lab, Human Adaptat & Countermeasures Div, Mail Code SK-272,2101 NASA Pkwy, Houston, TX 77058 USA. EM jean.sibonga-1@nasa.gov FU NASA Flight Analogs Project [M01 RR 0073] FX Sponsored by the NASA Flight Analogs Project; conducted at the NIH-funded (M01 RR 0073) General Clinical Research Center at the University of Texas Medical Branch, Galveston, TX. NR 20 TC 31 Z9 31 U1 0 U2 8 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 EI 1943-4448 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD MAY PY 2009 VL 80 IS 5 SU S BP A23 EP A28 DI 10.3357/ASEM.BR02.2009 PG 6 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 438JE UT WOS:000265550900004 PM 19476166 ER PT J AU Zwart, SR Oliver, SAM Fesperman, JV Kala, G Krauhs, J Ericson, K Smith, SM AF Zwart, Sara R. Oliver, Susan A. Mathews Fesperman, J. Vernell Kala, Geeta Krauhs, Jane Ericson, Karen Smith, Scott M. TI Nutritional Status Assessment Before, During, and After Long-Duration Head-Down Bed Rest SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE spaceflight; nutrition; weightlessness; bone resorption; parathyroid hormone; oxidative stress; antioxidants; iron; transferrin ID RED-BLOOD-CELL; SPACE-FLIGHT; BONE TURNOVER; CALCIUM-METABOLISM; SPACEFLIGHT; MARKERS; HUMANS; WEIGHTLESSNESS; UROLITHIASIS; BIOCHEMISTRY AB Introduction: Bed rest is a valuable ground-based model for many of the physiological changes that are associated with spaceflight. Nutritional changes during and after 60 or 90 cl of head-down bed rest were evaluated. Methods: A total of 13 subjects (8 men, 5 women; ages 2654 yr) participated in either 60 or 90 d of bed rest. Blood and urine were collected twice before bed rest and about once per month during bed rest. Samples were stored frozen and batch analyzed. Data were analyzed using repeated-measures analysis of variance. Results: During bed rest, markers of bone resorption (such as N-telopeptide excretion, P < 0.001) increased and serum concentration of parathyroid hormone decreased (P < 0.001). Also, oxidative damage markers such as superoxide dismutase increased (P < 0.05), and after 90 d of bed rest, total antioxidant capacity decreased (P < 0.05). During bed rest, iron status indices showed patterns of increased iron stores with a decreased concentration of transferrin receptors (P < 0.01). Discussion: These changes are similar to some of those observed during spaceflight, and further document the utility of bed rest as a model of spaceflight. C1 [Smith, Scott M.] NASA, Lyndon B Johnson Space Ctr, Nutr Biochem Lab, Human Adaptat & Countermeasures Div, Houston, TX 77058 USA. [Oliver, Susan A. Mathews; Fesperman, J. Vernell; Kala, Geeta] Enterprise Advisory Serv Inc, Houston, TX USA. [Ericson, Karen] Indiana Univ Purdue Univ, Ft Wayne, IN 46805 USA. [Zwart, Sara R.] Univ Space Res Assoc, Houston, TX USA. [Krauhs, Jane] Wyle, Houston, TX USA. RP Smith, SM (reprint author), NASA, Lyndon B Johnson Space Ctr, Nutr Biochem Lab, Human Adaptat & Countermeasures Div, Mail Code SK,2101 NASA Pkwy, Houston, TX 77058 USA. EM scott.m.smith@nasa.gov FU NASA Flight Analogs Project [M01 RR 0073] FX This project would not have been possible Without the NASA Flight Analogs Project Team. The effort to develop standardized bed rest conditions was not an easy one, and Jan Meck and her team did a phenomenal job with this project-hurricanes notwithstanding. We also thank the Subjects for their time and willingness to participate in these difficult long-duration Studies. We thank the staff of the UTMB General Clinical Research Center for their assistance in the conduct of this Study, The efforts of the staff of die NASA Johnson Space Center Nutritional Biochemistry Laboratory in planning, integrating, and executing the biological sample processing, laboratory analyses, and management of a tremendous amount of data are very much appreciated. We also thank Janis Davis-Street for reviewing the manuscript. Sponsored by the NASA Flight Analogs Project; conducted at the NIH-funded (M01 RR 0073) General Clinical Research Center at the University of Texas Medical Branch, Galveston, TX. NR 45 TC 26 Z9 26 U1 0 U2 1 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 MAY PY 2009 VL 80 IS 5 BP A15 EP A22 DI 10.3357/ASEM.BR07.2009 PG 8 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 438JE UT WOS:000265550900003 PM 19476165 ER PT J AU Campbell, JR Welton, EJ Spinhirne, JD AF Campbell, James R. Welton, Ellsworth J. Spinhirne, James D. TI Continuous Lidar Monitoring of Polar Stratospheric Clouds at the South Pole SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Editorial Material ID MICROPULSE LIDAR; DENITRIFICATION C1 [Campbell, James R.] Univ Corp Atmospher Res, USN, Res Lab, Visiting Scientist Programs, Monterey, CA 93943 USA. [Welton, Ellsworth J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Spinhirne, James D.] Univ Arizona, Dept Elect & Comp Engn, Tucson, AZ 85721 USA. RP Campbell, JR (reprint author), Univ Corp Atmospher Res, USN, Res Lab, Visiting Scientist Programs, Monterey, CA 93943 USA. EM jamesc@ucar.edu RI Welton, Ellsworth/A-8362-2012; Campbell, James/C-4884-2012 OI Campbell, James/0000-0003-0251-4550 NR 13 TC 1 Z9 2 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD MAY PY 2009 VL 90 IS 5 BP 613 EP 617 DI 10.1175/2008BAMS2754.1 PG 5 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 462LR UT WOS:000267354800003 ER PT J AU Pearson, JC Brauer, CS Drouin, BJ Xu, LH AF Pearson, J. C. Brauer, C. S. Drouin, Brian J. Xu, Li-Hong TI The rotational spectrum of methanol in the third excited torsional state SO CANADIAN JOURNAL OF PHYSICS LA English DT Article ID MICROWAVE STARK SPECTROSCOPY; FOURIER-TRANSFORM SPECTRA; FAR-INFRARED SPECTROSCOPY; DIPOLE-MOMENT; CH3OH; CH3-ROCKING; DATABASE; MASERS; LINE; BAND AB The rotational spectrum of methanol in its third excited torsional state, nu(t) = 3, as well as the K = 0 A-state of nu(t) = 4, has been recorded and analyzed in the 8-1654 GHz frequency range. The nu(t) = 3 state lies well above the top of the torsional barrier and the majority of the energy origins for the various K sub-bands lie below the C-O stretching fundamental vibration. Only the a-type R-branch spectrum was observed in this frequency range, suggesting that the near torsional degeneracy required for a b-type spectrum in the microwave accidentally reduces the torsional overlap, making these transitions very weak. The A-state K = 4 of nu(t) = 3 interaction with the C-O stretch torsional ground state K = 0(+) and K = 1(+) has been accounted for. The E-state K = -5 level could be fit directly with a power series in spite of its resonance with the C-O stretch torsional ground state K = -5 level. The (a)R-branch of the K = 0 A-state nu(t) = 4 sub-band is also provided and the origin of this band resonance with the C-O stretch is discussed. The data have been modeled with a power series to near experimental accuracy. The measured and calculated spectrum should facilitate radio astronomical assignments of nu(t) = 3 transitions in hot sources. C1 [Pearson, J. C.; Brauer, C. S.; Drouin, Brian J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Xu, Li-Hong] Univ New Brunswick, Dept Phys, CLAMS, St John, NB E2L 4L5, Canada. RP Pearson, JC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM john.c.pearson@jpl.nasa.gov RI Xu, Li-Hong/J-5095-2015 FU Natural Sciences and Engineering Research Council of Canada FX Portions of research described in this paper were carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA). We thank NASA for their support of Herschel heterodyne instrument for far-infrared guaranteed time holders, which facilitated this paper. LHX thanks the Natural Sciences and Engineering Research Council of Canada for financial support of this research. NR 31 TC 11 Z9 11 U1 0 U2 12 PU NATL RESEARCH COUNCIL CANADA-N R C RESEARCH PRESS PI OTTAWA PA BUILDING M 55, OTTAWA, ON K1A 0R6, CANADA SN 0008-4204 J9 CAN J PHYS JI Can. J. Phys. PD MAY PY 2009 VL 87 IS 5 BP 449 EP 467 DI 10.1139/P08-133 PG 19 WC Physics, Multidisciplinary SC Physics GA 494RV UT WOS:000269834000006 ER PT J AU Sung, K Brown, LR Toth, RA Crawford, TJ AF Sung, Keeyoon Brown, Linda R. Toth, Robert A. Crawford, Timothy J. TI Fourier transform infrared spectroscopy measurements of H2O-broadened half-widths of CO2 at 4.3 mu m SO CANADIAN JOURNAL OF PHYSICS LA English DT Article ID CONSTRAINED MULTISPECTRUM ANALYSIS; PRESSURE SHIFT COEFFICIENTS; CARBON-DIOXIDE; SPEED DEPENDENCE; LINE POSITIONS; 4750-7000 CM(-1); BANDS; TEMPERATURE; INTENSITIES; (CO2)-C-12-O-16 AB To support remote sensing of carbon dioxide in the troposphere, H2O pressure-broadened half-widths were obtained for 182 lines of CO2 in the 2250-2390 cm(-1) region. For this, six spectra of CO2 were recorded at 0.003 89 cm(-1) resolution using a Bruker IFS-125HR at the Jet Propulsion Laboratory. The absorption cell length was 6.14 cm, and the water pressures ranged from 20.1 to 26.5 torr (1 torr = 133.322 4 Pa) near room temperatures. Partial pressures of the species in the mixtures were determined by measuring selected line intensities in the nu(3) band of CO2 and the nu(2) band of H2O. Sample temperatures were validated by deriving rotational temperature from the nu(3) and nu(2) + nu(3) -nu(2) intensities of (CO2)-C-12 and those of CO (1-0). Positions, intensities, and half-widths were retrieved spectrum by spectrum using a nonlinear least-squares line-fitting algorithm, employing a standard Voigt line shape profile and an instrumental line shape consisting of a sinc function with aperture correction. Half-widths obtained for both the fundamental and the hot band of (CO2)-C-12 and the fundamental nu(3) band of (CO2)-C-13 had similar values. While half-widths of CO2 broadened by other atmospheric gases (such as N-2, O-2, CO2, and air) tend to decrease with increasing rotational quantum number J '', the H2O-broadened half-widths were observed to increase for intermediate J '' (8 <= J '' <= 42): similar to 0.127 cm(-1) atm(-1) near J '' = 8, and increasing to similar to 0.143 cm(-1) atm-1 (1 atm = 101.325 kPa) towards J '' = 42. Moreover, for 10 <= J '' <= 40, the empirical widths were within similar to 2%-3% of theoretical calculations. Since water vapor could reach up to 5% of ambient atmospheric surface pressure in the tropical regions, water broadened half-widths are required to model tropospheric CO2, particularly for high-precision remote sensing, to achieve a sub-percent precision in the measurements of CO2 column averaged mixing ratio. Since little vibrational dependence in line broadening has been seen, these results at 4.3 mu m can be used for other bands of CO2. C1 [Sung, Keeyoon; Brown, Linda R.; Toth, Robert A.; Crawford, Timothy J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Sung, K (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ksung@jpl.nasa.gov RI Sung, Keeyoon/I-6533-2015 NR 39 TC 21 Z9 21 U1 1 U2 9 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 1200 MONTREAL ROAD, BUILDING M-55, OTTAWA, ON K1A 0R6, CANADA SN 0008-4204 J9 CAN J PHYS JI Can. J. Phys. PD MAY PY 2009 VL 87 IS 5 BP 469 EP 484 DI 10.1139/P08-130 PG 16 WC Physics, Multidisciplinary SC Physics GA 494RV UT WOS:000269834000007 ER PT J AU Benner, DC Miller, CE Devi, VM AF Benner, D. Chris Miller, C. E. Devi, V. Malathy TI Constrained multispectrum analysis of CO2-Ar broadening at 6227 and 6348 cm(-1) SO CANADIAN JOURNAL OF PHYSICS LA English DT Article ID MOLECULAR SPECTROSCOPIC DATABASE; ANGULAR-MOMENTUM RELAXATION; POTENTIAL-ENERGY SURFACES; CARBON-DIOXIDE; PERTURBER DEPENDENCIES; SPEED DEPENDENCE; INFRARED-SPECTRA; CROSS-SECTIONS; DIFFERENT TEMPERATURES; NITROUS-OXIDE AB We report the first extensive experimental measurements of Ar-broadened half-width and pressure-induced shift coefficients, speed dependence parameters, and line mixing coefficients for the 30013 <- 00001 and 30012 <- 00001 bands of (OCO)-O-16-C-12-O-16 centered near 6227 and 6348 cm(-1), respectively. These parameters were determined from 15 self-broadened and six Ar-broadened CO2 spectra recorded at room temperature with long absorption path lengths (25 to 121 m) using the McMath-Pierce Fourier transform spectrometer (FTS) at the National Solar Observatory. All 21 spectra were fit simultaneously using a multispectrum nonlinear least-squares technique. The line positions and line intensities were constrained to quantum mechanical expressions to obtain maximum accuracies in the retrieved parameters. Speed-dependent line shapes with line mixing (via the relaxation matrix formalism) were required to remove systematic errors in the fit residuals using only the Voigt profile. Remaining fit residuals were minimized by adjusting the half-width and pressure-induced shift coefficients of the overlapping 31113 <- 01101 and 31112 <- 01101 hot bands. We compare the Ar-broadening parameters with those recently determined for self-and air-broadening in the 30012 <- 00001 and 30013/ 00001 bands and also with other Ar-broadening values from the literature, as appropriate. C1 [Benner, D. Chris; Devi, V. Malathy] Coll William & Mary, Williamsburg, VA 23187 USA. [Miller, C. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Benner, DC (reprint author), Coll William & Mary, Box 8795, Williamsburg, VA 23187 USA. EM dcbenn@wm.edu FU National Science Foundation [ATM-0338475] FX The material presented in this investigation is based upon work supported by the National Science Foundation under Grant No. ATM-0338475 to the College of William and Mary. The research at the Jet Propulsion Laboratory (JPL), California Institute of Technology, was performed under contract with National Aeronautics and Space Administration. The authors express sincere appreciation to M. Dulick of NOAO (National Optical Astronomy Observatory) for the assistance in obtaining the data. The authors thank NASA's Upper Atmosphere Research Program for support of the McMath-Pierce laboratory facility. NR 36 TC 8 Z9 7 U1 0 U2 6 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 1200 MONTREAL ROAD, BUILDING M-55, OTTAWA, ON K1A 0R6, CANADA SN 0008-4204 J9 CAN J PHYS JI Can. J. Phys. PD MAY PY 2009 VL 87 IS 5 BP 499 EP 515 DI 10.1139/P09-014 PG 17 WC Physics, Multidisciplinary SC Physics GA 494RV UT WOS:000269834000009 ER PT J AU Predoi-Cross, A McKellar, ARW Benner, DC Devi, VM Gamache, RR Miller, CE Toth, RA Brown, LR AF Predoi-Cross, A. McKellar, A. R. W. Benner, D. Chris Devi, V. Malathy Gamache, R. R. Miller, C. E. Toth, R. A. Brown, L. R. TI Temperature dependences for air-broadened Lorentz half-width and pressure shift coefficients in the 30013 <- 00001 and 30012 <- 00001 bands of CO2 near 1600 nm SO CANADIAN JOURNAL OF PHYSICS LA English DT Article ID DIODE-LASER MEASUREMENTS; CONSTRAINED MULTISPECTRUM ANALYSIS; SPEED DEPENDENCE; LINE-SHAPES; IR LINES; MU-M; INTENSITIES; CM(-1); TRANSITIONS; H2O AB In this study, 39 high-resolution spectra of pure and air-broadened CO2 recorded at temperatures between 215 and 294 K were analyzed using a multispectrum nonlinear least-squares technique to determine temperature dependences of air-broadened Lorentz half-width and air-induced pressure shift coefficients for over 100 individual (CO2)-C-12-O-16 transitions in the 30012 <- 00001 (at 6348 cm(-1)) and 30013 <- 00001 (at 6228 cm(-1)) bands. Data were recorded with two different Fourier transform spectrometers (Kitt Peak FTS at the National Solar Observatory in Arizona and the Bomem FTS at NRC, Ottawa), with absorption path lengths ranging between 25 and 121 m. The sample pressures varied between 11 torr (pure CO2) and 924 torr (CO2-air) with volume mixing ratios of CO2 in air between similar to 1.5% and 11% (1 torr = 133.322 4 Pa). To minimize systematic errors and increase the accuracy of the retrieved parameters, a constrained multispectrum nonlinear least-squares fitting technique was used to include theoretical quantum mechanical expressions for the rovibrational energies and intensity parameters rather than retrieving the individual positions and intensities line by line. The results suggest no detectable vibrational dependence for the temperature dependences for the air-broadened Lorentz half-width coefficients and the air-induced pressure shift coefficients. The half-width coefficients and temperature dependence exponents were modeled using semiclassical calculations based upon the Robert-Bonamy formalism. A good agreement is seen between the measurements and theoretical calculations. Beyond |m| = 26, a simple scaling factor (0.96) has been applied to the calculated half-width coefficients to match the experimental measurements. C1 [Predoi-Cross, A.] Univ Lethbridge, Dept Phys & Astron, Lethbridge, AB T1K 3M4, Canada. [McKellar, A. R. W.] Natl Res Council Canada, Steacie Inst Mol Sci, Ottawa, ON K1A 0R6, Canada. [Benner, D. Chris; Devi, V. Malathy] Coll William & Mary, Williamsburg, VA 23187 USA. [Gamache, R. R.] Univ Massachusetts, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA. [Miller, C. E.; Toth, R. A.; Brown, L. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Predoi-Cross, A (reprint author), Univ Lethbridge, Dept Phys & Astron, Lethbridge, AB T1K 3M4, Canada. EM adriana.predoicross@uleth.ca FU National Sciences and Engineering Research Council of Canada (NSERC); The research at the Jet Propulsion Laboratory (JPL); California Institute of Technology; National Aeronautics and Space Administration; National Science Foundation [ATM-0338475, ATM-0803135] FX A. Predoi-Cross and A. R. W. Mckellar are grateful for financial support from the National Sciences and Engineering Research Council of Canada (NSERC). The research at the Jet Propulsion Laboratory (JPL), California Institute of Technology, was performed under contract with National Aeronautics and Space Administration. The support received from the National Science Foundation under Grant No. ATM-0338475 to the College of William and Mary is greatly appreciated. R. R. Gamache is pleased to acknowledge support of this research by the National Science Foundation through Grant No. ATM-0803135. The authors thank Mike Dulick of the National Solar Observatory for his assistance in obtaining the data recorded at Kitt Peak. NR 38 TC 33 Z9 34 U1 0 U2 10 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 1200 MONTREAL ROAD, BUILDING M-55, OTTAWA, ON K1A 0R6, CANADA SN 0008-4204 J9 CAN J PHYS JI Can. J. Phys. PD MAY PY 2009 VL 87 IS 5 BP 517 EP 535 DI 10.1139/P08-137 PG 19 WC Physics, Multidisciplinary SC Physics GA 494RV UT WOS:000269834000010 ER PT J AU Bloem, M Alpcan, T Basar, T AF Bloem, Michael Alpcan, Tansu Basar, Tamer TI Optimal and robust epidemic response for multiple networks SO CONTROL ENGINEERING PRACTICE LA English DT Article; Proceedings Paper CT 46th IEEE Conference on Decision and Control CY DEC 12-14, 2007 CL New Orleans, LA SP IEEE Control Syst Soc, United Technol, Springer, Wiley Blackwell, Taylor & Francis, Princeton Univ Press, Maplesoft, Siam DE Epidemic response; Optimal control; LQR; H-infinity robust control AB This paper studies the optimization of malicious software removal or patch deployment processes across multiple networks. The well-known classical epidemic model is adapted to model malware propagation in this multi-network framework. The trade-off between the infection spread and the patching costs is captured in a cost function, leading to an optimal control problem. In the single network case the optimal feedback controller is found by solving an associated Hamilton-Jacobi-Bell-man equation. This control law is numerically compared to the proportional response strategy typically assumed by the epidemic model. In the higher dimensional multiple-networks case, the system is linearized to derive feedback controllers using pole-placement, linear quadratic regulator (LQR) optimal control, and H-infinity optimal control, where the measurement errors in the number of infected clients are explicitly modeled. The resulting patching strategies are analyzed numerically and their results are compared. (c) 2007 Elsevier Ltd. All rights reserved. C1 [Alpcan, Tansu] Deutsch Telekom Labs T Labs, D-10587 Berlin, Germany. [Bloem, Michael] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Basar, Tamer] Univ Illinois, Coordinated Sci Lab, Urbana, IL 61801 USA. RP Alpcan, T (reprint author), Deutsch Telekom Labs T Labs, D-10587 Berlin, Germany. EM michael.bloem@nasa.gov; tansu.alpcan@telekom.de; tbasar@control.csl.uiuc.edu RI Alpcan, Tansu/D-7089-2014 OI Alpcan, Tansu/0000-0002-7434-3239 NR 19 TC 12 Z9 12 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0967-0661 EI 1873-6939 J9 CONTROL ENG PRACT JI Control Eng. Practice PD MAY PY 2009 VL 17 IS 5 BP 525 EP 533 DI 10.1016/j.conengprac.2008.10.007 PG 9 WC Automation & Control Systems; Engineering, Electrical & Electronic SC Automation & Control Systems; Engineering GA 440RZ UT WOS:000265718700001 ER PT J AU Batki, SL Canfield, KM Smyth, E Ploutz-Snyder, R AF Batki, Steven L. Canfield, Kelly M. Smyth, Emily Ploutz-Snyder, Robert TI Health-related quality of life in methadone maintenance patients with untreated hepatitis C virus infection SO DRUG AND ALCOHOL DEPENDENCE LA English DT Article DE Hepatitis C; Methadone; Opioid; Substance abuse; Quality of life; Health; Psychiatry ID INJECTION-DRUG USERS; RISK-FACTORS; SURVEY QUESTIONNAIRE; HCV-INFECTION; PREVALENCE; DEPRESSION; INTERFERON-ALPHA-2B; MANAGEMENT; REDUCTION; EQUIPMENT AB Objective: To assess health-related quality of life (HRQOL) in methadone maintenance treatment (MMT) patients with untreated chronic HCV infection and to determine the clinical factors that predict HRQOL. Method: HRQOL was measured in 100 MMT patients entering an HCV treatment trial. Subjects were mostly male (61%) and white (81%) with a mean age of 43 (+/- 10). 57% had a current non-substance use psychiatric disorder. 55% had a current (past 12 months) substance use disorder, including 44% with current opioid or cocaine abuse/dependence. HRQOL in our sample was compared to published reports for the general population as well as for non-MMT HCV patients. To assess predictors of SF-36 HRQOL, hierarchical multiple regression techniques were used to assess model improvement with four blocks of baseline predictors: Demographics, Medical Severity, Addiction Severity, and Depression Severity. Results: HRQOL scores were significantly lower than scores for the general population and were also lower than scores reported for untreated HCV patients not in MMT. Regression analysis demonstrated a consistent pattern whereby Depression Severity increased predictive accuracy for HRQOL measures over simpler models. Beck Depression Inventory scores significantly predicted quality of life across both the mental and physical composite scores and all eight sub-scales of the SF-36. Conclusions: Untreated HCV patients in MMT had lower HRQOL than HCV patients not in MMT. Depression Severity was associated with significantly lower quality of life measures, suggesting that psychiatric evaluation and intervention prior to the start of HCV treatment may improve overall quality of life and could influence HCV treatment outcomes in MMT patients. (C) Published by Elsevier Ireland Ltd. C1 [Batki, Steven L.] Univ Calif San Francisco, San Francisco VA Med Ctr, Dept Psychiat, Addict Psychiat Res Program, San Francisco, CA 94121 USA. [Canfield, Kelly M.; Smyth, Emily] SUNY Upstate Med Univ, Dept Psychiat, Syracuse, NY 13210 USA. [Ploutz-Snyder, Robert] Univ Space Res Assoc, NASA JSC, Lyndon B Johnson Space Ctr, SK, Houston, TX 77058 USA. RP Batki, SL (reprint author), Univ Calif San Francisco, San Francisco VA Med Ctr, Dept Psychiat, Addict Psychiat Res Program, 4150 Clement St,116P, San Francisco, CA 94121 USA. EM steven.batki@ucsf.edu FU National Institute on Drug Abuse (NIDA) [R01 DA 016764] FX This work was supported by National Institute on Drug Abuse (NIDA) grant R01 DA 016764. NIDA had no further role in study design; in the collection, analysis, and interpretation of the data; in the writing of this report; and in the decision to Submit the paper for publication. NR 48 TC 11 Z9 11 U1 4 U2 8 PU ELSEVIER IRELAND LTD PI CLARE PA ELSEVIER HOUSE, BROOKVALE PLAZA, EAST PARK SHANNON, CO, CLARE, 00000, IRELAND SN 0376-8716 J9 DRUG ALCOHOL DEPEN JI Drug Alcohol Depend. PD MAY 1 PY 2009 VL 101 IS 3 BP 176 EP 182 DI 10.1016/j.drugalcdep.2008.12.012 PG 7 WC Substance Abuse; Psychiatry SC Substance Abuse; Psychiatry GA 430PY UT WOS:000265002200006 PM 19233573 ER PT J AU Newman, JA Willard, SA Smith, SW Piascik, RS AF Newman, John A. Willard, Scott A. Smith, Stephen W. Piascik, Robert S. TI Replica-based crack inspection SO ENGINEERING FRACTURE MECHANICS LA English DT Article DE Surface replica; Crack inspection; Small crack; Inconel 718 AB Surface replication has been proposed as a method for crack detection in space-shuttle main engine flowliner slots. The results of a feasibility study show that examination of surface replicas with a scanning electron microscope can result in the detection of cracks as small as 0.005 inch, and surface flaws as small as 0.001 inch, for the flowliner material. Published by Elsevier Ltd. C1 [Newman, John A.; Smith, Stephen W.; Piascik, Robert S.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Willard, Scott A.] Lockheed Martin Space Operat, Langley Res Ctr, Hampton, VA 23681 USA. RP Newman, JA (reprint author), NASA, Langley Res Ctr, MS 188E, Hampton, VA 23681 USA. EM john.a.newman@nasa.gov NR 6 TC 7 Z9 8 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0013-7944 J9 ENG FRACT MECH JI Eng. Fract. Mech. PD MAY PY 2009 VL 76 IS 7 BP 898 EP 910 DI 10.1016/j.engfracmech.2008.12.012 PG 13 WC Mechanics SC Mechanics GA 453QX UT WOS:000266627100006 ER PT J AU Preston, CM Marin, R Jensen, SD Feldman, J Birch, JM Massion, EI DeLong, EF Suzuki, M Wheeler, K Scholin, CA AF Preston, Christina M. Marin, Roman, III Jensen, Scott D. Feldman, Jason Birch, James M. Massion, Eugene I. DeLong, Edward F. Suzuki, Marcelino Wheeler, Kevin Scholin, Christopher A. TI Near real-time, autonomous detection of marine bacterioplankton on a coastal mooring in Monterey Bay, California, using rRNA-targeted DNA probes SO ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID DINOFLAGELLATE KARENIA-BREVIS; OLIGONUCLEOTIDE MICROARRAYS; HYBRIDIZATION FORMATS; MICROBIAL-POPULATIONS; QUANTITATIVE-ANALYSIS; INVERTEBRATE LARVAE; MOLECULAR-DETECTION; FLOW CYTOMETER; BACTERIA; PHYTOPLANKTON AB A sandwich hybridization assay (SHA) was developed to detect 16S rRNAs indicative of phylogenetically distinct groups of marine bacterioplankton in a 96-well plate format as well as low-density arrays printed on a membrane support. The arrays were used in a field-deployable instrument, the Environmental Sample Processor (ESP). The SHA employs a chaotropic buffer for both cell homogenization and hybridization, thus target sequences are captured directly from crude homogenates. Capture probes for seven of nine different bacterioplankton clades examined reacted specifically when challenged with target and non-target 16S rRNAs derived from in vitro transcribed 16S rRNA genes cloned from natural samples. Detection limits were between 0.10-1.98 and 4.43- 12.54 fmole ml(-1) homogenate for the 96-well plate and array SHA respectively. Arrays printed with five of the bacterioplankton-specific capture probes were deployed on the ESP in Monterey Bay, CA, twice in 2006 for a total of 25 days and also utilized in a laboratory time series study. Groups detected included marine alphaproteobacteria, SAR11, marine cyanobacteria, marine group I crenarchaea, and marine group II euryarchaea. To our knowledge this represents the first report of remote in situ DNA probe-based detection of marine bacterioplankton. C1 [Preston, Christina M.; Marin, Roman, III; Jensen, Scott D.; Feldman, Jason; Birch, James M.; Massion, Eugene I.; Wheeler, Kevin; Scholin, Christopher A.] Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA. [Feldman, Jason] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [DeLong, Edward F.] MIT, Dept Civil & Environm Engn, Cambridge, MA 02139 USA. [DeLong, Edward F.] MIT, Div Biol Engn, Cambridge, MA 02139 USA. [Suzuki, Marcelino] Univ Maryland, Chesapeake Biol Lab, Solomons, MD 20668 USA. [Wheeler, Kevin] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Preston, CM (reprint author), Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA. EM preston@mbari.org RI Suzuki, Marcelino/D-3329-2009 OI Suzuki, Marcelino/0000-0003-3868-6362 FU David and Lucille Packard Foundation; Keck Foundation; NSF Microbial Observatory; Gordon and Betty Moore Foundation FX We are grateful for the expertise and work of the engineers, technicians and machinists at MBARI for maintaining the instrument. We thank J. Zehr for providing the Synechococcus culture, V. Orphan for providing the group III euryarchaeal plasmid 1#6, and three anonymous reviewers for their editorial comments. We also thank the Moss Landing Marine Laboratories Small Boats Operation and the captains and crews of the R/V Zephyr. This work was supported in part by grants from the David and Lucille Packard Foundation to C.A.S., Keck Foundation to E.F.D. and C.A.S., NSF Microbial Observatory grant to E.F.D. and Gordon and Betty Moore Foundation grant to C.A.S and E.F.D. NR 50 TC 36 Z9 36 U1 0 U2 10 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1462-2912 J9 ENVIRON MICROBIOL JI Environ. Microbiol. PD MAY PY 2009 VL 11 IS 5 BP 1168 EP 1180 DI 10.1111/j.1462-2920.2009.01848.x PG 13 WC Microbiology SC Microbiology GA 437IW UT WOS:000265481600012 PM 19210704 ER PT J AU Bissaldi, E von Kienlin, A Lichti, G Steinle, H Bhat, PN Briggs, MS Fishman, GJ Hoover, AS Kippen, RM Krumrey, M Gerlach, M Connaughton, V Diehl, R Greiner, J van der Horst, AJ Kouveliotou, C McBreen, S Meegan, CA Paciesas, WS Preece, RD Wilson-Hodge, CA AF Bissaldi, E. von Kienlin, A. Lichti, G. Steinle, H. Bhat, P. N. Briggs, M. S. Fishman, G. J. Hoover, A. S. Kippen, R. M. Krumrey, M. Gerlach, M. Connaughton, V. Diehl, R. Greiner, J. van der Horst, A. J. Kouveliotou, C. McBreen, S. Meegan, C. A. Paciesas, W. S. Preece, R. D. Wilson-Hodge, C. A. TI Ground-based calibration and characterization of the Fermi gamma-ray burst monitor detectors SO EXPERIMENTAL ASTRONOMY LA English DT Article DE Fermi Gamma-Ray space telescope; GLAST; Gamma-Ray detectors; Calibration; NaI(Tl); BGO; Gamma-Ray burst ID HIGH-ENERGY; SPECTRAL PROPERTIES; BESSY-II; GLAST; SIMULATION; NAI(T1); BAMLINE; EGRET AB One of the scientific objectives of NASA's Fermi Gamma-ray Space Telescope is the study of Gamma-Ray Bursts (GRBs). The Fermi Gamma-Ray Burst Monitor (GBM) was designed to detect and localize bursts for the Fermi mission. By means of an array of 12 NaI(Tl) (8 keV to 1 MeV) and two BGO (0.2 to 40 MeV) scintillation detectors, GBM extends the energy range (20 MeV to > 300 GeV) of Fermi's main instrument, the Large Area Telescope, into the traditional range of current GRB databases. The physical detector response of the GBM instrument to GRBs is determined with the help of Monte Carlo simulations, which are supported and verified by on-ground individual detector calibration measurements. We present the principal instrument properties, which have been determined as a function of energy and angle, including the channel-energy relation, the energy resolution, the effective area and the spatial homogeneity. C1 [Bissaldi, E.; von Kienlin, A.; Lichti, G.; Steinle, H.; Diehl, R.; Greiner, J.; McBreen, S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Bhat, P. N.; Briggs, M. S.; Connaughton, V.; Paciesas, W. S.; Preece, R. D.] Univ Alabama, NSSTC, Huntsville, AL 35899 USA. [Fishman, G. J.; van der Horst, A. J.; Kouveliotou, C.; Meegan, C. A.; Wilson-Hodge, C. A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Hoover, A. S.; Kippen, R. M.] Los Alamos Natl Lab, Los Alamos, NM USA. [Krumrey, M.; Gerlach, M.] Phys Tech Bundesanstalt, Berlin, Germany. RP Bissaldi, E (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. EM ebs@mpe.mpg.de RI Krumrey, Michael/G-6295-2011; Bissaldi, Elisabetta/K-7911-2016; OI Bissaldi, Elisabetta/0000-0001-9935-8106; Preece, Robert/0000-0003-1626-7335 NR 35 TC 27 Z9 27 U1 1 U2 7 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0922-6435 EI 1572-9508 J9 EXP ASTRON JI Exp. Astron. PD MAY PY 2009 VL 24 IS 1-3 BP 47 EP 88 DI 10.1007/s10686-008-9135-4 PG 42 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 437SX UT WOS:000265508300003 ER PT J AU Hulot, G Olsen, N Thebault, E Hemant, K AF Hulot, Gauthier Olsen, Nils Thebault, Erwan Hemant, Kumar TI Crustal concealing of small-scale core-field secular variation SO GEOPHYSICAL JOURNAL INTERNATIONAL LA English DT Article DE Dynamo: theories and simulations; Magnetic anomalies: modelling and interpretation; Satellite magnetics ID EARTHS MAGNETIC-FIELD; GEOMAGNETIC-FIELD; SATELLITE DATA; REMANENT MAGNETIZATION; CHAMP; MODEL; SURFACE; SWARM; FLOWS; CONSTELLATION AB The Earth's magnetic field is mainly produced within the Earth's liquid and electrically conducting core, as a result of a process known as the geodynamo. Many other sources also contribute to the magnetic signal accessible to observation at the Earth's surface, partly obscuring the main core magnetic field signal. Thanks to a series of very successful satellites and to advances in magnetic field modelling techniques, considerable progress has, however, been made in the recent years toward better identifying the signal of each of these sources. In particular, temporal changes in the field of internal origin happen to be detectable now in spherical harmonic degrees up to, perhaps, 16. All of these changes are usually attributed to changes in the core field itself, the secular variation, on the ground that the lithospheric magnetization cannot produce such signals. It has, however, been pointed out, on empirical grounds, that temporal changes in the field of internal origin produced by the induced part of the lithospheric magnetization could dominate the core field signal beyond degree 22. This short note revisits this issue by taking advantage of our improved knowledge of the small-scale field changes and of the likely sources of the lithospheric field. We rely on a simple extrapolation of the observed spatial spectrum of the field changes beyond degree 16 and use a forward approach based on a recent geological model of lithospheric magnetization. This leads us to confirm that the main cause of the observed changes in the field of internal origin up to some critical degree, N(C), is indeed likely to be the secular variation of the core field, but that the signal produced by the time-varying lithospheric field is bound to dominate and conceal the time-varying core signal beyond that critical degree, in very much the same way the permanent component of the lithospheric field dominates and conceals the permanent component of the core field beyond degree 14. All uncertainties taken into account, we estimate N(C) to lie between 22 and 24. We, however, also note that in practice, the main limitation to the observation of the core field small-scale secular variation is not so much its concealing by the field of lithospheric origin but its fast changing nature and small magnitude. This leads us to conclude that whereas cumulative small-scale lithospheric field changes might be detected some day, detection of core-field secular variation beyond degree 18 is likely to remain a severe challenge for some time. C1 [Hulot, Gauthier; Thebault, Erwan] Univ Paris Diderot, Equipe Geomagnetisme, Inst Phys Globe Paris, CNRS,INSU, F-75252 Paris, France. [Olsen, Nils] Univ Copenhagen, DTU Space, DK-2100 Copenhagen, Denmark. [Olsen, Nils] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Hemant, Kumar] NASA, Goddard Space Flight Ctr, ORAU, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. RP Hulot, G (reprint author), Univ Paris Diderot, Equipe Geomagnetisme, Inst Phys Globe Paris, CNRS,INSU, 4 Pl Jussieu, F-75252 Paris, France. EM gh@ipgp.jussieu.fr RI Hulot, Gauthier/A-5627-2011; Olsen, Nils/H-1822-2011; Thebault, Erwan/A-5670-2011 OI Olsen, Nils/0000-0003-1132-6113; FU CNES FX Helpful comments by two anonymous reviewers are gratefully acknowledged. This study was partly supported by CNES. This is IPGP contribution no. 2480. NR 45 TC 14 Z9 18 U1 0 U2 2 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0956-540X J9 GEOPHYS J INT JI Geophys. J. Int. PD MAY PY 2009 VL 177 IS 2 BP 361 EP 366 DI 10.1111/j.1365-246X.2009.04119.x PG 6 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 430TR UT WOS:000265012200004 ER PT J AU Huang, CQ Kim, S Song, K Townshend, JRG Davis, P Altstatt, A Rodas, O Yanosky, A Clay, R Tucker, CJ Musinsky, J AF Huang, Chengquan Kim, Sunghee Song, Kuan Townshend, John R. G. Davis, Paul Altstatt, Alice Rodas, Oscar Yanosky, Alberto Clay, Rob Tucker, Compton J. Musinsky, John TI Assessment of Paraguay's forest cover change using Landsat observations SO GLOBAL AND PLANETARY CHANGE LA English DT Article; Proceedings Paper CT Fall Annual Meeting of the American-Geophysical-Union CY 2005 CL San Francisco, CA SP Amer Geophys Union DE Atlantic forest; Chaco Woodland; forest loss; protected area; Landsat; Paraguay ID PROTECTED AREAS; TROPICAL DEFORESTATION; CONSERVATION; BIODIVERSITY; REGROWTH; AMAZON; AVHRR; MODEL; CHACO AB Comprehensive assessments of Paraguay's forest cover (FC) change from the 1970s to the 2000s using Landsat observations were conducted, including a wall-to-wall mapping of changes across the whole country between the 1990s and 2000s, and an assessment of forest area in the Atlantic Forest ecoregion in the 1970s using a systematic sampling approach. The derived wall-to-wall FC change map was evaluated using available high resolution satellite images and aerial photos. The overall accuracy values were 92% or higher in the areas covered by those high resolution data sets. The results revealed that the Atlantic Forest ecoregion experienced the most forest loss, with the 73.4% forest cover in the 1970s decreasing precipitously down to 40.7% by the 1990s and further down to 24.9% by the 2000s. The rapid loss of Atlantic forests was driven by complex social economic forces, including widespread land disputes arising from long time inequalities and profits from exporting agricultural products. Forest changes in the Humid Chaco and the Chaco ecoregions were relatively moderate. However, extensive forests were converted to non-forest land use near a major population center. The results also revealed that so far the established protected areas were effective in protecting forest within their border. However, most of the forests surrounding the protected areas were lost by the 2000s. Loss of Atlantic forest is a major threat to the rich biodiversity found in this region. The alarming deforestation rates over the last three decades and the low percentage of Atlantic forest left by the 2000s call for immediate actions to halt the trends of forest loss. (C) 2009 Elsevier B.V. All rights reserved. C1 [Huang, Chengquan; Song, Kuan; Townshend, John R. G.; Davis, Paul; Altstatt, Alice; Tucker, Compton J.] Univ Maryland, Dept Geog, College Pk, MD 20742 USA. [Kim, Sunghee; Song, Kuan; Davis, Paul] Univ Maryland, Inst Adv Comp Studies, College Pk, MD 20742 USA. [Tucker, Compton J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Musinsky, John] Conservat Int, Washington, DC 20036 USA. RP Huang, CQ (reprint author), Univ Maryland, Dept Geog, 2181 LeFrak Hall, College Pk, MD 20742 USA. EM cqhuang@umd.edu; sunghee@wam.umd.edu OI Huang, Chengquan/0000-0003-0055-9798 NR 54 TC 51 Z9 59 U1 2 U2 25 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0921-8181 EI 1872-6364 J9 GLOBAL PLANET CHANGE JI Glob. Planet. Change PD MAY PY 2009 VL 67 IS 1-2 SI SI BP 1 EP 12 DI 10.1016/j.gloplacha.2008.12.009 PG 12 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 455JC UT WOS:000266754000002 ER PT J AU Melchiorri, R Encrenaz, T Drossart, P Fouchet, T Forget, F Titov, D Maltagliati, L Altieri, F Vincendon, M Langevin, Y Bibring, JP AF Melchiorri, R. Encrenaz, T. Drossart, P. Fouchet, T. Forget, F. Titov, D. Maltagliati, L. Altieri, F. Vincendon, M. Langevin, Y. Bibring, J. P. TI OMEGA/Mars Express: South Pole Region, water vapor daily variability SO ICARUS LA English DT Article DE Mars, atmosphere; Mars, polar caps; Spectroscopy ID MARTIAN ATMOSPHERE; THARSIS VOLCANOS; MARS; CYCLE; SURFACE; SPECTROMETER; AEROSOLS; DEPOSITS; MODEL AB Polar regions on Mars are the Most Suitable places to observe water vapor daily variability because in,any observation crossing the Pole we can observe very different local time and because the poles are considered to be the main permanent and seasonal water reservoir of the planet. We report on a daily variability of water vapor in the South Pole Region (SPR), observed by OMEGA/Mars Express during the South spring-summer period (Ls similar to 250 degrees-270 degrees) outside the CO(2) ice cap, that has never been observed before by other instruments. We have been able to estimate an increase of few precipitable microns during the day. A possible scenario includes the presence of regolith, or another component that could gather water front the atmosphere, adsorbing the water into the surface during the night time and desorbing it as soon as the Sun reaches sufficient height to heat the ground. This hypothesis is even more plausible considering the presence of observed local enhancements in the morning sections associated with the illumination of the Sun and the total absence in the data for water ice. (c) 2008 Elsevier Inc. All rights reserved. C1 [Melchiorri, R.] NASA, Ames Res Ctr, ORAU NASA Postdoctoral Program, Moffett Field, CA 94035 USA. [Melchiorri, R.; Encrenaz, T.; Drossart, P.; Fouchet, T.] Observ Paris, LESIA, Sect Meudon, Paris, France. [Forget, F.] Lab Metheorol Dynam, Paris, France. [Titov, D.; Maltagliati, L.] Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany. [Altieri, F.] Ist Fis Spazio & Mezzo Interstellare, Rome, Italy. [Vincendon, M.; Langevin, Y.; Bibring, J. P.] Inst Astrophys Spatiale, Orsay, France. RP Melchiorri, R (reprint author), NASA, Ames Res Ctr, ORAU NASA Postdoctoral Program, MS 245-3, Moffett Field, CA 94035 USA. EM riccardo.melchiorri-1@nasa.gov RI Fouchet, Thierry/C-6374-2017 OI Fouchet, Thierry/0000-0001-9040-8285 FU NASA/Ames Research Center FX This research was supported also by all appointment to the NASA Postdoctoral Program at the NASA/Ames Research Center administered by Oak Ridge Associated Universities through a contract with NASA. NR 32 TC 11 Z9 11 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD MAY PY 2009 VL 201 IS 1 BP 102 EP 112 DI 10.1016/j.icarus.2008.12.018 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 444CM UT WOS:000265957900007 ER PT J AU Brozovic, M Ostro, SJ Benner, LAM Giorgini, JD Jurgens, RF Rose, R Nolan, MC Hine, AA Magri, C Scheeres, DJ Margot, JL AF Brozovic, Marina Ostro, Steven J. Benner, Lance A. M. Giorgini, Jon D. Jurgens, Raymond F. Rose, Randy Nolan, Michael C. Hine, Alice A. Magri, Christopher Scheeres, Daniel J. Margot, Jean-Luc TI Radar observations and a physical model of Asteroid 4660 Nereus, a prime space mission target SO ICARUS LA English DT Article DE Radar observations; Asteroids ID NEAR-EARTH ASTEROIDS; 33342 1998 WT24; ENSTATITE ACHONDRITE; DYNAMICAL EVOLUTION; 1620 GEOGRAPHOS; 2867 STEINS; OBJECTS; POPULATION; ITOKAWA; TORQUES AB Near-Earth Asteroid 4660 Nereus has been identified as a potential spacecraft target since its 1982 discovery because of the low delta-V required for a spacecraft rendezvous. However. Surprisingly little is known about its physical characteristics. Here We report Arecibo (S-band, 2380-MHz, 13-cm) and Goldstone (X-band, 8560-MHz, 3.5-cm) radar observations of Nereus during its 2002 close approach. Analysis of an extensive dataset of delay-Doppler images and Continuous wave (CW) spectra yields a model that resembles an ellipsoid with principal axis dimensions X = 510 +/- 20 m, Y = 330 +/- 20 m and Z = 241(+80) m. The pole direction is approximately located at ecliptic pole longitude and latitude Of lambda = +25 degrees, beta = +80 degrees with the uncertainty radius of 10 degrees. Our modeling yields a refined rotation period of 15.16 +/- 0.04 h. Nereus has a circular polarization (SC/OC) ratio of 0.74 +/- 0.08, which implies Substantial near-surface centimeter-to-decimeter scale toughness. Dynamical analysis Of Our model suggests that YORP alteration of the rotation period may become evident within a few years. Nereus has two stable synchronous orbits where natural material may remain in orbit, while most asteroids observed to date do not have Such stable Synchronous orbits. We also find that spacecraft Orbits about Nereus are feasible. (c) 2009 Elsevier Inc. All rights reserved. C1 [Brozovic, Marina; Ostro, Steven J.; Benner, Lance A. M.; Giorgini, Jon D.; Jurgens, Raymond F.; Rose, Randy] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Nolan, Michael C.; Hine, Alice A.] Natl Astron & Ionosphere Ctr, Arecibo Observ, Arecibo, PR 00613 USA. [Magri, Christopher] Univ Maine, Farmington, ME 04938 USA. [Scheeres, Daniel J.] Univ Colorado, Boulder, CO 80309 USA. [Margot, Jean-Luc] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Brozovic, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM marina.brozovic@jpl.nasa.gov RI Margot, Jean-Luc/A-6154-2012; Nolan, Michael/H-4980-2012 OI Margot, Jean-Luc/0000-0001-9798-1797; Nolan, Michael/0000-0001-8316-0680 FU National Aeronautics and Space Administration (NASA) FX We thank the Arecibo and Goldstone technical and support staffs for help with the radar observations. The Arecibo Observatory is part of the National Astronomy and Ionosphere Center, which is operated by Cornell University under a cooperative agreement with the National Science Foundation (NSF) and, at the time of this experiment, also had support from the National Aeronautics and Space Administration (NASA). We are very much in debt to the reviewers, Bob Gaskell and in anonymous reviewer whose comments significantly improved this paper. We would also like to thank Michael W. Busch for useful discussion On SHAPE modeling. Some of this work was performed at the jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. This material is based in part upon work supported by NASA Under the Science Mission Directorate Research and Analysis Programs. NR 70 TC 9 Z9 10 U1 1 U2 1 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD MAY PY 2009 VL 201 IS 1 BP 153 EP 166 DI 10.1016/j.icarus.2008.12.029 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 444CM UT WOS:000265957900011 ER PT J AU Bellucci, A Sicardy, B Drossart, P Rannou, P Nicholson, PD Hedman, M Baines, KH Burrati, B AF Bellucci, A. Sicardy, B. Drossart, P. Rannou, P. Nicholson, P. D. Hedman, M. Baines, K. H. Burrati, B. TI Titan solar occultation observed by Cassini/VIMS: Gas absorption and constraints on aerosol composition SO ICARUS LA English DT Article DE Titan; Occultations; Atmospheres, composition ID DIFFUSE INTERSTELLAR-MEDIUM; MIXED VERTICAL PROFILE; CARBON-MONOXIDE; SPECTROSCOPIC DATABASE; OPTICAL-CONSTANTS; X-RAY; ATMOSPHERE; CO; HAZE; STRATOSPHERE AB A solar occultation by Titan's atmosphere has been observed through the solar port of the Cassini/VIMS instrument on January 15th, 2006. Transmission spectra acquired during solar egress probe the atmosphere in the altitude range 70 to 900 kin at the latitude of 71 degrees S. Several molecular absorption bands of CH(4) and CO are visible in these data. A line-by-line radiative transfer calculation in spherical geometry is used to model three methane hands (1.7, 2.3, 3.3 mu m) and the CO 4.7 mu m hand. Above 200 kin, the methane 2.3 pin hand is well fit with constant mixing ratio between 1.4 and 1.7%, in agreement with in situ and other Cassini measurements. Under 200 km, there are discrepancies between models and observations that are yet fully understood. Under 480 km, the 3.3 mu m CH4 hand is mixed with a large and deep additional absorption. It corresponds to the C-H stretching mode of aliphatic hydrocarbon chains attached to large organic molecules. The CO 4.7 pin hand is observed in the lower stratosphere (altitudes below 150 km) and is well fit with a model with constant mixing ratio of 33 +/- 10 ppm. The Continuum level of the observed transmission spectra provides new constraints on the aerosol content of the atmosphere. A model using fractal aggregates and optical properties of tholins produced by Khare et al. [Khare, B.N., Sagan, C., Arakawa, E.T., Suits, F, Callcott, T.A., Williams, M.W., 1984. Icarus 60, 127-137] is developed. Fractal aggregates with more than 1000 spheres of radius 0.05 mu m are needed to fit the data. Clear differences in the chemical composition are revealed between tholins and actual haze particles. Extinction and density profiles are also retrieved using an inversion of the continuum values. An exponential increase of the haze number density is observed under 420 km with a typical scale height of 60 km. (c) 2009 Elsevier Inc. All rights reserved. C1 [Bellucci, A.; Sicardy, B.; Drossart, P.] Univ Paris Diderot, Univ Paris 06, Observ Paris, Lab Etud Spatiales LESIA, F-92195 Meudon, France. [Sicardy, B.] Inst Univ France, F-75005 Paris, France. [Rannou, P.] Univ Reims, GSMA, UMR 6089, F-51687 Reims, France. [Rannou, P.] Univ Versailles St Quentin, Serv Aeron, UMR 7620, F-91370 Verrieres Le Buisson, France. [Nicholson, P. D.; Hedman, M.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Baines, K. H.; Burrati, B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Sicardy, B (reprint author), Univ Paris Diderot, Univ Paris 06, Observ Paris, Lab Etud Spatiales LESIA, 5 Pl Jules Janssen, F-92195 Meudon, France. EM bruno.sicardy@obspm.fr RI RANNOU, Pascal/I-9059-2012 FU Centre National d'Etudes Spatiales (CNES) FX We thank the Centre National d'Etudes Spatiales (CNES) for Supporting the VIMS data interpretation. We also thank B. Bezard and E. Lellouch for their help in the validation of the radiative transfer code and for the data interpretation. NR 42 TC 51 Z9 51 U1 0 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD MAY PY 2009 VL 201 IS 1 BP 198 EP 216 DI 10.1016/j.icarus.2008.12.024 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 444CM UT WOS:000265957900016 ER PT J AU Barnes, JW Brown, RH Soderblom, JM Soderblom, LA Jaumann, R Jackson, B Le Mouelic, S Sotin, C Buratti, BJ Pitman, KM Baines, KH Clark, RN Nicholson, PD Turtle, EP Perry, J AF Barnes, Jason W. Brown, Robert H. Soderblom, Jason M. Soderblom, Laurence A. Jaumann, Ralf Jackson, Brian Le Mouelic, Stephane Sotin, Christophe Buratti, Bonnie J. Pitman, Karly M. Baines, Kevin H. Clark, Roger N. Nicholson, Phillip D. Turtle, Elizabeth P. Perry, Jason TI Shoreline features of Titan's Ontario Lacus from Cussini/VIMS observations SO ICARUS LA English DT Article DE Titan ID CASSINI RADAR; SURFACE; CLOUDS; ETHANE; OCEAN; LAKES; DIVERSITY; IMAGES; DUNES; SEAS AB We analyze observations of Titan's South polar lake Ontario Lacus obtained by Cassini's Visual and Infrared Mapping Spectrometer during the 38th flyby of Titan (T38: 2007 December 5). These near-closest-approach observations have the highest signal-to-noise, the finest spatial resolution, and the least atmospheric influence of any near-infrared lake observation to date. We use the large, spatially flat, and low-albedo interior of Ontario Lacus as a calibration target allowing LIS to derive ail analytical atmospheric correction for emission angle. The dark lake interior is surrounded by two separate annuli that follow the lake interior's Contours. The inner annulus is uniformly dark, but not so much as the interior lake, and is generally 5-10 kilometers wide at the lake's southeastern margin. We propose that it represents wet lakebed sediments exposed by either tidal sloshing of the lake or seasonal methane loss leading to lower lake-volume. the exterior annulus is bright and shows a spectrum consistent with a relatively low water-ice content relative to the rest of Titan. It may represent fine-grained condensate deposits from a past era of higher lake level. Together, the annuli seem to indicate that the lake level for Ontario Lacus has changed over time. This hypothesis can be tested with observations scheduled for future Titan flybys. (c) 2008 Elsevier Inc. All rights reserved. C1 [Barnes, Jason W.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Barnes, Jason W.] Univ Idaho, Dept Phys, Moscow, ID 83844 USA. [Brown, Robert H.; Soderblom, Jason M.; Jackson, Brian; Perry, Jason] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Soderblom, Laurence A.] US Geol Survey, Flagstaff, AZ 86001 USA. [Jaumann, Ralf] DLR, Inst Planetary Res, D-12489 Berlin, Germany. [Le Mouelic, Stephane] Univ Nantes, CNRS, Lab Planetol & Geodynam, UMR6112, Nantes, France. [Sotin, Christophe; Buratti, Bonnie J.; Pitman, Karly M.; Baines, Kevin H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Clark, Roger N.] US Geol Survey, Denver, CO 80225 USA. [Nicholson, Phillip D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Turtle, Elizabeth P.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Barnes, JW (reprint author), NASA, Ames Res Ctr, Mail Stop 244-30, Moffett Field, CA 94035 USA. EM jason@barnesos.net RI Barnes, Jason/B-1284-2009; Turtle, Elizabeth/K-8673-2012; OI Barnes, Jason/0000-0002-7755-3530; Turtle, Elizabeth/0000-0003-1423-5751; Soderblom, Jason/0000-0003-3715-6407 FU NASA Postdoctoral Program Fellowship at NASA Ames Research Center; Cassini VIMS team FX J.W.B. is supported by a NASA Postdoctoral Program Fellowship at NASA Ames Research Center administrated by Oak Ridge Associated Universities. J.W.B. also acknowledges support from the Cassini VIMS team. Thank you to the 2008 LPL beaches field trip participants for their comments and patience. NR 35 TC 43 Z9 43 U1 1 U2 2 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD MAY PY 2009 VL 201 IS 1 BP 217 EP 225 DI 10.1016/j.icarus.2008.12.028 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 444CM UT WOS:000265957900017 ER PT J AU Wiegert, P Vaubaillon, J Campbell-Brown, M AF Wiegert, Paul Vaubaillon, Jeremie Campbell-Brown, Margaret TI A dynamical model of the sporadic meteoroid complex SO ICARUS LA English DT Article DE Meteors; Comets; Asteroids; Interplanetary dust; Earth ID VELOCITY DISTRIBUTION; HEAD-ECHOES; SOLAR-SYSTEM; HIGH-POWER; 2003 EH1; RADAR; COMET; ORBIT; DISTRIBUTIONS; PARENT AB Sporadic meteoroids are the most abundant yet least understood component of tire Earth's meteoroid complex. This paper aims to build a physics-based model of this complex calibrated with five years of radar observations. The model of the sporadic meteoroid complex presented here Includes the effects of the Sun and all eight planets, radiation forces and collisions. The model Uses the observed meteor patrol radar strengths of the sporadic meteors to solve for the dust production rates of the populations of cornets modeled, as well as the mass index. The model can explain sonic of the differences between the meteor velocity distributions seen by transverse versus radial scatter radars. The different ionization limits Of the two techniques result in their looking, at different populations with different velocity distributions. Radial scatter radars see primarily meteors from 55P/Tempel-Tuttle (or an orbitally similar lost comet), while transverse scatter radars are dominated by larger meteoroids from the Jupiter-family comets. In fact our results suggest that the sporadic complex is better understood as originating from a small number of cornets which transfer material to near-Earth space quite efficiently, rather than as a product of the cometary population as a whole. The model also sheds light on variations in the mass index reported by different radars, revealing it to be a result of their sampling different portions of the meteorois population. In addition, we find that a mass index of s = 2.34 as observed at Faith requires a shallower index (s = 2.2) at the time of meteoroid production because of size-dependent processes in the evolution of meteoroids. The model also reveals the origin of the 55 degrees radius ring seen centered on the Earth's apex (a result of high-inclination meteoroids undergoing Kozai oscillation) and the central condensations seen in the apex sources, as well as providing insight into the strength asymmetry of the helion and anti-helion sources. (c) 2009 Elsevier Inc. All rights reserved. C1 [Wiegert, Paul; Campbell-Brown, Margaret] Univ Western Ontario, Dept Phys & Astron, London, ON, Canada. [Vaubaillon, Jeremie] CALTECH, Jet Prop Lab, Spitzer Space Ctr, Pasadena, CA 91125 USA. RP Wiegert, P (reprint author), Univ Western Ontario, Dept Phys & Astron, London, ON, Canada. EM pwiegert@uwo.ca FU NASA Meteoroid Environment Office; Natural Sciences and Engineering Research Council of Canada FX We thank David Asher and an anonymous referee for their through reviews which much improved this work. This research was supported in part by the NASA Meteoroid Environment Office and the Natural Sciences and Engineering Research Council of Canada. NR 48 TC 42 Z9 42 U1 1 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAY PY 2009 VL 201 IS 1 BP 295 EP 310 DI 10.1016/j.icarus.2008.12.030 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 444CM UT WOS:000265957900022 ER PT J AU Smith, AW Lissauer, JJ AF Smith, Andrew W. Lissauer, Jack J. TI Orbital stability of systems of closely-spaced planets SO ICARUS LA English DT Article DE Planetary dynamics; Celestial mechanics; Extrasolar planets ID PROTOPLANET SYSTEM; INSTABILITY; DYNAMICS AB An investigation of the stability of systems of 1 M(circle plus) (Earth-mass) bodies orbiting a Sun-like star has been conducted for Virtual times reaching 10 billion years. For the majority of the tests, a symplectic integrator with a fixed timestep of between 1 and 10 clays was employed: however, smaller timesteps and a Bulirsch-Stoer integrator were also selectively utilized to increase confidence in the results. In most cases, the planets were started on initially coplanar, circular orbits, and the longitudinal initial positions of neighboring planets were widely separated. The ratio of the semimajor axes of consecutive planets in each system Was approximately uniform (so the spacing between consecutive planets increased slowly in terms of distance from the star). The stability time for a system was taken to be the time at which the orbits of two or more planets crossed. Our results show that, for a given class of system (e.g., three 1 M(circle plus) planets), orbit crossing times vary with planetary spacing approximately as a power law over a wide range of separation in semimajor axis, Chaos tests indicate that deviations from this power law persist for changed initial longitudes and also for small but non-trivial changes in orbital spacing. We find that the stability time increases more rapidly at large initial orbital separations than the power-law dependence predicted from moderate initial orbital separations. Systems of five planets are less stable than systems of three planets for a specified semimajor axis spacing. Furthermore, systems of less massive planets can be packed more closely, being about as stable as 1 M(circle plus) planets when the radial separation between planets is scaled using the Mutual Hin radius. Finally, systems with retrograde planets can be packed Substantially more closely than prograde systems with equal numbers of planets. (c) 2008 Elsevier Inc. All rights reserved. C1 [Lissauer, Jack J.] NASA, Div Space Sci, Ames Res Ctr, Moffett Field, CA 94035 USA. [Smith, Andrew W.] Stanford Univ, Dept Mech Engn, Stanford, CA 94305 USA. RP Lissauer, JJ (reprint author), NASA, Div Space Sci, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA. EM awsmith@stanford.edu; Jack.J.Lissauer@nasa.gov FU NASA's Planetary Geology & Geophysics Program [RTOP 344-30-50-01] FX This work was supported by NASA's Planetary Geology & Geophysics Program through RTOP 344-30-50-01. We thank Eric Ford, John Charribers, Tony Dobrovolskis, and Kevin Zahnle for helpful comments on the manuscript, Amanda Hoffmann for her generous donation of CPU time, and Jason Barnes for helpful discussions regarding integrators. NR 18 TC 62 Z9 62 U1 0 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD MAY PY 2009 VL 201 IS 1 BP 381 EP 394 DI 10.1016/j.icarus.2008.12.027 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 444CM UT WOS:000265957900026 ER PT J AU Chapin, E Chen, CW AF Chapin, Elaine Chen, Curtis W. TI Airborne Along-Track Interferometry for GMTI SO IEEE AEROSPACE AND ELECTRONIC SYSTEMS MAGAZINE LA English DT Article CT 2008 IEEE Radar Conference CY MAY 26-30, 2008 CL Rome, ITALY SP IEEE, FINMECCANICA, SELEX, Agilent Technol, Dappolonia, Gedae, IDS, IET, MBDA, McGraw Hill, Natl Instruments, Off Naval Res, Sci & Technol, ROHDE & SCHWARZ, Tektronix, Thales Alenia, altran, ACCSCO, Raytheon AB Synthetic Aperture Radar (SAR) Along-Track Interferometry (ATI) has been used extensively to measure ocean surface currents. Given its ability to measure small velocities (similar to 10 cm/s) of relatively radar-dark water surfaces, there is great potential that this technique can be adapted for ground moving target indication (GMTI) applications, particularly as a method for detecting very slow targets with small radar cross-sections. Herein, we describe preliminary results from an ATI GMTI experiment. The SAR data described were collected by the dual-frequency NASA/JPL airborne radar in its standard dual-baseline ATI mode. The radar system imaged a variety of control targets including a pick-up truck, sport utility vehicles, passenger cars, a bicycle, and pedestrians over multiple flight passes. The control targets had horizontal velocities of less than 5 m/s. The cross-sections of the targets were not purposely enhanced, although the targets' reflectivities may have been affected by the existence of the GPS equipment used to record the targets' positions. Single-look and multiple-look interferograms processed to the full azimuth resolution were analyzed. In the data processed to date, all of the targets were observed by visual inspection in at least one of the four combinations of dual-frequency, dual-baseline interferometric data. This extremely promising result demonstrates the potential of ATI for GMTI applications. C1 [Chapin, Elaine; Chen, Curtis W.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Chapin, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Rd, Pasadena, CA 91125 USA. NR 6 TC 8 Z9 19 U1 0 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0885-8985 J9 IEEE AERO EL SYS MAG JI IEEE Aerosp. Electron. Syst. Mag. PD MAY PY 2009 VL 24 IS 5 BP 13 EP 18 PG 6 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA 460DP UT WOS:000267168400004 ER PT J AU Najafizadeh, L Adams, JS Phillips, SD Moen, KA Cressler, JD Aslam, S Stevenson, TR Meloy, RM AF Najafizadeh, Laleh Adams, Joseph S. Phillips, Stanley D. Moen, Kurt A. Cressler, John D. Aslam, Shahid Stevenson, Thomas R. Meloy, Robert M. TI Sub-1-K Operation of SiGe Transistors and Circuits SO IEEE ELECTRON DEVICE LETTERS LA English DT Article DE Analog integrated circuits; BiCMOS; cryogenic temperatures; heterojunction bipolar transistor (HBT); silicon germanium (SiGe); SiGe HBTs; voltage reference ID TEMPERATURE; ELECTRONICS; REFERENCES AB We present the first measurement results for silicon-germanium (SiGe) heterojunction bipolar transistors (HBTs) and SiGe BiCMOS circuits operating in the sub-1-K regime. Robust transistor operation of a first-generation 0.5 x 2.5 x 4-mu m(2) SiGe transistor is demonstrated at package temperatures as low as 300 mK. In addition, a SiGe BiCMOS bandgap voltage reference is verified to be fully functional at operating temperatures below 700 mK. The SiGe voltage reference exhibits a temperature coefficient of 160 ppm/degrees C over the temperature range of 700 mK-300 K. C1 [Najafizadeh, Laleh; Phillips, Stanley D.; Moen, Kurt A.; Cressler, John D.] Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. [Adams, Joseph S.] Univ Maryland, Baltimore, MD 21250 USA. [Aslam, Shahid; Meloy, Robert M.] MEI Technol Inc, Lanham, MD 20706 USA. [Aslam, Shahid; Stevenson, Thomas R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Najafizadeh, L (reprint author), Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. EM laleh@ece.gatech.edu; Joseph.S.Adams@nasa.gov; stan.phillips@gatech.edu; kmoen@ece.gatech.edu; cressler@ece.gatech.edu; Shahid.Aslam-1@nasa.gov; Thomas.R.Stevens6@nasa.gov; bmeloy@hst.nasa.gov RI Aslam, Shahid/D-1099-2012 FU National Aeronautics and Space Administration FX Manuscript received January 15, 2009; revised February 21, 2009. Current version published April 28, 2009. This work was supported by the National Aeronautics and Space Administration. The review of this letter was arranged by Editor M, Ostling. NR 16 TC 15 Z9 15 U1 0 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0741-3106 J9 IEEE ELECTR DEVICE L JI IEEE Electron Device Lett. PD MAY PY 2009 VL 30 IS 5 BP 508 EP 510 DI 10.1109/LED.2009.2016767 PG 3 WC Engineering, Electrical & Electronic SC Engineering GA 440PH UT WOS:000265711700028 ER PT J AU White, RJ Peng, GCY Demir, SS AF White, Ronald J. Peng, Grace C. Y. Demir, Semahat S. TI Multiscale Modeling of Biomedical, Biological, and Behavioral Systems (Part 2) Understanding the Body from Atoms to Cells to Tissues to Organs to Populations SO IEEE ENGINEERING IN MEDICINE AND BIOLOGY MAGAZINE LA English DT Editorial Material C1 [Peng, Grace C. Y.] Natl Inst Biomed Imaging & Bioengn, NIH, Bethesda, MD 20892 USA. [Peng, Grace C. Y.] Catholic Univ Amer, Washington, DC 20064 USA. [Peng, Grace C. Y.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [White, Ronald J.] NASA, Human Res Program, Washington, DC USA. [White, Ronald J.] Baylor Coll Med, Houston, TX 77030 USA. [White, Ronald J.] NASA Headquarters, Div Life Sci, Washington, DC USA. [White, Ronald J.] Uniformed Serv Univ Hlth Sci, Bethesda, MD 20814 USA. [White, Ronald J.] Univ Louisiana Lafayette, Lafayette, LA USA. [Demir, Semahat S.] NASA, SLS 1, Washington, DC USA. [Demir, Semahat S.] NASA, IML 1, Washington, DC USA. [Demir, Semahat S.] NASA, US Component German Spacelab Miss D 2, Washington, DC USA. RP Peng, GCY (reprint author), Natl Inst Biomed Imaging & Bioengn, NIH, 6707 Democracy Blvd,Suite 200,MSC 5469, Bethesda, MD 20892 USA. EM penggr@mail.nih.gov NR 0 TC 4 Z9 4 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0739-5175 J9 IEEE ENG MED BIOL JI IEEE Eng. Med. Biol. Mag. PD MAY-JUN PY 2009 VL 28 IS 3 BP 8 EP 9 DI 10.1109/MEMB.2009.932490 PG 2 WC Engineering, Biomedical; Medical Informatics SC Engineering; Medical Informatics GA 449BK UT WOS:000266305600004 PM 19457728 ER PT J AU Levin, J Ioannou, P AF Levin, Jason Ioannou, Petros TI Adaptive Mode-Suppression and Disturbance-Rejection Scheme With Application to Disk Drives SO IEEE TRANSACTIONS ON CONTROL SYSTEMS TECHNOLOGY LA English DT Article DE Adaptive control; disk drives; disturbance rejection; neural networks; radial basis functions (RBFs); servo control ID NOTCH FILTER; SYSTEM-IDENTIFICATION; RUNOUT COMPENSATION; NEURAL-NETWORKS; SERVO CONTROL; CONTROLLER AB The goal of a track-following controller for a disk drive is to maintain as close to perfect tracking as possible. Better tracking allows for more data to be stored on a single disk. There are several factors which make this control problem difficult, such as high-frequency resonant modes, unknown disturbances, and a preset sampling rate. The resonant modes of a disk drive are often uncertain and vary between units and can also lie near or beyond the Nyquist frequency. Suppressing these modes can be difficult. However, a multirate adaptive notch filter and adaptive bandwidth controller is proposed to suppress these resonant modes. A robust online estimator that estimates the mode frequencies is used to allow the multirate adaptive notch filter to track the disk drive's modes. By adding a multirate scheme to the adaptive notch filter, it can suppress modes at higher frequencies, which are close to or beyond the Nyquist frequency of the preset sampling rate. As the multirate adaptive notch filter tracks the plant mode frequencies, the adaptive bandwidth controller ensures that stability and performance requirements are satisfied by using the online estimate of the mode frequencies. An adaptive disturbance rejector is added to the adaptive mode-suppression scheme and broken into two parts: a part to suppress the repeatable runout and another to attenuate the residual disturbance by using a neural model. Both parts are adapted online and combined with the mode-suppression scheme to ensure good disturbance rejection even in the presence of unknown or changing resonant modes. Simulation results with a hard disk drive as the application are included and show that the adaptive mode-suppression scheme is able to maintain stability and better performance than a nonadaptive counterpart for an uncertain resonant-mode frequency. When combined with the adaptive disturbance-rejection scheme, stability is maintained and an improvement of as much as 14.3% in 3 sigma is seen. This improvement in tracking can allow for data to be stored more densely on a single disk, providing larger storage media for the same size of disk drive. C1 [Levin, Jason; Ioannou, Petros] Univ So Calif, Dept Elect Engn Syst, So Calif Ctr Adv Transportat Technol, Los Angeles, CA 90089 USA. [Levin, Jason] Jet Prop Lab, Pasadena, CA 91103 USA. [Ioannou, Petros] Univ So Calif, Dept Aerosp & Mech Engn, Los Angeles, CA 90089 USA. RP Levin, J (reprint author), Univ So Calif, Dept Elect Engn Syst, So Calif Ctr Adv Transportat Technol, Los Angeles, CA 90089 USA. EM levinj@usc.edu; ioannou@usc.edu FU NSF Award [CMS-0510921]; NASA [NCC4-158] FX This work was supported in part by NSF Award CMS-0510921 and by NASA Grant NCC4-158. NR 37 TC 6 Z9 6 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1063-6536 EI 1558-0865 J9 IEEE T CONTR SYST T JI IEEE Trans. Control Syst. Technol. PD MAY PY 2009 VL 17 IS 3 BP 620 EP 632 DI 10.1109/TCST.2008.2002813 PG 13 WC Automation & Control Systems; Engineering, Electrical & Electronic SC Automation & Control Systems; Engineering GA 440PG UT WOS:000265711600011 ER PT J AU Trigwell, S Captain, JG Arens, EE Quinn, JW Calle, CI AF Trigwell, Steve Captain, James G. Arens, Ellen E. Quinn, Jacqueline W. Calle, Carlos I. TI The Use of Tribocharging in the Electrostatic Beneficiation of Lunar Simulant SO IEEE TRANSACTIONS ON INDUSTRY APPLICATIONS LA English DT Article; Proceedings Paper CT Joint Conference of the Electrostatics-Society-of-America/IEEE-Industrial-Applications-Society/I nstitute-of-Electrostatics-Japan/Societe-Francaise-of-Electrostatique CY JUN 06-09, 2006 CL Berkeley, CA SP Electrostat Soc Amer, IEEE Ind Applicat Soc, Inst Electrostat Japan, Soc Francaise Electrostat DE Beneficiation; lunar simulant; tribocharging; work function; X-ray photoelectron spectroscopy (XPS) AB The use of tribocharging as a potential method to provide sufficient charge to several different lunar simulants for electrostatic beneficiation was investigated. The objective was to determine whether specific minerals of interest (e.g., ilmenite) that are present in lunar regolith could be enriched in concentration by beneficiation that would therefore allow for more efficient extraction for in situ resource utilization use. The production of oxygen, water, and other resources on the Moon from raw materials is vital for future missions to the Moon. Successful separation of ilmenite was achieved for a prepared simulant (KSC-1), which is a mixture of pure commercially supplied pyroxene, olivine, feldspar, and ilmenite, in a 4:4: 1 : 1 ratio, showing proof of concept when tribocharged against three different charging materials, namely, Al, Cu, and PTFE. Separation by chemical composition was also observed for existing lunar simulants JSC-1 and JSC-1A; however, the interpretation of the separation was difficult due to the complex mineralogy of the simulants compared to the simple prepared mixture. C1 [Trigwell, Steve; Captain, James G.] ASRC Aerosp ASRC 24, Appl Sci & Technol Dept, Kennedy Space Ctr, FL 32899 USA. [Arens, Ellen E.; Quinn, Jacqueline W.; Calle, Carlos I.] NASA, Kennedy Space Ctr, FL 32899 USA. RP Trigwell, S (reprint author), ASRC Aerosp ASRC 24, Appl Sci & Technol Dept, Kennedy Space Ctr, FL 32899 USA. EM steven.trigwell-1@nasa.gov; james.g.captain@nasa.gov; ellen.e.arens@nasa.gov; jacqueline.w.quinn@nasa.gov; carlos.i.calle@nasa.gov NR 14 TC 11 Z9 11 U1 1 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0093-9994 J9 IEEE T IND APPL JI IEEE Trans. Ind. Appl. PD MAY-JUN PY 2009 VL 45 IS 3 BP 1060 EP 1067 DI 10.1109/TIA.2009.2018976 PG 8 WC Engineering, Multidisciplinary; Engineering, Electrical & Electronic SC Engineering GA 451EE UT WOS:000266452700018 ER PT J AU Hatamleh, O AF Hatamleh, Omar TI A comprehensive investigation on the effects of laser and shot peening on fatigue crack growth in friction stir welded AA 2195 joints SO INTERNATIONAL JOURNAL OF FATIGUE LA English DT Article DE Friction stir welding; Laser peening; Shot peening; Fatigue crack growth; Stress ratio, 2195 ID RESIDUAL-STRESS MEASUREMENTS; ALUMINUM-ALLOYS; MECHANICAL-PROPERTIES; WELDING SPEED; BEHAVIOR; MICROSTRUCTURE; CORROSION; PROPAGATION; LITHIUM; LIFE AB The effects of various surface treatment techniques on the fatigue crack growth performance of friction stir welded 2195 aluminum alloy were investigated. The objective was to reduce fatigue crack growth rates and enhance the fatigue life of welded joints. The crack growth rates were assessed and characterized for different peening conditions at a stress ratio (R) of 0.1, and 0.7. The surface and through-thickness residual stress distribution were also investigated and presented for the various regions in the weld. Tensile residual stresses introduced during the welding process were found to become significantly compressive, particularly after laser peening. The effect of the compressive stresses was deemed responsible for increasing the resistance to fatigue crack growth of the welds. The results indicate a significant reduction in fatigue crack growth rates using laser peening compared to shot peening and native welded specimens. This reduced fatigue crack growth rate was comparable to the base unwelded material. Published by Elsevier Ltd. C1 NASA, Lyndon B Johnson Space Ctr, Struct Branch, Houston, TX 77058 USA. RP Hatamleh, O (reprint author), NASA, Lyndon B Johnson Space Ctr, Struct Branch, Houston, TX 77058 USA. EM omar.hatamleh-1@nasa.gov NR 68 TC 48 Z9 50 U1 1 U2 27 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0142-1123 J9 INT J FATIGUE JI Int. J. Fatigue PD MAY PY 2009 VL 31 IS 5 BP 974 EP 988 DI 10.1016/j.ijfatigue.2008.03.029 PG 15 WC Engineering, Mechanical; Materials Science, Multidisciplinary SC Engineering; Materials Science GA 421JK UT WOS:000264355000019 ER PT J AU Carney, KS Pereira, JM Revilock, DM Matheny, P AF Carney, K. S. Pereira, J. M. Revilock, D. M. Matheny, P. TI Jet engine fan blade containment using an alternate geometry SO INTERNATIONAL JOURNAL OF IMPACT ENGINEERING LA English DT Article DE Containment; Fan case; Blade off; Turbine engine; Very high strain rate material behavior ID STRAIN-RATE COMPRESSION; ALLOYS AB With a goal of reducing jet engine weight. simulations of a fan blade containment system with an alternate geometry were tested and analyzed. A projectile simulating a fan blade was shot at two alternate geometry containment case configurations using a gas gun. The first configuration was a flat plate representing a standard case configuration. The second configuration was a flat plate with a radially convex curve section at the impact point. The curved surface was designed to force the blade to deform plastically, dissipating energy before the full impact of the blade is received by the plate. The curved case was able to tolerate a higher impact velocity before failure. The computational model was developed and correlated with the tests and a weight savings assessment was performed. For the particular test configuration used in this study the ballistic impact velocity of the curved plate was approximately 60 m/s (200 ft/s) greater than that of the flat plate. For the computational model to successfully duplicate the test, the very high strain rate behavior of the materials had to be incorporated. Published by Elsevier Ltd. C1 [Carney, K. S.; Pereira, J. M.; Revilock, D. M.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Matheny, P.] Florida Turbine Technol, W Palm Beach, FL USA. RP Carney, KS (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM kelly.s.carney@nasa.gov NR 24 TC 15 Z9 17 U1 1 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0734-743X J9 INT J IMPACT ENG JI Int. J. Impact Eng. PD MAY PY 2009 VL 36 IS 5 BP 720 EP 728 DI 10.1016/j.ijimpeng.2008.10.002 PG 9 WC Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA 421MB UT WOS:000264361900008 ER PT J AU Vaishampayan, P Miyashita, M Ohnishi, A Satomi, M Rooney, A La Duc, MT Venkateswaran, K AF Vaishampayan, Parag Miyashita, Mika Ohnishi, Akihiro Satomi, Masataka Rooney, Alejandro La Duc, Myron T. Venkateswaran, Kasthuri TI Description of Rummeliibacillus stabekisii gen. nov., sp nov and reclassification of Bacillus pycnus Nakamura et al. 2002 as Rummeliibacillus pycnus comb. nov. SO INTERNATIONAL JOURNAL OF SYSTEMATIC AND EVOLUTIONARY MICROBIOLOGY LA English DT Article ID SPACECRAFT-ASSEMBLY FACILITY; CLASSIFICATION; SPHAERICUS; RESISTANT; BACTERIA; PROPOSAL; NEIDEI; SPORES AB Strains of aerobic, Gram-positive, rod-shaped, round-spore-forming bacteria were isolated from different geographical locations and a subsequent polyphasic study was undertaken to clarify the T taxonomic position of the round-spore-forming isolates strain KSC-SF6g(T), strain M32 and strain NBRC 12622. 16S rRNA gene sequence similarities demonstrated that these strains were most closely affiliated with Bacillus pycnus NRRL NRS-1691(T) (98%), with species of Kurthia (96%) and Viridibacillus (94-96%) as the next nearest relatives. However, while DNA-DNA hybridization studies showed approx. 70% reassociation among strains KSC-SF6g(T), M32 and NBRC 12622, DNA-DNA hybridization values between these strains and B. pycnus NRRL NRS-1691(T) never exceeded 13%. Differences in the molecular structure of the cell-wall peptidoglycan could not differentiate these strains sufficiently from other closely related genera (Viridibacillus and Kurthia). However, Lys-Asp was present in strains KSC-SF6g(T), M32 and NBRC 12622, whereas L-Lys-D-Glu was reported in B. pycnus NRRL NRS-1691(T). The menaquinone MK-7 was dominant in strains KSC-SF6g(T), M32 and NBRC 12622 and members of the genus Kurthia, whereas MK-8 was abundant in Viridibacillus species. Strains KSC-SF6g(T), M32 and NBRC 12622 exhibited fatty acid profiles consisting of major amounts of anteiso-C(15:0) (similar to 50%) and iso-C(15:0) (similar to 25%) and moderate amounts of anteiso-C(17:0) (similar to 7%), which discriminated them from closely related B. pycnus NRRL NRS-1691(T) and species of Viridibacillus (iso-C15:0; 46-74%). The authors propose that strains KSC-SF6g(T), M32 and NBRC 12622 and B. pycnus NRRL NRS-1691(T) be reclassified into a separate genus based on clear-cut differences in discriminative taxonomic markers and the distant placement of B. pycnus and the novel strains described herein from other species of this clade according to current 16S rRNA gene sequence-based relatedness (similar to 4% difference in sequence). We propose the placement of these isolates into the novel genus Rummeliibacillus gen. nov. For the new taxon comprising strains KSC-SF6g(T), M32 and NBRC 12622, we propose the name Rummeliibacillus stabekisii gen. nov., sp. nov. (the type species of Rummeliibacillus), represented by the type strain KSC-SF6g(T) (=NRRL B-51320(T) =NBRC 104870(T)). In addition, Bacillus pycnus, which bears traits distinct from other round-spore-forming species [i.e. absence of growth at high NaCl (7%), positive reaction for gelatin liquefaction], is reclassified as Rummeliibacillus pycnus comb. nov. (type strain JCM 11075(T) =NRRL NRS-1691(T)) based on phylogenetic affiliations and phenotypic characterization. C1 [Vaishampayan, Parag; La Duc, Myron T.; Venkateswaran, Kasthuri] CALTECH, Biotechnol & Planetary Protect Grp, Jet Prop Lab, Pasadena, CA 91109 USA. [Miyashita, Mika] Biol Res Ctr, Natl Inst Technol & Evaluat, Chiba 2920818, Japan. [Ohnishi, Akihiro] Tokyo Univ Agr, Dept Fermentat Sci, Fac Appl Biosci, Setagaya Ku, Tokyo 1568502, Japan. [Satomi, Masataka] Fisheries Res Agcy, Natl Res Inst Fisheries Sci, Yokohama, Kanagawa 2368648, Japan. [Rooney, Alejandro] Natl Ctr Agr Utilizat Res, USDA, Peoria, IL 61604 USA. RP Venkateswaran, K (reprint author), CALTECH, Biotechnol & Planetary Protect Grp, Jet Prop Lab, Pasadena, CA 91109 USA. EM kjvenkat@jpl.nasa.gov FU National Aeronautics and Space Administration; NRA-ROSES; Cassie Conley FX The research described in this publication was carried out at the jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This research was funded by a 2006 NRA-ROSES grant. We are grateful to Cassie Conley for such funding. The authors extend thanks to Shariff Osman for sampling and to all of the members of the JPL Biotechnology and Planetary Protection Group for technical assistancc. NR 24 TC 19 Z9 26 U1 0 U2 8 PU SOC GENERAL MICROBIOLOGY PI READING PA MARLBOROUGH HOUSE, BASINGSTOKE RD, SPENCERS WOODS, READING RG7 1AG, BERKS, ENGLAND SN 1466-5026 J9 INT J SYST EVOL MICR JI Int. J. Syst. Evol. Microbiol. PD MAY PY 2009 VL 59 BP 1094 EP 1099 DI 10.1099/ijs.0.006098-0 PG 6 WC Microbiology SC Microbiology GA 450UL UT WOS:000266426400030 PM 19406799 ER PT J AU Foster, JS Green, SJ Ahrendt, SR Golubic, S Reid, RP Hetherington, KL Bebout, L AF Foster, Jamie S. Green, Stefan J. Ahrendt, Steven R. Golubic, Stjepko Reid, R. Pamela Hetherington, Kevin L. Bebout, Lee TI Molecular and morphological characterization of cyanobacterial diversity in the stromatolites of Highborne Cay, Bahamas SO ISME JOURNAL LA English DT Article DE cyanobacteria; stromatolites; microbial diversity ID MODERN MARINE STROMATOLITES; HYPERSALINE MICROBIAL MAT; POLYMERIC SECRETIONS EPS; RIBOSOMAL-RNA GENES; COMMUNITY STRUCTURE; SP-NOV; ENDOLITHIC CYANOBACTERIA; SUBTIDAL STROMATOLITES; FORMING CYANOBACTERIA; VERTICAL MIGRATION AB Stromatolites are sedimentary deposits that are the direct result of interactions between microbes and their surrounding environment. Once dominant on ancient Earth, actively forming stromatolites now occur in just a few remote locations around the globe, such as the island of Highborne Cay, Bahamas. Although the stromatolites of Highborne Cay contain a wide range of metabolically diverse organisms, photosynthetic cyanobacteria are the driving force for stromatolite development. In this study, we complement previous morphological data by examining the cyanobacterial phylogenetic and physiological diversity of Highborne Cay stromatolites. Molecular analysis of both clone and culture libraries identified 33 distinct phylotypes within the stromatolites. Culture libraries exhibited several morphologically similar but genetically distinct ecotypes, which may contribute to ecosystem stability within the stromatolites. Several of the cultured isolates exhibited both a positive phototactic response and light-dependent extracellular polymeric secretions production, both of which are critical phenotypes for stromatolite accretion and development. The results of this study reveal that the genetic diversity of the cyanobacterial populations within the Highborne Cay stromatolites is far greater than previous estimates, indicating that the mechanisms of stromatolite formation and accretion may be more complex than had been previously assumed. The ISME Journal (2009) 3, 573-587; doi:10.1038/ismej.2008.129; published online 15 January 2009 C1 [Foster, Jamie S.; Ahrendt, Steven R.; Hetherington, Kevin L.] Univ Florida, Space Life Sci Lab, Dept Microbiol & Cell Sci, Kennedy Space Ctr, FL 32899 USA. [Green, Stefan J.] Florida State Univ, Dept Oceanog, Tallahassee, FL 32306 USA. [Golubic, Stjepko] Boston Univ, Dept Biol, Boston, MA 02215 USA. [Reid, R. Pamela] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. [Bebout, Lee] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA. RP Foster, JS (reprint author), Univ Florida, Space Life Sci Lab, Dept Microbiol & Cell Sci, Bldg M6-1025,Room 234, Kennedy Space Ctr, FL 32899 USA. EM jfoster@ufl.edu RI Green, Stefan/C-8980-2011; OI Green, Stefan/0000-0003-2781-359X FU Florida Space Research and Education, Florida Space Grant Consortium (UCF) [UCF-0000127787]; Department of Microbiology and Cell Science, University of Florida [0649198]; NSF Biocomplexity [EAR-0221796] FX We would like to thank Olivier Braissant, John Stolz and Pieter Visscher for helpful discussions and critical review of this article. We would also like to thank Tracy Cote and Alice Herbert for their technical assistance. This work was supported by a Florida Space Research and Education grant awarded to JSF by the Florida Space Grant Consortium (UCF Project no. UCF-0000127787). An NSF REU grant (no. 0649198) awarded to the Department of Microbiology and Cell Science, University of Florida supported SA Transportation and field collection was supported by the NSF Biocomplexity grant EAR-0221796 awarded to RPR. NR 86 TC 53 Z9 55 U1 2 U2 22 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1751-7362 J9 ISME J JI ISME J. PD MAY PY 2009 VL 3 IS 5 BP 573 EP 587 DI 10.1038/ismej.2008.129 PG 15 WC Ecology; Microbiology SC Environmental Sciences & Ecology; Microbiology GA 444DK UT WOS:000265960400007 PM 19148145 ER PT J AU Dick, SJ AF Dick, Steven J. TI The Transit of Venus Enterprise in Victorian Britain. SO JOURNAL FOR THE HISTORY OF ASTRONOMY LA English DT Book Review C1 [Dick, Steven J.] NASA, Washington, DC 20546 USA. RP Dick, SJ (reprint author), NASA, Washington, DC 20546 USA. EM Steven.J.Dick@nasa.gov NR 1 TC 0 Z9 0 U1 0 U2 2 PU SCIENCE HISTORY PUBLICATIONS LTD PI CAMBRIDGE PA 16 RUTHERFORD RD, CAMBRIDGE CB2 2HH, ENGLAND SN 0021-8286 J9 J HIST ASTRON JI J. Hist. Astron. PD MAY PY 2009 VL 40 BP 232 EP 233 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 445QB UT WOS:000266065500016 ER PT J AU Jardin, MR Mueller, ER AF Jardin, Matt R. Mueller, Eric R. TI Optimized Measurements of Unmanned-Air-Vehicle Mass Moment of Inertia with a Bifilar Pendulum SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT AIAA Guidance, Navigation, and Control Conference CY AUG 20-23, 2007 CL Hilton Head Isl, SC AB A bifilar (two-wire) pendulum is a torsional pendulum consisting of a test object suspended by two thin parallel wires. The pendulum oscillates about the vertical axis. The restoring torque of the bifilar pendulum is provided by the gravitational force as rotations from the rest state cause the test object to raise slightly. The mass moment of inertia is computed using dynamic modeling, measurements of the oscillation period, and the physical dimensions of the bifilar pendulum such as the length and separation displacement of the pendulum wires. A simulation technique is described that improves estimates of the mass moment of inertia by considering the nonlinear effects of damping and large angular displacements. An analysis of the error variance of mass moment of inertia measurements is also described. The resulting expression for the error variance is used to optimize the physical parameters of the bifilar pendulum to obtain the moment of inertia measurement with the minimum error variance. Monte Carlo simulations were used to validate the parameter optimization technique. Experimental results are presented for a uniform-density test object for which the moment of inertia is straightforward to compute from geometric considerations. Results are also presented for a small unmanned air vehicle, which was the intended application for this moment of inertia measurement technique. C1 [Jardin, Matt R.] MathWorks Inc, Consulting Serv Grp, Natick, MA 01760 USA. [Mueller, Eric R.] NASA, Ames Res Ctr, Automat Concepts Res Branch, Moffett Field, CA 94035 USA. RP Jardin, MR (reprint author), MathWorks Inc, Consulting Serv Grp, 3 Apple Hill Dr, Natick, MA 01760 USA. NR 10 TC 2 Z9 5 U1 1 U2 3 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD MAY-JUN PY 2009 VL 46 IS 3 BP 763 EP 775 DI 10.2514/1.34015 PG 13 WC Engineering, Aerospace SC Engineering GA 456ZQ UT WOS:000266894200004 ER PT J AU Mavriplis, DJ Vassberg, JC Tinoco, EN Mani, M Brodersen, OP Eisfeld, B Wahls, RA Morrison, JH Zickuhr, T Levy, D Murayama, M AF Mavriplis, Dimitri J. Vassberg, John C. Tinoco, Edward N. Mani, Mori Brodersen, Olaf P. Eisfeld, Bernhard Wahls, Richard A. Morrison, Joseph H. Zickuhr, Tom Levy, David Murayama, Mitsuhiro TI Grid Quality and Resolution Issues from the Drag Prediction Workshop Series SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT AIAA 46th Aerospace Sciences Meeting and Exhibit CY JAN 07-10, 2008 CL Reno, NV SP Amer Inst Aeronaut & Astronaut ID COMPUTATIONS AB The drag prediction workshop series, held over the last six years and sponsored by the AIAA Applied Aerodynamics Committee, has been extremely useful in providing an assessment of the state of the art in computationally based aerodynamic drag prediction. An emerging consensus from the three-workshop series has been the identification of spatial discretization errors as a dominant error source in absolute as well as incremental drag prediction. This paper provides an overview of the collective experience from the workshop series regarding the effect of grid-related issues on overall drag prediction accuracy. Examples based on workshop results are used to illustrate the effect of grid resolution and grid quality on drag prediction, and grid convergence behavior is examined in detail. For fully attached flows, various accurate and successful workshop results are demonstrated, and anomalous behavior is identified for a number of cases involving substantial regions of separated flow. Based on collective workshop experiences, recommendations for improvements in mesh generation technology that have the potential to impact the state of the art of aerodynamic drag prediction are given. C1 [Mavriplis, Dimitri J.] Univ Wyoming, Dept Mech Engn, Laramie, WY 82071 USA. [Vassberg, John C.] Boeing Co, Huntington Beach, CA 92647 USA. [Tinoco, Edward N.] Boeing Co, Seattle, WA 98124 USA. [Mani, Mori] Boeing Co, St Louis, MO 63301 USA. [Brodersen, Olaf P.; Eisfeld, Bernhard] German Aerosp Ctr, DLR, Inst Aerodynam & Flow Technol, D-38108 Braunschweig, Germany. [Wahls, Richard A.] NASA, Langley Res Ctr, Configurat Aerodynam Branch, Hampton, VA 23681 USA. [Morrison, Joseph H.] NASA, Langley Res Ctr, Computat Aerosci Branch, Hampton, VA 23681 USA. [Zickuhr, Tom; Levy, David] Cessna Aircraft Co, Wichita, KS 67218 USA. [Murayama, Mitsuhiro] Japan Aerosp Explorat Agcy, Civil Transport Team, Aviat Program Grp, Chofu, Tokyo 1828522, Japan. RP Mavriplis, DJ (reprint author), Univ Wyoming, Dept Mech Engn, Laramie, WY 82071 USA. NR 37 TC 9 Z9 9 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 MAY-JUN PY 2009 VL 46 IS 3 BP 935 EP 950 DI 10.2514/1.39201 PG 16 WC Engineering, Aerospace SC Engineering GA 456ZQ UT WOS:000266894200020 ER PT J AU Herring, GC AF Herring, G. C. TI Noninvasive Measurement of Velocity, Pressure, and Temperature in Unseeded Supersonic Air Vortices SO JOURNAL OF AIRCRAFT LA English DT Article C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Herring, GC (reprint author), NASA, Langley Res Ctr, Mail Stop 493, Hampton, VA 23681 USA. EM Gregory.C.Herring@nasa.gov NR 10 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 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD MAY-JUN PY 2009 VL 46 IS 3 BP 1074 EP 1076 DI 10.2514/1.42004 PG 3 WC Engineering, Aerospace SC Engineering GA 456ZQ UT WOS:000266894200036 ER PT J AU Housman, JA Kiris, CC Hafez, MM AF Housman, Jeffrey A. Kiris, Cetin C. Hafez, Mohamed M. TI Time-Derivative Preconditioning Methods for Multicomponent Flows-Part II: Two-Dimensional Applications SO JOURNAL OF APPLIED MECHANICS-TRANSACTIONS OF THE ASME LA English DT Article DE hybrid conservative/nonconservative method; split coefficient matrix (SCM) method; time-derivative preconditioning; dual time stepping AB A time-derivative preconditioned system of equations suitable for the numerical simulation of multicomponent/multiphase inviscid flows at all speeds was described in Part I of this paper. The system was shown to be hyperbolic in time and remain well conditioned in the incompressible limit, allowing time marching numerical methods to remain an efficient solution strategy. Application of conservative numerical methods to multicomponent flows containing sharp fluid interfaces was shown to generate nonphysical pressure and velocity oscillations across the contact surface, which separates the fluid components. It was demonstrated using the one-dimensional Riemann problem that these oscillations may lead to stability problems when the interface separates fluids with large density ratios, such as water and air. The effect of which leads to the requirement of small physical time steps and slow subiteration convergence for the implicit time marching numerical method. Alternatively, the nonconservative and hybrid formulations developed by the present authors were shown to eliminate this nonphysical behavior. While the nonconservative method did not converge to the correct weak solution for flow containing shocks, the hybrid method was able to capture the physically correct entropy solution and converge to the exact solution of the Riemann problem as the grid is refined. In Part II of this paper, the conservative, nonconservative, and hybrid formulations described in Part I are implemented within a two-dimensional structured body-fitted overset grid solver, and a study of two unsteady flow applications is reported. In the first application, a multiphase cavitating flow around a NACA0015 hydrofoil contained in a channel is solved, and sensitivity to the cavitation number and the spatial order of accuracy of the discretization are discussed. Next, the interaction of a shock moving in air with a cylindrical bubble of another fluid is analyzed. In the first case, the cylindrical bubble is filled with helium gas, and both the conservative and hybrid approaches perform similarly. In the second case, the bubble is filled with water and the conservative method fails to maintain numerical stability. The performance of the hybrid method is shown to be unchanged when the gas is replaced with a liquid, demonstrating the robustness and accuracy of the hybrid approach. [DOI:10.1115/1.3086592] C1 [Housman, Jeffrey A.; Hafez, Mohamed M.] Univ Calif Davis, Davis, CA 95616 USA. [Kiris, Cetin C.] NASA, Ames Res Ctr, Adv Supercomp Div, Moffett Field, CA 94035 USA. RP Housman, JA (reprint author), Univ Calif Davis, 2132 Bainer Hall,1 Shields Ave, Davis, CA 95616 USA. NR 12 TC 0 Z9 0 U1 0 U2 1 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA SN 0021-8936 J9 J APPL MECH-T ASME JI J. Appl. Mech.-Trans. ASME PD MAY PY 2009 VL 76 IS 3 AR 031013 DI 10.1115/1.3086592 PG 12 WC Mechanics SC Mechanics GA 442EC UT WOS:000265821800013 ER PT J AU Roithmayr, CM Hodges, DH AF Roithmayr, Carlos M. Hodges, Dewey H. TI An Argument Against Augmenting the Lagrangean for Nonholonomic Systems SO JOURNAL OF APPLIED MECHANICS-TRANSACTIONS OF THE ASME LA English DT Article DE holonomic constraint equations; nonholonomic constraint equations; Lagrangean; Kane's method; constraint forces ID CONSTRAINTS AB Although it is known that correct dynamical equations of motion for a nonholonomic system cannot be obtained from a Lagrangean that has been augmented with a sum of the nonholonomic constraint equations weighted with multipliers, previous publications suggest otherwise. One published example that was proposed in support of augmentation purportedly demonstrates that an accepted method fails to produce correct equations of motion whereas augmentation leads to correct equations. This present paper shows that, in fact, the opposite is true. The correct equations, previously discounted on the basis of a flawed application of the Newton-Euler method, are verified by using Kane's method together with a new approach for determining the directions of constraint forces. [DOI:10.1115/1.3086435] C1 [Roithmayr, Carlos M.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Hodges, Dewey H.] Georgia Inst Technol, Sch Aerosp Engn, Atlanta, GA 30332 USA. RP Roithmayr, CM (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM c.m.roithmayr@larc.nasa.gov; dhodges@gatech.edu NR 12 TC 2 Z9 2 U1 1 U2 1 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA SN 0021-8936 J9 J APPL MECH-T ASME JI J. Appl. Mech.-Trans. ASME PD MAY PY 2009 VL 76 IS 3 AR 034501 DI 10.1115/1.3086435 PG 3 WC Mechanics SC Mechanics GA 442EC UT WOS:000265821800018 ER PT J AU Sengupta, A AF Sengupta, Anita TI Magnetic confinement in a ring-cusp ion thruster discharge plasma SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID CROSS-SECTIONS; CONTAINMENT; MULTIPOLAR AB An experimental investigation, in conjunction with a volume averaged analytical model, has been developed to improve the confinement and production of the discharge plasma for plasma thrusters and ion sources. The research conducted explores the discharge performance of a ring-cusp ion source based on the magnetic field configuration, geometry, and power level. Analytical formulations for electron and ion confinement are developed to predict the ionization efficiency for a given discharge chamber design. Explicit determination of discharge loss and volume averaged plasma parameters are obtained via a series of experimental measurements on a ring-cusp NASA Solar Technology Application Readiness (NSTAR) ion thruster to assess the validity of the analytical model. Measurements of the discharge loss with multiple magnetic field configurations compare well with plasma parameter predictions for propellant utilizations between 80% and 95%. The results indicate that increasing the magnetic strength of the first closed magnetic contour line reduces Maxwellian electron diffusion and electrostatically confines the ion population and subsequent loss to the anode wall. The results also indicate that increasing the strength and minimizing the area of the magnetic cusps improves primary electron confinement, increasing the probability of an ionization collision prior to loss at the cusp. (C) 2009 American Institute of Physics. [DOI: 10.1063/1.3106087] C1 CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. RP Sengupta, A (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM anita.sengupta@jpl.nasa.gov FU National Aeronautics and Space Administration FX The Jet Propulsion Laboratory, California Institute of Technology funded the research described in this paper under a contract with the National Aeronautics and Space Administration. NR 31 TC 5 Z9 5 U1 1 U2 6 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-8979 J9 J APPL PHYS JI J. Appl. Phys. PD MAY 1 PY 2009 VL 105 IS 9 AR 093303 DI 10.1063/1.3106087 PG 10 WC Physics, Applied SC Physics GA 448LE UT WOS:000266263300023 ER PT J AU Wang, JX Wolff, DB AF Wang, Jianxin Wolff, David B. TI Comparisons of Reflectivities from the TRMM Precipitation Radar and Ground-Based Radars SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID MEASURING MISSION TRMM; VALIDATION; SATELLITE; KWAJALEIN; AIRBORNE; CALIBRATION; WSR-88D; SPACE; SITE AB Given the decade-long and highly successful Tropical Rainfall Measuring Mission (TRMM), it is now possible to provide quantitative comparisons between ground-based radars (GRs) and the spaceborne TRMM precipitation radar (PR) with greater certainty over longer time scales in various tropical climatological regions. This study develops an automated methodology to match and compare simultaneous TRMM PR and GR reflectivities at four primary TRMM Ground Validation (GV) sites: Houston, Texas (HSTN); Melbourne, Florida (MELB); Kwajalein, Republic of the Marshall Islands (KWAJ); and Darwin, Australia (DARW). Data from each instrument are resampled into a three-dimensional Cartesian coordinate system. The horizontal displacement during the PR data resampling is corrected. Comparisons suggest that the PR suffers significant attenuation at lower levels, especially in convective rain. The attenuation correction performs quite well for convective rain but appears to slightly overcorrect in stratiform rain. The PR and GR observations at HSTN, MELB, and KWAJ agree to about 61 dB on average with a few exceptions, whereas the GR at DARW requires +1 to -5 dB calibration corrections. One of the important findings of this study is that the GR calibration offset is dependent on the reflectivity magnitude. Hence, it is proposed that the calibration should be carried out by using a regression correction rather than by simply adding an offset value to all GR reflectivities. This methodology is developed to assist TRMM GV efforts to improve the accuracy of tropical rain estimates, but can also be applied to the proposed Global Precipitation Measurement and other related activities over the globe. C1 [Wang, Jianxin] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Sci Syst & Applicat Inc, Lanham, MD USA. RP Wang, JX (reprint author), NASA, Goddard Space Flight Ctr, Code 613-1, Greenbelt, MD 20771 USA. EM jianxin.wang@nasa.gov RI Wolff, David/H-5502-2012 FU NASA [NNG06HX15] FX This study was supported by NASA Grant NNG06HX15. We thank Dr. Ramesh Kakar (NASA headquarters), Mr. Richard Lawrence (Chief, NASA Goddard Space Flight Center TRMM Satellite Validation Office), Dr. Scott Braun (TRMM Project Scientist), and Dr. Robert Adler (former TRMM Project Scientist) for their support and guidance for the TRMM GV Program. Our GV colleagues D. A. Marks, D. S. Silberstein, and J. L. Pippitt provided KWAJ version 7 GR products and monthly Ze-R relations. The PR version 6 and GR version 5 products were obtained from the Distributed Active Archive Center at NASA's Goddard Space Flight Center. NR 27 TC 18 Z9 21 U1 0 U2 4 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD MAY PY 2009 VL 26 IS 5 BP 857 EP 875 DI 10.1175/2008JTECHA1175.1 PG 19 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 456HA UT WOS:000266833600001 ER PT J AU Condron, A Winsor, P Hill, C Menemenlis, D AF Condron, Alan Winsor, Peter Hill, Chris Menemenlis, Dimitris TI Simulated Response of the Arctic Freshwater Budget to Extreme NAO Wind Forcing SO JOURNAL OF CLIMATE LA English DT Article ID NORTH-ATLANTIC OSCILLATION; GREAT SALINITY ANOMALIES; COLD HALOCLINE LAYER; ICE-OCEAN MODEL; SEA-ICE; THERMOHALINE CIRCULATION; CLIMATE VARIABILITY; IMPACT; ARCHIPELAGO; THICKNESS AB The authors investigate the response of the Arctic Ocean freshwater budget to changes in the North Atlantic Oscillation (NAO) using a regional-ocean configuration of the Massachusetts Institute of Technology GCM (MITgcm) and carry out several different 10-yr and 30-yr integrations. At 1/6 degrees (similar to 18 km) resolution the model resolves the major Arctic transport pathways, including Bering Strait and the Canadian Archipelago. Two main calculations are performed by repeating the wind fields of two contrasting NAO years in each run for the extreme negative and positive NAO phases of 1969 and 1989, respectively. These calculations are compared both with a control run and the compiled observationally based freshwater budget estimate of Serreze et al. The results show a clear response in the Arctic freshwater budget to NAO forcing, that is, repeat NAO negative wind forcing results in virtually all freshwater being retained in the Arctic, with the bulk of the freshwater content being pooled in the Beaufort gyre. In contrast, repeat NAO positive forcing accelerates the export of freshwater out of the Arctic to the North Atlantic, primarily via Fram Strait (similar to 900 km(3) yr(-1)) and the Canadian Archipelago (similar to 500 km(3) yr(-1)), with a total loss in freshwater storage of similar to 13 000 km(3) (15%) after 10 yr. The large increase in freshwater export through the Canadian Archipelago highlights the important role that this gateway plays in redistributing the freshwater of the Arctic to subpolar seas, by providing a direct pathway from the Arctic basin to the Labrador Sea, Gulf Stream system, and Atlantic Ocean. The authors discuss the sensitivity of the Arctic Ocean to long-term fixed extreme NAO states and show that the freshwater content of the Arctic is able to be restored to initial values from a depleted freshwater state after similar to 20 yr. C1 [Condron, Alan; Hill, Chris] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Winsor, Peter] Univ Alaska Fairbanks, Sch Fisheries & Marine Sci, Fairbanks, AK USA. [Menemenlis, Dimitris] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Condron, A (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. EM acondron@whoi.edu NR 69 TC 29 Z9 29 U1 1 U2 9 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 MAY PY 2009 VL 22 IS 9 BP 2422 EP 2437 DI 10.1175/2008JCLI2626.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 448TT UT WOS:000266285600010 ER PT J AU Kwok, R AF Kwok, R. TI Outflow of Arctic Ocean Sea Ice into the Greenland and Barents Seas: 1979-2007 SO JOURNAL OF CLIMATE LA English DT Article ID NORTH-ATLANTIC OSCILLATION; FRESH-WATER BALANCE; CIRCULATION; DECADES AB Twenty-nine years of Arctic sea ice outflow into the Greenland and Barents Seas are summarized. Outflow is computed at three passages: Fram Strait, between Svalbard and Franz Josef Land (S-FJL), and between Franz Josef Land and Severnaya Zemlya (FJL-SZ). Ice drift at the flux gates has been reprocessed using a consistent and updated time series of passive microwave brightness temperature and ice concentration (IC) fields. Over the record, the mean annual area outflow at the Fram Strait is 706(113) x 10(3) km(2); it was highest in 1994/95 (1002 x 10(3) km(2)) when the North Atlantic Oscillation (NAO) index was near its 29-yr peak. The strength of the "Transpolar Drift Stream" (TDS) was high during the late 1980s through the mid-1990s. There is no statistically significant trend in the Fram Strait area flux. Even though there is a positive trend in the gradient of cross-strait sea level pressure, the outflow has not increased because of a negative trend in IC. Seasonally, the area outflow during recent summers (in 2005 and 2007) has been higher (> 2 sigma from the mean) than average, contributing to the decline of summer ice coverage. Without updated ice thickness estimates, the best estimate of mean annual volume flux (between 1991 and 1999) stands at similar to 2200 km(3) yr(-1) (similar to 0.07 Sv: Sv equivalent to 10(6) m(3) s(-1)). Net annual outflow at the S-FJL passage is 37(39) x 10(3) km(2); the large outflow of multiyear ice in 2002-03, marked by an area and volume outflow of 141 x 10(3) km(2) and similar to 300 km(3), was unusual over the record. At the FJL-SZ passage, there is a mean annual inflow of 103(93) x 10(3) km(2) of seasonal ice into the Arctic. While the recent pattern of winter Arctic circulation and sea level pressure (SLP) has nearly reverted to its conditions typical of the 1980s, the summer has not. Compared to the 1980s, the recent summer SLP distributions show much lower SLPs (2-3 hPa) over much of the Arctic. Overall, there is a strengthening of the summer TDS. Examination of the exchanges between the Pacific and Atlantic sectors shows a long-term trend that favors the summer advection of sea ice toward the Atlantic associated with a shift in the mean summer circulation patterns. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kwok, R (reprint author), CALTECH, Jet Prop Lab, MS 300-235,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ron.kwok@jpl.nasa.gov RI Kwok, Ron/A-9762-2008 OI Kwok, Ron/0000-0003-4051-5896 FU National Science Foundation and the National Aeronautics and Space Administration FX I wish to thank S. S. Pang at JPL for her software support during the preparation of this manuscript. The SMMR, SSM/I, and AMSR-E brightness temperature and ice concentration fields are provided by World Data Center A for Glaciology/National Snow and Ice Data Center, University of Colorado, Boulder, Colorado. This work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, and is sponsored by the National Science Foundation and the National Aeronautics and Space Administration. NR 33 TC 88 Z9 92 U1 1 U2 28 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 MAY PY 2009 VL 22 IS 9 BP 2438 EP 2457 DI 10.1175/2008JCLI2819.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 448TT UT WOS:000266285600011 ER PT J AU Wang, HL Schubert, S Suarez, M Chen, JY Hoerling, M Kumar, A Pegion, P AF Wang, Hailan Schubert, Siegfried Suarez, Max Chen, Junye Hoerling, Martin Kumar, Arun Pegion, Philip TI Attribution of the Seasonality and Regionality in Climate Trends over the United States during 1950-2000 SO JOURNAL OF CLIMATE LA English DT Article ID GENERAL-CIRCULATION MODELS; SPATIOTEMPORAL STRUCTURE; COUPLED MODEL; SEA-ICE; PART I; SIMULATIONS; VARIABILITY; REANALYSES; US AB The observed climate trends over the United States during 1950-2000 exhibit distinct seasonality and regionality. The surface air temperature exhibits a warming trend during winter, spring, and early summer and a modest countrywide cooling trend in late summer and fall, with the strongest warming occurring over the northern United States in spring. Precipitation trends are positive in all seasons, with the largest trend occurring over the central and southern United States in fall. This study investigates the causes of the seasonality and regionality of those trends, with a focus on the cooling and wetting trends in the central United States during late summer and fall. In particular, the authors examine the link between the seasonality and regionality of the climate trends over the United States and the leading patterns of sea surface temperature (SST) variability, including a global warming (GW) pattern and a Pacific decadal variability (PDV) pattern. A series of idealized atmospheric general circulation model (AGCM) experiments were performed forced by SST trends associated with these leading SST patterns, as well as the residual trend pattern ( obtained by removing the GW and PDV contributions). The results show that the observed seasonal and spatial variations of the climate trends over the United States are to a large extent explained by changes in SST. Among the leading patterns of SST variability, the PDV pattern plays a prominent role in producing both the seasonality and regionality of the climate trends over the United States. In particular, it is the main contributor to the apparent cooling and wetting trends over the central United States. The residual SST trend, a manifestation of phase changes of the Atlantic multidecadal SST variation during 1950-2000, also exerts influences that show strong seasonality with important contributions to the central U. S. temperature and precipitation during the summer and fall seasons. In contrast, the response over the United States to the GW SST pattern is an overall warming with little seasonality or regional variation. These results highlight the important contributions of decadal and multidecadal variability in the Pacific and Atlantic in explaining the observed seasonality and regionality of the climate trends over the United States during the period of 1950-2000. C1 [Wang, Hailan] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. [Chen, Junye] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Kumar, Arun; Pegion, Philip] NOAA, Climate Predict Ctr, Natl Ctr Environm Predict, Boulder, CO USA. RP Wang, HL (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off UMBC GEST, Code 610-1, Greenbelt, MD 20771 USA. EM hailan.wang@nasa.gov RI Chen, Junye/G-4301-2011; Pegion, Philip/E-5247-2012 FU NASA; Office of Science, U.S. Department of Energy FX This study is supported by the NASA Modeling, Analysis, and Prediction ( MAP) project on Climate Transitions in the 1970s. We wish to acknowledge the international modeling groups for providing their data for analysis, the Program for Climate Model Diagnosis and Intercomparison (PCMDI) for collecting and archiving the model data, the JSC/CLIVAR WGCM and their Coupled Model Intercomparison Project (CMIP) and Climate Simulation Panel for organizing the model data analysis activity, and the IPCC WG1 TSU for technical support. The IPCC Data Archive at Lawrence Livermore National Laboratory is supported by the Office of Science, U.S. Department of Energy. We thank two anonymous reviewers for their constructive comments and suggestions, which led to many improvements in the presentation of the results. NR 40 TC 57 Z9 57 U1 1 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 MAY PY 2009 VL 22 IS 10 BP 2571 EP 2590 DI 10.1175/2008JCLI2359.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 453CG UT WOS:000266587200006 ER PT J AU Lin, WY Zhang, MH Loeb, NG AF Lin, Wuyin Zhang, Minghua Loeb, Norman G. TI Seasonal Variation of the Physical Properties of Marine Boundary Layer Clouds off the California Coast SO JOURNAL OF CLIMATE LA English DT Article ID LOWER-TROPOSPHERIC STABILITY; STRATOCUMULUS; REANALYSIS; MODEL; TEMPERATURE; TRANSITION; SATELLITE; DYNAMICS; ICOADS; ASTEX AB Marine boundary layer (MBL) clouds can significantly regulate the sensitivity of climate models, yet they are currently poorly simulated. This study aims to characterize the seasonal variations of physical properties of these clouds and their associated processes by using multisatellite data. Measurements from several independent satellite datasets [ International Satellite Cloud Climatology Project (ISCCP), Clouds and the Earth's Radiant Energy System-Moderate Resolution Imaging Spectroradiometer (CERES-MODIS), Geoscience Laser Altimeter System (GLAS), and Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation (CALIPSO)], in conjunction with balloon soundings from the mobile facility of the Atmospheric Radiation Measurement ( ARM) program at Point Reyes and reanalysis products, are used to characterize the seasonal variations of MBL cloud-top and cloud-base heights, cloud thickness, the degree of decoupling between clouds and MBL, and inversion strength off the California coast. The main results from this study are as follows: (i) MBL clouds over the northeast subtropical Pacific in the summer are more prevalent and associated with a larger in-cloud water path than in winter. The cloud-top and cloud-base heights are lower in the summer than in the winter. (ii) Although the lower-tropospheric stability of the atmosphere is higher in the summer, the MBL inversion strength is only weakly stronger in the summer because of a negative feedback from the cloud-top altitude. Summertime MBL clouds are more homogeneous and are associated with lower surface latent heat flux than those in the winter. (iii) Seasonal variations of low-cloud properties from summer to winter resemble the downstream stratocumulus-to-cumulus transition of MBL clouds in terms of MBL depth, cloud-top and cloud-base heights, inversion strength, and spatial homogeneity. The "deepening-warming'' mechanism of Bretherton and Wyant for the stratocumulus-to-trade-cumulus transition downstream of the cold eastern ocean can also explain the seasonal variation of low clouds from the summer to the winter, except that warming of the sea surface temperature needs to be taken as relative to the free-tropospheric air temperature, which occurs in the winter. The observed variation of low clouds from summer to winter is attributed to the much larger seasonal cooling of the free-tropospheric air temperature than that of the sea surface temperature. C1 [Lin, Wuyin; Zhang, Minghua] SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA. [Loeb, Norman G.] Hampton Univ, NASA, Langley Res Ctr, Hampton, VA 23668 USA. RP Lin, WY (reprint author), SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA. EM wlin@atmsci.msrc.sunysb.edu NR 35 TC 35 Z9 36 U1 0 U2 14 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 MAY PY 2009 VL 22 IS 10 BP 2624 EP 2638 DI 10.1175/2008JCLI2478.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 453CG UT WOS:000266587200009 ER PT J AU Koch, D Menon, S Del Genio, A Ruedy, R Alienov, I Schmidt, GA AF Koch, Dorothy Menon, Surabi Del Genio, Anthony Ruedy, Reto Alienov, Igor Schmidt, Gavin A. TI Distinguishing Aerosol Impacts on Climate over the Past Century SO JOURNAL OF CLIMATE LA English DT Article ID BLACK CARBON; SULFATE AEROSOLS; GREENHOUSE-GAS; GISS MODELE; ICE-SHEET; SIMULATION; SNOW; SENSITIVITY; PARAMETERIZATION; DEPOSITION AB Aerosol direct ( DE), indirect (IE), and black carbon-snow albedo (BAE) effects on climate between 1890 and 1995 are compared using equilibrium aerosol-climate simulations in the Goddard Institute for Space Studies General Circulation Model coupled to a mixed layer ocean. Pairs of control (1890)-perturbation ( 1995) with successive aerosol effects allow isolation of each effect. The experiments are conducted both with and without concurrent changes in greenhouse gases (GHG). Anew scheme allowing dependence of snow albedo on black carbon snow concentration is introduced. The fixed GHG experiments global surface air temperature ( SAT) changed by -0.2 degrees, -1.0 degrees, and +0.2 degrees C from the DE, IE, and BAE. Ice and snow cover increased 1% from the IE and decreased 0.3% from the BAE. These changes were a factor of 4 larger in the Arctic. Global cloud cover increased by 0.5% from the IE. Net aerosol cooling effects are about half as large as the GHG warming, and their combined climate effects are smaller than the sum of their individual effects. Increasing GHG did not affect the IE impact on cloud cover, however they decreased aerosol effects on SAT by 20%, and on snow/ice cover by 50%; they also obscure the BAE on snow/ ice cover. Arctic snow, ice, cloud, and shortwave forcing changes occur mostly during summer-fall, but SAT, sea level pressure, and longwave forcing changes occur during winter. An explanation is that aerosols impact the cryosphere during the warm season but the associated SAT effect is delayed until winter. C1 [Koch, Dorothy; Del Genio, Anthony; Alienov, Igor; Schmidt, Gavin A.] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Menon, Surabi] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. [Ruedy, Reto] Sigma Space Partners, New York, NY USA. RP Koch, D (reprint author), Columbia Univ, NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM dkoch@giss.nasa.gov RI Del Genio, Anthony/D-4663-2012; Schmidt, Gavin/D-4427-2012 OI Del Genio, Anthony/0000-0001-7450-1359; Schmidt, Gavin/0000-0002-2258-0486 FU Clean Air Task Force; NASA FX We thank Stephen Warren for assistance in development of the model BC-albedo parameterization. Support for this research is from the Clean Air Task Force, the NASA Radiation Science Program, and the NASA Modeling, Analysis, and Prediction Program. NR 49 TC 68 Z9 68 U1 3 U2 23 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 MAY PY 2009 VL 22 IS 10 BP 2659 EP 2677 DI 10.1175/2008JCLI2573.1 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 453CG UT WOS:000266587200011 ER PT J AU Wang, AH Bohn, TJ Mahanama, SP Koster, RD Lettenmaier, DP AF Wang, Aihui Bohn, Theodore J. Mahanama, Sarith P. Koster, Randal D. Lettenmaier, Dennis P. TI Multimodel Ensemble Reconstruction of Drought over the Continental United States SO JOURNAL OF CLIMATE LA English DT Article ID CATCHMENT-BASED APPROACH; LAND-SURFACE PROCESSES; MESOSCALE ETA-MODEL; SEVERITY INDEX; SOIL-MOISTURE; GREAT-PLAINS; CLIMATE; PARAMETERIZATION; PRECIPITATION; DATASET AB Retrospectively simulated soil moisture from an ensemble of six land surface/hydrological models was used to reconstruct drought events over the continental United States for the period 1920-2003. The simulations were performed at one-half-degree spatial resolution, using a common set of atmospheric forcing data and model-specific soil and vegetation parameters. Monthly simulated soil moisture was converted to percentiles using Weibull plotting position statistics, and the percentiles were then used to represent drought severities and durations. An ensemble method, based on an inverse mapping of the average of the individual model's soil moisture percentiles, was also used to combine all models' simulations. Major results are 1) all models and the ensemble reconstruct the known severe drought events during the last century. The spatial extents and severities of drought are plausible for the individual models although substantial among-model disparities exist. 2) The simulations are in more agreement with each other over the eastern than over the western United States. 3) Most of the models show that soil moisture memory is much longer over the western than over the eastern United States. The results provide some insights into how a hydrological nowcast system can be developed, and also early results from a test application within the University of Washington's real-time national Surface Water Monitor and a review of the multimodel nowcasts during the southeastern drought beginning in summer 2007 are included. C1 [Wang, Aihui; Bohn, Theodore J.; Lettenmaier, Dennis P.] Univ Washington, Dept Civil & Environm Engn, Seattle, WA 98195 USA. [Mahanama, Sarith P.; Koster, Randal D.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. RP Lettenmaier, DP (reprint author), Univ Washington, Dept Civil & Environm Engn, 164 Wilcox Hall,Box 352700, Seattle, WA 98195 USA. EM dennisl@u.washington.edu RI Koster, Randal/F-5881-2012; Bohn, Theodore/K-4494-2012; lettenmaier, dennis/F-8780-2011 OI Koster, Randal/0000-0001-6418-6383; Bohn, Theodore/0000-0002-1880-9129; lettenmaier, dennis/0000-0003-3317-1327 FU U.S. Department of Energy [DE-FG02-04ER63873]; Institute of Atmospheric Physics [KZCX2-YW-217] FX The work was supported by the U.S. Department of Energy under DOE Agreement Number DE-FG02-04ER63873 to the University of Washington, and the CAS Fund (KZCX2-YW-217) at the Institute of Atmospheric Physics. We appreciate the assistance of Ben Livneh of the University of NR 49 TC 80 Z9 85 U1 3 U2 14 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 MAY PY 2009 VL 22 IS 10 BP 2694 EP 2712 DI 10.1175/2008JCLI2586.1 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 453CG UT WOS:000266587200013 ER PT J AU Tessler, A Di Sciuva, M Gherlone, M AF Tessler, Alexander Di Sciuva, Marco Gherlone, Marco TI A Refined Zigzag Beam Theory for Composite and Sandwich Beams SO JOURNAL OF COMPOSITE MATERIALS LA English DT Article; Proceedings Paper CT 6th International Conference on Advanced Composites CY MAY 16-18, 2007 CL Univ Patras, Corfu, GREECE SP Greek Soc Composite Mat HO Univ Patras DE Timoshenko beam theory; zigzag kinematics; shear deformation; composite beams; sandwich beams; virtual work principle ID THICK LAMINATED BEAMS; DYNAMIC-RESPONSE; PLATES; SHEAR; SHELLS AB A new refined theory for laminated composite and sandwich beams that contains the kinematics of the Timoshenko Beam Theory as a proper baseline subset is presented. This variationally consistent theory is derived from the virtual work principle and employs a novel piecewise linear zigzag function that provides a more realistic representation of the deformation states of transverse-shear flexible beams than other similar theories. This new zigzag function is unique in that it vanishes at the top and bottom bounding surfaces of a beam. The formulation does not enforce continuity of the transverse shear stress across the beam's cross-section, yet is robust. Two major shortcomings that are inherent in the previous zigzag theories, shear-force inconsistency and difficulties in simulating clamped boundary conditions, and that have greatly limited the utility of these previous theories are discussed in detail. An approach that has successfully resolved these shortcomings is presented herein. Exact solutions for simply supported and cantilevered beams subject to static loads are derived and the improved modelling capability of the new 'zigzag' beam theory is demonstrated. In particular, extensive results for thick beams with highly heterogeneous material lay-ups are discussed and compared with corresponding results obtained from elasticity solutions, two other 'zigzag' theories, and high-fidelity finite element analyses. Comparisons with the baseline Timoshenko Beam Theory are also presented. The comparisons clearly show the improved accuracy of the new, refined 'zigzag' theory presented herein over similar existing theories. This new theory can be readily extended to plate and shell structures, and should be useful for obtaining relatively low-cost, accurate estimates of structural response needed to design an important class of high-performance aerospace structures. C1 [Di Sciuva, Marco; Gherlone, Marco] Politecn Torino, Dept Aeronaut & Space Engn, I-10129 Turin, Italy. [Tessler, Alexander] NASA Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA. RP Gherlone, M (reprint author), Politecn Torino, Dept Aeronaut & Space Engn, Corso Duca Abruzzi 24, I-10129 Turin, Italy. EM marco.gherlone@polito.it RI Tessler, Alexander/A-4729-2009; OI Gherlone, Marco/0000-0002-5711-0046 NR 24 TC 46 Z9 48 U1 2 U2 10 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0021-9983 EI 1530-793X J9 J COMPOS MATER JI J. Compos Mater. PD MAY PY 2009 VL 43 IS 9 BP 1051 EP 1081 DI 10.1177/0021998308097730 PG 31 WC Materials Science, Composites SC Materials Science GA 437VF UT WOS:000265514300010 ER PT J AU Yamaleev, NK Carpenter, MH AF Yamaleev, Nail K. Carpenter, Mark H. TI Third-order Energy Stable WENO scheme SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE High-order finite difference methods; Weighted essentially non-oscillatory schemes; Energy estimate; Numerical stability; Artificial dissipation ID ESSENTIALLY NONOSCILLATORY SCHEMES; DISCONTINUOUS GALERKIN METHOD; FINITE-DIFFERENCE APPROXIMATIONS; SCALAR CONSERVATION-LAWS; HIGH-ORDER; UNSTRUCTURED GRIDS; ENTROPY INEQUALITY; HYPERBOLIC SYSTEMS; ACCURACY; CONVERGENCE AB A new third-order Energy Stable Weighted Essentially Non-Oscillatory (ESWENO) finite difference scheme for scalar and vector hyperbolic equations with piecewise continuous initial conditions is developed. The new scheme is proven to be linearly stable in the energy norm for both continuous and discontinuous solutions. In contrast to the existing high-resolution shock-capturing schemes, no assumption that the reconstruction should be total variation bounded (TVB) is explicitly required to prove stability of the new scheme. We also present new weight functions which drastically improve the accuracy of the third-order ESWENO scheme. Based on a truncation error analysis, we show that the ESWENO scheme is design-order accurate for smooth solutions with any number of vanishing derivatives, if its tuning parameters satisfy certain constraints. Numerical results show that the new ESWENO scheme is stable and significantly outperforms the conventional third-order WENO scheme of Jiang and Shu in terms of accuracy, while providing essentially non-oscillatory solutions near strong discontinuities. (C) 2009 Elsevier Inc. All rights reserved. C1 [Yamaleev, Nail K.] N Carolina Agr & Tech State Univ, Dept Math, Greensboro, NC 27411 USA. [Carpenter, Mark H.] NASA, Langley Res Ctr, Computat Aerosci Branch, Hampton, VA 23681 USA. RP Yamaleev, NK (reprint author), N Carolina Agr & Tech State Univ, Dept Math, Greensboro, NC 27411 USA. EM nkyamale@ncat.edu FU Army Research Laboratory [W911NF-06-R-006] FX The work of the first author was supported in part by the Army Research Laboratory under Grant W911NF-06-R-006. NR 35 TC 30 Z9 31 U1 1 U2 11 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0021-9991 EI 1090-2716 J9 J COMPUT PHYS JI J. Comput. Phys. PD MAY 1 PY 2009 VL 228 IS 8 BP 3025 EP 3047 DI 10.1016/j.jcp.2009.01.011 PG 23 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA 426CK UT WOS:000264685000018 ER PT J AU Calle, CI Buhler, CR McFall, JL Snyder, SJ AF Calle, C. I. Buhler, C. R. McFall, J. L. Snyder, S. J. TI Particle removal by electrostatic and dielectrophoretic forces for dust control during lunar exploration missions SO JOURNAL OF ELECTROSTATICS LA English DT Article CT 11th International Conference on Electrostatics CY MAY 27-29, 2009 CL Valencia, SPAIN SP Inst Elect Technol, Polytech Univ Valencia DE Dielectrophoretic forces; Electric fields; Particle charging; Space applications ID FIELD AB Particle removal during lunar exploration activities is of prime importance for the Success of robotic and human exploration of the moon. We report on our efforts to use electrostatic and dielectrophoretic forces to develop a dust removal technology that prevents the accumulation of dust oil solar panels and removes dust adhering to those surfaces. Testing of several prototypes showed solar shield output above 90% of the initial potentials after dust clearing. Published by Elsevier B.V. C1 [Calle, C. I.] NASA, Electrostat & Surface Phys Lab, Kennedy Space Ctr, FL 32899 USA. [Buhler, C. R.; McFall, J. L.; Snyder, S. J.] ASRC Aerosp, Kennedy Space Ctr, FL 32899 USA. RP Calle, CI (reprint author), NASA, Electrostat & Surface Phys Lab, Kennedy Space Ctr, FL 32899 USA. EM carlos.i.calle@nasa.gov NR 17 TC 43 Z9 47 U1 1 U2 17 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0304-3886 J9 J ELECTROSTAT JI J. Electrost. PD MAY PY 2009 VL 67 IS 2-3 BP 89 EP 92 DI 10.1016/j.elstat.2009.02.012 PG 4 WC Engineering, Electrical & Electronic SC Engineering GA 444ZN UT WOS:000266019500004 ER PT J AU Buhler, C Calle, C Clements, JS Trigwell, S Ritz, M AF Buhler, Charles Calle, Carlos Clements, J. S. Trigwell, Steven Ritz, Mindy TI New techniques to evaluate the incendivity of insulators SO JOURNAL OF ELECTROSTATICS LA English DT Article CT 11th International Conference on Electrostatics CY MAY 27-29, 2009 CL Valencia, SPAIN SP Inst Elect Technol, Polytech Univ Valencia DE Incendivity; Safety and hazards; Incendiary behavior; Brush discharges; Insulators; Flammable atmospheres AB New techniques for evaluating the incendiary behavior of insulators is presented. The onset of incendive brush discharges in air is evaluated using standard spark probe techniques for the case Simulating approaches of all electrically grounded sphere to a charged insulator in the presence of a flammable atmosphere. However, this standard technique is unsuitable for the case of brush discharges that may occur during the charging-separation process for two insulator materials. We present experimental techniques to evaluate this hazard in the presence of a flammable atmosphere which is ideally suited to measure the incendiary nature of micro-discharges upon separation, a measurement never before performed. Other measurement techniques unique to this study include: Surface potential measurements of insulators before, during and after contact and separation, as well as methods to verify fieldmeter calibrations using a charge insulator surface opposed to standard high voltage plates. (C) 2009 Elsevier B.V. All rights reserved. C1 [Buhler, Charles; Trigwell, Steven; Ritz, Mindy] ASRC Aerosp, Electrostat & Surface Phys Lab, Kennedy Space Ctr, FL 32899 USA. [Calle, Carlos] NASA, Electrostat & Surface Phys Lab, Kennedy Space Ctr, FL 32899 USA. [Clements, J. S.] Appalachian State Univ, Dept Phys & Astron, Boone, NC 28608 USA. RP Buhler, C (reprint author), ASRC Aerosp, Electrostat & Surface Phys Lab, Kennedy Space Ctr, FL 32899 USA. EM charles.r.buhler@nasa.gov; carlos.i.calle@nasa.gov; clementsjs@appstate.edu; steven.trigwell-1@nasa.gov NR 14 TC 1 Z9 1 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0304-3886 J9 J ELECTROSTAT JI J. Electrost. PD MAY PY 2009 VL 67 IS 2-3 BP 285 EP 290 DI 10.1016/j.elstat.2009.01.017 PG 6 WC Engineering, Electrical & Electronic SC Engineering GA 444ZN UT WOS:000266019500040 ER PT J AU Scott, JH AF Scott, John H. TI Fuel Cell Development for NASA's Human Exploration Program: Benchmarking With "The Hydrogen Economy" SO JOURNAL OF FUEL CELL SCIENCE AND TECHNOLOGY LA English DT Article CT 2nd European Fuel Cell Technology and Applications Conference CY DEC, 2007 CL Rome, ITALY DE fuel cell power plants; fuel cell vehicles; hydrogen economy; life cycle costing AB The theoretically high efficiency and low temperature operation of hydrogen-oxygen fuel cells have motivated them to be the subject of much study since their invention in the 19th century, but their relatively high life cycle costs have kept them as a "solution in search of a problem" for many years. The first problem for which fuel cells presented a truly cost effective solution was that of providing a power source for NASA's human spaceflight vehicles in the 1960s. NASA thus invested, and continues to invest, in the development of fuel cell power plants for this application. This development program continues to place its highest priorities on requirements for minimum system mass and maximum durability and reliability. These priorities drive fuel cell power plant design decisions at all levels, even that of catalyst support. However, since the mid-1990s, prospective environmental regulations have driven increased governmental and industrial interest in "green power" and "the hydrogen economy." This has in turn stimulated greatly increased investment in fuel cell development for a variety of commercial applications. This investment is bringing about notable advances in fuel cell technology, but as these development efforts place their highest priority on requirements for minimum life cycle cost and field safety, these advances are yielding design solutions quite different at almost every level from those needed for spacecraft applications. This environment thus presents both opportunities and challenges for NASA's Human Exploration program. C1 NASA, Lyndon B Johnson Space Ctr EP3, Div Energy Syst, Houston, TX 77058 USA. RP Scott, JH (reprint author), NASA, Lyndon B Johnson Space Ctr EP3, Div Energy Syst, Houston, TX 77058 USA. EM john.h.scott@nasa.gov NR 7 TC 1 Z9 1 U1 1 U2 7 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA SN 1550-624X J9 J FUEL CELL SCI TECH JI J. Fuel Cell Sci. Technol. PD MAY PY 2009 VL 6 IS 2 AR 021011 DI 10.1115/1.2972170 PG 7 GA 416SD UT WOS:000264024900012 ER PT J AU Bezard, B Tsang, CCC Carlson, RW Piccioni, G Marcq, E Drossart, P AF Bezard, Bruno Tsang, Constantine C. C. Carlson, Robert W. Piccioni, Giuseppe Marcq, Emmanuel Drossart, Pierre TI Water vapor abundance near the surface of Venus from Venus Express/VIRTIS observations SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID LOWER ATMOSPHERE; DEEP ATMOSPHERE; SPECTRA; NIGHTSIDE; GALILEO; PROBES; SIDE AB Nightside observations of the 1.18-mu m atmospheric window by the Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) aboard the Venus Express spacecraft were analyzed to measure and map the water vapor abundance in the lower atmosphere. Thermal emission in this window originates partly from the surface and partly from the first scale height (0-15 km) of the atmosphere. Constraints on the CO(2) continuum absorption, which is the dominant source of gaseous opacity in the window, were obtained from the variation of the 1.185-mu m intensity with surface elevation. An absorption coefficient of 1 +/- 0.4 x 10(-9) cm(-1) amagat(-2) best fits the observed variation. We retrieved a water vapor mole fraction of 44 +/- 9 ppm from various selections of VIRTIS spectra in the southern hemisphere, in agreement with previous analyses of the nightside emission. This value is somewhat larger than that previously determined at higher altitudes from the 2.3- and 1.74-mu m nightside windows, but the error bars still allow a constant with height H(2)O mole fraction from the surface up to 40 km. Using the intensity ratio in the two wings of the 1.18-mm window as a proxy, we searched for horizontal variations of the H2O abundance in various VIRTIS observational sequences. We derived stringent upper limits for any possible latitudinal variations on the night side: +/- 1.5% in the range 60 degrees S-25 degrees N and +/- 3% for the broader range 80 degrees S-25 degrees N. The lack of detectable latitudinal variations is consistent with a constant with height water profile in the lower atmosphere and probably precludes any strong concentration gradient near the surface. C1 [Bezard, Bruno; Marcq, Emmanuel; Drossart, Pierre] Univ Paris Diderot, UPMC, CNRS, Observ Paris,LESIA, F-92190 Meudon, France. [Tsang, Constantine C. C.] Univ Oxford, Dept Phys, Clarendon Lab, Oxford OX1 3PU, England. [Carlson, Robert W.] Jet Prop Lab, Pasadena, CA 91109 USA. [Piccioni, Giuseppe] IASF, INAF, I-00133 Rome, Italy. RP Bezard, B (reprint author), Univ Paris Diderot, UPMC, CNRS, Observ Paris,LESIA, 5 Pl Jules Janssen, F-92190 Meudon, France. EM Bruno.Bezard@obspm.fr OI Piccioni, Giuseppe/0000-0002-7893-6808 FU Centre National d'Etudes Spatiales (CNES); Agenzia Spaziale Italiana (ASI) FX B. B., E. M., and P. D. acknowledge support from Centre National d'Etudes Spatiales (CNES). G. P. was supported by Agenzia Spaziale Italiana (ASI). We gratefully thank the VIRTIS technical team for their continuous support. NR 24 TC 39 Z9 39 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAY 1 PY 2009 VL 114 AR E00B39 DI 10.1029/2008JE003251 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 440BE UT WOS:000265672000001 ER PT J AU Xue, M Kopardekar, P AF Xue, Min Kopardekar, Parimal TI High-Capacity Tube Network Design Using the Hough Transform SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article; Proceedings Paper CT AIAA Guidance, Navigation, and Control Conference CY AUG 17-20, 2008 CL Honolulu, HI SP AIAA AB A new airspace design concept, tube networks, could enable high-density operations with less air traffic control workload. To construct tubes optimally, it is necessary to identify the commonality of flight trajectories. This paper proposes a new strategy to cluster great circle flight trajectories for forming tubes. The Hough transform is applied to identify groups or clusters of great circle trajectories that could form the tube networks. The genetic algorithm is then applied to optimize the tube network. Results show that small deviations from great circle routes could yield tubes that accommodate significant traffic levels within feasible computational time. C1 [Xue, Min] Univ Calif Santa Cruz, Moffett Field, CA 94035 USA. [Kopardekar, Parimal] NASA, Ames Res Ctr, Automat Concepts Branch, Moffett Field, CA 94035 USA. RP Xue, M (reprint author), Univ Calif Santa Cruz, Mail Stop 210-10, Moffett Field, CA 94035 USA. EM Min.Xue@nasa.gov; Parimal.H.Kopardekar@nasa.gov NR 11 TC 5 Z9 6 U1 0 U2 0 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD MAY-JUN PY 2009 VL 32 IS 3 BP 788 EP 795 DI 10.2514/1.40386 PG 8 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 445NL UT WOS:000266057400008 ER PT J AU Grabbe, S Sridhar, B Mukherjee, A AF Grabbe, Shon Sridhar, Banavar Mukherjee, Avijit TI Sequential Traffic Flow Optimization with Tactical Flight Control Heuristics SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article; Proceedings Paper CT AIAA Guidance, Navigation, and Control Conference CY AUG 18-21, 2008 CL Honolulu, HI SP Amer Inst Aeronaut & Astronaut (AIAA) AB A sequential optimization method is applied to manage air traffic flow under uncertainty in airspace capacity and demand. To support its testing, a decision support system is developed by integrating a deterministic integer programming model for assigning delays to aircraft under en route capacity constraints with a fast-time simulation environment to reactively account for system uncertainties. To reduce computational complexity, the model assigns only departure controls, and a tactical control loop consisting of a shortest-path routing algorithm and an airbornedelay algorithm refines the strategic plan to keep flights from deviating into capacity-constrained airspace. This integrated approach was used to conduct 32 six-hour fast-time simulation experiments to explore variations in the number and severity of departure controls, tactical reroutes, and airborne-delay controls. These experiments highlighted a fundamental difference in the manner in which weather translation is performed at the strategic and tactical levels. Although tactical weather translation explicitly accounts for the direct impact of weather on individual flights, strategic weather translation, which is accomplished by calculating a reduced capacity fora region of airspace such as a sector, typically fails to account for these flow-based impacts. Finally, an initial validation of the rerouting algorithm, which was the dominant control strategy for avoiding en route weather in the experiments, indicates that the algorithm is able to generate reroutes that are, on average, shorter than operationally flown weather-avoidance routes, when regions of airspace that flights are likely to avoid are identified using the convective-weather-avoidance model. C1 [Grabbe, Shon] NASA, Ames Res Ctr, Automat Concepts Res Branch, Moffett Field, CA 94035 USA. [Sridhar, Banavar] NASA, Ames Res Ctr, Aviat Syst Div, Moffett Field, CA 94035 USA. [Mukherjee, Avijit] Univ Calif Santa Cruz, Moffett Field, CA 94035 USA. RP Grabbe, S (reprint author), NASA, Ames Res Ctr, Automat Concepts Res Branch, Mail Stop 210-10, Moffett Field, CA 94035 USA. EM shon.r.grabbe@nasa.gov NR 27 TC 10 Z9 10 U1 0 U2 3 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD MAY-JUN PY 2009 VL 32 IS 3 BP 810 EP 820 DI 10.2514/1.40300 PG 11 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 445NL UT WOS:000266057400010 ER PT J AU Morelli, EA AF Morelli, Eugene A. TI Flight-Test Experiment Design for Characterizing Stability and Control of Hypersonic Vehicles SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article; Proceedings Paper CT United States Air Force T&E Days Conference 2008 CY FEB 05-07, 2008 CL Los Angeles, CA AB A maneuver design method that is particularly well suited for determining the stability and control characteristics of hypersonic vehicles is described in detail. Analytical properties of the maneuver design are explained. The importance of these analytical properties for maximizing information content in flight data is discussed, along with practical implementation issues. Results from flight tests of the X-43A hypersonic research vehicle (also called Hyper-X) are used to demonstrate the excellent modeling results obtained using this maneuver design approach. A detailed design procedure for generating the maneuvers is given to allow application to other flight-test programs. C1 NASA, Langley Res Ctr, Dynam Syst & Control Branch, Hampton, VA 23681 USA. RP Morelli, EA (reprint author), NASA, Langley Res Ctr, Dynam Syst & Control Branch, Mail Stop 308, Hampton, VA 23681 USA. NR 10 TC 16 Z9 19 U1 2 U2 16 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD MAY-JUN PY 2009 VL 32 IS 3 BP 949 EP 959 DI 10.2514/1.37092 PG 11 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 445NL UT WOS:000266057400022 ER PT J AU Gyekenyesi, AL Martin, RE Morscher, GN Owen, RB AF Gyekenyesi, Andrew L. Martin, Richard E. Morscher, Gregory N. Owen, Robert B. TI Impedance-based Structural Health Monitoring of a Ceramic Matrix Composite SO JOURNAL OF INTELLIGENT MATERIAL SYSTEMS AND STRUCTURES LA English DT Article DE structural health monitoring; ceramic matrix composite; piezoelectric patch; SiC/SiC; thermal protection system; aerospace ID TRANSDUCERS; SENSORS; DAMAGE AB This article addresses the use of electro-mechanical impedance-based structural health monitoring for assessing damage in a woven ceramic matrix composite consisting of a silicon carbide fibers and silicon carbide matrix. Controlled levels of damage were induced by conducting quasi-static, load/unload/reload tensile tests. The specimen's localized mechanical impedance was assessed using piezoelectric-ceramic patches that act as both actuator and sensor. The impedance results were correlated to damage and compared to acoustic emissions data, stress-strain response, and data from previous studies concerning the material system. The impedance data was shown to correlate well with the progressive damage mechanisms within the composite material system. C1 [Gyekenyesi, Andrew L.; Morscher, Gregory N.] NASA, GRC, Ohio Aerosp Inst, Cleveland, OH 44135 USA. [Martin, Richard E.] Cleveland State Univ, NASA, GRC, Cleveland, OH 44135 USA. [Owen, Robert B.] Extreme Diagnost Inc, Boulder, CO 80302 USA. RP Gyekenyesi, AL (reprint author), NASA, GRC, Ohio Aerosp Inst, 21000 Brookpk Rd,MS 6-1, Cleveland, OH 44135 USA. EM andrew.l.gyekenyesi@grc.nasa.gov NR 22 TC 4 Z9 4 U1 1 U2 3 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1045-389X J9 J INTEL MAT SYST STR JI J. Intell. Mater. Syst. Struct. PD MAY PY 2009 VL 20 IS 7 BP 875 EP 882 DI 10.1177/1045389X08099033 PG 8 WC Materials Science, Multidisciplinary SC Materials Science GA 446FV UT WOS:000266107100009 ER PT J AU Washer, G Brooks, T Saulsberry, R AF Washer, Glenn Brooks, Thomas Saulsberry, Regor TI Characterization of Kevlar Using Raman Spectroscopy SO JOURNAL OF MATERIALS IN CIVIL ENGINEERING LA English DT Article ID DEFORMATION-BEHAVIOR; FIBERS; COMPOSITES; TEREPHTHALAMIDE); POLYMER AB This paper explores the characterization of Kevlar composite materials using Raman spectroscopy. The goal of the research is to develop and understand the Raman spectrum of Kevlar materials to provide a foundation for the development of nondestructive evaluation (NDE) technologies based on the interaction of laser light with the polymer Kevlar. The paper discusses the fundamental aspects of experimental characterization of the spectrum of Kevlar, including the effects of incident wavelength, polarization, and laser power. The effects of environmental exposure of Kevlar materials on certain characteristics of its Raman spectrum are explored. These data may provide a foundation for the development of NDE technologies intended to detect the in situ deterioration of Kevlar materials used for engineering applications that can later be extended to other materials such as carbon fiber composites. C1 [Washer, Glenn; Brooks, Thomas] Univ Missouri, Dept Civil & Environm Engn, Columbia, MO 65211 USA. [Saulsberry, Regor] NASA White Sands Test Facil, Las Cruces, NM 88012 USA. RP Washer, G (reprint author), Univ Missouri, Dept Civil & Environm Engn, 2503 Lafferre Hall, Columbia, MO 65211 USA. NR 24 TC 7 Z9 9 U1 1 U2 22 PU ASCE-AMER SOC CIVIL ENGINEERS PI RESTON PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA SN 0899-1561 J9 J MATER CIVIL ENG JI J. Mater. Civ. Eng. PD MAY PY 2009 VL 21 IS 5 BP 226 EP 234 DI 10.1061/(ASCE)0899-1561(2009)21:5(226) PG 9 WC Construction & Building Technology; Engineering, Civil; Materials Science, Multidisciplinary SC Construction & Building Technology; Engineering; Materials Science GA 433WL UT WOS:000265236400005 ER PT J AU Capo-Lugo, PA Bainum, PM AF Capo-Lugo, Pedro A. Bainum, Peter M. TI DEPLOYMENT PROCEDURE FOR THE TETRAHEDRON CONSTELLATION SO JOURNAL OF MECHANICS OF MATERIALS AND STRUCTURES LA English DT Article DE discrete linear quadratic regulator; impulse maneuvers; deployment procedure; tetrahedron constellation ID GAUSS PSEUDOSPECTRAL METHOD; DISTANCE CONSTRAINTS AB The NASA Benchmark Tetrahedron Constellation is a four-satellite formation that requires a nominal separation distance at every apogee point. The deployment procedure of a tetrahedron constellation is complex and depends on the separation distance between any pair of satellites within the constellation. In this paper, the deployment procedure of the tetrahedron constellation will be divided into two stages: the deployment from a circular parking orbit to an elliptical orbit, and the correction of the separation distance between pairs of satellites within the constellation. The solution of this problem will be implemented with a combination of Hohmann transfer maneuvers and the digital linear quadratic regulator control scheme showing a minimum consumption of fuel. In summary, the combination of these two techniques will provide a different approach to the deployment procedure of the NASA benchmark tetrahedron constellation. C1 [Capo-Lugo, Pedro A.; Bainum, Peter M.] Howard Univ, Dept Mech Engn, Washington, DC 20059 USA. RP Capo-Lugo, PA (reprint author), NASA, George C Marshall Space Flight Ctr, Guidance Nav & Control Syst Design & Anal Branch, EV41, Huntsville, AL 35812 USA. EM pcapo@howard.edu; pbainum@fac.howard.edu FU Alliances for Graduate Education and Professoriate (AGEP) Program FX Research supported by Alliances for Graduate Education and Professoriate (AGEP) Program. NR 15 TC 1 Z9 1 U1 0 U2 3 PU MATHEMATICAL SCIENCE PUBL PI BERKELEY PA UNIV CALIFORNIA, DEPT MATHEMATICS, BERKELEY, CA 94720-3840 USA SN 1559-3959 J9 J MECH MATER STRUCT JI J. Mech. Mater. Struct. PD MAY PY 2009 VL 4 IS 5 SI SI BP 837 EP 854 DI 10.2140/jomms.2009.4.837 PG 18 WC Materials Science, Multidisciplinary; Mechanics SC Materials Science; Mechanics GA 505VR UT WOS:000270727700005 ER PT J AU Kopasakis, G DeLaat, JC Chang, CT AF Kopasakis, George DeLaat, John C. Chang, Clarence T. TI Adaptive Instability Suppression Controls Method for Aircraft Gas Turbine Engine Combustors SO JOURNAL OF PROPULSION AND POWER LA English DT Article ID ACTIVE CONTROL AB An adaptive controls method for instability suppression in gas-turbine engine combustors has been developed and successfully tested with a realistic aircraft engine combustor rig. This testing was part of a program that demonstrated, for the first time, successful active combustor instability control in an aircraft gas-turbine enginelike environment. The controls method is called adaptive sliding phasor averaged control. Testing of the control method has been conducted in an experimental rig with different configurations designed to simulate combustors with instabilities of about 530 and 315 Hz. Results demonstrate the effectiveness of this method in suppressing combustor instabilities. In addition, a dramatic improvement in suppression of the instability was achieved by focusing control on the second harmonic of the instability. This is believed to be due to coupling in the form of energy exchange between different frequency modes in the combustor. These results may have implications for future research in combustor instability control. C1 [Kopasakis, George; DeLaat, John C.] NASA, John H Glenn Res Ctr Lewis Field, Controls & Dynam Branch, Cleveland, OH 44135 USA. [Chang, Clarence T.] NASA, John H Glenn Res Ctr Lewis Field, Combust Branch, Cleveland, OH 44135 USA. RP Kopasakis, G (reprint author), NASA, John H Glenn Res Ctr Lewis Field, Controls & Dynam Branch, 21000 Brookpk Rd, Cleveland, OH 44135 USA. NR 36 TC 3 Z9 3 U1 0 U2 2 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 EI 1533-3876 J9 J PROPUL POWER JI J. Propul. Power PD MAY-JUN PY 2009 VL 25 IS 3 BP 618 EP 627 DI 10.2514/1.36777 PG 10 WC Engineering, Aerospace SC Engineering GA 452AX UT WOS:000266513100008 ER PT J AU Longmier, BW Reid, BM Gallimore, AD Chang-Diaz, FR Squire, JP Glover, TW Chavers, G Bering, EA AF Longmier, Benjamin W. Reid, Bryan M. Gallimore, Alec D. Chang-Diaz, Franklin R. Squire, Jared P. Glover, Tim W. Chavers, Greg Bering, Edgar A., III TI Validating a Plasma Momentum Flux Sensor to an Inverted Pendulum Thrust Stand SO JOURNAL OF PROPULSION AND POWER LA English DT Article; Proceedings Paper CT AIAA/ASME/SAE/ASEE 44th Joint Propulsion Conference and Exhibit CY JUL 20-23, 2008 CL Hartford, CT SP AIAA, ASME, SAE, ASEE ID INSTRUMENT AB The accuracy of a plasma impact force sensor was compared with that of the more commonly used inverted pendulum thrust stand using a 5 kW Xe Hall effect thruster. An improved plasma momentum flux sensor was designed and constructed based on a previous design. Real-time force measurements were made with both the plasma momentum flux sensor and the inverted pendulum thrust stand. The plasma momentum flux sensor measured the force exerted onto it by the Hall effect thruster exhaust plume with a resolution of 0.1 mN and an average discrepancy of 2% compared with thrust stand measurements. Experiments were completed using a 9 m by 6 m cylindrical vacuum chamber. The total force from the Hall effect thruster was modulated from 34 to 356 mN by varying both the anode voltage, from 150 to 500 V, and the neutral Xe gas flow rate, from 5 to 15 mg/s. C1 [Longmier, Benjamin W.; Bering, Edgar A., III] Univ Houston, Dept Phys, Houston, TX 77204 USA. [Reid, Bryan M.] Univ Michigan, Ann Arbor, MI 48109 USA. [Chang-Diaz, Franklin R.; Squire, Jared P.; Glover, Tim W.] Ad Astra Rocket Co, Webster, TX 77598 USA. [Chavers, Greg] NASA, George C Marshall Space Flight Ctr, Mission Operat Lab, Huntsville, AL 35812 USA. RP Longmier, BW (reprint author), Univ Houston, Dept Phys, 141 W Bay Area Blvd, Houston, TX 77204 USA. NR 17 TC 18 Z9 18 U1 1 U2 10 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 MAY-JUN PY 2009 VL 25 IS 3 BP 746 EP 752 DI 10.2514/1.35706 PG 7 WC Engineering, Aerospace SC Engineering GA 452AX UT WOS:000266513100021 ER PT J AU Frederick, RA Whitehead, JJ AF Frederick, Robert A., Jr. Whitehead, J. Joshua TI Predicting Hybrid Propellant Regression Rate Using Response Surfaces SO JOURNAL OF PROPULSION AND POWER LA English DT Article; Proceedings Paper CT AIAA/ASME/SAE/ASEE 41st Joint Propulsion Conference CY JUL 10-13, 2005 CL Tucson, AZ SP AIAA, ASME, SAE, ASEE AB Applied mixture theory allows for estimation of propellant characteristics (such as regression rate or specific impulse) over an extended range of formulations from a limited number of tests. A mixed-oxidizer hybrid system was tested using fuel formulations of 25-30% ammonium perchlorate, 0-5% iron oxide, and 70-75% hydroxyl-terminated polybutadiene fired with gaseous oxygen. Through application of a reduced form of the cubic response equation, functional relationships were developed that correlate fuel composition to regression rate in the form of a three-dimensional response surface. The maximum regression rate was then estimated to occur at approximately 2% iron oxide and 27.5% ammonium perchlorate based on the response surface developed from experimental results at an oxidizer flux of 0.3 Ib(m)/in(2).s (0.211 kg/m(2).s) and a chamber pressure of 350 psia (2.41 MPa). C1 [Frederick, Robert A., Jr.] Univ Alabama, Propul Res Ctr, Huntsville, AL 35899 USA. [Whitehead, J. Joshua] NASA, George C Marshall Space Flight Ctr, ATK Launch Syst, Huntsville, AL 35812 USA. RP Frederick, RA (reprint author), Univ Alabama, Propul Res Ctr, 5000 Technol Dr, Huntsville, AL 35899 USA. NR 8 TC 2 Z9 2 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 MAY-JUN PY 2009 VL 25 IS 3 BP 815 EP 818 DI 10.2514/1.14418 PG 4 WC Engineering, Aerospace SC Engineering GA 452AX UT WOS:000266513100029 ER PT J AU Johnston, CO Gnoffo, PA Sutton, K AF Johnston, Christopher O. Gnoffo, Peter A. Sutton, Kenneth TI Influence of Ablation on Radiative Heating for Earth Entry SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT AIAA 40th Thermophysics Conference CY JUN 23-26, 2008 CL Seattle, WA SP AIAA ID CHEMICAL-KINETIC PROBLEMS; LUNAR-RETURN CONDITIONS; SHOCK-LAYER RADIATION; FUTURE NASA MISSIONS; COUPLED RADIATION; SPALLED PARTICLES; NONEQUILIBRIUM; CAPSULE; FLOWFIELD; INJECTION AB Using the coupled ablation and radiation capability recently included in the LAURA flowfield solver, this paper investigates the influence of ablation on the shock-layer radiative heating for Earth entry. The extension of the HARA radiation model, which provides the radiation predictions in LAURA, to treat a gas consisting of the elements carbon, hydrogen, oxygen, and nitrogen is discussed. It is shown that the absorption coefficient of air is increased with the introduction of the carbon and hydrogen elements. A simplified shock-layer model is studied to show the impact of temperature, as well as the abundance of carbon and hydrogen, on the net absorption or emission from an ablation contaminated boundary layer. It is found that the ablation species reduce the radiative flux in the vacuum ultraviolet, through increased absorption, for all temperatures. However, in the infrared region of the spectrum, the ablation species increase the radiative flux, through strong emission, for temperatures above 3000 K. Thus, depending on the temperature and abundance of ablation species, the contaminated boundary layer may either provide a net increase or decrease in the radiative flux reaching the wall. To assess the validity of the coupled ablation and radiation LAURA analysis, a previously analyzed Mars-return case (15.24 km/s), which contains significant ablation and radiation coupling, is studied. Exceptional agreement with previous viscous-shock-layer results is obtained. A 40% decrease in the radiative flux is predicted for ablation rates equal to 20% of the freestream mass flux. The Apollo 4 peak-heating case (10.24 km/s) is also studied. For ablation rates up to 3.4% of the freestream mass flux, the radiative heating is reduced by up to 19%, whereas the convective heating is reduced by up to 87%. Good agreement with the Apollo 4 radiometer data is obtained by considering absorption in the radiometer cavity. For both the Marsreturn and the Apollo 4 cases, coupled radiation alone is found to reduce the radiative heating by 30-60% and the convective heating by less than 5%. C1 [Johnston, Christopher O.; Gnoffo, Peter A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Sutton, Kenneth] Natl Inst Aerosp, Hampton, VA 24060 USA. RP Johnston, CO (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 83 TC 18 Z9 18 U1 0 U2 1 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAY-JUN PY 2009 VL 46 IS 3 BP 481 EP 491 DI 10.2514/1.40290 PG 11 WC Engineering, Aerospace SC Engineering GA 456ZX UT WOS:000266895100001 ER PT J AU Everhart, JL AF Everhart, Joel L. TI Supersonic/Hypersonic Laminar Heating Correlations for Rectangular and Impact-Induced Open and Closed Cavities SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT 46th AIAA Aerospace Sciences Meeting and Exhibit CY JAN 07-11, 2008 CL Reno, NV SP AIAA ID SEPARATED FLOWS AB An analysis of existing baseline, zero-pressure-gradient, idealized, rectangular-geometry cavity-heating data is presented, yielding new laminar correlations for the floor-averaged heating, peak cavity endwall heating, and downstream decay rate. Correlation parameters are derived in terms of cavity geometry and local flow conditions. Prediction-limit uncertainty values are provided at the 95, 99, and 99.9% levels of significance. Nonbaseline conditions, including nonrectangular geometries and flows with known pressure gradients, are used to assess the range of applicability of the new correlations. All data variations fall within the 99% prediction-limit uncertainty bounds. Both open-flow and closed-flow cavity heating are combined into a single-curve parameterization of the heating predictions and provide a concise mathematical model of the laminar heating flowfield of stream-aligned cavities with known uncertainty. C1 NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA. RP Everhart, JL (reprint author), NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA. NR 44 TC 4 Z9 4 U1 0 U2 0 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAY-JUN PY 2009 VL 46 IS 3 BP 545 EP 560 DI 10.2514/1.36830 PG 16 WC Engineering, Aerospace SC Engineering GA 456ZX UT WOS:000266895100006 ER PT J AU Mazarico, E Zuber, MT Lemoine, FG Smith, DE AF Mazarico, Erwan Zuber, Maria T. Lemoine, Frank G. Smith, David E. TI Effects of Self-Shadowing on Nonconservative Force Modeling for Mars-Orbiting Spacecraft SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT AIAA/AAS Astrodynamics Specialist and Exhibit CY AUG 18-21, 2008 CL Honolulu, HI SP AIAA, AAS ID GRAVITY-FIELD AB Modeling improvements of nonconservative forces affecting Mars-orbiting spacecraft are presented in this study. Recent high-resolution gravity fields enable the recovery of smaller signals in the radio tracking data, previously obscured by mismodeled gravitational anomalies. In particular, the estimation of the atmospheric drag experienced by the spacecraft benefits from the new force models. More precise calculations of the spacecraft cross-sectional areas entering the equations for the atmospheric drag and direct solar radiation pressure are possible by accounting for the interplate self-shadowing of the spacecraft physical model. The relevant surface areas can change by as much as 20% on average, and the effects can be very variable within one orbit (10%). The benefits of these updated models are assessed with two spacecraft, the Mars Odyssey and the Mars Reconnaissance Orbiter. The changes in the nonconservative forces can significantly impact the reconstructed spacecraft trajectory and the estimated model parameters depend on the spacecraft geometry and orbit. The atmospheric density estimated by the Mars Odyssey is much improved with self-shadowing applied to the solar radiation, but improvements to both the drag force and the solar radiation are important in this case of the Mars Reconnaissance Orbiter. C1 [Mazarico, Erwan; Zuber, Maria T.] MIT, Cambridge, MA 02139 USA. [Lemoine, Frank G.; Smith, David E.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. RP Mazarico, E (reprint author), MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA. RI Lemoine, Frank/D-1215-2013; Mazarico, Erwan/N-6034-2014 OI Mazarico, Erwan/0000-0003-3456-427X NR 19 TC 15 Z9 15 U1 0 U2 1 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAY-JUN PY 2009 VL 46 IS 3 BP 662 EP 669 DI 10.2514/1.41679 PG 8 WC Engineering, Aerospace SC Engineering GA 456ZX UT WOS:000266895100017 ER PT J AU Squire, TH Milos, FS Hartlieb, GC AF Squire, T. H. Milos, F. S. Hartlieb, G. C. TI Aerospace Materials Property Database (TPSX) SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article C1 [Squire, T. H.; Milos, F. S.] NASA, Ames Res Ctr, Thermal Protect Mat & Syst Branch, Moffett Field, CA 94035 USA. [Hartlieb, G. C.] ELORET Corp, Thermal Protect Mat & Syst Branch, Sunnyvale, CA 94086 USA. RP Squire, TH (reprint author), NASA, Ames Res Ctr, Thermal Protect Mat & Syst Branch, Mail Stop 234-1, Moffett Field, CA 94035 USA. NR 15 TC 5 Z9 5 U1 0 U2 0 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAY-JUN PY 2009 VL 46 IS 3 BP 733 EP 736 DI 10.2514/1.43777 PG 4 WC Engineering, Aerospace SC Engineering GA 456ZX UT WOS:000266895100028 ER PT J AU De Witt, JK Lee, SMC Wilson, CA Hagan, RD AF De Witt, John K. Lee, Stuart M. C. Wilson, Cassie A. Hagan, R. Donald TI DETERMINANTS OF TIME TO FATIGUE DURING NONMOTORIZED TREADMILL EXERCISE SO JOURNAL OF STRENGTH AND CONDITIONING RESEARCH LA English DT Article ID NEGATIVE-PRESSURE EXERCISE; UPRIGHT EXERCISE; BED REST AB De Witt, JK, Lee, SMC, Wilson, CA, and Hagan, RD. Determinants of time to fatigue during nonmotorized treadmill exercise. J Strength Cond Res 23(3): 883-890, 2009-Treadmill exercise is commonly used for aerobic and anaerobic conditioning. During nonmotorized treadmill exercise, the subject must provide the power necessary to drive the treadmill belt. The purpose of this study was to determine what factors affected the time to fatigue on a pair of nonmotorized treadmills. Twenty subjects (10 men/10 women) attempted to complete 5 minutes of locomotion during separate trials at 3.22, 4.83, 6.44, 8.05, 9.66, and 11.27 km.h(-1). Total exercise time (<= 5 minutes) was recorded. Exercise time was converted to the number of 15-second intervals completed. Peak oxygen uptake ((V) over dotO(2)) was measured using a graded exercise test on a standard treadmill, and anthropometric measures were collected from each subject before their entrance into the study. A Cox proportional hazards regression model was used to determine significant predictive factors in a multivariate analysis. Treadmill speed and absolute peak (V) over dotO(2) were found to be significant predictors of exercise time, but there was no effect of anthropometric characteristics. Gender was found to be a predictor of treadmill time, but this was likely attributable to a higher peak (V) over dotO(2) in men than in women. The results were not affected by the type of treadmill tested in this study. Coaches and therapists should consider the cardiovascular fitness of an athlete or client when prescribing target speed because these factors are related to the total exercise time that can be achieved on a nonmotorized treadmill. C1 [De Witt, John K.; Lee, Stuart M. C.] Wyles Life Sci Grp, Houston, TX USA. [Wilson, Cassie A.] JES Tech, Houston, TX USA. [Hagan, R. Donald] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP De Witt, JK (reprint author), Wyles Life Sci Grp, Houston, TX USA. EM john.k.dewitt@nasa.gov NR 16 TC 1 Z9 1 U1 0 U2 1 PU LIPPINCOTT WILLIAMS & WILKINS PI PHILADELPHIA PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA SN 1064-8011 J9 J STRENGTH COND RES JI J. Strength Cond. Res. PD MAY PY 2009 VL 23 IS 3 BP 883 EP 890 DI 10.1519/JSC.0b013e3181a04de9 PG 8 WC Sport Sciences SC Sport Sciences GA 514NF UT WOS:000271400900025 PM 19387389 ER PT J AU Dong, W Yen, SP Paik, JA Sakamoto, J AF Dong, Winny Yen, Shiao-Pin Paik, Jong-Ah Sakamoto, Jeff TI The Role of Acetic Acid and Glycerol in the Synthesis of Amorphous MgO Aerogels SO JOURNAL OF THE AMERICAN CERAMIC SOCIETY LA English DT Article ID METAL-OXIDE PARTICLES; SOL-GEL TECHNIQUE; MAGNESIUM-OXIDE; NANOCRYSTALLINE MGO; THIN-FILMS; THERMAL-DECOMPOSITION; CHEMICAL REAGENTS; PARTIAL OXIDATION; CATALYSTS; SURFACE AB Although sol-gel-derived magnesium-oxide (MgO) aerogels have a wide variety of applications, mostly thin films and powders of brucite, i.e. Mg(OH)(2) aerogels, have been reported. Typically, the brucite structure is converted to the periclase form of MgO upon heat-treatment. We report the role of acetic acid (HAc) and glycerol in the synthesis of amorphous MgO aerogel monoliths through the alkoxide sol-gel method. The two ligands work in concert to retard the nucleophilic substitution with water and decrease the rate of gelation, allowing for Mg-O bond formation while reducing the number of hydroxyl bonds. The amorphous material crystallizes to the periclase (MgO) phase at 400 degrees C without going through the brucite transition, resulting in a novel amorphous MgO aerogel. Specifically, we discuss the modi. cation of the Pechini process to an Mg-alkoxide sol-gel process. The roles of the ligands are investigated in the MgO gelation process through Fourier transform infrared spectroscopy, X-ray diffractometry, and thermogravimetric analysis/DSC. The physical properties of the aerogels are also reported. C1 [Dong, Winny] Calif State Polytech Univ Pomona, Pomona, CA 91768 USA. [Yen, Shiao-Pin; Paik, Jong-Ah] CALTECH, Jet Prop Lab, Power & Sensor Technol Sect, Pasadena, CA USA. [Sakamoto, Jeff] Michigan State Univ, E Lansing, MI 48824 USA. RP Dong, W (reprint author), Calif State Polytech Univ Pomona, Pomona, CA 91768 USA. EM winnydong@csupomona.edu FU NASA through the Jupiter Icy Moons Orbiter [NAS7-03001] FX This work is supported by NASA through the Jupiter Icy Moons Orbiter Project (NAS7-03001). NR 51 TC 5 Z9 5 U1 0 U2 23 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-7820 J9 J AM CERAM SOC JI J. Am. Ceram. Soc. PD MAY PY 2009 VL 92 IS 5 BP 1011 EP 1016 DI 10.1111/j.1551-2916.2009.02997.x PG 6 WC Materials Science, Ceramics SC Materials Science GA 444WT UT WOS:000266012300007 ER PT J AU Springman, KR Short, J Rice, SD AF Springman, K. R. Short, J. Rice, S. D. TI Comments on the misuse of SPMDs in recent articles by Springman et al. (2008a,b) and Short et al. (2008) Response SO MARINE ENVIRONMENTAL RESEARCH LA English DT Letter ID PRINCE-WILLIAM-SOUND; EXXON-VALDEZ OIL; SEMIPERMEABLE-MEMBRANE DEVICES; SITE-SPECIFIC CONTAMINANTS; HYDROCARBON SOURCES; ALASKA; INDUCTION; SPILL; FISH; CYTOCHROME-P4501A C1 [Springman, K. R.] Univ Calif Davis, Littleriver, CA 95456 USA. [Short, J.; Rice, S. D.] NOAA, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Juneau, AK 99801 USA. RP Springman, KR (reprint author), Univ Calif Davis, POB 315, Littleriver, CA 95456 USA. EM krspringman@gmail.com NR 21 TC 1 Z9 1 U1 1 U2 3 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0141-1136 J9 MAR ENVIRON RES JI Mar. Environ. Res. PD MAY-JUN PY 2009 VL 67 IS 4-5 BP 259 EP 261 DI 10.1016/j.marenvres.2009.03.004 PG 3 WC Environmental Sciences; Marine & Freshwater Biology; Toxicology SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Toxicology GA 457DA UT WOS:000266904800011 ER PT J AU van Breukelen, C Simpson, C Rawlings, S Akiyama, M Bonfield, D Clewley, L Jarvis, MJ Mauch, T Readhead, T Stobbart, AM Swinbank, M Watson, M AF van Breukelen, Caroline Simpson, Chris Rawlings, Steve Akiyama, Masayuki Bonfield, David Clewley, Lee Jarvis, Matt J. Mauch, Tom Readhead, Tony Stobbart, Ann-Marie Swinbank, Mark Watson, Mike TI Evidence of a link between the evolution of clusters and their AGN fraction SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: clusters: general; radio continuum: galaxies; X-rays: galaxies; X-rays: galaxies: clusters ID ACTIVE GALACTIC NUCLEI; DEEP FIELD-SOUTH; X-RAY SOURCES; LUMINOSITY FUNCTIONS; RADIO GALAXIES; REDSHIFT SURVEY; SKY SURVEY; CHANDRA; SUBMILLIMETER; ENVIRONMENTS AB We discuss the optical properties, X-ray detections and active galactic nucleus (AGN) populations of four clusters at z similar to 1 in the Subaru-XMM Deep Field (SXDF). The velocity distribution and plausible extended X-ray detections are examined, as well as the number of X-ray point sources and radio sources associated with the clusters. We find that the two clusters that appear virialized and have an extended X-ray detection contain few, if any, AGN, whereas the two pre-virialized clusters have a large AGN population. This constitutes evidence that the AGN fraction in clusters is linked to the clusters' evolutionary stage. The number of X-ray AGN in the pre-virialized clusters is consistent with an overdensity of a factor of similar to 200; the radio AGN appear to be clustered with a factor of 3 to 6 higher. The median K-band luminosities of L(K) = 1.7 +/- 0.7 L* for the X-ray sources and L(K) = 2.3 +/- 0.1 L* for the radio sources support the theory that these AGN are triggered by galaxy interaction and merging events in sub-groups with low internal velocity distributions, which make up the cluster environment in a pre-virialization evolutionary stage. C1 [van Breukelen, Caroline] UCL, London WC1E 6BT, England. [van Breukelen, Caroline; Rawlings, Steve; Clewley, Lee; Mauch, Tom] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Simpson, Chris] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Akiyama, Masayuki] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Bonfield, David] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Jarvis, Matt J.] Univ Hertfordshire, Ctr Astrophys, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England. [Readhead, Tony] CALTECH, Owens Valley Radio Observ, Pasadena, CA 91125 USA. [Stobbart, Ann-Marie; Watson, Mike] Univ Leicester, Dept Phys & Astron, Xray Astron Grp, Leicester LE1 7RH, Leics, England. [Swinbank, Mark] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England. RP van Breukelen, C (reprint author), UCL, Gower St, London WC1E 6BT, England. EM cvb@star.ucl.ac.uk FU STFC; W. M. Keck Foundation FX The authors would like to thank Doi, Morokuma, Miyazaki, Saito, Yamada, Satoshi, Smail and Croom for sharing their redshifts in the SXDF master list. CVB acknowledges support from STFC in the form of a postdoctoral fellowship. This paper is partly based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministrio da Cincia e Tecnologia (Brazil) and SECYT (Argentina). Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. NR 59 TC 11 Z9 11 U1 0 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 1 PY 2009 VL 395 IS 1 BP 11 EP 27 DI 10.1111/j.1365-2966.2009.14513.x PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 431QS UT WOS:000265078700022 ER PT J AU Page, KL Willingale, R O'Brien, PT Tanvir, NR Osborne, JP Zhang, B Holland, ST Levan, AJ Melandri, A Starling, RLC Bersier, D Burrows, DN Geach, JE Maxted, P AF Page, K. L. Willingale, R. O'Brien, P. T. Tanvir, N. R. Osborne, J. P. Zhang, B. Holland, S. T. Levan, A. J. Melandri, A. Starling, R. L. C. Bersier, D. Burrows, D. N. Geach, J. E. Maxted, P. TI The unusual X-ray light curve of GRB 080307: the onset of the afterglow? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiation mechanisms: non-thermal; gamma-rays: bursts; X-rays: individual: GRB 080307 ID SWIFT XRT DATA; BURST AFTERGLOW; ENGINE ACTIVITY; 1ST SURVEY; TELESCOPE; BRIGHT; SUPERNOVA; EVOLUTION; EMISSION; FLARES AB Swift-detected GRB080307 showed an unusual smooth rise in its X-ray light curve around 100 s after the burst, at the start of which the emission briefly softened. This 'hump' has a longer duration than is normal for a flare at early times and does not demonstrate a typical flare profile. Using a two-component power-law-to-exponential model, the rising emission can be modelled as the onset of the afterglow, something which is very rarely seen in Swift-X-ray light curves. We cannot, however, rule out that the hump is a particularly slow early-time flare, or that it is caused by upscattered reverse shock electrons. C1 [Page, K. L.; Willingale, R.; O'Brien, P. T.; Tanvir, N. R.; Osborne, J. P.; Starling, R. L. C.] Univ Leicester, Xray & Observat Astron Grp, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Zhang, B.] Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. [Holland, S. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Holland, S. T.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Levan, A. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Melandri, A.; Bersier, D.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Burrows, D. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Geach, J. E.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Maxted, P.] Univ Keele, Astrophys Grp, Keele ST5 5BG, Staffs, England. RP Page, KL (reprint author), Univ Leicester, Xray & Observat Astron Grp, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. EM kpa@star.le.ac.uk NR 72 TC 5 Z9 5 U1 0 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 1 PY 2009 VL 395 IS 1 BP 328 EP 334 DI 10.1111/j.1365-2966.2009.14509.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 431QS UT WOS:000265078700045 ER PT J AU Oates, SR Page, MJ Schady, P de Pasquale, M Koch, TS Breeveld, AA Brown, PJ Chester, MM Holland, ST Hoversten, EA Kuin, NPM Marshall, FE Roming, PWA Still, M Berk, DEV Zane, S Nousek, JA AF Oates, S. R. Page, M. J. Schady, P. de Pasquale, M. Koch, T. S. Breeveld, A. A. Brown, P. J. Chester, M. M. Holland, S. T. Hoversten, E. A. Kuin, N. P. M. Marshall, F. E. Roming, P. W. A. Still, M. Berk, D. E. Vanden Zane, S. Nousek, J. A. TI A statistical study of gamma-ray burst afterglows measured by the Swift Ultraviolet Optical Telescope SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gamma-rays: bursts ID LIGHT CURVES; 2-COMPONENT JET; LORENTZ FACTOR; REVERSE SHOCK; XRT DATA; EMISSION; FLASHES; SPECTRA; IDENTIFICATION; LUMINOSITIES AB We present the first statistical analysis of 27 Ultraviolet Optical Telescope (UVOT) optical/ultraviolet light curves of gamma-ray burst (GRB) afterglows. We have found, through analysis of the light curves in the observer's frame, that a significant fraction rise in the first 500 s after the GRB trigger, all light curves decay after 500 s, typically as a power law with a relatively narrow distribution of decay indices, and the brightest optical afterglows tend to decay the quickest. We find that the rise could be either produced physically by the start of the forward shock, when the jet begins to plough into the external medium, or geometrically where an off-axis observer sees a rising light curve as an increasing amount of emission enters the observers line of sight, which occurs as the jet slows. We find that at 99.8 per cent confidence, there is a correlation, in the observed frame, between the apparent magnitude of the light curves at 400 s and the rate of decay after 500 s. However, in the rest frame, a Spearman rank test shows only a weak correlation of low statistical significance between luminosity and decay rate. A correlation should be expected if the afterglows were produced by off-axis jets, suggesting that the jet is viewed from within the half-opening angle. or within a core of a uniform energy density theta(c). We also produced logarithmic luminosity distributions for three rest-frame epochs. We find no evidence for bimodality in any of the distributions. Finally, we compare our sample of UVOT light curves with the X-ray Telescope (XRT) light-curve canonical model. The range in decay indices seen in UVOT light curves at any epoch is most similar to the range in decay of the shallow decay segment of the XRT canonical model. However, in the XRT canonical model, there is no indication of the rising behaviour observed in the UVOT light curves. C1 [Oates, S. R.; Page, M. J.; Schady, P.; de Pasquale, M.; Breeveld, A. A.; Kuin, N. P. M.; Still, M.; Zane, S.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Koch, T. S.; Brown, P. J.; Chester, M. M.; Hoversten, E. A.; Roming, P. W. A.; Berk, D. E. Vanden; Nousek, J. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Holland, S. T.; Marshall, F. E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Holland, S. T.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Holland, S. T.] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Code 688 8, Greenbelt, MD 20771 USA. RP Oates, SR (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM sro@mssl.ucl.ac.uk FU STFC FX This research has made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC) and the Leicester Data base and Archive Service (LEDAS), provided by NASA's Goddard Space Flight Center and the Department of Physics and Astronomy, Leicester University, UK, respectively. SRO acknowledges the support of an STFC studentship. SZ thanks STFC for its support through an STFC advanced fellowship. NR 77 TC 79 Z9 79 U1 0 U2 4 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 1 PY 2009 VL 395 IS 1 BP 490 EP 503 DI 10.1111/j.1365-2966.2009.14544.x PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 431QS UT WOS:000265078700061 ER PT J AU Kuin, NPM Landsman, W Page, MJ Schady, P Still, M Breeveld, AA De Pasquale, M Roming, PWA Brown, PJ Carter, M James, C Curran, PA Cucchiara, A Gronwall, C Holland, ST Hoversten, EA Hunsberger, S Kennedy, T Koch, S Lamoureux, H Marshall, FE Oates, SR Parsons, A Palmer, DM Smith, PJ AF Kuin, N. P. M. Landsman, W. Page, M. J. Schady, P. Still, M. Breeveld, A. A. De Pasquale, M. Roming, P. W. A. Brown, P. J. Carter, M. James, C. Curran, P. A. Cucchiara, A. Gronwall, C. Holland, S. T. Hoversten, E. A. Hunsberger, S. Kennedy, T. Koch, S. Lamoureux, H. Marshall, F. E. Oates, S. R. Parsons, A. Palmer, D. M. Smith, P. J. TI GRB 081203A: Swift UVOT captures the earliest ultraviolet spectrum of a gamma-ray burst SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE instrumentation: spectrographs; gamma-rays: bursts ID TELESCOPE; DUST; ABSORPTION; GAS; SPECTROSCOPY; MISSION; STAR; HI AB We present the earliest ultraviolet (UV) spectrum of a gamma-ray burst (GRB) as observed with the Swift Ultra-Violet/Optical Telescope (UVOT). The GRB 081203A spectrum was observed for 50 s with the UV-grism starting 251 s after the Swift-Burst-Alert-Telescope (BAT) trigger. During this time, the GRB was approximate to 13.4 mag (u filter) and was still rising to its peak optical brightness. In the UV-grism spectrum, we find a damped Ly alpha line, Ly beta and the Lyman continuum break at a redshift z = 2.05 +/- 0.01. A model fit to the Lyman absorption implies a gas column density of log N(HI) = 22.0 +/- 0.1 cm(-2), which is typical of GRB host galaxies with damped Ly alpha absorbers. This observation of GRB 081203A demonstrates that for brighter GRBs (v approximate to 14 mag) with moderate redshift (0.5 < z < 3.5) the UVOT is able to provide redshifts, and probe for damped Ly alpha absorbers within 4-6 min from the time of the Swift-BAT trigger. C1 [Kuin, N. P. M.; Page, M. J.; Schady, P.; Still, M.; Breeveld, A. A.; De Pasquale, M.; Carter, M.; James, C.; Curran, P. A.; Kennedy, T.; Lamoureux, H.; Oates, S. R.; Smith, P. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Landsman, W.; Holland, S. T.; Marshall, F. E.; Parsons, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Roming, P. W. A.; Brown, P. J.; Cucchiara, A.; Gronwall, C.; Hoversten, E. A.; Hunsberger, S.; Koch, S.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Palmer, D. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RP Kuin, NPM (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM npmk@mssl.ucl.ac.uk RI Parsons, Ann/I-6604-2012; Curran, Peter/B-5293-2013 OI Curran, Peter/0000-0003-3003-4626 FU UK Science and Technology Facilities Council; NASA [NAS5-00136] FX This work was supported by the UK Science and Technology Facilities Council through a grant for Swift Post Launch Support at UCL-MSSL. This work is sponsored at PSU by NASA contract NAS5-00136. We acknowledge useful comments by the anonymous referee which led to improvement of the grism analysis. We would like to dedicate this Letter to the late Richard Bingham, whose visionary optical design for the UVOT grism made these observations possible. NR 27 TC 22 Z9 22 U1 0 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 1 PY 2009 VL 395 IS 1 BP L21 EP L24 DI 10.1111/j.1745-3933.2009.00632.x PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 431QS UT WOS:000265078700005 ER PT J AU Daescu, DN Todling, R AF Daescu, Dacian N. Todling, Ricardo TI Adjoint Estimation of the Variation in Model Functional Output due to the Assimilation of Data SO MONTHLY WEATHER REVIEW LA English DT Article ID OBSERVATION IMPACT; OBSERVATION SENSITIVITY; ANALYSIS SYSTEM; IMPLEMENTATION; APPROXIMATIONS; ATLANTIC; 4D-VAR AB A parametric approach to the adjoint estimation of the variation in model functional output due to the assimilation of data is considered as a tool to analyze and develop observation impact measures. The parametric approach is specialized to a linear analysis scheme and it is used to derive various high-order approximation equations. This framework includes the Kalman filter and incremental three-a nd four-dimensional variational data assimilation schemes implementing a single outer loop iteration. Distinction is made between Taylor series methods and numerical quadrature methods. The novel quadrature approximations require minimal additional software development and are suitable for testing and implementation at operational numerical weather prediction centers where a data assimilation system (DAS) and the associated adjoint DAS are in place. Their potential use as tools for observation impact estimates needs to be further investigated. Preliminary numerical experiments are provided using the fifth-generation NASA Goddard Earth Observing System (GEOS-5) atmospheric DAS. C1 [Daescu, Dacian N.] Portland State Univ, Dept Math & Stat, Portland, OR 97207 USA. [Todling, Ricardo] NASA GSFC, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. RP Daescu, DN (reprint author), Portland State Univ, Dept Math & Stat, POB 751, Portland, OR 97207 USA. EM daescu@pdx.edu RI Daescu, Dacian /B-3457-2010 FU Atmospheric Data Assimilation Development component of the NASA Modeling, Analysis, and Prediction Program [MAP/04-0000-0080]; NASA Modeling, Analysis, and Prediction Program [NNG06GC67G] FX The numerical results in this work were obtained on the Linux Explore System through a cooperation with the NASA Center for Computational Sciences at Goddard Space Flight Center. The work of D. N. Daescu was supported by the NASA Modeling, Analysis, and Prediction Program under Award NNG06GC67G. The work of R. Todling was partially supported by the Atmospheric Data Assimilation Development component of the NASA Modeling, Analysis, and Prediction Program (MAP/04-0000-0080). We thank two anonymous reviewers whose thoughtful comments and suggestions helped to improve themanuscript. NR 36 TC 18 Z9 18 U1 0 U2 3 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0027-0644 J9 MON WEATHER REV JI Mon. Weather Rev. PD MAY PY 2009 VL 137 IS 5 BP 1705 EP 1716 DI 10.1175/2008MWR2659.1 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 451UC UT WOS:000266495000014 ER PT J AU Sola, F Biaggi-Labiosa, A Fonseca, LF Resto, O Lebron-Colon, M Meador, MA AF Sola, F. Biaggi-Labiosa, A. Fonseca, L. F. Resto, O. Lebron-Colon, M. Meador, M. A. TI Field Emission and Radial Distribution Function Studies of Fractal-like Amorphous Carbon Nanotips SO NANOSCALE RESEARCH LETTERS LA English DT Article DE Carbon nanotips; Graphite-like a-C; EELS; EFED; Field emission ID THIN-FILMS; ASPECT-RATIO; GROWTH; FABRICATION; NANOWIRES; NANOTUBES; SILICON; ARRAYS AB The short-range order of individual fractal-like amorphous carbon nanotips was investigated by means of energy-filtered electron diffraction in a transmission electron microscope (TEM). The nanostructures were grown in porous silicon substrates in situ within the TEM by the electron beam-induced deposition method. The structure factor S(k) and the reduced radial distribution function G(r) were calculated. From these calculations a bond angle of 124A degrees was obtained which suggests a distorted graphitic structure. Field emission was obtained from individual nanostructures using two micromanipulators with sub-nanometer positioning resolution. A theoretical three-stage model that accounts for the geometry of the nanostructures provides a value for the field enhancement factor close to the one obtained experimentally from the Fowler-Nordheim law. C1 [Sola, F.; Biaggi-Labiosa, A.; Fonseca, L. F.; Resto, O.] Univ Puerto Rico, Inst Funct Nanomat, Dept Phys, San Juan, PR 00931 USA. [Lebron-Colon, M.; Meador, M. A.] NASA, Glenn Res Ctr, Polymer Mat Branch, Mat & Struct Div, Cleveland, OH 44135 USA. RP Fonseca, LF (reprint author), Univ Puerto Rico, Inst Funct Nanomat, Dept Phys, POB 23343, San Juan, PR 00931 USA. EM luis.upr@gmail.com FU NASA [NNX08BA48A, NNG05GG78H]; NSF [0701525]; U. S. Department of Energy [DE-AC02-05CH11231] FX This study was supported by the following grants numbers and projects: NASA NNX08BA48A, NASA Space Grant NNG05GG78H, NSF 0701525, Fundamental Aeronautics Program and Subsonic Fixed Wing Project. The authors acknowledge the National Center for Electron Microscopy, Lawrence Berkeley Lab, which is supported by the U. S. Department of Energy under Contract # DE-AC02-05CH11231,and in particular to Dr. A. Minor for helping us with the FE experimental setup. F.S. kindly acknowledges Dr. D. J. H. Cockayne from Oxford University and D. Hull from NASA GRC for providing helpful information related to the electron diffraction analysis. NR 30 TC 9 Z9 11 U1 1 U2 10 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1556-276X J9 NANOSCALE RES LETT JI Nanoscale Res. Lett. PD MAY PY 2009 VL 4 IS 5 BP 431 EP 436 DI 10.1007/s11671-009-9270-5 PG 6 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Science & Technology - Other Topics; Materials Science; Physics GA 423HQ UT WOS:000264487800006 ER PT J AU Svanda, M Klvana, M Sobotka, M Kosovichev, AG Duvall, TL AF Svanda, M. Klvana, M. Sobotka, M. Kosovichev, A. G. Duvall, T. L., Jr. TI Large-scale horizontal flows in the solar photosphere IV. On the vertical structure of large-scale horizontal flows SO NEW ASTRONOMY LA English DT Article DE The Sun: photosphere; Sun: interior; Sun: helioseismology ID TIME-DISTANCE HELIOSEISMOLOGY; RAY APPROXIMATIONS; ACTIVE-REGION; SUPERGRANULATION; SUN; SUPERROTATION; OSCILLATION; TOMOGRAPHY; ACCURACY; ROTATION AB In the recent papers, we introduced a method utilised to measure the flow field. The method is based on the tracking of supergranular structures. We did not precisely know, whether its results represent the flow field in the photosphere or in some subphotospheric layers. In this paper, in combination with helioseismic data, we are able to estimate the depths in the solar convection envelope, where the detected large-scale flow field is well represented by the surface measurements. We got a clear answer to question what kind of structures we track in full-disc Dopplergrams. It seems that in the quiet Sun regions the supergranular structures are tracked, while in the regions with the magnetic field the structures of the magnetic field are dominant. This observation seems obvious, because the nature of Doppler Structures is different in the magnetic regions and in the quiet Sun. We show that the large-scale flow detected by our method represents the motion of plasma in layers down to similar to 10 Mm. The supergranules may therefore be treated as the objects carried by the underlying large-scale velocity field. (C) 2008 Elsevier B.V. All rights reserved. C1 [Svanda, M.] Charles Univ Prague, Astron Inst, Fac Math & Phys, CZ-18000 Prague 8, Czech Republic. [Svanda, M.; Klvana, M.; Sobotka, M.] Acad Sci Czech Republic, Astron Inst, CZ-25165 Ondrejov, Czech Republic. [Kosovichev, A. G.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Duvall, T. L., Jr.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. RP Svanda, M (reprint author), Charles Univ Prague, Astron Inst, Fac Math & Phys, V Holesovickach 2, CZ-18000 Prague 8, Czech Republic. EM michal@astronomie.cz; mklvana@asu.cas.cz; msobotka@asu.cas.cz; sasha@quake.stanford.edu; thomas.l.duvall@nasa.gov RI Svanda, Michal/A-6576-2008; Duvall, Thomas/C-9998-2012; Sobotka, Michal/G-9042-2014; Klvana, Miroslav/G-9026-2014 OI Svanda, Michal/0000-0002-6345-1007; Sobotka, Michal/0000-0001-5439-7822; FU Academy of Sciences of the Czech Republic [IAA30030808]; ESA-PECS [98030]; Astronomical Institute of ASCR [AV0Z10030501]; Astronomical Institute of Charles University [MSM0021620860] FX M.S., M.K., and M.S. were supported by the Grant Agency of Academy of Sciences of the Czech Republic under grant IAA30030808, M.. additionally by ESA-PECS under grant No. 98030. The Astronomical Institute of ASCR is working on the Research project AV0Z10030501 (Academy of Sciences of CR), the Astronomical Institute of Charles University on the Research program MSM0021620860 (Ministry of Education of CR). SOHO is a project of international cooperation between ESA and NASA. NR 29 TC 7 Z9 7 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1384-1076 J9 NEW ASTRON JI New Astron. PD MAY PY 2009 VL 14 IS 4 BP 429 EP 434 DI 10.1016/j.newast.2008.12.003 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 409TH UT WOS:000263528200011 ER PT J AU Barnes, NP Walsh, BM Reichle, DJ DeYoung, RJ AF Barnes, Norman P. Walsh, Brian M. Reichle, Donald J. DeYoung, Russell J. TI Tm:fiber lasers for remote sensing SO OPTICAL MATERIALS LA English DT Article; Proceedings Paper CT 3rd International Workshop on Photonic and Electronic Materials CY JUL 04-06, 2007 CL San Sebastian, SPAIN SP Donostia Int Phys Ctr AB Tm:fiber lasers are an attractive choice for remote sensing of water under and conditions, such as found on Mars. Renewed interest in Martian exploration and discovery Of huge deposits of water at the Martian south pole fuel interest in a water vapor lidar. The potential for high efficiency and the robust and compact nature of fiber lasers are very attractive features. Laser diodes, suitable for pumping Tm:fiber lasers, operate around 0.8 mu m. Tm:fiber lasers operate around 1.9 mu m, in a strong water vapor absorption region. For the laser to be highly efficient, Tm: fiber lasers must operate with a quantum efficiency of two. That is, two laser photons are produced for one absorbed pump photon. The role the fiber material plays and the dynamics of the Tin self quenching process must be understood to optimize this device. Both the physics and experimental results will be presented. Published by Elsevier B.V. C1 [Barnes, Norman P.; Walsh, Brian M.; Reichle, Donald J.; DeYoung, Russell J.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Barnes, NP (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM norman.p.barnes@nasa.gov NR 1 TC 16 Z9 17 U1 4 U2 9 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0925-3467 J9 OPT MATER JI Opt. Mater. PD MAY PY 2009 VL 31 IS 7 BP 1061 EP 1064 DI 10.1016/j.optmat.2007.11.037 PG 4 WC Materials Science, Multidisciplinary; Optics SC Materials Science; Optics GA 449WH UT WOS:000266360600005 ER PT J AU Kwoun, OI Lu, Z AF Kwoun, Oh-ig Lu, Zhong TI Multi-temporal RADARSAT-1 and ERS Backscattering Signatures of Coastal Wetlands in Southeastern Louisiana SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING LA English DT Article ID SYNTHETIC-APERTURE RADAR; AMAZON FLOODPLAIN; UNITED-STATES; SAR DATA; VEGETATION; IMAGERY; INTERFEROMETRY; JERS-1; AREA AB Using multi-temporal European Remote-sensing Satellites (ERS-1/-2) and Canadian Rodar Satellite (RADARSAT-1) synthetic aperture radar (SAR) data over the Louisiana coastal zone, we characterize seasonal variations of radar backscattering according to vegetation type. Our main findings are as follows. First, ERS-1/-2 and HADARSAT-1 require careful radiometric calibration to perform multi-temporal backscattering analysis for wetland mapping. We use SAR backscattering signals from cities for the relative calibration. Second, using seasonally averaged backscattering coefficients from ERS-1/-2 and RADARSAT-1, we can differentiate most forests (bottomland and swamp forests) and marshes (freshwater, intermediate, brackish, and saline marshes) in coastal wetlands. The student t-test results support the usefulness of season-averaged backscatter data for classification. Third, combining SAR backscattering coefficients and an optical-sensor-based normalized difference vegetation index can provide further insight into vegetation type and enhance the separation between forests and marshes. Our study demonstrates that SAR can provide necessary information to characterize coastal wetlands and monitor their changes. C1 [Kwoun, Oh-ig] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kwoun, Oh-ig] US Geol Survey, SAIC, EROS Data Ctr, Sioux Falls, SD 57198 USA. [Lu, Zhong] USGS EROS Ctr, Vancouver, WA 98683 USA. [Lu, Zhong] Cascades Volcano Observ, Vancouver, WA 98683 USA. RP Kwoun, OI (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM kwoun@jpl.nasa.gov; lu@usgs.gov FU U.S. Geological Survey (USCS) Director Venture Capital Fund; USGS Eastern Region Venture Capital Fund; USGS Land Remote Sensing Program; USGS [O3CRCN0001] FX ERS-1/ERS-2 SAR images are copyrighted @ 1992, 1993, 1996, 1997, and 1998 by the European Space Agency (ESA) and were provided by the ESA using the Category-1 Project 2853. RADARSAT-1 images are copyrighted (D 2002, 2003, and 2004 by the Canadian Space Agency (CSA) and were provided. by the Alaska Satellite Facility (ASF). This research was supported by funding from the U.S. Geological Survey (USCS) Director Venture Capital Fund, USGS Eastern Region Venture Capital Fund, USGS Land Remote Sensing Program, and USGS contract O3CRCN0001. We thank Elijah Ramsey and Terry Sohl for careful reviews and constructive comments. NR 41 TC 8 Z9 10 U1 2 U2 10 PU AMER SOC PHOTOGRAMMETRY PI BETHESDA PA 5410 GROSVENOR LANE SUITE 210, BETHESDA, MD 20814-2160 USA SN 0099-1112 EI 2374-8079 J9 PHOTOGRAMM ENG REM S JI Photogramm. Eng. Remote Sens. PD MAY PY 2009 VL 75 IS 5 BP 607 EP 617 PG 11 WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Geology; Remote Sensing; Imaging Science & Photographic Technology GA 446PQ UT WOS:000266134000011 ER PT J AU Nielsen, KE Gull, TR AF Nielsen, Krister E. Gull, Theodore R. TI Eta Carinae: an Astrophysical Laboratory SO PHYSICA SCRIPTA LA English DT Article; Proceedings Paper CT 9th International Conference on Atomic Spectroscopy and Oscillator Strengths for Astrophysical and Laboratory Plasma CY AUG 07-10, 2007 CL Lund Univ, Lund Observatory & Phys Dept, Lund, SWEDEN HO Lund Univ, Lund Observatory & Phys Dept ID HOMUNCULUS-NEBULA; 2003.5 MINIMUM; EJECTA ABSORPTION; EMISSION-LINES; II EMISSION; ULTRAVIOLET; SPECTRUM; VARIABILITY; DISCOVERY; COMPANION AB Eta Carinae provides a unique example to investigate a massive star in a late evolutionary phase and how CNO-processed material is ejected and mixed with the interstellar medium. The absorbing gas surrounding Eta Carinae (eta Car) shows similar characteristics to the intervening gas in spectra of gamma ray burst progenitors. Consequently, the eta Car spectrum may provide clues about the nature of other extreme objects such as hypernovae and supernova impostors. In the 1840s, eta Car underwent a massive ejection, which was repeated to a lesser extent in the 1890s. Today we see the Homunculus, a bipolar expanding neutral shell, and the Little Homunculus, an interior, spectroscopically time-variable, ionized structure. The eta Car system is ideal as a laboratory for absorption and emission line spectroscopy. In the line-of-sight towards eta Car, multiple narrow absorption lines are observed from environments with densities around 10(7) cm(-3) and temperatures ranging from 60 to 7000 K. Thousands of neutral/singly ionized metal lines are identified, in addition to molecular lines in species such as H(2), CH, OH and NH. The input from the laboratory spectroscopy community has furthered the analysis of eta Car. Future observations of eta Car in the infrared through radio wavelength region will enable new detections of atomic and molecular transitions, most notably of hydrides and nitrides. We will demonstrate how experimentally derived atomic data have improved our spectral analysis, and illuminate where future work is needed. C1 [Nielsen, Krister E.; Gull, Theodore R.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Nielsen, KE (reprint author), Catholic Univ Amer, Washington, DC 20064 USA. EM krister.nielsen@nasa.gov RI Gull, Theodore/D-2753-2012 OI Gull, Theodore/0000-0002-6851-5380 NR 28 TC 2 Z9 2 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0031-8949 J9 PHYS SCRIPTA JI Phys. Scr. PD MAY PY 2009 VL T134 AR 014002 DI 10.1088/0031-8949/2009/T134/014002 PG 9 WC Physics, Multidisciplinary SC Physics GA 465UG UT WOS:000267612800003 ER PT J AU Drasco, S AF Drasco, Steve TI Verifying black hole orbits with gravitational spectroscopy SO PHYSICAL REVIEW D LA English DT Article ID MASS-RATIO INSPIRALS; KERR SPACETIME; ADIABATIC EVOLUTION; CIRCULAR ORBIT; POINT MASSES; RADIATION; LISA; PERTURBATIONS; RELATIVITY; PARAMETERS AB Gravitational waves from test masses bound to geodesic orbits of rotating black holes are simulated, using Teukolsky's black hole perturbation formalism, for about ten thousand generic orbital configurations. Each binary radiates power exclusively in modes with frequencies that are integer-linear combinations of the orbit's three fundamental frequencies. General spectral properties are found with a survey of orbits about a black hole taken to be rotating at 80% of the maximal spin. The orbital eccentricity is varied from 0.1 to 0.9. Inclination ranges from 20 degrees to 160 degrees and comes to within 20 degrees of polar. Semilatus rectum is varied from 1.2 to 3 times the value at the innermost stable circular orbits. The following general spectral properties are found: (i) 99% of the radiated power is typically carried by a few hundred modes, and at most by about a thousand modes, (ii) the dominant frequencies can be grouped into a small number of families defined by fixing two of the three integer frequency multipliers, and (iii) the specifics of these trends can be qualitatively inferred from the geometry of the orbit under consideration. Detections using triperiodic analytic templates modeled on these general properties would constitute a verification of radiation from an adiabatic sequence of black hole orbits and would recover the evolution of the fundamental orbital frequencies. In an analogy with ordinary spectroscopy, this would compare to observing the Bohr model's atomic hydrogen spectrum without being able to rule out alternative atomic theories or nuclei. The suitability of such a detection technique is demonstrated using snapshots computed at 12-hour intervals throughout the last three years before merger of a kludged inspiral. The system chosen is typical of those thought to occur in galactic nuclei and to be observable with space-based gravitational wave detectors like LISA. Because of circularization, the number of excited modes decreases as the binary evolves. A hypothetical detection algorithm that tracks mode families dominating the first 12 hours of the inspiral would capture 98% of the total power over the remaining three years. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Drasco, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 64 TC 4 Z9 4 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 EI 1550-2368 J9 PHYS REV D JI Phys. Rev. D PD MAY PY 2009 VL 79 IS 10 AR 104016 DI 10.1103/PhysRevD.79.104016 PG 18 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 451WP UT WOS:000266501900070 ER PT J AU Tinto, M Dick, GJ Prestage, JD Armstrong, JW AF Tinto, Massimo Dick, George J. Prestage, John D. Armstrong, J. W. TI Improved spacecraft radio science using an on-board atomic clock: Application to gravitational wave searches SO PHYSICAL REVIEW D LA English DT Article ID DOPPLER TRACKING; RADIATION; LINKS AB Recent advances in space-qualified atomic clocks (low-mass, low power-consumption, frequency stability comparable to that of ground-based clocks) can enable interplanetary spacecraft radio science experiments at unprecedented Doppler sensitivities. The addition of an on-board digital receiver would allow the up- and down-link Doppler frequencies to be measured separately. Such separate, high-quality measurements allow optimal data combinations that suppress the currently leading noise sources: phase scintillation noise from the Earth's atmosphere and Doppler noise caused by mechanical vibrations of the ground antenna. Here we provide a general expression for the optimal combination of ground and on-board Doppler data and compute the sensitivity such a system would have to low-frequency gravitational waves (GWs). Assuming a plasma scintillation noise calibration comparable to that already demonstrated with the multilink CASSINI radio system, the space-clock/digital-receiver instrumentation enhancements would give GW strain sensitivity of 3.7x10(-14) Hz(-1/2) for randomly polarized, monochromatic GW signals isotropically distributed over the celestial sphere, over a two-decade (similar to 0.0001-0.01 Hz) region of the low-frequency band. This is about an order of magnitude better than currently achieved with traditional two-way coherent Doppler experiments. The utility of optimally combining simultaneous up- and down-link observations is not limited to GW searches. The Doppler tracking technique discussed here could be performed at minimal incremental cost to improve also other radio science experiments (i.e., tests of relativistic gravity, planetary and satellite gravity field measurements, atmospheric and ring occultations) on future interplanetary missions. C1 [Tinto, Massimo; Dick, George J.; Prestage, John D.; Armstrong, J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Tinto, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Massimo.Tinto@jpl.nasa.gov; George.J.Dick@jpl.nasa.gov; John.D.Prestage@jpl.nasa.gov; John.W.Armstrong@jpl.nasa.gov NR 27 TC 3 Z9 3 U1 0 U2 2 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 MAY PY 2009 VL 79 IS 10 AR 102003 DI 10.1103/PhysRevD.79.102003 PG 9 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 451WP UT WOS:000266501900009 ER PT J AU Kuranz, CC Drake, RP Grosskopf, MJ Budde, A Krauland, C Marion, DC Visco, AJ Ditmar, JR Robey, HF Remington, BA Miles, AR Cooper, ABR Sorce, C Plewa, T Hearn, NC Killebrew, KL Knauer, JP Arnett, D Donajkowski, T AF Kuranz, C. C. Drake, R. P. Grosskopf, M. J. Budde, A. Krauland, C. Marion, D. C. Visco, A. J. Ditmar, J. R. Robey, H. F. Remington, B. A. Miles, A. R. Cooper, A. B. R. Sorce, C. Plewa, T. Hearn, N. C. Killebrew, K. L. Knauer, J. P. Arnett, D. Donajkowski, T. TI Three-dimensional blast-wave-driven Rayleigh-Taylor instability and the effects of long-wavelength modes SO PHYSICS OF PLASMAS LA English DT Article; Proceedings Paper CT 50th Annual Meeting of the Division of Plasma Physics of the American-Physical-Society CY NOV 17-21, 2008 CL Dallas, TX SP Amer Phys Soc, Div Plasma Phys DE explosions; helium; hydrogen; plasma production by laser; plasma shock waves; plasma simulation; Rayleigh-Taylor instability ID 2-DIMENSIONAL SIMULATIONS; HYDRODYNAMICS CODE; SUPERNOVA-REMNANTS; EARLY EVOLUTION; LIGHT-CURVE; SN-1987A; GROWTH; ASTROPHYSICS; SYSTEM; LASERS AB This paper describes experiments exploring the three-dimensional (3D) Rayleigh-Taylor instability at a blast-wave-driven interface. This experiment is well scaled to the He/H interface during the explosion phase of SN1987A. In the experiments, similar to 5 kJ of energy from the Omega laser was used to create a planar blast wave in a plastic disk, which is accelerated into a lower-density foam. These circumstances induce the Richtmyer-Meshkov instability and, after the shock passes the interface, the system quickly becomes dominated by the Rayleigh-Taylor instability. The plastic disk has an intentional pattern machined at the plastic/foam interface. This perturbation is 3D with a basic structure of two orthogonal sine waves with a wavelength of 71 mu m and an amplitude of 2.5 mu m. Additional long-wavelength modes with a wavelength of either 212 or 424 mu m are added onto the single-mode pattern. The addition of the long-wavelength modes was motivated by the results of previous experiments where material penetrated unexpectedly to the shock front, perhaps due to an unintended structure. The current experiments and simulations were performed to explore the effects of this unintended structure; however, we were unable to reproduce the previous results. C1 [Kuranz, C. C.; Drake, R. P.; Grosskopf, M. J.; Budde, A.; Krauland, C.; Marion, D. C.; Visco, A. J.; Ditmar, J. R.] Univ Michigan, Ann Arbor, MI 48109 USA. [Robey, H. F.; Remington, B. A.; Miles, A. R.; Cooper, A. B. R.; Sorce, C.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Plewa, T.] Florida State Univ, Dept Comp Sci, Tallahassee, FL 32306 USA. [Hearn, N. C.] Univ Chicago, ASC Flash Ctr, Chicago, IL 60637 USA. [Killebrew, K. L.] Sandia Natl Labs, Albuquerque, NM 87185 USA. [Knauer, J. P.] Univ Rochester, Laser Energet Lab, Rochester, NY USA. [Arnett, D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Donajkowski, T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kuranz, CC (reprint author), Univ Michigan, Ann Arbor, MI 48109 USA. RI Plewa, Tomasz/C-1470-2010; OI Plewa, Tomasz/0000-0002-1762-2565; Drake, R Paul/0000-0002-5450-9844 NR 43 TC 18 Z9 19 U1 1 U2 13 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 1070-664X EI 1089-7674 J9 PHYS PLASMAS JI Phys. Plasmas PD MAY PY 2009 VL 16 IS 5 AR 056310 DI 10.1063/1.3099320 PG 10 WC Physics, Fluids & Plasmas SC Physics GA 451WC UT WOS:000266500600123 ER PT J AU Galli, GLJ Shiels, HA Brill, RW AF Galli, Gina L. J. Shiels, Holly A. Brill, Richard W. TI Temperature Sensitivity of Cardiac Function in Pelagic Fishes with Different Vertical Mobilities: Yellowfin Tuna (Thunnus albacares), Bigeye Tuna (Thunnus obesus), Mahimahi (Coryphaena hippurus), and Swordfish (Xiphias gladius) SO PHYSIOLOGICAL AND BIOCHEMICAL ZOOLOGY LA English DT Article ID TROUT ONCORHYNCHUS-MYKISS; ISOLATED VENTRICULAR TRABECULAE; FORCE FREQUENCY RELATIONSHIPS; ATLANTIC BLUEFIN TUNA; SARCOPLASMIC-RETICULUM; RAINBOW-TROUT; ADRENERGIC-STIMULATION; THERMAL-ACCLIMATION; CALCIUM CHANNELS; HAWAIIAN-ISLANDS AB We measured the temperature sensitivity, adrenergic sensitivity, and dependence on sarcoplasmic reticulum (SR) Ca(2+) of ventricular muscle from pelagic fishes with different vertical mobility patterns: bigeye tuna (Thunnus obesus), yellowfin tuna (Thunnus albacares), and mahimahi (Coryphaena hippurus) and a single specimen from swordfish (Xiphias gladius). Ventricular muscle from the bigeye tuna and mahimahi exhibited a biphasic response to an acute decrease in temperature (from 26 degrees to 7 degrees C); twitch force and kinetic parameters initially increased and then declined. The magnitude of this response was larger in the bigeye tuna than in the mahimahi. Under steady state conditions at 26 degrees C, inhibition of SR Ca(2+) release and reuptake with ryanodine and thapsigargin decreased twitch force and kinetic parameters, respectively, in the bigeye tuna only. However, the initial inotropy associated with decreasing temperature was abolished by SR inhibition in both the bigeye tuna and the mahimahi. Application of adrenaline completely reversed the effects of ryanodine and thapsigargin, but this effect was diminished at cold temperatures. In the yellowfin tuna, temperature and SR inhibition had minor effects on twitch force and kinetics, while adrenaline significantly increased these parameters. Limited data suggest that swordfish ventricular muscle responds to acute temperature reduction, SR inhibition, and adrenergic stimulation in a manner similar to that of bigeye tuna ventricular muscle. In aggregate, our results show that the temperature sensitivity, SR dependence, and adrenergic sensitivity of pelagic fish hearts are species specific and that these differences reflect species-specific vertical mobility patterns. C1 [Galli, Gina L. J.; Shiels, Holly A.] Univ Manchester, Fac Life Sci, Core Technol Facil, Manchester M13 9NT, Lancs, England. [Brill, Richard W.] Virginia Inst Marine Sci, Natl Marine Fisheries Serv, NE Fisheries Sci Ctr, Cooperat Marine Educ & Res Program, Gloucester Point, VA 23062 USA. RP Galli, GLJ (reprint author), Univ British Columbia, 2357 Main Mall, Vancouver, BC V6T 1Z4, Canada. EM ggalli@interchange.ubc.ca FU Biotechnology and Biological Sciences Research Council NR 68 TC 19 Z9 19 U1 0 U2 9 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1522-2152 J9 PHYSIOL BIOCHEM ZOOL JI Physiol. Biochem. Zool. PD MAY-JUN PY 2009 VL 82 IS 3 BP 280 EP 290 DI 10.1086/597484 PG 11 WC Physiology; Zoology SC Physiology; Zoology GA 431DZ UT WOS:000265042800008 PM 19284308 ER PT J AU Blank, JG Green, S Blake, D Valley, JW Kita, NT Treiman, A Dobson, PF AF Blank, J. G. Green, Sj. Blake, D. Valley, J. W. Kita, N. T. Treiman, A. Dobson, P. F. TI An alkaline spring system within the Del Puerto Ophiolite (California, USA): A Mars analog site SO PLANETARY AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Symposium on Exploring Mars and its Earth Analogues CY JUN 19-23, 2007 CL Trento, ITALY DE Mars analog; Dolomite; Alkaline springs; Biosignature ID OXYGEN-ISOTOPE FRACTIONATION; 16S RIBOSOMAL-RNA; MODERN MARINE STROMATOLITES; LITHIFIED MICRITIC LAMINAE; MARTIAN METEORITE ALH84001; SULFATE-REDUCING BACTERIA; ALLAN HILLS 84001; MERIDIANI-PLANUM; GEOCHEMICAL EVIDENCE; DOLOMITE FORMATION AB Mars appears to have experienced little compositional differentiation of primitive lithosphere, and thus much of the surface of Mars is covered by mafic lavas. On Earth, mafic and ultramafic rocks present in ophiolites, oceanic crust and upper mantle that have been obducted onto land, are therefore good analogs for Mars. The characteristic mineralogy, aqueous geochemistry, and microbial communities of cold-water alkaline springs associated with these mafic and ultramafic rocks represent a particularly compelling analog for potential life-bearing systems. Serpentinization, the reaction of water with mafic minerals Such as olivine and pyroxene, yields fluids with unusual chemistry (Mg-OH and Ca-OH waters with pH values up to similar to 12), as well as heat and hydrogen gas that can sustain subsurface, chemosynthetic ecosystems. The recent observation of seeps from pole-facing crater and canyon walls in the higher Martian latitudes supports the hypothesis that even present conditions might allow for a rock-hosted chemosynthetic biosphere in near-surface regions of the Martian crust. The generation of methane within a zone of active serpentinization, through either abiogenic or biogenic processes, could account for the presence of methane detected in the Martian atmosphere. For all of these reasons, studies of terrestrial alkaline springs associated with mafic and ultramafic rocks are particularly timely. This study focuses on the alkaline Adobe Springs, emanating from mafic and ultramafic rocks of the California Coast Range, where a community of novel bacteria is associated with the precipitation of Mg-Ca carbonate cements. The carbonates may serve as a biosignature that could be used in the search for evidence of life on Mars. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Blank, J. G.] SETI Inst, Mountain View, CA 94043 USA. [Blank, J. G.; Green, Sj.; Blake, D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Valley, J. W.; Kita, N. T.] Univ Wisconsin, Dept Geol & Geophys, Madison, WI 53706 USA. [Treiman, A.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Dobson, P. F.] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Earth Sci, Berkeley, CA 94720 USA. RP Blank, JG (reprint author), SETI Inst, 515 N Whisman Rd, Mountain View, CA 94043 USA. EM jblank@seti.org RI Valley, John/B-3466-2011; Green, Stefan/C-8980-2011; Dobson, Patrick/D-8771-2015; Kita, Noriko/H-8035-2016; OI Valley, John/0000-0003-3530-2722; Dobson, Patrick/0000-0001-5031-8592; Kita, Noriko/0000-0002-0204-0765; Green, Stefan/0000-0003-2781-359X NR 84 TC 34 Z9 37 U1 0 U2 20 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD MAY PY 2009 VL 57 IS 5-6 BP 533 EP 540 DI 10.1016/j.pss.2008.11.018 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 456QX UT WOS:000266863400003 ER PT J AU Burr, DM Bruno, BC Lanagan, PD Glaze, LS Jaeger, WL Soare, RJ Tseung, JMWB Skinner, JA Baloga, SM AF Burr, Devon M. Bruno, Barbara C. Lanagan, Peter D. Glaze, Lori S. Jaeger, Windy L. Soare, Richard J. Tseung, Jean-Michel Wan Bun Skinner, James A., Jr. Baloga, Stephen M. TI Mesoscale raised rim depressions (MRRDs) on Earth: A review of the characteristics, processes, and spatial distributions of analogs for Mars SO PLANETARY AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Symposium on Exploring Mars and its Earth Analogues CY JUN 19-23, 2007 CL Trento, ITALY DE Mars; Surface; Terrestrial analogs; Spatial analysis ID WESTERN-ARCTIC-COAST; MUD VOLCANISM; GROUND ICE; HYDROVOLCANIC EXPLOSIONS; ACCRETIONARY COMPLEX; COLUMBIA PLATEAU; ATHABASCA VALLES; NORTHERN PLAINS; UTOPIA PLANITIA; RING STRUCTURES AB Fields of mesoscale raised rim depressions (MRRDs) of various origins are found on Earth and Mars. Examples include rootless cones, mud volcanoes, collapsed pingos, rimmed kettle holes, and basaltic ring structures. Correct identification of MRRDs on Mars is valuable because different MRRD types have different geologic and/or climatic implications and are often associated with volcanism and/or water, which may provide locales for biotic or prebiotic activity. In order to facilitate correct identification of fields of MRRDs on Mars and their implications, this work provides a review of common terrestrial MRRD types that. Occur in fields. in this review, MRRDs by formation mechanism, including hydrovolcanic (phreatomagmatic cones, basaltic ring structures), sedimentological (mud volcanoes), and ice-related (pingos, volatile ice-block forms) mechanisms. For each broad mechanism, we present a comparative synopsis of (i) morphology and observations, (ii) physical formation processes, and (iii) published hypothesized locations on Mars. Because the morphology for MRRDs may be ambiguous, an additional tool is provided for distinguishing fields of MRRDs by origin on Mars, namely, spatial distribution analyses for MRRDs within fields on Earth. We find that MRRDs have both distinguishing and similar characteristics, and observation that applies both to their mesoscale morphology and to their spatial distribution statistics. Thus, this review provides tools for distinguishing between various MRRDs, while highlighting the utility of the Multiple working hypotheses approach. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Burr, Devon M.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Burr, Devon M.] SETI Inst, Mountain View, CA 94043 USA. [Bruno, Barbara C.] Univ Hawaii, Sch Ocean & Earth Sci & Technol, Honolulu, HI 96822 USA. [Bruno, Barbara C.; Glaze, Lori S.; Baloga, Stephen M.] Proxemy Res, Gaithersburg, MD 20882 USA. [Lanagan, Peter D.] Coll So Nevada, Henderson, NV 89002 USA. [Glaze, Lori S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Jaeger, Windy L.; Skinner, James A., Jr.] US Geol Survey, Astrogeol Team, Flagstaff, AZ 86001 USA. [Soare, Richard J.] Concordia Univ, Dept Geog & Planning & Environm, Montreal, PQ H3G 1M8, Canada. [Soare, Richard J.] Univ Calgary, Dept Geog, Calgary, AB T2N 1N4, Canada. [Soare, Richard J.] Univ Western Ontario, Dept Earth Sci & Phys & Astron, London, ON N6A 5B7, Canada. [Tseung, Jean-Michel Wan Bun] Dawson Coll, Dept Geog, Montreal, PQ H3Z 1A4, Canada. RP Burr, DM (reprint author), Univ Tennessee, Dept Earth & Planetary Sci, 1412 Circle Dr, Knoxville, TN 37996 USA. EM dburr1@utk.edu RI Glaze, Lori/D-1314-2012; Skinner, James/M-7966-2014 NR 153 TC 20 Z9 20 U1 1 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD MAY PY 2009 VL 57 IS 5-6 SI SI BP 579 EP 596 DI 10.1016/j.pss.2008.11.011 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 456QX UT WOS:000266863400007 ER PT J AU Dohm, JM Baker, VR Boynton, WV Fairen, AG Ferris, JC Finch, M Furfaro, R Hare, TM Janes, DM Kargel, JS Karunatillake, S Keller, J Kerry, K Kim, KJ Komatsu, G Mahaney, WC Schulze-Makuch, D Marinangeli, L Ori, GG Ruiz, J Wheelock, SJ AF Dohm, James M. Baker, Victor R. Boynton, William V. Fairen, Alberto G. Ferris, Justin C. Finch, Michael Furfaro, Roberto Hare, Trent M. Janes, Daniel M. Kargel, Jeffrey S. Karunatillake, Suniti Keller, John Kerry, Kris Kim, Kyeong J. Komatsu, Goro Mahaney, William C. Schulze-Makuch, Dirk Marinangeli, Lucia Ori, Gian G. Ruiz, Javier Wheelock, Shawn J. TI GRS evidence and the possibility of paleooceans on Mars SO PLANETARY AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Symposium on Exploring Mars and its Earth Analogues CY JUN 19-23, 2007 CL Trento, ITALY DE Mars; Gamma-ray spectrometer; Oceans; Water; Elemental; Hydrogeology ID MARTIAN NORTHERN PLAINS; ALTIMETER MOLA DATA; MERIDIANI-PLANUM; AQUEOUS SEDIMENTATION; GLOBAL DISTRIBUTION; CHAOTIC OBLIQUITY; ROOTLESS CONES; GROUND ICE; WATER; DEPOSITS AB The Gamma Ray Spectrometer (Mars Odyssey spacecraft) has revealed elemental distributions of potassium (K), thorium (Th), and iron (Fe) on Mars that require fractionation of K (and possibly Th and Fe) consistent with aqueous activity. This includes weathering, evolution of soils, and transport, sorting, and deposition, as well as with the location of first-order geomorphological demarcations identified as possible paleoocean boundaries. The element abundances occur in patterns consistent with weathering in situ and possible presence of relict or exhumed paleosols, deposition of weathered materials (salts and clastic minerals), and weathering/transport under neutral to acidic brines. The abundances are explained by hydrogeology consistent with the possibly overlapping alternatives of paleooceans and/or heterogeneous rock compositions from diverse provenances (e.g., differing igneous compositions). (C) 2008 Elsevier Ltd. All rights reserved. C1 [Dohm, James M.; Baker, Victor R.; Kargel, Jeffrey S.; Wheelock, Shawn J.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. [Dohm, James M.; Baker, Victor R.; Boynton, William V.; Finch, Michael; Janes, Daniel M.; Kerry, Kris] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Fairen, Alberto G.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Ferris, Justin C.] US Geol Survey, Calif Water Sci Ctr, Sacramento, CA 95819 USA. [Furfaro, Roberto] Univ Arizona, Dept Aerosp & Mech Engn, Tucson, AZ 85721 USA. [Hare, Trent M.] US Geol Survey, Flagstaff, AZ 86001 USA. [Karunatillake, Suniti] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [Keller, John] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA USA. [Kim, Kyeong J.] Korea Inst Geosci & Mineral Resources, Geol & Environm Hazards Div, Taejon, South Korea. [Komatsu, Goro; Marinangeli, Lucia; Ori, Gian G.] Univ G DAnnunzio, Int Res Sch Planetary Sci, Pescara, Italy. [Mahaney, William C.] York Univ, Atkinson Coll, Geomorphol & Pedol Lab, N York, ON M3J 1P3, Canada. [Mahaney, William C.] Quaternary Surveys, Thornhill, ON L4J 1J4, Canada. [Schulze-Makuch, Dirk] Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99164 USA. [Ruiz, Javier] CSIC, Museo Nacl Ciencias Nat, E-28006 Madrid, Spain. RP Dohm, JM (reprint author), Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. EM jmd@hwr.arizona.edu RI Karunatillake, Suniti/A-5934-2009; Wheelock, Shawn/A-7627-2010; Dohm, James/A-3831-2014; Ruiz, Javier/P-3975-2015; Komatsu, Goro/I-7822-2012; OI Karunatillake, Suniti/0000-0001-9891-1432; Ruiz, Javier/0000-0002-3937-8380; Komatsu, Goro/0000-0003-4155-108X; Kim, Kyeong J/0000-0001-6220-8411; Hare, Trent/0000-0001-8842-389X; Schulze-Makuch, Dirk/0000-0002-1923-9746; ORI, Gian Gabriele/0000-0002-6460-1476 NR 146 TC 40 Z9 41 U1 1 U2 12 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 MAY PY 2009 VL 57 IS 5-6 SI SI BP 664 EP 684 DI 10.1016/j.pss.2008.10.008 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 456QX UT WOS:000266863400016 ER PT J AU Shin, DS Jung, YD AF Shin, Dong-Soo Jung, Young-Dae TI Nonthermal and screening effects on photoionizations in Lorentzian plasmas SO PLASMA PHYSICS AND CONTROLLED FUSION LA English DT Article AB The nonthermal and plasma screening effects on the x-ray photoionization process are investigated in astrophysical Lorentzian plasmas. The screened atomic wave function and energy eigenvalue of the target ion in Lorentzian plasmas are obtained by the Rayleigh-Ritz variational method. The x-ray retardation and screened Coulomb corrections are considered to obtain a photoionization cross section as a function of the spectral index and plasma parameters. It is shown that the nonthermal character of the Lorentzian plasma suppresses the photoionization cross section. Hence, the photoionization cross sections in nonthermal plasmas are found to be always smaller than those in thermal plasmas. It is also shown that the plasma screening effect is more significant for small spectral indices. In addition, the nonthermal effect on the photoionization cross section is found to be decreased with an increase in the Debye length. C1 [Shin, Dong-Soo; Jung, Young-Dae] Hanyang Univ, Dept Appl Phys, Ansan 426791, Kyunggi Do, South Korea. [Jung, Young-Dae] NASA, George C Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. RP Shin, DS (reprint author), Hanyang Univ, Dept Appl Phys, Ansan 426791, Kyunggi Do, South Korea. EM ydjung@hanyang.ac.kr NR 24 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0741-3335 EI 1361-6587 J9 PLASMA PHYS CONTR F JI Plasma Phys. Control. Fusion PD MAY PY 2009 VL 51 IS 5 AR 055007 DI 10.1088/0741-3335/51/5/055007 PG 8 WC Physics, Fluids & Plasmas SC Physics GA 438VQ UT WOS:000265584300007 ER PT J AU Rubin, B Farnell, C Williams, J Vaughn, J Schneider, T Ferguson, D AF Rubin, B. Farnell, C. Williams, J. Vaughn, J. Schneider, T. Ferguson, D. TI Magnetic filter type plasma source for ground-based simulation of low earth orbit environment SO PLASMA SOURCES SCIENCE & TECHNOLOGY LA English DT Article ID ION-SOURCE; ELECTRICAL BREAKDOWN; TECHNOLOGY; COLLECTION; SPACECRAFT; BEAMS; ARRAY AB Simulation of the low Earth orbit (LEO) plasma environment in ground-based vacuum facilities is important for studies of spacecraft interaction with ionospheric plasmas. In this paper we describe the design and performance of a magnetic filter-equipped plasma source. Experimental data collected in the expanding plasma downstream of the source suggest it is a good candidate for use as a LEO plasma simulator in that the expanding plasma has a very low electron temperature and contains streaming ions-the plasma environment encountered by satellites in LEO. Adjustable plasma source operating conditions of flow rate, discharge current and discharge voltage enable production of plasma electron temperatures over the range from 0.17 to 0.35 eV and streaming ion energies over the range from 1 to 4 eV. C1 [Rubin, B.; Farnell, C.; Williams, J.] Colorado State Univ, Dept Mech Engn, Ft Collins, CO 80523 USA. [Vaughn, J.; Schneider, T.; Ferguson, D.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Williams, J (reprint author), Colorado State Univ, Dept Mech Engn, Ft Collins, CO 80523 USA. EM john.d.williams@colostate.edu FU NASA Space Environment and Effects FX Funding for the final development of the plasma source was provided by the NASA Space Environment and Effects (SEE) Program. The authors would like to thank Kenneth Wright (University of Alabama in Huntsville) for assistance in analyzing the plasma data. NR 25 TC 6 Z9 6 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0963-0252 J9 PLASMA SOURCES SCI T JI Plasma Sources Sci. Technol. PD MAY PY 2009 VL 18 IS 2 AR 025015 DI 10.1088/0963-0252/18/2/025015 PG 9 WC Physics, Fluids & Plasmas SC Physics GA 438UL UT WOS:000265580800018 ER PT J AU Slavin, JA Acuna, MH Anderson, BJ Baker, DN Benna, M Boardsen, SA Gloeckler, G Gold, RE Ho, GC Korth, H Krimigis, SM McNutt, RL Raines, JM Sarantos, M Schriver, D Solomon, SC Travnicek, P Zurbuchen, TH AF Slavin, James A. Acuna, Mario H. Anderson, Brian J. Baker, Daniel N. Benna, Mehdi Boardsen, Scott A. Gloeckler, George Gold, Robert E. Ho, George C. Korth, Haje Krimigis, Stamatios M. McNutt, Ralph L., Jr. Raines, Jim M. Sarantos, Menelaos Schriver, David Solomon, Sean C. Travnicek, Pavel Zurbuchen, Thomas H. TI MESSENGER Observations of Magnetic Reconnection in Mercury's Magnetosphere SO SCIENCE LA English DT Article ID GEOTAIL OBSERVATIONS; EARTHS MAGNETOPAUSE; FLUX-TRANSFER; 1ST FLYBY; FIELD; SUBSTORMS; MAGNETOTAIL; TAIL AB Solar wind energy transfer to planetary magnetospheres and ionospheres is controlled by magnetic reconnection, a process that determines the degree of connectivity between the interplanetary magnetic field (IMF) and a planet's magnetic field. During MESSENGER's second flyby of Mercury, a steady southward IMF was observed and the magnetopause was threaded by a strong magnetic field, indicating a reconnection rate similar to 10 times that typical at Earth. Moreover, a large flux transfer event was observed in the magnetosheath, and a plasmoid and multiple traveling compression regions were observed in Mercury's magnetotail, all products of reconnection. These observations indicate that Mercury's magnetosphere is much more responsive to IMF direction and dominated by the effects of reconnection than that of Earth or the other magnetized planets. C1 [Slavin, James A.; Boardsen, Scott A.; Sarantos, Menelaos] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Acuna, Mario H.; Benna, Mehdi] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Anderson, Brian J.; Gold, Robert E.; Ho, George C.; Korth, Haje; Krimigis, Stamatios M.; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Baker, Daniel N.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA. [Benna, Mehdi; Boardsen, Scott A.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Gloeckler, George; Raines, Jim M.; Zurbuchen, Thomas H.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Gloeckler, George] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Krimigis, Stamatios M.] Acad Athens, Athens 11527, Greece. [Schriver, David; Travnicek, Pavel] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Travnicek, Pavel] Acad Sci Czech Republic, Inst Astron, Prague 14131, Czech Republic. RP Slavin, JA (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. EM james.a.slavin@nasa.gov RI McNutt, Ralph/E-8006-2010; Anderson, Brian/I-8615-2012; Slavin, James/H-3170-2012; Sarantos, Menelaos/H-8136-2013; 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; FU NASA Discovery Program [NAS5-97271]; Johns Hopkins University Applied Physics Laboratory; Carnegie Institution of Washington [NASW-00002] FX We deeply mourn the loss of our colleague and MESSENGER Co-Investigator Mario Acuna during the preparation of this manuscript; his many contributions to the MESSENGER mission and the space science community live on. We also thank all who contributed to the success of the first and second MESSENGER flybys of Mercury. Data visualization and graphics support by J. Feggans, C. Liebrecht, and M. Marosy are gratefully acknowledged. The MESSENGER project is supported by the NASA Discovery Program under contracts NAS5-97271 to the Johns Hopkins University Applied Physics Laboratory and NASW-00002 to the Carnegie Institution of Washington. NR 26 TC 107 Z9 107 U1 2 U2 13 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD MAY 1 PY 2009 VL 324 IS 5927 BP 606 EP 610 DI 10.1126/science.1172011 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 439DW UT WOS:000265608800034 PM 19407194 ER PT J AU Catling, DC Zahnle, KL AF Catling, David C. Zahnle, Kevin L. TI The Planetary Air Leak SO SCIENTIFIC AMERICAN LA English DT Article C1 [Catling, David C.] NASA, Ames Res Ctr, Washington, DC USA. OI Catling, David/0000-0001-5646-120X NR 3 TC 5 Z9 5 U1 1 U2 1 PU SCI AMERICAN INC PI NEW YORK PA 415 MADISON AVE, NEW YORK, NY 10017 USA SN 0036-8733 J9 SCI AM JI Sci.Am. PD MAY PY 2009 VL 300 IS 5 BP 36 EP 43 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 434LO UT WOS:000265276400031 PM 19438047 ER PT J AU Christian, ER Kaiser, ML Kucera, TA St Cyr, OC van Driel-Gesztelyi, L Mandrini, CH AF Christian, Eric R. Kaiser, Michael L. Kucera, Therese A. St Cyr, O. C. van Driel-Gesztelyi, Lidia Mandrini, Cristina H. TI STEREO SCIENCE RESULTS AT SOLAR MINIMUM - Preface SO SOLAR PHYSICS LA English DT Editorial Material C1 [Christian, Eric R.; Kaiser, Michael L.; Kucera, Therese A.; St Cyr, O. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [van Driel-Gesztelyi, Lidia] Observ Paris, CNRS, UMR 8109, LESIA, F-92195 Meudon, France. [van Driel-Gesztelyi, Lidia] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [van Driel-Gesztelyi, Lidia] Hungarian Acad Sci, Konkoly Observ Budapest, Budapest, Hungary. [Mandrini, Cristina H.] Univ Buenos Aires, CONICET, Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. RP Christian, ER (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Eric.R.Christian@nasa.gov; Therese.A.Kucera@nasa.gov; Chris.StCyr@nasa.gov; Lidia.vanDriel@obspm.fr; mandrini@iafe.uba.ar RI Kucera, Therese/C-9558-2012; Christian, Eric/D-4974-2012 OI Christian, Eric/0000-0003-2134-3937 NR 0 TC 0 Z9 0 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 MAY PY 2009 VL 256 IS 1-2 BP 1 EP 2 DI 10.1007/s11207-009-9365-2 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 438OC UT WOS:000265563900001 ER PT J AU Liewer, PC De Jong, EM Hall, JR Howard, RA Thompson, WT Culhane, JL Bone, L van Driel-Gesztelyi, L AF Liewer, P. C. De Jong, E. M. Hall, J. R. Howard, R. A. Thompson, W. T. Culhane, J. L. Bone, L. van Driel-Gesztelyi, L. TI Stereoscopic Analysis of the 19 May 2007 Erupting Filament SO SOLAR PHYSICS LA English DT Article DE Corona; Prominences; Filaments; Eruptions; Stereoscopy ID MAGNETIC CLOUDS; SOLAR-FLARES; PROMINENCES; DYNAMICS; SECCHI; EUVI AB A filament eruption, accompanied by a B9.5 flare, coronal dimming, and an EUV wave, was observed by the Solar TERrestrial Relations Observatory (STEREO) on 19 May 2007, beginning at about 13:00 UT. Here, we use observations from the SECCHI/EUVI telescopes and other solar observations to analyze the behavior and geometry of the filament before and during the eruption. At this time, STEREO A and B were separated by about 8.5A degrees, sufficient to determine the three-dimensional structure of the filament using stereoscopy. The filament could be followed in SECCHI/EUVI 304 A... stereoscopic data from about 12 hours before to about 2 hours after the eruption, allowing us to determine the 3D trajectory of the erupting filament. From the 3D reconstructions of the filament and the chromospheric ribbons in the early stage of the eruption, simultaneous heating of both the rising filamentary material and the chromosphere directly below is observed, consistent with an eruption resulting from magnetic reconnection below the filament. Comparisons of the filament during eruption in 304 A... and H alpha show that when it becomes emissive in He II, it tends to disappear in H alpha , indicating that the disappearance probably results from heating or motion, not loss, of filamentary material. C1 [Liewer, P. C.; De Jong, E. M.; Hall, J. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Howard, R. A.] USN, Res Lab, Washington, DC 20375 USA. [Thompson, W. T.] Adnet Syst Inc, Lanham, MD 20706 USA. [Culhane, J. L.; Bone, L.; van Driel-Gesztelyi, L.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [van Driel-Gesztelyi, L.] Observ Paris, CNRS, FRE 2461, LESIA, F-92195 Meudon, France. Hungarian Acad Sci, Konkoly Observ Budapest, Budapest, Hungary. RP Liewer, PC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Paulett.Liewer@jpl.nasa.gov RI Thompson, William/D-7376-2012 FU NASA; USAF Space Test Program; Office of Naval Research; European Commission [218816] FX We thank K.E.J. Kilpua, Y.Li, J. Luhmann, B. Lynch, S. Martin, O. Penasco, and A. Vourlidas for very valuable conversation on this solar event. We thank N. Rich, S. Suzuki, and J.-P. Wuesler for their help with the SECCHI/EUVI data. The STEREO/SECCHI data used here are produced by an international consortium of the Naval Research Laboratory (USA), Lockheed-Martin Solar and Astrophysics Lab (USA), NASA Goddard Space Flight Center (USA), Rutherford Appleton Laboratory (UK), University of Birmingham ( UK), Max-Planck-Institut fur Sonnensystemforschung (Germany), Centre Spatiale de Liege (Belgium), Institut d'Optique Theorique et Appliquee (France), Institut d'Astrophysique Spatiale (France). The USA institutions were funded by NASA; the UK institutions by Particle Physics and Astronomy Research Council (PPARC); the German institutions by Deutsches Zentrum fur Luft- und Raumfahrt e. V. (DLR); the Belgian institutions by Belgian Science Policy Office; the French institutions by Centre National d'Etudes Spatiales (CNES) and the Centre National de la Recherche Scientifique (CNRS). The NRL effort was also supported by the USAF Space Test Program and the Office of Naval Research. A portion of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. J.L.C. acknowledges the award of a Leverhulme Emeritus Fellowship. Financial support for LvDG by the European Commission through the SOTERIA Network (EU FP7 Space Science Project No. 218816) is gratefully acknowledged. NR 25 TC 60 Z9 62 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD MAY PY 2009 VL 256 IS 1-2 BP 57 EP 72 DI 10.1007/s11207-009-9363-4 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 438OC UT WOS:000265563900004 ER PT J AU Rouillard, AP Savani, NP Davies, JA Lavraud, B Forsyth, RJ Morley, SK Opitz, A Sheeley, NR Burlaga, LF Sauvaud, JA Simunac, KDC Luhmann, JG Galvin, AB Crothers, SR Davis, CJ Harrison, RA Lockwood, M Eyles, CJ Bewsher, D Brown, DS AF Rouillard, A. P. Savani, N. P. Davies, J. A. Lavraud, B. Forsyth, R. J. Morley, S. K. Opitz, A. Sheeley, N. R. Burlaga, L. F. Sauvaud, J. -A. Simunac, K. D. C. Luhmann, J. G. Galvin, A. B. Crothers, S. R. Davis, C. J. Harrison, R. A. Lockwood, M. Eyles, C. J. Bewsher, D. Brown, D. S. TI A Multispacecraft Analysis of a Small-Scale Transient Entrained by Solar Wind Streams SO SOLAR PHYSICS LA English DT Article DE Sun: magnetic field; Sun: corotating interaction regions; Interplanetary medium: coronal mass ejection ID CORONAL MASS EJECTIONS; MAGNETIC CLOUDS; HOLES; INTERFACES; EXPLORER; SECCHI; CYCLE; EARTH; FIELD AB The images taken by the Heliospheric Imagers (HIs), part of the SECCHI imaging package onboard the pair of STEREO spacecraft, provide information on the radial and latitudinal evolution of the plasma compressed inside corotating interaction regions (CIRs). A plasma density wave imaged by the HI instrument onboard STEREO-B was found to propagate towards STEREO-A, enabling a comparison between simultaneous remote-sensing and in situ observations of its structure to be performed. In situ measurements made by STEREO-A show that the plasma density wave is associated with the passage of a CIR. The magnetic field compressed after the CIR stream interface (SI) is found to have a planar distribution. Minimum variance analysis of the magnetic field vectors shows that the SI is inclined at 54A degrees to the orbital plane of the STEREO-A spacecraft. This inclination of the CIR SI is comparable to the inclination of the associated plasma density wave observed by HI. A small-scale magnetic cloud with a flux rope topology and radial extent of 0.08 AU is also embedded prior to the SI. The pitch-angle distribution of suprathermal electrons measured by the STEREO-A SWEA instrument shows that an open magnetic field topology in the cloud replaced the heliospheric current sheet locally. These observations confirm that HI observes CIRs in difference images when a small-scale transient is caught up in the compression region. C1 [Rouillard, A. P.; Lockwood, M.] Univ Southampton, Sch Phys & Astron, Space Environm Phys Grp, Southampton SO17 1BJ, Hants, England. [Rouillard, A. P.; Davies, J. A.; Crothers, S. R.; Davis, C. J.; Harrison, R. A.; Lockwood, M.; Eyles, C. J.; Bewsher, D.] Rutherford Appleton Lab, Space Sci & Technol Dept, Chilton OX11 0QX, Oxon, England. [Savani, N. P.; Forsyth, R. J.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BW, England. [Lavraud, B.; Opitz, A.; Sauvaud, J. -A.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, Toulouse, France. [Lavraud, B.; Opitz, A.; Sauvaud, J. -A.] CNRS, UMR 5187, Toulouse, France. [Morley, S. K.] Univ Newcastle, Ctr Space Phys, Newcastle, NSW 2308, Australia. [Sheeley, N. R.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Burlaga, L. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Simunac, K. D. C.; Galvin, A. B.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Luhmann, J. G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Eyles, C. J.] Univ Valencia, Grp Astron & Ciencias Espacio, Valencia, Spain. [Bewsher, D.; Brown, D. S.] Aberystwyth Univ, Inst Math & Phys Sci, Aberystwyth SY23 3BZ, Dyfed, Wales. RP Rouillard, AP (reprint author), Univ Southampton, Sch Phys & Astron, Space Environm Phys Grp, Southampton SO17 1BJ, Hants, England. EM alexisrouillard@yahoo.co.uk RI Morley, Steven/A-8321-2008; Lockwood, Mike/G-1030-2011; Galvin, Antoinette/A-6114-2013; Savani, Neel/G-4066-2014; Scott, Christopher/H-8664-2012; OI Bewsher, Danielle/0000-0002-6351-5170; Morley, Steven/0000-0001-8520-0199; Lockwood, Mike/0000-0002-7397-2172; Savani, Neel/0000-0002-1916-7877; Scott, Christopher/0000-0001-6411-5649; Brown, Daniel/0000-0002-1618-8816 FU STFC (UK) FX This work was funded by STFC (UK). The STEREO/SECCHI data are produced by a consortium of RAL (UK), NRL (USA), LMSAL (USA), GSFC (USA), MPS (Germany), CSL (Belgium), IOTA (France) and IAS (France). The PLASTIC and IMPACT data are produced by a consortium of the CESR (France), the University of New Hampshire and the University of California. NR 41 TC 59 Z9 59 U1 0 U2 5 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 MAY PY 2009 VL 256 IS 1-2 BP 307 EP 326 DI 10.1007/s11207-009-9329-6 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 438OC UT WOS:000265563900018 ER PT J AU Opitz, A Karrer, R Wurz, P Galvin, AB Bochsler, P Blush, LM Daoudi, H Ellis, L Farrugia, CJ Giammanco, C Kistler, LM Klecker, B Kucharek, H Lee, MA Mobius, E Popecki, M Sigrist, M Simunac, K Singer, K Thompson, B Wimmer-Schweingruber, RF AF Opitz, A. Karrer, R. Wurz, P. Galvin, A. B. Bochsler, P. Blush, L. M. Daoudi, H. Ellis, L. Farrugia, C. J. Giammanco, C. Kistler, L. M. Klecker, B. Kucharek, H. Lee, M. A. Moebius, E. Popecki, M. Sigrist, M. Simunac, K. Singer, K. Thompson, B. Wimmer-Schweingruber, R. F. TI Temporal Evolution of the Solar Wind Bulk Velocity at Solar Minimum by Correlating the STEREO A and B PLASTIC Measurements SO SOLAR PHYSICS LA English DT Article DE Solar wind; STEREO; Plasma; Multipoint spacecraft observations ID PLASMA CORRELATIONS; SPEED VARIATIONS AB The two STEREO spacecraft with nearly identical instrumentation were launched near solar activity minimum and they separate by about 45A degrees per year, providing a unique tool to study the temporal evolution of the solar wind. We analyze the solar wind bulk velocity measured by the two PLASTIC plasma instruments onboard the two STEREO spacecraft. During the first half year of our measurements (March -aEuro parts per thousand August 2007) we find the typical alternating slow and fast solar wind stream pattern expected at solar minimum. To evaluate the temporal evolution of the solar wind bulk velocity we exclude the spatial variations and calculate the correlation between the solar wind bulk velocity measured by the two spacecraft. We account for the different spacecraft positions in radial distance and longitude by calculating the corresponding time lag. After adjusting for this time lag we compare the solar wind bulk velocity measurements at the two spacecraft and calculate the correlation between the two time-shifted datasets. We show how this correlation decreases as the time difference between two corresponding measurements increases. As a result, the characteristic temporal changes in the solar wind bulk velocity can be inferred. The obtained correlation is 0.95 for a time lag of 0.5 days and 0.85 for 2 days. C1 [Opitz, A.] Univ Toulouse, CNRS, UPS, Ctr Etud Spatiale Rayonnements, Toulouse, France. [Opitz, A.; Karrer, R.; Wurz, P.; Bochsler, P.; Blush, L. M.; Daoudi, H.; Giammanco, C.; Sigrist, M.] Univ Bern, Inst Phys, Dept Space Sci & Planetol, Bern, Switzerland. [Galvin, A. B.; Ellis, L.; Farrugia, C. J.; Kistler, L. M.; Kucharek, H.; Lee, M. A.; Moebius, E.; Popecki, M.; Simunac, K.; Singer, K.] Univ New Hampshire, SSC, Durham, NH 03824 USA. [Klecker, B.] MPI Extraterr Phys, Garching, Germany. [Thompson, B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wimmer-Schweingruber, R. F.] Univ Kiel, Inst Expt & Appl Phys, Kiel, Germany. RP Opitz, A (reprint author), Univ Toulouse, CNRS, UPS, Ctr Etud Spatiale Rayonnements, Toulouse, France. EM opitz@cesr.fr RI Thompson, Barbara/C-9429-2012; Galvin, Antoinette/A-6114-2013; OI Giammanco, Corrado/0000-0001-5405-0095; Moebius, Eberhard/0000-0002-2745-6978 FU Swiss National Fund for the University of Bern; NASA; CNES FX The authors would like to thank Jack T. Gosling and Alexis P. Rouillard for helpful discussions, as well as Christopher T. Russell for his comments. This work was supported by the Swiss National Fund for the University of Bern. It was also supported by the NASA STEREO/PLASTIC Grant for the University of New Hampshire and by a CNES Grant for CESR (CNRS-UPS). The authors acknowledge contributions from the entire STEREO group. NR 12 TC 20 Z9 20 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 MAY PY 2009 VL 256 IS 1-2 BP 365 EP 377 DI 10.1007/s11207-008-9304-7 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 438OC UT WOS:000265563900021 ER PT J AU Mason, GM Desai, MI Mall, U Korth, A Bucik, R von Rosenvinge, TT Simunac, KD AF Mason, G. M. Desai, M. I. Mall, U. Korth, A. Bucik, R. von Rosenvinge, T. T. Simunac, K. D. TI In situ Observations of CIRs on STEREO, Wind, and ACE During 2007-2008 SO SOLAR PHYSICS LA English DT Article DE Acceleration of particles; Sun: abundances; Solar wind; Interplanetary medium; Cosmic rays; Shock waves ID COROTATING INTERACTION REGIONS; ENERGETIC PARTICLES; SOLAR-WIND; ACCELERATION PROCESSES; HEAVY-IONS; HELIOSPHERE; SPACECRAFT; INJECTION; AU; ENHANCEMENTS AB During the 2007 and 2008 solar minimum period, STEREO, Wind, and ACE observed numerous Corotating Interaction Regions (CIRs) over spatial separations that began with all the spacecraft close to Earth, through STEREO separation angles of similar to aEuro parts per thousand 80 degrees in the fall of 2008. Over 35 CIR events were of sufficient intensity to allow measurement of He and heavy ion spectra using the IMPACT/SIT, EPACT/STEP and ACE/ULEIS instruments on STEREO, Wind, and ACE, respectively. In addition to differences between the spacecraft expected on the basis of simple corotation, we observed several events where there were markedly different time-intensity profiles from one spacecraft to the next. By comparing the energetic particle intensities and spectral shapes along with solar wind speed we examine the extent to which these differences are due to temporal evolution of the CIR or due to variations in connection to a relatively stable interaction region. Comparing CIRs in the 1996 -aEuro parts per thousand 1997 solar minimum period vs. 2007 -aEuro parts per thousand 2008, we find that the 2007 -aEuro parts per thousand 2008 period had many more CIRs, reflecting the presence of more high-speed solar wind streams, whereas 1997 had almost no CIR activity. C1 [Mason, G. M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Desai, M. I.] SW Res Inst, San Antonio, TX 78238 USA. [Mall, U.; Korth, A.; Bucik, R.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [von Rosenvinge, T. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Simunac, K. D.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. RP Mason, GM (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM glenn.mason@jhuapl.edu RI Bucik, Radoslav/B-6501-2016 OI Bucik, Radoslav/0000-0001-7381-6949 FU NASA [NNX07AP69G]; University of California Berkeley [SA4889-26309]; Max-Planck-Gesellschaft zur Foerderung der Wissenschaften; Bundesministerium fur Bildung und Forschung (BMBF) [50 OC 0501] FX We thank the Wind/SWE team for solar wind speed data used here and the ACE/MAG team for their list of transients and disturbances maintained on the ACE Science Center web site. Figure 8 was produced using the Solar Weather Browser, sponsored by the Royal Observatory of Belgium and ESA. Sunspot numbers in Figure 10, and SEP event sizes in Figure 11 were obtained from the NOAA ftp site. The work at the Johns Hopkins University/Applied Physics Laboratory was supported by NASA under grant NNX07AP69G and contract SA4889-26309 from the University of California Berkeley. This work was also supported by the Max-Planck-Gesellschaft zur Foerderung der Wissenschaften and the Bundesministerium fur Bildung und Forschung (BMBF) under grant 50 OC 0501. NR 31 TC 31 Z9 31 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 MAY PY 2009 VL 256 IS 1-2 BP 393 EP 408 DI 10.1007/s11207-009-9367-0 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 438OC UT WOS:000265563900023 ER PT J AU von Rosenvinge, TT Richardson, IG Reames, DV Cohen, CMS Cummings, AC Leske, RA Mewaldt, RA Stone, EC Wiedenbeck, ME AF von Rosenvinge, T. T. Richardson, I. G. Reames, D. V. Cohen, C. M. S. Cummings, A. C. Leske, R. A. Mewaldt, R. A. Stone, E. C. Wiedenbeck, M. E. TI The Solar Energetic Particle Event of 14 December 2006 SO SOLAR PHYSICS LA English DT Article DE Solar energetic particles; STEREO; Magnetic cloud ID MAGNETIC CLOUDS; FLARE PARTICLES; ANISOTROPY; TOPOLOGY; SPACE; WIND; FLUX AB The solar energetic particle event on 14 December 2006 was observed by several near-Earth spacecraft including the Advanced Composition Explorer (ACE), STEREO A and B, SOHO and Wind. An interesting feature of this event is a series of unusual fluctuations in the particle intensity that occurred during the first few hours. These fluctuations were observed inside a magnetic cloud that originated in a solar event on 13 December and show both similarities and variations at the different spacecraft. Interestingly, the most striking difference is between observations at the two closely-separated STEREO spacecraft. In particular, large fluctuations in the proton intensity were seen by the High Energy Telescope (HET) on STEREO A, and to a lesser extent at Wind and ACE, but not by the STEREO B HET. We conclude that the differences in intensity-time profiles were caused by anisotropies in the particle distribution and the different viewing directions of the individual particle telescopes. The intensity/anisotropy variations suggest that flux tubes with different particle propagation conditions existed within this magnetic cloud despite the absence of local magnetic field signatures associated with these regions. The intensity fluctuations are similar to those occasionally seen in impulsive particle events. There were also spacecraft-to-spacecraft differences during the onset of the particle event. An initial rapid onset of energetic (> 40 MeV) protons was observed by the STEREO A and B spacecraft outside the magnetic cloud, but not by spacecraft such as SOHO that were already inside the magnetic cloud at this time. The latter spacecraft observed a slower, lower intensity increase. Evidently, energetic proton propagation from the solar event to the vicinity of Earth was inhibited within the magnetic cloud compared to outside. C1 [von Rosenvinge, T. T.; Richardson, I. G.; Reames, D. V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cohen, C. M. S.; Cummings, A. C.; Leske, R. A.; Mewaldt, R. A.; Stone, E. C.] CALTECH, Pasadena, CA 91125 USA. [Wiedenbeck, M. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Richardson, I. G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Richardson, I. G.] Univ Maryland, CRESST, College Pk, MD 20742 USA. RP von Rosenvinge, TT (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. EM tycho.t.vonrosenvinge@nasa.gov; ian.g.richardson@nasa.gov; Donald.V.Reames@nasa.gov; cohen@srl.caltech.edu; ace@srl.caltech.edu; ral@srl.caltech.edu; rmewaldt@srl.caltech.edu; ecs@srl.caltech.edu; mark.e.wiedenbeck@jpl.nasa.gov OI Richardson, Ian/0000-0002-3855-3634 FU NASA [SA2715-26309, NAS5-03131]; University of California, Berkeley FX We thank Janet Luhmann of the University of California, Berkeley, for her steadfast support as the Principal Investigator of the STEREO/IMPACT investigation. The work at GSFC, Caltech and JPL was supported by NASA (Caltech and JPL were funded under subcontract SA2715-26309 from the University of California, Berkeley, under NASA Contract NAS5-03131). The ACE observations used in this paper are from the ACE Science Center (http://www.srl.caltech.edu/ACE/ASC/), and the STEREO magnetic fields were obtained from the STEREO archive at UCLA (http://www-ssc.igpp.ucla.edu/forms/stereo/). The SOHO/ERNE data were obtained from the Space Research Laboratory, University of Turku (http://www.srl.utu.fi/erne_data/). NR 21 TC 17 Z9 17 U1 1 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD MAY PY 2009 VL 256 IS 1-2 BP 443 EP 462 DI 10.1007/s11207-009-9353-6 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 438OC UT WOS:000265563900026 ER PT J AU Meyer-Vernet, N Maksimovic, M Czechowski, A Mann, I Zouganelis, I Goetz, K Kaiser, ML St Cyr, OC Bougeret, JL Bale, SD AF Meyer-Vernet, N. Maksimovic, M. Czechowski, A. Mann, I. Zouganelis, I. Goetz, K. Kaiser, M. L. St Cyr, O. C. Bougeret, J. -L. Bale, S. D. TI Dust Detection by the Wave Instrument on STEREO: Nanoparticles Picked up by the Solar Wind? SO SOLAR PHYSICS LA English DT Article DE Plasma physics; Solar wind; Waves, plasma ID ION FORMATION; IMPACT; SPACECRAFT; PARTICLES; STREAMS; GRAINS; ORIGIN; SATURN; SYSTEM; RADIO AB The STEREO wave instrument (S/WAVES) has detected a very large number of intense voltage pulses. We suggest that these events are produced by impact ionisation of nanoparticles striking the spacecraft at a velocity of the order of magnitude of the solar wind speed. Nanoparticles, which are half-way between micron-sized dust and atomic ions, have such a large charge-to-mass ratio that the electric field induced by the solar wind magnetic field accelerates them very efficiently. Since the voltage produced by dust impacts increases very fast with speed, such nanoparticles produce signals as high as do much larger grains of smaller speeds. The flux of 10-nm radius grains inferred in this way is compatible with the interplanetary dust flux model. The present results may represent the first detection of fast nanoparticles in interplanetary space near Earth orbit. C1 [Meyer-Vernet, N.; Maksimovic, M.; Zouganelis, I.; Bougeret, J. -L.] Univ Paris Diderot, Observ Paris, CNRS, UPMC,LESIA, F-92190 Meudon, France. [Zouganelis, I.] UPMC, CNRS, LPP, Ecole Polytech, F-94107 St Maur Des Fosses, France. [Czechowski, A.] Polish Acad Sci, Space Res Ctr, PL-00716 Warsaw, Poland. [Mann, I.] Kindai Univ, Sch Sci & Engn, Osaka 5778502, Japan. [Goetz, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Kaiser, M. L.; St Cyr, O. C.] NASA, GSFC, Greenbelt, MD 20771 USA. [Bale, S. D.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Meyer-Vernet, N (reprint author), Univ Paris Diderot, Observ Paris, CNRS, UPMC,LESIA, 5 Pl Jules Janssen, F-92190 Meudon, France. EM nicole.meyer@obspm.fr; ace@cbk.waw.pl; mann@kindai.ac.jp; yannis.zouganelis@lpp.polytechnique.fr; goetz@waves.space.umn.edu; michael.kaiser@nasa.gov; bale@ssl.berkeley.edu RI Bale, Stuart/E-7533-2011 OI Bale, Stuart/0000-0002-1989-3596 FU CNES; CNRS; Polish Ministry of Science [4 T12E 002 30] FX We thank the team who conceived, designed, built, and tested the S/WAVES instrument, and are very grateful to P.-L. Astier for simulations of the response to transient pulses. The French part was supported by CNES and CNRS. A. C. was supported by the Polish Ministry of Science grant 4 T12E 002 30. We thank the International Space Science Institute for fostering discussions within the working group 'Dust-plasma interactions: observations in the interplanetary medium and in the environment of solar system objects'. We are grateful to an anonymous referee for helpful comments. NR 33 TC 66 Z9 66 U1 0 U2 7 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD MAY PY 2009 VL 256 IS 1-2 BP 463 EP 474 DI 10.1007/s11207-009-9349-2 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 438OC UT WOS:000265563900027 ER PT J AU St Cyr, OC Kaiser, ML Meyer-Vernet, N Howard, RA Harrison, RA Bale, SD Thompson, WT Goetz, K Maksimovic, M Bougeret, JL Wang, D Crothers, S AF St Cyr, O. C. Kaiser, M. L. Meyer-Vernet, N. Howard, R. A. Harrison, R. A. Bale, S. D. Thompson, W. T. Goetz, K. Maksimovic, M. Bougeret, J. -L. Wang, D. Crothers, S. TI STEREO SECCHI and S/WAVES Observations of Spacecraft Debris Caused by Micron-Size Interplanetary Dust Impacts SO SOLAR PHYSICS LA English DT Article ID MISSION; LASCO AB Early in the STEREO mission observers noted that the white-light instruments of the SECCHI suite were detecting significantly more spacecraft-related "debris" than any previously flown coronagraphic instruments. Comparison of SECCHI "debris storms" with S/WAVES indicates that almost all are coincident with the most intense transient emissions observed by the radio and plasma waves instrument. We believe the debris is endogenous (i.e., from the spacecraft thermal blanketing), and the storms appear to be caused by impacts of large interplanetary dust grains that are detected by S/WAVES. Here we report the observations, compare them to interplanetary dust distributions, and document a reminder for future spacebased coronagraphic instrument builders. C1 [St Cyr, O. C.; Kaiser, M. L.; Thompson, W. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Meyer-Vernet, N.; Maksimovic, M.; Bougeret, J. -L.] Univ Paris Diderot, Observ Paris, UPMC, LESIA,CNRS, F-92190 Meudon, France. [Howard, R. A.; Wang, D.] Naval Res Lab, Washington, DC USA. [Harrison, R. A.; Crothers, S.] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Bale, S. D.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Thompson, W. T.] Adnet Syst Inc, Rockville, MD USA. [Goetz, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Wang, D.] Interferometrics, Herndon, VA USA. [Bale, S. D.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP St Cyr, OC (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. EM chris.stcyr@nasa.gov RI Bale, Stuart/E-7533-2011; Thompson, William/D-7376-2012 OI Bale, Stuart/0000-0002-1989-3596; FU NASA; Particle Physics and Astronomy Research Council; Deutsches Zentrum fur Luft- und Raumfahrt e.V.; Belgian Science Policy Office; Centre National d'Etudes Spatiales; Centre National de la Recherche Scientifique; USAF Space Test Program; Office of Naval Research; CNRS FX The SECCHI data used here are produced by an international consortium of the Naval Research Laboratory, Lockheed Martin Solar and Astrophysics Laboratory, and NASA Goddard Space Flight Center (USA), Rutherford Appleton Laboratory and University of Birmingham (UK), Max-Planck-Institut fur Sonnensystemforschung (Germany), Centre Spatiale de Liege (Belgium), Institut d'Optique Theorique et Appliquee, and Institut d'Astrophysique Spatiale (France). The USA institutions were funded by NASA; the UK institutions by Particle Physics and Astronomy Research Council; the German institutions by Deutsches Zentrum fur Luft- und Raumfahrt e. V.; the Belgian institutions by Belgian Science Policy Office; the French institutions by Centre National d'Etudes Spatiales and the Centre National de la Recherche Scientifique. The NRL effort was also supported by the USAF Space Test Program and the Office of Naval Research. The S/WAVES data used here are produced by an international consortium of the Observatoire de Paris (France), the University of Minnesota (USA), the University of California Berkeley (USA), and NASA Goddard Space Flight Center (USA). The French contribution was funded by CNRS, and the USA institutions were funded by NASA. We also gratefully acknowledge contributions from K. Baldwin (NRL), J.-P. Olive (ESA), A. Dreisman (JHU/APL), and C. Edgerton (Edge Space Systems). NR 18 TC 12 Z9 12 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD MAY PY 2009 VL 256 IS 1-2 BP 475 EP 488 DI 10.1007/s11207-009-9362-5 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 438OC UT WOS:000265563900028 ER PT J AU De Keyser, J Carpenter, DL Darrouzet, F Gallagher, DL Tu, JN AF De Keyser, Johan Carpenter, Donald L. Darrouzet, Fabien Gallagher, Dennis L. Tu, Jiannan TI CLUSTER and IMAGE: New Ways to Study the Earth's Plasmasphere SO SPACE SCIENCE REVIEWS LA English DT Review DE Plasmasphere; CLUSTER; IMAGE; Measurement techniques ID ELECTROMAGNETIC-WAVE FIELD; ELECTRON-DENSITY PROFILES; NONTHERMAL CONTINUUM; MAGNETIC-FIELD; INNER MAGNETOSPHERE; 6-COMPONENT MEASUREMENTS; POTENTIAL MEASUREMENTS; MAGNETOPAUSE CURRENT; GRADIENT CALCULATION; PLASMAPAUSE REGION AB Ground-based instruments and a number of space missions have contributed to our knowledge of the plasmasphere since its discovery half a century ago, but it is fair to say that many questions have remained unanswered. Recently, NASA's Image and ESA's Cluster probes have introduced new observational concepts, thereby providing a non-local view of the plasmasphere. Image carried an extreme ultraviolet imager producing global pictures of the plasmasphere. Its instrumentation also included a radio sounder for remotely sensing the spacecraft environment. The Cluster mission provides observations at four nearby points as the four-spacecraft configuration crosses the outer plasmasphere on every perigee pass, thereby giving an idea of field and plasma gradients and of electric current density. This paper starts with a historical overview of classical single-spacecraft data interpretation, discusses the non-local nature of the Image and Cluster measurements, and emphasizes the importance of the new data interpretation tools that have been developed to extract non-local information from these observations. The paper reviews these innovative techniques and highlights some of them to give an idea of the flavor of these methods. In doing so, it is shown how the non-local perspective opens new avenues for plasmaspheric research. C1 [De Keyser, Johan; Darrouzet, Fabien] Belgian Inst Space Aeron, B-1180 Brussels, Belgium. [Carpenter, Donald L.] Stanford Univ, Space Telecommun & Radiosci Lab, Stanford, CA 94305 USA. [Gallagher, Dennis L.] NASA, George C Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Huntsville, AL 35812 USA. [Tu, Jiannan] Univ Massachusetts, Ctr Atmospher Res, Lowell, MA USA. RP De Keyser, J (reprint author), Belgian Inst Space Aeron, Ringlaan 3, B-1180 Brussels, Belgium. EM Johan.DeKeyser@aeronomie.be; dlc@nova.stanford.edu; Fabien.Darrouzet@aeronomie.be; dennis.l.gallagher@nasa.gov; Jiannan_Tu@uml.edu NR 192 TC 2 Z9 2 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD MAY PY 2009 VL 145 IS 1-2 BP 7 EP 53 DI 10.1007/s11214-008-9464-7 PG 47 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 457FT UT WOS:000266914600003 ER PT J AU Darrouzet, F Gallagher, DL Andre, N Carpenter, DL Dandouras, I Decreau, PME De Keyser, J Denton, RE Foster, JC Goldstein, J Moldwin, MB Reinisch, BW Sandel, BR Tu, JN AF Darrouzet, Fabien Gallagher, Dennis L. Andre, Nicolas Carpenter, Donald L. Dandouras, Iannis Decreau, Pierrette M. E. De Keyser, Johan Denton, Richard E. Foster, John C. Goldstein, Jerry Moldwin, Mark B. Reinisch, Bodo W. Sandel, Bill R. Tu, Jiannan TI Plasmaspheric Density Structures and Dynamics: Properties Observed by the CLUSTER and IMAGE Missions SO SPACE SCIENCE REVIEWS LA English DT Review DE Plasmasphere; CLUSTER; IMAGE; Plasma Structures ID EXTREME-ULTRAVIOLET IMAGER; RADIO PLASMA IMAGER; FIELD-ALIGNED IRREGULARITIES; ELECTRON-DENSITY; OUTER PLASMASPHERE; WHISTLER EVIDENCE; PROPAGATION CHARACTERISTICS; EARTHS MAGNETOSPHERE; MAGNETIC STORMS; TOPSIDE-SOUNDER AB Plasmaspheric density structures have been studied since the discovery of the plasmasphere in the late 1950s. But the advent of the Cluster and Image missions in 2000 has added substantially to our knowledge of density structures, thanks to the new capabilities of those missions: global imaging with Image and four-point in situ measurements with Cluster. The study of plasma sources and losses has given new results on refilling rates and erosion processes. Two-dimensional density images of the plasmasphere have been obtained. The spatial gradient of plasmaspheric density has been computed. The ratios between H+, He+ and O+ have been deduced from different ion measurements. Plasmaspheric plumes have been studied in detail with new tools, which provide information on their morphology, dynamics and occurrence. Density structures at smaller scales have been revealed with those missions, structures that could not be clearly distinguished before the global images from Image and the four-point measurements by Cluster became available. New terms have been given to these structures, like "shoulders", "channels", "fingers" and "crenulations". This paper reviews the most relevant new results about the plasmaspheric plasma obtained since the start of the Cluster and Image missions. C1 [Darrouzet, Fabien; De Keyser, Johan] Belgian Inst Space Aeron IASB BIRA, B-1180 Brussels, Belgium. [Gallagher, Dennis L.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Andre, Nicolas] ESA, RSSD, Noordwijk, Netherlands. [Carpenter, Donald L.] Stanford Univ, Space Telecommun & Radiosci Lab, Stanford, CA 94305 USA. [Dandouras, Iannis] Univ Toulouse, CNRS, CESR, Toulouse, France. [Decreau, Pierrette M. E.] Univ Orleans, CNRS, LPCE, Orleans, France. [Denton, Richard E.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Foster, John C.] MIT, Haystack Observ, Westford, MA 01886 USA. [Goldstein, Jerry] SW Res Inst, San Antonio, TX USA. [Moldwin, Mark B.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [Reinisch, Bodo W.; Tu, Jiannan] UML, Ctr Atmospher Res, Lowell, MA USA. [Sandel, Bill R.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. RP Darrouzet, F (reprint author), Belgian Inst Space Aeron IASB BIRA, 3 Ave Circulaire, B-1180 Brussels, Belgium. EM Fabien.Darrouzet@oma.be; dennis.l.gallagher@nasa.gov; nandre@rssd.esa.int; dlc@nova.stanford.edu; Iannis.Dandouras@cesr.fr; Pierrette.Decreau@cnrs-orleans.fr; Johan.DeKeyser@oma.be; richard.e.denton@dartmouth.edu; jfoster@haystack.mit.edu; jgoldstein@swri.edu; mmoldwin@igpp.ucla.edu; Bodo_Reinisch@uml.edu; sandel@arizona.edu; Jiannan_Tu@uml.edu RI Moldwin, Mark/F-8785-2011; OI Moldwin, Mark/0000-0003-0954-1770; Dandouras, Iannis/0000-0002-7121-1118; Darrouzet, Fabien/0000-0002-2927-6858 NR 155 TC 58 Z9 58 U1 2 U2 11 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 MAY PY 2009 VL 145 IS 1-2 BP 55 EP 106 DI 10.1007/s11214-008-9438-9 PG 52 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 457FT UT WOS:000266914600004 ER PT J AU Matsui, H Foster, JC Carpenter, DL Dandouras, I Darrouzet, F De Keyser, J Gallagher, DL Goldstein, J Puhl-Quinn, PA Vallat, C AF Matsui, Hiroshi Foster, John C. Carpenter, Donald L. Dandouras, Iannis Darrouzet, Fabien De Keyser, Johan Gallagher, Dennis L. Goldstein, Jerry Puhl-Quinn, Pamela A. Vallat, Claire TI Electric Fields and Magnetic Fields in the Plasmasphere: A Perspective From CLUSTER and IMAGE SO SPACE SCIENCE REVIEWS LA English DT Review DE Plasmasphere; Electric Field; Magnetic Field; CLUSTER; IMAGE ID SUBAURORAL ION DRIFTS; EDI CONVECTION MEASUREMENTS; WHISTLER MODE SIGNALS; MAGNETOSPHERIC CONVECTION; IONOSPHERIC CONVECTION; INNER MAGNETOSPHERE; RING CURRENT; SOLAR-WIND; POLARIZATION STREAM; OUTER PLASMASPHERE AB The electric field and magnetic field are basic quantities in the plasmasphere measured since the 1960s. In this review, we first recall conventional wisdom and remaining problems from ground-based whistler measurements. Then we show scientific results from Cluster and Image, which are specifically made possible by newly introduced features on these spacecraft, as follows. 1. In situ electric field measurements using artificial electron beams are successfully used to identify electric fields originating from various sources. 2. Global electric fields are derived from sequences of plasmaspheric images, revealing how the inner magnetospheric electric field responds to the southward interplanetary magnetic fields and storms/substorms. 3. Understanding of sub-auroral polarization stream (SAPS) or sub-auroral ion drifts (SAID) are advanced through analysis of a combination of magnetospheric and ionospheric measurements from Cluster, Image, and DMSP. 4. Data from multiple spacecraft have been used to estimate magnetic gradients for the first time. C1 [Matsui, Hiroshi; Puhl-Quinn, Pamela A.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Foster, John C.] MIT, Westford, MA USA. [Carpenter, Donald L.] Stanford Univ, Space Telecommun & Radiosci Lab, Stanford, CA 94305 USA. [Dandouras, Iannis] CESR, Toulouse, France. [Darrouzet, Fabien; De Keyser, Johan] Belgian Inst Space Aeron BIRA IASB, Brussels, Belgium. [Gallagher, Dennis L.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Goldstein, Jerry] SW Res Inst, San Antonio, TX USA. [Vallat, Claire] ESA, Villafranca, Spain. RP Matsui, H (reprint author), Univ New Hampshire, Ctr Space Sci, Morse Hall,39 Coll Rd, Durham, NH 03824 USA. EM hiroshi.matsui@unh.edu; jfoster@haystack.mit.edu; dlc@nova.stanford.edu; Iannis.Dandouras@cesr.fr; Fabien.Darrouzet@oma.be; Johan.DeKeyser@oma.be; dennis.l.gallagher@nasa.gov; jgoldstein@swri.edu; pamela.puhlquinn@unh.edu; Claire.Vallat@sciops.esa.int OI Dandouras, Iannis/0000-0002-7121-1118 FU NASA [NNG05GG50G, NNX07AI03G]; Belgian Federal Science Policy Office (BELSPO) [13127/98/NL/VJ] FX H. Matsui and P. A. Puhl- Quinn acknowledge the support by NASA through grants NNG05GG50G and NNX07AI03G. J. De Keyser and F. Darrouzet acknowledge the support by the Belgian Federal Science Policy Office (BELSPO) through the ESA/PRODEX CLUSTER project (contract 13127/98/NL/VJ (IC)). This paper is an outcome of the workshop " The Earth's plasmasphere: A CLUSTER, IMAGE, and modeling perspective", organized by the Belgian Institute for Space Aeronomy in Brussels in September 2007. NR 110 TC 2 Z9 2 U1 0 U2 2 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 MAY PY 2009 VL 145 IS 1-2 BP 107 EP 135 DI 10.1007/s11214-008-9471-8 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 457FT UT WOS:000266914600005 ER PT J AU Masson, A Santolik, O Carpenter, DL Darrouzet, F Decreau, PME Mazouz, FE Green, JL Grimald, S Moldwin, MB Nemec, F Sonwalkar, VS AF Masson, Arnaud Santolik, Ondrej Carpenter, Donald L. Darrouzet, Fabien Decreau, Pierrette M. E. Mazouz, Farida El-Lemdani Green, James L. Grimald, Sandrine Moldwin, Mark B. Nemec, Frantisek Sonwalkar, Vikas S. TI Advances in Plasmaspheric Wave Research with CLUSTER and IMAGE Observations SO SPACE SCIENCE REVIEWS LA English DT Review DE Plasmasphere; CLUSTER; IMAGE; Waves ID FIELD LINE RESONANCES; RADIO PLASMA IMAGER; STORM-TIME CHORUS; NONTHERMAL CONTINUUM RADIATION; PROTON CYCLOTRON ECHOES; WHISTLER-MODE CHORUS; EQUATORIAL NOISE; ELECTRON-DENSITY; LOW-LATITUDE; VLF HISS AB This paper highlights significant advances in plasmaspheric wave research with Cluster and Image observations. This leap forward was made possible thanks to the new observational capabilities of these space missions. On one hand, the multipoint view of the four Cluster satellites, a unique capability, has enabled the estimation of wave characteristics impossible to derive from single spacecraft measurements. On the other hand, the Image experiments have enabled to relate large-scale plasmaspheric density structures with wave observations and provide radio soundings of the plasmasphere with unprecedented details. After a brief introduction on Cluster and Image wave instrumentation, a series of sections, each dedicated to a specific type of plasmaspheric wave, put into context the recent advances obtained by these two revolutionary missions. C1 [Masson, Arnaud] ESA ESTEC, Sci Operat Dept, NL-2201 AZ Noordwijk, Netherlands. [Santolik, Ondrej; Nemec, Frantisek] Charles Univ Prague, Fac Math & Phys, Inst Atmospher Phys, Prague, Czech Republic. [Carpenter, Donald L.] Stanford Univ, Space Telecommun & Radiosci Lab, Stanford, CA 94305 USA. [Darrouzet, Fabien] Belgian Inst Space Aeron BIRA IASB, Brussels, Belgium. [Decreau, Pierrette M. E.; Mazouz, Farida El-Lemdani] Univ Orleans, CNRS, LPC2E, Orleans, France. [Green, James L.] NASA Headquarters, Washington, DC USA. [Grimald, Sandrine] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Moldwin, Mark B.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [Sonwalkar, Vikas S.] Univ Alaska Fairbanks, Dept Elect & Comp Engn, Fairbanks, AK USA. RP Masson, A (reprint author), ESA ESTEC, Sci Operat Dept, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. EM Arnaud.Masson@esa.int; ondrej.santolik@mff.cuni.cz; dlc@nova.stanford.edu; Fabien.Darrouzet@oma.be; Pierrette.Decreau@cnrs-orleans.fr; mazouz@cnrs-orleans.fr; James.L.Green@nasa.gov; sg2@mssl.ucl.ac.uk; mmoldwin@igpp.ucla.edu; frantisek.nemec@mff.cuni.cz; ffvss@uaf.edu RI Moldwin, Mark/F-8785-2011; Nemec, Frantisek/H-7027-2013; Santolik, Ondrej/F-7766-2014 OI Moldwin, Mark/0000-0003-0954-1770; Nemec, Frantisek/0000-0002-3233-2718; NR 154 TC 7 Z9 7 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 MAY PY 2009 VL 145 IS 1-2 BP 137 EP 191 DI 10.1007/s11214-009-9508-7 PG 55 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 457FT UT WOS:000266914600006 ER PT J AU Reinisch, BW Moldwin, MB Denton, RE Gallagher, DL Matsui, H Pierrard, V Tu, JN AF Reinisch, Bodo W. Moldwin, Mark B. Denton, Richard E. Gallagher, Dennis L. Matsui, Hiroshi Pierrard, Viviane Tu, Jiannan TI Augmented Empirical Models of Plasmaspheric Density and Electric Field Using IMAGE and CLUSTER Data SO SPACE SCIENCE REVIEWS LA English DT Review DE Inner magnetosphere; Plasmasphere; Empirical models; Plasma density; Electric field; CLUSTER; IMAGE ID INTERPLANETARY MAGNETIC-FIELD; HIGH-LATITUDE IONOSPHERE; PLASMA-MASS DENSITY; MAGNETOSPHERIC CONVECTION; INNER MAGNETOSPHERE; RING CURRENT; ULF WAVES; EARTHS MAGNETOSPHERE; TEMPORAL VARIATIONS; TOPSIDE IONOSPHERE AB Empirical models for the plasma densities in the inner magnetosphere, including plasmasphere and polar magnetosphere, have been in the past derived from in situ measurements. Such empirical models, however, are still in their initial phase compared to magnetospheric magnetic field models. Recent studies using data from CRRES, Polar, and Image have significantly improved empirical models for inner-magnetospheric plasma and mass densities. Comprehensive electric field models in the magnetosphere have been developed using radar and in situ observations at low altitude orbits. To use these models at high altitudes one needs to rely strongly on the assumption of equipotential magnetic field lines. Direct measurements of the electric field by the Cluster mission have been used to derive an equatorial electric field model in which reliance on the equipotential assumption is less. In this paper we review the recent progress in developing empirical models of plasma densities and electric fields in the inner magnetosphere with emphasis on the achievements from the Image and Cluster missions. Recent results from other satellites are also discussed when they are relevant. C1 [Reinisch, Bodo W.; Tu, Jiannan] Univ Massachusetts, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA. [Moldwin, Mark B.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [Denton, Richard E.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Gallagher, Dennis L.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Matsui, Hiroshi] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Pierrard, Viviane] Belgian Inst Space Aeron BIRA IASB, Brussels, Belgium. RP Reinisch, BW (reprint author), Univ Massachusetts, Dept Environm Earth & Atmospher Sci, 600 Suffolk St, Lowell, MA 01854 USA. EM bodo_reinisch@uml.edu; mmoldwin@igpp.ucla.edu; richard.e.denton@dartmouth.edu; dennis.l.gallagher@nasa.gov; hiroshi.matsui@unh.edu; viviane.pierrard@oma.be; jiannan_tu@uml.edu RI Moldwin, Mark/F-8785-2011; OI Moldwin, Mark/0000-0003-0954-1770; Pierrard, Viviane/0000-0001-5014-7682 FU NASA [NNX07AG38G]; SwRI [83822]; NSF [0518227, ATM-0632740, ATM-0120950]; AFRL [FA8718-06-C-0072] FX The work at UML was supported by NASA grant NNX07AG38G, NASA grant via subcontract 83822 from SwRI, NSF grant 0518227, and AFRL contract FA8718-06-C-0072 to the University of Massachusetts Lowell. The work at Dartmouth College was supported by NSF grants ATM-0632740 and ATM-0120950 (Center for Integrated Space Weather Modeling, CISM, funded by the Science and Technology Centers Program). This paper is an outcome of the workshop " The Earth's plasmasphere: A CLUSTER, IMAGE, and modeling perspective", organized by the Belgian Institute for Space Aeronomy in Brussels in September 2007. The use of Figs. 2, 3, 5 and 6 is with the permission of Elsevier. NR 135 TC 22 Z9 23 U1 0 U2 4 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 MAY PY 2009 VL 145 IS 1-2 BP 231 EP 261 DI 10.1007/s11214-008-9481-6 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 457FT UT WOS:000266914600008 ER PT J AU Hasan, AR Kabir, CS Wang, X AF Hasan, A. R. Kabir, C. S. Wang, X. TI A Robust Steady-State Model for Flowing-Fluid Temperature in Complex Wells SO SPE PRODUCTION & OPERATIONS LA English DT Article ID 2-PHASE FLOW; WELLBORE/RESERVOIR SIMULATOR; HEAT-TRANSFER AB This paper presents an analytic model for computing the wellbore-fluid-temperature profile for steady fluid flow. Although wells with a constant-deviation angle can be handled with existing analytic models, complex well architectures demand rigorous treatment. For example, changing geothermal-temperature-gradient and deepwater wells present significant challenges. Additionally, available analytic models rarely provide calculation methods for various required thermal parameters, such as the Joule-Thompson (J-T) coefficient and fluid expansivity. The approach taken in this study entails dividing the wellbore into many sections of uniform thermal properties and deviation angle. The governing differential equation is solved for each section. with fluid temperature from the prior section as the boundary condition. This piecewise approach makes the model versatile, allowing step-by-step calculation of fluid temperature for the entire wellbore. We present simple, thermodynamically sound approaches for estimating thermal parameters. Success is indicated when performance of the proposed model is compared with data from three wells, producing two-phase gas/oil mixture, single-phase oil, and single-phase gas. Sensitivity of the estimated fluid temperatures to various thermal properties is also examined with our model. Overall, the effects of the J-T coefficient and liquid expansivity are found to be significant. C1 [Hasan, A. R.] Univ Minnesota, Duluth, MN 55812 USA. [Hasan, A. R.] NASA, Washington, DC USA. [Kabir, C. S.] Hess, Houston, TX USA. RP Hasan, AR (reprint author), Univ Minnesota, Duluth, MN 55812 USA. EM rhasan@d.umn.edu; skabir@hess.com; shawn.wang@bakerhughes.com OI Kabir, Shah/0000-0002-1421-5761 NR 20 TC 18 Z9 21 U1 0 U2 5 PU SOC PETROLEUM ENG PI RICHARDSON PA 222 PALISADES CREEK DR,, RICHARDSON, TX 75080 USA SN 1930-1855 J9 SPE PROD OPER JI SPE Prod. Oper. PD MAY PY 2009 VL 24 IS 2 BP 269 EP 276 PG 8 WC Engineering, Petroleum SC Engineering GA 447IN UT WOS:000266184900005 ER PT J AU Molod, A AF Molod, Andrea TI Running GCM physics and dynamics on different grids: algorithm and tests SO TELLUS SERIES A-DYNAMIC METEOROLOGY AND OCEANOGRAPHY LA English DT Article ID GENERAL-CIRCULATION MODEL; VERTICAL RESOLUTION; OCEAN; REPRESENTATION; CONVECTION; SCALE AB An 'alternate grid' (GridAlt) technique is presented, which allows the different components of a general circulation model's governing equations to be computed on distinct grids chosen for that component or process. In the implementation presented here, the tendencies of state variables from the physical parametrizations are computed on a vertical grid with very fine resolution near the surface, whereas the remaining terms in the equations of motion are computed using an Eta coordinate with coarser vertical resolution. Results from a suite of aquaplanet experiments show that much of the benefit of increased vertical resolution in the whole model can be realized by enhancing the vertical resolution of the 'physics grid' using GridAlt. The benefit is realized in the fields which are computed directly in the physical parametrizations, and in the vertical structure of the relative humidity and mass streamfunction. Results from a suite of realistically configured simulations demonstrated an impact of GridAlt that was similar to its impact in the simplified simulations, as well as an improved response to El Nino Southern Oscillation forcing. It is concluded that the present implementation of GridAlt offers a practical way to allow GCMs to better capture the near-surface structure of the atmosphere. C1 [Molod, Andrea] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Molod, Andrea] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. RP Molod, A (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. EM Andrea.Molod@nasa.gov FU Climate Modeling Initiative (CMI); Alliance for Computational Earth Sciences (ACES) FX The author wishes to thank Jean-Michel Campin for all the helpful consultations during the development of this work. In addition, the author thanks Chris Hill and Joe Tribbia for their insights and comments about the work and the manuscript. This work was supported under the Climate Modeling Initiative (CMI), and the computations were funded under the Alliance for Computational Earth Sciences (ACES). NR 22 TC 2 Z9 2 U1 0 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0280-6495 J9 TELLUS A JI Tellus Ser. A-Dyn. Meteorol. Oceanol. PD MAY PY 2009 VL 61 IS 3 BP 381 EP 393 DI 10.1111/j.1600-0870.2009.00394.x PG 13 WC Meteorology & Atmospheric Sciences; Oceanography SC Meteorology & Atmospheric Sciences; Oceanography GA 427ZZ UT WOS:000264818900005 ER PT J AU Johnson, DR Perry, HM Lyczkowski-Shultz, J Hanisko, D AF Johnson, Donald R. Perry, Harriet M. Lyczkowski-Shultz, Joanne Hanisko, David TI Red Snapper Larval Transport in the Northern Gulf of Mexico SO TRANSACTIONS OF THE AMERICAN FISHERIES SOCIETY LA English DT Article ID WEST FLORIDA SHELF; LUTJANUS-CAMPECHANUS; CONTINENTAL-SHELF; MITOCHONDRIAL-DNA; CIRCULATION; MOVEMENT; HABITAT; PLUME AB This study examines the advection of red snapper Lutjanus campechanus larvae in the northern Gulf of Mexico. The potential for repopulating the eastern Gulf stock through larval transport from the more populous western stock is addressed. Transport pathways across topographic features that inhibit alongshelf flow (e.g., the Mississippi River delta. DeSoto Canyon, and the Apalachicola peninsula) and interregional larval transport are considered. An advective field of currents is developed front a large database of drifter and moored Currents. augmented by an operational model to fill gaps. The starting points for larval transport are the locations and day of the year of larval captures from the Southeast Area Monitoring and Assessment program ichthyoplankton surveys. Because the Field Of Currents is derived front near-surface observations and the depth distribution of larvae is uncertain. findings are expressed in terms of maximal transport pathways. Transport pathways were principally vectored toward the west during September. October, and May under the influence of relatively strong climatological westward wind stress. Eastward pathways Occurred in June. July. and August under the influence of weaker shoreward wind stress. Westward transport pathways past the Mississippi delta were found near the delta. whereas eastward transport pathways were found in deeper waters beyond the continental shelf break, away front typical juvenile settlement habitat. Water movement front east to west across the Apalachicola peninsula occurred in the fall. suggesting the potential for genetic exchange front the eastern to the western Gulf. Eastward water movement across the Apalachicola peninsula occurred in July. but only along the outer shelf. C1 [Johnson, Donald R.; Perry, Harriet M.] Univ So Mississippi, Gulf Coast Res Lab, Ocean Springs, MS 39564 USA. [Lyczkowski-Shultz, Joanne; Hanisko, David] Natl Marine Fisheries Serv, SE Fisheries Sci Ctr, Pascagoula, MS 39567 USA. RP Johnson, DR (reprint author), Univ So Mississippi, Gulf Coast Res Lab, 703 E Beach Dr, Ocean Springs, MS 39564 USA. EM donald.r.johnson@usm.edu FU National Marine Fisheries Service's Southeastern Regional Office FX We gratefully acknowledge funding for this study from the Marine Fisheries Initiative program of the National Marine Fisheries Service's Southeastern Regional Office. The Study would not have been possible without the generous contributions of data from a number of research scientists. Many of the Current observations are from several large Minerals Management Service (MMS) projects in the northern Gulf Of Mexico. We would especially like to acknowledge W. Johnson (MMS) and P. Niiler (Scripps Institution of Oceanography). Other programs involved Florida State University and the University of South Florida. Drifter and moored current data were provided by J. Blaha. C. Szczechowski, and S. Dinnel (Naval Oceanographic Office). Research scientists at Texas A&M and Louisiana State universities contributed ton CD-ROM data set that is available through the National Oceanographic Data Center. We are grateful to J. Waters and D. Carter (National Oceanic and Atmospheric Administration) for discussions Oil the impact of recreational fisheries. Finally, we acknowledge L. Kantha, who has,generously Shared his Model data archive for several different fisheries Studies, including this one. NR 33 TC 9 Z9 9 U1 0 U2 13 PU AMER FISHERIES SOC PI BETHESDA PA 5410 GROSVENOR LANE SUITE 110, BETHESDA, MD 20814-2199 USA SN 0002-8487 J9 T AM FISH SOC JI Trans. Am. Fish. Soc. PD MAY PY 2009 VL 138 IS 3 BP 458 EP 470 DI 10.1577/T08-008.1 PG 11 WC Fisheries SC Fisheries GA 477EJ UT WOS:000268501100002 ER PT J AU Moss, JH Farley, EV Feldmann, AM Ianelli, JN AF Moss, Jamal H. Farley, Edward V., Jr. Feldmann, Angela M. Ianelli, James N. TI Spatial Distribution, Energetic Status, and Food Habits of Eastern Bering Sea Age-0 Walleye Pollock SO TRANSACTIONS OF THE AMERICAN FISHERIES SOCIETY LA English DT Article ID EARLY MARINE GROWTH; THERAGRA-CHALCOGRAMMA; PRIBILOF ISLANDS; PELAGIC ECOSYSTEM; CLASS STRENGTH; SALMON; SIZE; ALASKA; SHELF; ZOOPLANKTON AB Age-0 walleye pollock Theragra chalcogramma were collected from the eastern Bering Sea during years when ocean temperatures were anomalously warm (2004-2005) and cool (2006-2007). Variability in spatial distribution, food habits, energetic condition, and recruitment to the age-1 life stage was investigated in relation to thermal regime. Age-0 walleye pollock were large in size and widely distributed during warm years, whereas they were small and largely confined to the middle domain of the eastern Bering Sea during cool years. Energy density as positively correlated with body weight and was greater during years when conditions were anomalously cool. The proportion of smaller age-0 walleye pollock in the diet of larger individuals was high when conditions were warm (21.9% of diet by weight), and euphausiids were the most important prey (36.5% of diet by weight) when conditions were cool. Eastern Bering Sea age-0 walleye pollock were abundant and broadly distributed from Bristol Bay to offshore and northern locations during warm years: during cool years, age-0 fish were less abundant and their distribution was constricted to the southeastern Bering Sea. An inverse relationship between brood year abundance and survival from age 0 to age 1 was found. Our results indicate that when spring (summer) sea temperatures on the eastern Bering, Sea shelf are very warm and when the water column is highly stratified during summer, age-0 walleye pollock allocate more energy to growth than to lipid storage. leading to low energy density before winter and thus to higher overwinter mortality. C1 [Moss, Jamal H.; Farley, Edward V., Jr.; Feldmann, Angela M.] Ted Stevens Marine Res Inst, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Labs, Juneau, AK 99801 USA. [Ianelli, James N.] Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Seattle, WA 98115 USA. RP Moss, JH (reprint author), Ted Stevens Marine Res Inst, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Labs, 17109 Point Lena Loop Rd, Juneau, AK 99801 USA. EM jamal.moss@noaa.gov NR 46 TC 42 Z9 45 U1 0 U2 14 PU AMER FISHERIES SOC PI BETHESDA PA 5410 GROSVENOR LANE SUITE 110, BETHESDA, MD 20814-2199 USA SN 0002-8487 J9 T AM FISH SOC JI Trans. Am. Fish. Soc. PD MAY PY 2009 VL 138 IS 3 BP 497 EP 505 DI 10.1577/T08-126.1 PG 9 WC Fisheries SC Fisheries GA 477EJ UT WOS:000268501100005 ER PT J AU Sturdevant, MV Sigler, MF Orsi, JA AF Sturdevant, M. V. Sigler, M. F. Orsi, J. A. TI Sablefish Predation on Juvenile Pacific Salmon in the Coastal Marine Waters of Southeast Alaska in 1999 SO TRANSACTIONS OF THE AMERICAN FISHERIES SOCIETY LA English DT Review ID EARLY-LIFE-HISTORY; WHITING MERLANGIUS-MERLANGUS; PINK ONCORHYNCHUS-GORBUSCHA; ANOPLOPOMA-FIMBRIA PALLAS; SIZE-SELECTIVE MORTALITY; COD GADUS-MORHUA; GASTRIC EVACUATION; CHUM SALMON; DAILY RATION; COHO SALMON AB A1-sea observations of predation by age-1 and older (age-1+) sablefish Anoplopoma fimbria oil juvenile Pacific salmon Oncorhynchus spp. were combined with laboratory studies to determine gastric evacuation rates and were used to estimate summer predation impact in file northern region of Southeast Alaska. In June and July 1999, tip to 63% of sablefish examined from trawl catches in strait habitat had each consumed one to four juvenile pink salmon O. gorbuscha, chum salmon O. keta, or sockeye salmon O. nerka. In two laboratory experiments, field-captured sablefish were acclimated without food in compartmentalized flow-through tanks with conditions manipulated to reflect the photoperiod and temperature regimes of summer. These sablefish were each offered one whole, preweighed juvenile chum salmon: Consumption events were observed, and the sablefish were then sacrificed at predetermined time intervals. Prey biomass remaining in the stomach of each sablefish predator was weighed, and all exponential model of the decline in percent biomass over time was used to yield instantaneous evacuation rates of 0.049 at 12 degrees C and 0.027 at 7 degrees C. From field data combined with model-derived estimates of meal frequency, we estimated that 0.8-6.0 million juvenile salmon were Consumed by age-1+ sablefish in the 500-km(2) area of Icy Strait during a 33-d period. Moreover, a 10-year time series of catches indicated that 1999 was a year of unusually high age-1+ sablefish abundance and relatively low juvenile salmon abundance. We speculate that sablefish predation in 1999 Could have affected abundance of out-migrating juveniles and contributed to low harvests Of returning, adult pink salmon in 2000 and adult churn salmon in 2002. Our results suggest that sablefish predation oil juvenile Pacific salmon call occur during episodic strong year-classes of sablefish and may affect adult salmon returns. C1 [Sturdevant, M. V.; Sigler, M. F.; Orsi, J. A.] Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Labs, Juneau, AK 99801 USA. RP Sturdevant, MV (reprint author), Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Labs, 17109 Point Lena Loop Rd, Juneau, AK 99801 USA. EM molly.sturdevant@noaa.gov NR 126 TC 6 Z9 7 U1 0 U2 1 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0002-8487 EI 1548-8659 J9 T AM FISH SOC JI Trans. Am. Fish. Soc. PD MAY PY 2009 VL 138 IS 3 BP 675 EP 691 DI 10.1577/T08-157.1 PG 17 WC Fisheries SC Fisheries GA 477EJ UT WOS:000268501100019 ER PT J AU Mace, GG Zhang, QQ Vaughan, M Marchand, R Stephens, G Trepte, C Winker, D AF Mace, Gerald G. Zhang, Qiuqing Vaughan, Mark Marchand, Roger Stephens, Graeme Trepte, Chip Winker, Dave TI A description of hydrometeor layer occurrence statistics derived from the first year of merged Cloudsat and CALIPSO data SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID HIGH-LEVEL CLOUDS; VERTICAL STRUCTURE; RADAR; MISSION; ISCCP; CLIMATOLOGY; LIDAR; HIRS AB The occurrence statistics of hydrometeor layers covering the Earth's surface is described using the first year of millimeter radar data collected by Cloudsat merged with lidar data collected by CALIPSO (July 2006 to June 2007). These satellites are flown in a tight orbital configuration so that they probe nearly the same volumes of the atmosphere within 10-15 s of each other. This configuration combined with the capacity for millimeter radar to penetrate optically thick hydrometeor layers and the ability of the lidar to detect optically thin clouds has allowed us to characterize the vertical and horizontal structure of hydrometeor layers with unprecedented precision. We find that the global hydrometeor coverage averages 76% and demonstrates a fairly smooth annual cycle with a range of 3% peaking in October 2006 and reaching a minimum in March 2007. The geographic distribution of hydrometeor layers defined in terms of layer base, layer top, and layer thickness is described. The predominance of geometrically thin boundary layer clouds is illustrated as is the spatial distribution of upper tropospheric ice clouds in the tropics. The cooccurrence of multiple layers is shown to be a strong function of latitude and geography with cooccurring middle-level (3 km < layer base < 6 km) and high-level (base > 6 km) layers being predominant over the continents. Cloud layer overlap is also examined, and a bias due to an assumption of maximum fractional overlap in coarse resolution models is quantified and shown to be on the order of -5 to -7% globally maximizing over the high- latitude continents of the Northern Hemisphere. C1 [Mace, Gerald G.; Zhang, Qiuqing] Univ Utah, Dept Meteorol, Salt Lake City, UT 84112 USA. [Marchand, Roger] Univ Washington, Joint Inst Study Atmosphere & Oceans, Seattle, WA 98105 USA. [Vaughan, Mark; Trepte, Chip; Winker, Dave] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Stephens, Graeme] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. RP Mace, GG (reprint author), Univ Utah, Dept Meteorol, Salt Lake City, UT 84112 USA. FU NASA FX We would like to acknowledge the efforts of the engineers and scientists at the Jet Propulsion Laboratory, NASA Langley Research Center, Centre National d'Etudes Spatiales (CNES), Ball Aerospace, and the Cooperative Institute for Research in the Atmosphere (CIRA). Support for this work was provided by NASA through a contract issued by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. NR 42 TC 176 Z9 177 U1 3 U2 24 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD APR 30 PY 2009 VL 114 AR D00A26 DI 10.1029/2007JD009755 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 439ZN UT WOS:000265667300001 ER PT J AU Preusse, P Eckermann, SD Ern, M Oberheide, J Picard, RH Roble, RG Riese, M Russell, JM Mlynczak, MG AF Preusse, Peter Eckermann, Stephen D. Ern, Manfred Oberheide, Jens Picard, Richard H. Roble, Raymond G. Riese, Martin Russell, James M., III Mlynczak, Martin G. TI Global ray tracing simulations of the SABER gravity wave climatology SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID CRYOGENIC INFRARED SPECTROMETERS; ATMOSPHERE RESEARCH SATELLITE; STRATOSPHERIC MOUNTAIN WAVES; GENERAL-CIRCULATION MODELS; GPS OCCULTATION DATA; MIDDLE ATMOSPHERE; SPECTRAL PARAMETERIZATION; LATITUDINAL VARIATIONS; MOMENTUM DEPOSITION; CRISTA TEMPERATURES AB Since February 2002, the SABER (sounding of the atmosphere using broadband emission radiometry) satellite instrument has measured temperatures throughout the entire middle atmosphere. Employing the same techniques as previously used for CRISTA (cryogenic infrared spectrometers and telescopes for the atmosphere), we deduce from SABER V1.06 data 5 years of gravity wave (GW) temperature variances from altitudes of 20 to 100 km. A typical annual cycle is presented by calculating averages for the individual calendar months. Findings are consistent with previous results from various satellite missions. Based on zonal mean, SABER data for July and zonal mean GW momentum flux from CRISTA, a homogeneous and isotropic launch distribution for the GROGRAT (gravity wave regional or global ray tracer) is tuned. The launch distribution contains different phase speed mesoscale waves, some of very high-phase speed and extremely low amplitudes, as well as waves with horizontal wavelengths of several thousand kilometers. Global maps for different seasons and altitudes, as well as time series of zonal mean GW squared amplitudes based on this launch distribution, match the observations well. Based on this realistic observation-tuned model run, we calculate quantities that cannot be measured directly and are speculated to be major sources of uncertainty in current GW parameterization schemes. Two examples presented in this paper are the average cross-latitude propagation of GWs and the relative acceleration contributions provided by saturation and dissipation, on the one hand, and the horizontal refraction of GWs by horizontal gradients of the mean flow, on the other hand. C1 [Preusse, Peter; Ern, Manfred; Riese, Martin] Forschungszentrum Julich, Inst Chem & Dynam Geosphere, Res Ctr Juelich,ICG Stratosphere 1, D-52425 Julich, Germany. [Eckermann, Stephen D.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Oberheide, Jens] Berg Univ Wuppertal, Dept Phys, D-42097 Wuppertal, Germany. [Picard, Richard H.] USAF, Res Lab, RVBYM, Hanscom AFB, MA 01731 USA. [Roble, Raymond G.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Russell, James M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. [Mlynczak, Martin G.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Preusse, P (reprint author), Forschungszentrum Julich, Inst Chem & Dynam Geosphere, Res Ctr Juelich,ICG Stratosphere 1, Postfach 1913, D-52425 Julich, Germany. EM p.preusse@fz-juelich.de; stephen.eckermann@nrl.navy.mil RI Oberheide, Jens/C-6156-2011; Mlynczak, Martin/K-3396-2012; Preusse, Peter/A-1193-2013; Riese, Martin/A-3927-2013; Ern, Manfred/I-8839-2016 OI Oberheide, Jens/0000-0001-6721-2540; Preusse, Peter/0000-0002-8997-4965; Riese, Martin/0000-0001-6398-6493; Ern, Manfred/0000-0002-8565-2125 FU DFG CAWSES [OB 299/2-2, ER 474/1-1]; NASA SABER Program Office; U.S. Air Force Office of Scientific Research FX Jens Oberheide is supported by DFG CAWSES grant OB 299/2-2. Part of the work of Manfred Ern was supported by DFG CAWSES grant ER 474/1-1. Richard H. Picard acknowledges support from NASA SABER Program Office and Dr. Kent Miller of U.S. Air Force Office of Scientific Research. We thank three anonymous reviewers for their helpful comments on the determination of the intermittency factors, discussions, and data presentation. NR 87 TC 54 Z9 54 U1 4 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 APR 30 PY 2009 VL 114 AR D08126 DI 10.1029/2008JD011214 PG 25 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 439ZN UT WOS:000265667300006 ER PT J AU Rutan, D Rose, F Roman, M Manalo-Smith, N Schaaf, C Charlock, T AF Rutan, David Rose, Fred Roman, Miguel Manalo-Smith, Natividad Schaaf, Crystal Charlock, Tom TI Development and assessment of broadband surface albedo from Clouds and the Earth's Radiant Energy System Clouds and Radiation Swath data product SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID REFLECTANCE DISTRIBUTION FUNCTION; BIDIRECTIONAL REFLECTANCE; SATELLITE-OBSERVATIONS; OPTICAL-PROPERTIES; CLAMS EXPERIMENT; VALIDATION; AEROSOL; MODEL; MODIS; RETRIEVALS AB We describe a method to determine broadband albedo globally over land viewed by the Clouds and the Earth's Radiant Energy System (CERES) scanning radiometers on board the TRMM, Terra, and Aqua satellites. This albedo is used as a surface boundary condition for a fast radiation transfer code in the Surface and Atmospheric Radiation Budget (SARB) subsystem of the CERES processing scheme. Cloudy sky surface albedo is estimated from derived clear sky values. Clear sky surface albedo is assessed by comparing the CERES/SARB-based surface albedo with the bidirectional reflectance distribution function (BRDF)-based surface albedo supplied by the MODIS land surfaces group. The SARB method employs broadband observations at the top of atmosphere (TOA) and assumes relative spectral shape of surface albedo. The MODIS group uses higher spatial resolution observations in several shortwave window channels to retrieve spectral surface albedos and then scales up to broadband surface albedo. Comparisons over snow-free land show good agreement between the two independent products on the scale of the CERES footprint. Biases run approximately 0.005 absolute or 0.02 relative with SARB albedo, generally lower than MODIS. We find little dependence on view geometry and slight functional dependence on aerosol optical depth. The value selected for a priori surface spectral albedo is important, but not critical, when retrieving broadband surface albedo with broadband TOA data. However, based on calculations, aerosol forcing to TOA flux changes in spectral albedo shape can affect aerosol forcing for as much as would a 15% absolute change in the original broadband surface albedo. C1 [Rutan, David; Rose, Fred; Manalo-Smith, Natividad] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. [Charlock, Tom] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Roman, Miguel; Schaaf, Crystal] Boston Univ, Ctr Remote Sensing, Dept Geog, Boston, MA 02215 USA. RP Rutan, D (reprint author), Sci Syst & Applicat Inc, 1 Enterprise Pkwy,Suite 200, Hampton, VA 23666 USA. EM david.a.rutan@nasa.gov RI Roman, Miguel/D-4764-2012; OI Roman, Miguel/0000-0003-3953-319X; Rose, Fred G/0000-0003-0769-0772 FU NASA [NNX08AE94A]; DOE [DE-FG02-06ER64178] FX The authors would like to thank the anonymous reviewers whose close reading and suggestions led to a better-organized and stronger paper. CERES data are supplied from the NASA Langley Research Center Atmospheric Sciences Data Center. MODIS data are supplied from the NASA Goddard Distributed Active Archive Center. ARM data are made available through the U.S. Department of Energy as part of the Atmospheric Radiation Measurement Program. GMD data are made available through the NOAA's Earth System Research Laboratory/Global Monitoring Division-Radiation (G-RAD). SURFRAD data are made available through NOAA's Air Resources Laboratory/Surface Radiation Research Branch. IGBP and Global Ecosystem maps are made available from the USGS Earth Resources Observation and Science (EROS) data Center. C. Schaaf and M. Roman are supported by NASA NNX08AE94A and DOE DE-FG02-06ER64178. NR 51 TC 41 Z9 41 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 APR 30 PY 2009 VL 114 AR D08125 DI 10.1029/2008JD010669 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 439ZN UT WOS:000265667300003 ER PT J AU Wolkenberg, P Grassi, D Formisano, V Rinaldi, G D'Amore, M Smith, M AF Wolkenberg, P. Grassi, D. Formisano, V. Rinaldi, G. D'Amore, M. Smith, M. TI Simultaneous observations of the Martian atmosphere by Planetary Fourier Spectrometer on Mars Express and Miniature Thermal Emission Spectrometer on Mars Exploration Rover SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID WAVELENGTH CHANNEL; TEMPERATURES; CALIBRATION; RADIATION; RETRIEVAL; MISSION; TES AB In this study we present temperature profiles in the lower atmosphere of Mars from simultaneous observations performed by the Planetary Fourier Spectrometer (PFS) aboard the Mars Express spacecraft and the Miniature Thermal Emission Spectrometer (Mini-TES) aboard the Mars Exploration Rovers. Thermal infrared spectra were collected in both the upward and downward looking geometries from the surface and from orbit, respectively. We used two sets of criteria to select PFS observations. These criteria took into account the location around the landing sites of the rovers, the local time (LT), and the solar longitude (L-s) corresponding to the Martian solar day (sol). The first set of criteria included PFS measurements carried out within +/-1 degrees in latitude and longitude, within 1 h in local time, and on the same sol. From the restricted set of measurements we conclude that the PFS data are consistent with the Mini-TES data. The next set of criteria covered the area 5 degrees x 5 degrees around the landing sites, within 1 h in local time and within 9 sols. The latter criteria allow us to study the variation of parameters LT, distance, and Ls and their influence on changes of temperature profiles. This comparison for the group with relaxed criteria showed also that local time has strongest effect on temperature differences. The main purpose of this study is to confirm the validity of PFS temperature profiles close to the surface. Atmospheric temperatures below 5 km are retrieved from satellite measurements with a large uncertainty because of poor pieces of information in the wings of the CO2 absorption band at 667 cm(-1). The Mini-TES temperature profiles span atmospheric layers below 2 km. The good correspondence observed in a number of cases confirms the possibility of using PFS measurements to investigate the lower atmosphere. C1 [Wolkenberg, P.; Grassi, D.; Formisano, V.; Rinaldi, G.; D'Amore, M.] INAF, IFSI, I-00133 Rome, Italy. [Smith, M.] Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Wolkenberg, P (reprint author), INAF, IFSI, Via Fosso Cavaliere 100, I-00133 Rome, Italy. EM paulina.wolkenberg@ifsi-roma.inaf.it RI Smith, Michael/C-8875-2012 NR 21 TC 3 Z9 3 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD APR 30 PY 2009 VL 114 AR E04012 DI 10.1029/2008JE003216 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 440BV UT WOS:000265674100002 ER PT J AU Schmidt, G Archer, D AF Schmidt, Gavin Archer, David TI CLIMATE CHANGE Too much of a bad thing SO NATURE LA English DT Editorial Material ID INTERFERENCE C1 [Schmidt, Gavin] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Archer, David] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. RP Schmidt, G (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM gschmidt@giss.nasa.gov; d-archer@uchicago.edu RI Schmidt, Gavin/D-4427-2012; Archer, David/K-7371-2012 OI Schmidt, Gavin/0000-0002-2258-0486; Archer, David/0000-0002-4523-7912 NR 8 TC 8 Z9 8 U1 0 U2 9 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 APR 30 PY 2009 VL 458 IS 7242 BP 1117 EP 1118 DI 10.1038/4581117a PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 441FL UT WOS:000265754600029 PM 19407786 ER PT J AU Laurenza, M Cliver, EW Hewitt, J Storini, M Ling, AG Balch, CC Kaiser, ML AF Laurenza, M. Cliver, E. W. Hewitt, J. Storini, M. Ling, A. G. Balch, C. C. Kaiser, M. L. TI A technique for short-term warning of solar energetic particle events based on flare location, flare size, and evidence of particle escape SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID CORONAL MASS EJECTIONS; III RADIO-BURSTS; X-RAY FLARES; PROTON EVENTS; MICROWAVE BURSTS; ACCELERATION; EMISSION; ELECTRON; DENSITY; SHOCKS AB We have developed a technique to provide short-term warnings of solar energetic proton (SEP) events that meet or exceed the Space Weather Prediction Center threshold of J (>10 MeV) = 10 pr cm(-2) s(-1) sr(-1). The method is based on flare location, flare size, and evidence of particle acceleration/escape as parameterized by flare longitude, time-integrated soft X-ray intensity, and time-integrated intensity of type III radio emission at similar to 1 MHz, respectively. In this technique, warnings are issued 10 min after the maximum of >= M2 soft X-ray flares. For the solar cycle 23 (1995-2005) data on which it was developed, the method has a probability of detection of 63% (47/75), a false alarm rate of 42% (34/81), and a median warning time of similar to 55 min for the 19 events successfully predicted by our technique for which SEP event onset times were provided by Posner (2007). These measures meet or exceed verification results for competing automated SEP warning techniques but, at the present stage of space weather forecasting, fall well short of those achieved with a human (aided by techniques such as ours) making the ultimate yes/no SEP event prediction. We give some suggestions as to how our method could be improved and provide our flare and SEP event database in the auxiliary material to facilitate quantitative comparisons with techniques developed in the future. C1 [Laurenza, M.; Storini, M.] INAF, Inst Interplanetary Space Phys, I-00133 Rome, Italy. [Balch, C. C.] NOAA, Space Weather Predict Ctr, Boulder, CO 80305 USA. [Cliver, E. W.; Hewitt, J.] AFRL, Space Vehicles Directorate, Hanscom AFB, MA 01731 USA. [Ling, A. G.] Atmospher Environm Res Inc, Lexington, MA 02421 USA. [Kaiser, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Laurenza, M (reprint author), INAF, Inst Interplanetary Space Phys, Via Fosso Cavaliere 100, I-00133 Rome, Italy. EM monica.laurenza@ifsi-roma.inaf.it FU ASI [I/090/06/0]; European Office of Aerospace Research and Development FX Part of the work by M. L. and M. S. was performed under COST 724 Action and part under the ASI contract I/090/06/0. E. W. C. was supported through the Window on Europe program of the European Office of Aerospace Research and Development. We acknowledge a helpful discussion with Kent Doggett of the SWPC. NR 71 TC 28 Z9 28 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD APR 30 PY 2009 VL 7 AR S04008 DI 10.1029/2007SW000379 PG 18 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 440CQ UT WOS:000265676400001 ER PT J AU Lin, WY Zhang, MH Wu, JB AF Lin, Wuyin Zhang, Minghua Wu, Jingbo TI Simulation of low clouds from the CAM and the regional WRF with multiple nested resolutions SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID PLANETARY BOUNDARY-LAYER; ATMOSPHERE; CONVECTION; STREETS; MODELS; FLOWS AB Current climate models have shown systematic simulation biases of low clouds that have cast great uncertainties on the climate sensitivity of these models. Among them is the deficient amount of low clouds over the storm tracks. This study uses the NCAR Community Atmospheric Model (CAM) and the Weather Research and Forecasting model (WRF) to study the cause of the failure of the global model in simulating low clouds associated with a frontal passage over the North Atlantic. The global model is shown to simulate the large-scale circulation that can support the boundary layer instabilities responsible for the observed clouds, but because the global model does not resolve the unstable modes, the instability cannot be realized. The resolution requirement of cloud simulations is discussed. This study also demonstrates the feasibility of cloud parameterization by nesting high resolution models into coarse resolution models to tap into the dynamical properties of the large-scale flows. Citation: Lin, W., M. Zhang, and J. Wu (2009), Simulation of low clouds from the CAM and the regional WRF with multiple nested resolutions, Geophys. Res. Lett., 36, L08813, doi:10.1029/2008GL037088. C1 [Lin, Wuyin; Zhang, Minghua] SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA. [Wu, Jingbo] Columbia Univ, NASA GISS, New York, NY 10025 USA. RP Lin, WY (reprint author), SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA. EM wlin@atmsci.msrc.sunysb.edu FU NASA MAP; DOE ARM; National Science Foundation to Stony Brook University FX This research is supported under the NASA MAP program to Stony Brook University. Partial support is also from the DOE ARM and CCPP program and the National Science Foundation to Stony Brook University. NR 21 TC 4 Z9 4 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 APR 29 PY 2009 VL 36 AR L08813 DI 10.1029/2008GL037088 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 439YV UT WOS:000265664800002 ER PT J AU Pogorzelski, RJ AF Pogorzelski, Ronald J. TI Beam steering dynamics in coupled oscillator based phased arrays with coupling delay SO RADIO SCIENCE LA English DT Article AB A continuum solution for the phase evolution of a coupled oscillator array with coupling delay, when one oscillator is step detuned in time, is derived from the discrete model solution previously published. From this Green's function a differential equation is derived for the Laplace transform of the phase dynamics. The solution of this differential equation is expressed as a sum of the eigenfunctions of the differential operator for a finite length array with one oscillator detuned. The dynamic behavior of the aperture phase for beam steering is obtained by superposing two of the Green's function solutions corresponding to antisymmetric excitation at each end of the array. The far zone beam steering behavior is obtained by summing the elemental radiated signals. Generalization to planar arrays appears to be straightforward. An alternative more flexible formulation suitable for early times is also presented. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Pogorzelski, RJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ronald.j.pogorzelski@jpl.nasa.gov FU JPL Mars Technology Program; Interplanetary Network Directorate Technology Program; NASA FX The work reported here was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA). Partial support from the JPL Mars Technology Program, the Interplanetary Network Directorate Technology Program, and the JPL Advanced Concepts Office of the NASA Office of Space Exploration are gratefully acknowledged. Thanks are due Vahraz Jamnejad of JPL for helpful theoretical discussions during the early stages of the present work and R. A. York of the University of California, Santa Barbara, for his early insight (circa 1998) concerning the Sturm- Liouville nature of the differential equations and the concomitant simple inverse Laplace transform of the Green's function without coupling delay. Particular thanks are due Jason Martinez of Wolfram Research for his help with the plots. Much of the computation and graphing associated with this work was done using Mathematica1 byWolfram Research. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not constitute or imply its endorsement by the United States Government or the Jet Propulsion Laboratory, California Institute of Technology. NR 6 TC 0 Z9 0 U1 2 U2 3 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 APR 29 PY 2009 VL 44 AR RS2019 DI 10.1029/2008RS004056 PG 9 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications GA 440CP UT WOS:000265676300002 ER PT J AU Salmun, H Molod, A Albrecht, J Santos, F AF Salmun, Haydee Molod, Andrea Albrecht, Jochen Santos, Fernanda TI Scales of variability of surface vegetation: Calculation and implications for climate models SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article ID CONVECTIVE BOUNDARY-LAYER; AMAZONIAN DEFORESTATION; LAND-USE; LANDSCAPE; HETEROGENEITY; AGGREGATION; IMPACT; RESOLUTION; PATTERNS; FLUXES AB The presence in the vegetation landscape of many varied scales of organization implies a complex set of land/atmosphere interactions. Larger scales of variability at the surface induce boundary layer heterogeneity and may induce secondary boundary layer circulation patterns. The quantification of the scales of heterogeneity in the surface vegetation, therefore, is essential to the understanding and modeling of the land/atmosphere interactions. The present study analyzes the scales of heterogeneity in the surface vegetation by using a satellite-derived land class category map and a discrete analysis tool. Results show substantial variability in scales near 1000 km for most land class categories other than Deciduous Broadleaf Forest. Implications for GCM modeling approaches to the land/atmosphere interactions were drawn based on the results of the study. Results are consistent with the use of a 'mosaic' rather than a 'mixture' approach and with extending the 'mosaic' approach up through the boundary layer. C1 [Salmun, Haydee; Albrecht, Jochen; Santos, Fernanda] CUNY Hunter Coll, Dept Geog, New York, NY 10065 USA. [Molod, Andrea] Univ Maryland Baltimore Cty, Goddard Modeling & Assimilat Off, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. RP Salmun, H (reprint author), CUNY Hunter Coll, Dept Geog, 695 Pk Ave, New York, NY 10065 USA. EM hsalmun@hunter.cuny.edu OI Santos, Fernanda/0000-0001-9155-5623 FU CUNY Research Foundation through PSC-CUNY award [65266-00 34]; NSF's ADVANCE [0620087]; Society of Women Geographers FX We gratefully acknowledge the partial support for this work provided the CUNY Research Foundation through PSC-CUNY award 65266-00 34. Final stages of the analysis and the writing of this manuscript were accomplished under the auspices of the NSF's ADVANCE grant 0620087. F. S. was partially supported by an award from the Society of Women Geographers, and the calculations she contributed to this work constitute an M. A. thesis in the Department of Geography at Hunter College of CUNY. The authors also wish to acknowledge the constructive critique of the two anonymous reviewers. NR 36 TC 3 Z9 3 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-BIOGEO JI J. Geophys. Res.-Biogeosci. PD APR 28 PY 2009 VL 114 AR G02007 DI 10.1029/2008JG000762 PG 13 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 440AC UT WOS:000265669000001 ER PT J AU Gounelle, M Chaussidon, M Morbidelli, A Barrat, JA Engrand, C Zolensky, ME McKeegan, KD AF Gounelle, Matthieu Chaussidon, Marc Morbidelli, Alessandro Barrat, Jean-Alix Engrand, Cecile Zolensky, Michael E. McKeegan, Kevin D. TI A unique basaltic micrometeorite expands the inventory of solar system planetary crusts SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE asteroids; cosmic dust; differentiation ID ANTARCTIC MICROMETEORITES; COSMIC SPHERULES; OXYGEN ISOTOPES; ACCRETION RATE; PARENT BODY; SOUTH-POLE; MAIN BELT; METEORITES; VESTA; COLLECTION AB Micrometeorites with diameter approximate to 100-200 mu m dominate the flux of extraterrestrial matter on Earth. The vast majority of micrometeorites are chemically, mineralogically, and isotopically related to carbonaceous chondrites, which amount to only 2.5% of meteorite falls. Here, we report the discovery of the first basaltic micrometeorite (MM40). This micrometeorite is unlike any other basalt known in the solar system as revealed by isotopic data, mineral chemistry, and trace element abundances. The discovery of a new basaltic asteroidal surface expands the solar system inventory of planetary crusts and underlines the importance of micrometeorites for sampling the asteroids' surfaces in a way complementary to meteorites, mainly because they do not suffer dynamical biases as meteorites do. The parent asteroid of MM40 has undergone extensive metamorphism, which ended no earlier than 7.9 Myr after solar system formation. Numerical simulations of dust transport dynamics suggest that MM40 might originate from one of the recently discovered basaltic asteroids that are not members of the Vesta family. The ability to retrieve such a wealth of information from this tiny (a few micrograms) sample is auspicious some years before the launch of a Mars sample return mission. C1 [Gounelle, Matthieu] CNRS, UMR 7202, Lab Mineral, F-75005 Paris, France. [Gounelle, Matthieu] CNRS, UMR 7202, Museum Natl Hist Nat, Cosmochim Museum, F-75005 Paris, France. [Chaussidon, Marc] Nancy Univ, CNRS, UPR 2300, Ctr Rech Petrog & Geochim, Notre Dame Des Pauvres, France. [Morbidelli, Alessandro] Observ Cote Azur, F-06304 Nice, France. [Barrat, Jean-Alix] Univ Bretagne Occidentale, Inst Univ Europeen Mer, CNRS, UMR 6538 Domaines Ocean, F-29280 Plouzane, France. [Engrand, Cecile] Univ Paris 11, Ctr Spectrometrie Nucl & Spectrometrie Masse, CNRS, F-91405 Orsay, France. [Zolensky, Michael E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [McKeegan, Kevin D.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. RP Gounelle, M (reprint author), CNRS, UMR 7202, Lab Mineral, CP52,57 Rue Cuvier, F-75005 Paris, France. EM gounelle@mnhn.fr RI McKeegan, Kevin/A-4107-2008; Jean-Alix, BARRAT/F-8035-2012; UCLA, SIMS/A-1459-2011; Barrat, Jean-Alix/C-8416-2017; Chaussidon, Marc/E-7067-2017 OI McKeegan, Kevin/0000-0002-1827-729X; Barrat, Jean-Alix/0000-0003-3158-3109; FU Program National de Planetologie (PNP); Centre National de la Recherche Scientifique [2006-3482]; European Grant ORIGINS [MRTN-CT-2006-035519]; Institut Polaire Francais Paul-Emile Victor (IPEV) FX We thank Michel Maurette and Gero Kurat for their pioneering work on micrometeorites and for fruitful discussions and insights on the origin of this particle, and two anonymous reviewers for their very constructive comments, and for bringing our attention to the basaltic clasts in ordinary chondrites. This work was supported by the Program National de Planetologie (PNP), the France-Etats-Unis fund from Centre National de la Recherche Scientifique [2006-3482], and European Grant ORIGINS [MRTN-CT-2006-035519]. The Institut Polaire Francais Paul-Emile Victor (IPEV) constantly supported the efforts of the Orsay group to collect micrometeorites. This is CRPG contribution # 1989. NR 47 TC 18 Z9 18 U1 1 U2 4 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD APR 28 PY 2009 VL 106 IS 17 BP 6904 EP 6909 DI 10.1073/pnas.0900328106 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 438VS UT WOS:000265584500009 PM 19366660 ER PT J AU Hiraga, JS Kobayashi, Y Tamagawa, T Hayato, A Bamba, A Terada, Y Petre, R Katagiri, H Tsunemi, H AF Hiraga, Junko S. Kobayashi, Yusuke Tamagawa, Toru Hayato, Asami Bamba, Aya Terada, Yukikatsu Petre, Robert Katagiri, Hideaki Tsunemi, Hiroshi TI Search for Sc-K Line Emission from RX J0852.0-4622 Supernova Remnant with Suzaku SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE ISM: supernova remnant; X-ray: individual [RX J0852.0-4622 (Vela Jr.)] ID X-RAY; GALACTIC SUPERNOVA; BOARD SUZAKU; TI-44; J0852-4642; CASSIOPEIA; CAS AB We searched for evidence of line emission around 4 keV from the northwestern rim of the supernova remnant RX J0852.0-4622 using Suzaku XIS data. Several papers have reported on the detection of an emission line around 4.1 keV from this region of the sky. This line Would arise from K-band fluorescence by Sc-44, the immediate decay product of Ti-44. We performed spectral analysis for the entire portion of the NW rim of the remnant within the XIS field of view, as well as various regions corresponding to regions of published claims of line emission. We found no line emission around 4.1 keV anywhere, and are able to set a restrictive Upper limit to the X-ray flux: 1.1 x 10(-6) s(-1) cm(-2) for the entire field. For every region, our flux upper limit falls below that of the previously claimed detection. Therefore, we conclude that, to date, no definite X-ray line feature from Sc-K emission has been detected in the NW rim of RX J0852.0-4622. Our negative-detection supports the recent claim that RX J0852-4622 is neither young (1700-4000 yr) nor nearby (similar to 750 pc). C1 [Hiraga, Junko S.; Tamagawa, Toru; Hayato, Asami] RIKEN, Wako, Saitama 3510198, Japan. [Kobayashi, Yusuke; Bamba, Aya] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Tamagawa, Toru; Hayato, Asami] Tokyo Univ Sci, Dept Phys, Shinjuku Ku, Tokyo 1628601, Japan. [Terada, Yukikatsu] Saitama Univ, Dept Phys, Sakura Ku, Saitama 3388570, Japan. [Petre, Robert] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Katagiri, Hideaki] Hiroshima Univ, Grad Sch Sci, Dept Phys Sci, Hiroshima 7398526, Japan. [Tsunemi, Hiroshi] Osaka Univ, Grad Sch Sci Earth & Space Sci, Osaka 5600043, Japan. RP Hiraga, JS (reprint author), RIKEN, 2-1 Hirosawa, Wako, Saitama 3510198, Japan. EM jhiraga@crab.riken.jp RI Terada, Yukikatsu/A-5879-2013; XRAY, SUZAKU/A-1808-2009 OI Terada, Yukikatsu/0000-0002-2359-1857; NR 20 TC 10 Z9 10 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD APR 25 PY 2009 VL 61 IS 2 BP 275 EP 281 DI 10.1093/pasj/61.2.275 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 447YP UT WOS:000266228300012 ER PT J AU Uchida, H Tsunemi, H Katsuda, S Kimura, M Kosugi, H AF Uchida, Hiroyuki Tsunemi, Hiroshi Katsuda, Satoru Kimura, Masashi Kosugi, Hiroko TI Ejecta Distributions of Heavy Elements in the Cygnus Loop SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE ISM: abundances; ISM: individual (Cygnus Loop); ISM: supernova remnants; X-rays: ISM ID X-RAY-SPECTRUM; SUPERNOVA REMNANT; NORTHEASTERN RIM; SOUTHWESTERN RIM; PLASMA STRUCTURE; SUZAKU; EMISSION; NUCLEOSYNTHESIS; ABSORPTION; EXPLOSION AB We analyzed the metal distribution of the Cygnus Loop using 14 and 7 pointing observation data obtained by the Suzaku and XMM-Newton observatories, respectively. The spectral analysis shows that all of the spectra are well fitted by a two-kT(e) nonequilibrium ionization plasma model, as shown by earlier observations. From the best-fit parameters of the high-kT(e), component, we calculated the emission measures about Various elements. and showed the metal distribution of the ejecta component. We found that the distributions of Si and Fe are centered South of the geometric center toward the blow-out region. From the best-fit parameters, we also estimated the progenitor mass of the Cygnus Loop from our field of view (FOV) and the metal-rich region with a radius of 25' from the metal center. The result obtained from the metal circle is similar to that obtained from our entire FOV which suggests a mixing of the metal. From the results, the mass of the progenitor star was estimated at 12-15 M-circle dot. C1 [Uchida, Hiroyuki; Tsunemi, Hiroshi; Katsuda, Satoru; Kimura, Masashi; Kosugi, Hiroko] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Osaka 5600043, Japan. [Katsuda, Satoru] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Uchida, H (reprint author), Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Osaka 5600043, Japan. EM uchida@ess.sci.osaka-u.ac.jp RI XRAY, SUZAKU/A-1808-2009 FU Ministry of Education, Culture, Sports, Science and Technology [16002004]; JSPS Research Fellowship for Young Scientists FX This work is partly supported by a Grant-in-Aid for Scientific Research by the Ministry of Education, Culture, Sports, Science and Technology (16002004). This study is also carried out as part of the 21st Century COE Program, "Towards a new basic science: depth and synthesis". H. U. and S. K. are supported by JSPS Research Fellowship for Young Scientists. NR 33 TC 10 Z9 10 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD APR 25 PY 2009 VL 61 IS 2 BP 301 EP 308 DI 10.1093/pasj/61.2.301 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 447YP UT WOS:000266228300015 ER PT J AU Cravens, TE McNutt, RL Waite, JH Robertson, IP Luhmann, JG Kasprzak, W Ip, WH AF Cravens, T. E. McNutt, R. L., Jr. Waite, J. H., Jr. Robertson, I. P. Luhmann, J. G. Kasprzak, W. Ip, W. -H. TI Plume ionosphere of Enceladus as seen by the Cassini ion and neutral mass spectrometer SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SATURNS MAGNETOSPHERE; PLASMA; ATMOSPHERE; CHEMISTRY; DYNAMICS AB The Cassini spacecraft passed within 168 km of the surface of Enceladus on 14 July 2005 during the E2 flyby and passed closer (50 km) during the E3 encounter on 13 March 2008. During both flybys the ion and neutral mass spectrometer (INMS) detected a plume atmosphere mainly composed of water. During the E3 flyby, the INMS measured an ion mass spectrum with a large peak at mass number of 19 Daltons (interpreted as H(3)O(+) ions) but not at the mass numbers of other water group ion species (including H(2)O(+), OH(+), O(+)). In addition, the INMS observed ion species at mass numbers 36 and 37 possibly the water cluster ion species H(2)O(+) - H(2)O and H(3)O(+) - H(2)O. The INMS detection of cold H3O+ in the plume combined with the almost complete absence of cold H2O+ ions is attributed to an active ion-neutral chemistry operating in a plume "ionosphere.'' Citation: Cravens, T. E., R. L. McNutt Jr., J. H. Waite Jr., I. P. Robertson, J. G. Luhmann, W. Kasprzak, and W.-H. Ip (2009), Plume ionosphere of Enceladus as seen by the Cassini ion and neutral mass spectrometer, Geophys. Res. Lett., 36, L08106, doi:10.1029/2009GL037811. C1 [Cravens, T. E.; Robertson, I. P.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Ip, W. -H.] Natl Cent Univ, Inst Astron, Jhongli 32001, Taiwan. [Ip, W. -H.] Natl Cent Univ, Inst Space Sci, Jhongli 32001, Taiwan. [Kasprzak, W.] NASA, Goddard Spaceflight Ctr, Greenbelt, MD 20771 USA. [Luhmann, J. G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [McNutt, R. L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Waite, J. H., Jr.] SW Res Inst, San Antonio, TX 78238 USA. RP Cravens, TE (reprint author), Univ Kansas, Dept Phys & Astron, 1251 Wescoe Hall Dr, Lawrence, KS 66045 USA. EM cravens@ku.edu RI McNutt, Ralph/E-8006-2010 OI McNutt, Ralph/0000-0002-4722-9166 FU NASA Cassini [NFP45280] FX Support from the NASA Cassini project ( grant NFP45280 via subcontract from Southwest Research Institute) is acknowledged. NR 25 TC 23 Z9 23 U1 1 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD APR 24 PY 2009 VL 36 AR L08106 DI 10.1029/2009GL037811 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 438CR UT WOS:000265534000003 ER PT J AU Choi, HJ Chun, HY Song, IS AF Choi, Hyun-Joo Chun, Hye-Yeong Song, In-Sun TI Gravity wave temperature variance calculated using the ray-based spectral parameterization of convective gravity waves and its comparison with Microwave Limb Sounder observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MOMENTUM FLUX SPECTRUM; LARGE-SCALE MODELS; DRAG PARAMETERIZATION; CUMULUS CONVECTION; MIDDLE ATMOSPHERE; STRATOSPHERE; FORMULATION; REANALYSIS; GENERATION AB The ray-based spectral parameterization of convective gravity wave drag, which explicitly calculates the gravity wave propagation properties, is validated against the Microwave Limb Sounder (MLS) on the Upper Atmosphere Research Satellite (UARS). Offline calculations of the ray-based parameterization are performed using global reanalysis data and gravity wave temperature variances calculated from the parameterization are compared with those measured from the MLS. The parameterized temperature variances are calculated from gravity wave packets that are visible from the MLS to allow for comparison. The MLS visibility is analytically obtained using the three-dimensional MLS filter function. Comparisons between the parameterization calculations and MLS measurements show that both the magnitude and spatial distribution of the MLS-filtered temperature variances in the ray-based parameterization are in good agreement with observations. However, the MLS-filtered temperature variances are found to be sensitive to the source-level wave propagation direction, which, until now, has been regarded as a free parameter in the ray-based parameterization. This result indicates that the wave propagation direction can be crucial for more realistic parameterization of gravity wave (GW) effects and thus needs to be reasonably determined. Comparisons between the ray-based parameterization and columnar parameterization, which considers the gravity wave propagation only in the vertical direction, are also made in terms of temperature variance, and both results, after filtered, are similar to MLS observations. However, the magnitude of the unfiltered temperature variance in the equatorial regions with weak MLS visibility is smaller in the ray-based parameterization than in the columnar parameterization. C1 [Choi, Hyun-Joo; Chun, Hye-Yeong] Yonsei Univ, Dept Atmospher Sci, Seoul 120749, South Korea. [Song, In-Sun] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. [Song, In-Sun] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. RP Choi, HJ (reprint author), Yonsei Univ, Dept Atmospher Sci, 262 Seongsanno, Seoul 120749, South Korea. EM chunhy@yonsei.ac.kr FU Ministry of Science and Technology of Korea [M10500000114-06J0000-11410] FX This work was supported by the Ministry of Science and Technology of Korea through the National Research Laboratory Program (M10500000114-06J0000-11410). The DCH data set was provided by the cooperative research project of the NCEP-DOE Atmospheric Model Intercomparison Project (AMIP-II) reanalysis (R-2) by NCEP and DOE. The ECMWF ERA-40 reanalysis data set was provided by ECMWF from their data server. NR 36 TC 16 Z9 16 U1 1 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 APR 24 PY 2009 VL 114 AR D08111 DI 10.1029/2008JD011330 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 438DB UT WOS:000265535000006 ER PT J AU Suess, ST Ko, YK von Steiger, R Moore, RL AF Suess, S. T. Ko, Y. -K. von Steiger, R. Moore, R. L. TI Quiescent current sheets in the solar wind and origins of slow wind SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID CORONAL MASS EJECTION; HELIOSPHERIC CURRENT SHEET; PHYSICAL-PROPERTIES; HELIUM ABUNDANCE; STREAMER BOUNDARIES; FLOW; EVOLUTION; SPEEDS; FLARES; AU AB Solar wind near the heliospheric current sheet is investigated using Ulysses and ACE data in a superposed epoch analysis for several days on either side of the current sheets. Only data near sunspot minima are used, minimizing the influence of transients. New results are shown for composition and ionization state. Existing results showing a similar to 2 day wide depletion in He/H (He(++)/H(+)) at the current sheet are confirmed, although the depletion is generally more narrow. A recent finding of a broad 5-10 day wide reduction in He/H around the current sheet is also confirmed. An important result is that the narrow depletion is not a real phenomenon but is instead a statistical consequence of the superposition of transient depletions that also create the broad reduction in the averages. These transient depletions last from a few hours up to several days, come from the core of streamers, and are embedded in a quasi-steady flow from streamers' legs. Most depletions contain a current sheet just inside one edge, leading to the apparent narrow depletion at the current sheet in the superposed epoch analysis. These results lead us to a hypothesis for how the He/H depletions form with a current sheet just inside one edge. Fe/O fluctuations associated with the He/H fluctuations further show that mixing of plasma from coronal holes adjacent to streamer brightness boundaries into outflow inside the brightness boundary is not an important process. C1 [Suess, S. T.] NASA, George C Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Huntsville, AL 35812 USA. [Ko, Y. -K.] USN, Res Lab, Washington, DC 20375 USA. [von Steiger, R.] Int Space Sci Inst, Bern, Switzerland. RP Suess, ST (reprint author), NASA, George C Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Mail Code VP62, Huntsville, AL 35812 USA. EM stevesuess@bellsouth.net; yko@ssd5.nrl.navy.mil; vsteiger@issibern.ch; ronald.1.moore@nasa.gov RI Von Steiger, Rudolf/F-6822-2011 OI Von Steiger, Rudolf/0000-0002-3350-0023 FU ONR; NASA [NNX07AL72G] FX We would like to thank the International Space Science Institute, Bern, Switzerland, for the hospitality provided to our team studying the Role of Current Sheets in Solar Eruptive Phenomena, where many of the ideas presented in this work have been discussed. S. T. S. thanks the Ulysses/SWOOPS instrument team for its long support of his research and the Osservatorio Astrofisico di Arcetri for its hospitality while much of this paper was being written. Y. K. K. acknowledges the support by ONR and NASA grant NNX07AL72G. NR 38 TC 26 Z9 26 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD APR 24 PY 2009 VL 114 AR A04103 DI 10.1029/2008JA013704 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 438EQ UT WOS:000265539100002 ER PT J AU Wu, EYS Ade, P Bock, J Bowden, M Brown, ML Cahill, G Castro, PG Church, S Culverhouse, T Friedman, RB Ganga, K Gear, WK Gupta, S Hinderks, J Kovac, J Lange, AE Leitch, E Melhuish, SJ Memari, Y Murphy, JA Orlando, A Piccirillo, L Pryke, C Rajguru, N Rusholme, B Schwarz, R O'Sullivan, C Taylor, AN Thompson, KL Turner, AH Zemcov, M AF Wu, E. Y. S. Ade, P. Bock, J. Bowden, M. Brown, M. L. Cahill, G. Castro, P. G. Church, S. Culverhouse, T. Friedman, R. B. Ganga, K. Gear, W. K. Gupta, S. Hinderks, J. Kovac, J. Lange, A. E. Leitch, E. Melhuish, S. J. Memari, Y. Murphy, J. A. Orlando, A. Piccirillo, L. Pryke, C. Rajguru, N. Rusholme, B. Schwarz, R. O'Sullivan, C. Taylor, A. N. Thompson, K. L. Turner, A. H. Zemcov, M. CA QUaD Collaboration TI Parity Violation Constraints Using Cosmic Microwave Background Polarization Spectra from 2006 and 2007 Observations by the QUaD Polarimeter SO PHYSICAL REVIEW LETTERS LA English DT Article ID LORENTZ; PROBE; CMB AB We constrain parity-violating interactions to the surface of last scattering using spectra from the QUaD experiment's second and third seasons of observations by searching for a possible systematic rotation of the polarization directions of cosmic microwave background photons. We measure the rotation angle due to such a possible "cosmological birefringence" to be 0.55 degrees +/- 0.82 degrees (random) +/- 0.5 degrees (systematic) using QUaD's 100 and 150 GHz temperature-curl and gradient-curl spectra over the spectra over the multipole range 200
80 eV, providing for the first time direct evidence of the stark temperature disparity between the two sides of an astrophysical CD and constraining the role of magnetic fields and heat conduction accordingly. Two colliding-wind binaries are noted to have similar RRCs suggesting a temperature jump, and CD crossing by ions may be a common feature of stellar-wind shocks. C1 [Nordon, Raanan; Behar, Ehud; Soker, Noam] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel. [Kastner, Joel H.; Yu, Young Sam] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA. [Behar, Ehud] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Nordon, R (reprint author), Max Planck Inst Extraterr Phys, Postfach 1312, D-85741 Garching, Germany. EM nordon@mpe.mpg.de; behar@milkyway.gsfc.nasa.gov; soker@physics.technion.ac.il; jhkpci@cis.rit.edu; yxy7181@cis.rit.edu FU NASA [GO5-6008X, NAS8-03060] FX We thank A. Laor, M. Leutenegger, and J. Raymond for useful discussions and comments. The research at Rochester Institute of Technology was supported by NASA through Chandra award GO5-6008X issued by the Chandra X-ray observatory center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. NR 40 TC 3 Z9 3 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2009 VL 695 IS 2 BP 834 EP 843 DI 10.1088/0004-637X/695/2/834 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430VS UT WOS:000265018300005 ER PT J AU Geballe, TR Saumon, D Golimowski, DA Leggett, SK Marley, MS Noll, KS AF Geballe, T. R. Saumon, D. Golimowski, D. A. Leggett, S. K. Marley, M. S. Noll, K. S. TI SPECTROSCOPIC DETECTION OF CARBON MONOXIDE IN TWO LATE-TYPE T DWARFS SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: general; stars: individual (Gliese 570D, 2MASS J09373487+2931409); stars: low-mass, brown dwarfs ID GLIESE 229B; BROWN DWARFS; SPECTRAL CLASSIFICATION; ATMOSPHERIC CHEMISTRY; CHEMICAL-EQUILIBRIUM; ULTRACOOL DWARFS; SOLAR-SYSTEM; ABUNDANCES; PHOTOMETRY; JUPITER AB M-band spectra of two late-type T dwarfs, 2MASS J09373487+2931409, and Gliese 570D, confirm evidence from photometry that photospheric carbon monoxide (CO) is present at abundance levels far in excess of those predicted from chemical equilibrium. These new and unambiguous detections of CO, together with an earlier spectroscopic detection of CO in Gliese 229B and existing M-band photometry of a large selection of T dwarfs, suggest that vertical mixing in the photosphere drives the CO abundance out of chemical equilibrium and is a common, and likely universal feature of mid-to-late-type T dwarfs. The M-band spectra allow determinations of the timescale of vertical mixing in the radiative region of the atmosphere of each object, the first such measurements of this important parameter in late T dwarfs. A detailed analysis of the spectral energy distribution of 2MASS J09373487+2931409 results in the following values for metallicity, temperature, surface gravity, and luminosity: [M/H] similar to -0.3, T(eff) = 925-975 K, log g = 5.20-5.47, and log L/L(circle dot) = -5.308 +/- 0.027. The age is 3-10 Gyr and the mass is in the range 45-69 M(Jup). C1 [Geballe, T. R.; Leggett, S. K.] Gemini Observ, Hilo, HI 96720 USA. [Saumon, D.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Golimowski, D. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Marley, M. S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Noll, K. S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Geballe, TR (reprint author), Gemini Observ, 670 N Aohoku Pl, Hilo, HI 96720 USA. EM tgeballe@gemini.edu RI Noll, Keith/C-8447-2012; Marley, Mark/I-4704-2013 NR 47 TC 34 Z9 34 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2009 VL 695 IS 2 BP 844 EP 854 DI 10.1088/0004-637X/695/2/844 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430VS UT WOS:000265018300006 ER PT J AU Jung, YD AF Jung, Young-Dae TI RESONANT COMPTON SCATTERING IN NONTHERMAL ASTROPHYSICAL PLASMAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic data; atomic processes; plasmas ID DEBYE LENGTH; ELECTRONS AB The nonthermal effect on the resonant Compton scattering process is investigated in Lorentzian astrophysical plasmas. The screened atomic wave functions and energies for the hydrogenic ion in Lorentzian plasmas are obtained by the Rayleigh-Ritz variational method. The resonance Compton scattering cross section in Lorentzian plasmas is also obtained as a function of the spectral index and plasma parameters by the photon-perturbation Hamiltonian in the dipole representation. It is shown that the nonthermal character of the Lorentzian plasma enhances the resonant Compton scattering cross section. In addition, the nonthermal effect on the cross section is found to be more significant in plasmas with higher densities. C1 [Jung, Young-Dae] Hanyang Univ, Dept Appl Phys, Ansan 426791, Kyunggi Do, South Korea. [Jung, Young-Dae] NASA, George C Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. RP Jung, YD (reprint author), Hanyang Univ, Dept Appl Phys, Ansan 426791, Kyunggi Do, South Korea. EM ydjung@hanyang.ac.kr FU Korean Government [KRF-2007-313-C00169] FX The author gratefully acknowledges S. L. O'Dell and M. Weisskopf for useful discussions and warm hospitality while visiting NASA/Marshall Space Flight Center. The author would like to thank S. Federman and the anonymous referee for suggesting improvements to this text. This work was supported by the Korea Research Foundation Grant funded by the Korean Government (MOEHRD, Basic Research Promotion Fund; KRF-2007-313-C00169). NR 19 TC 11 Z9 11 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2009 VL 695 IS 2 BP 917 EP 920 DI 10.1088/0004-637X/695/2/917 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430VS UT WOS:000265018300013 ER PT J AU Birn, J Fletcher, L Hesse, M Neukirch, T AF Birn, J. Fletcher, L. Hesse, M. Neukirch, T. TI ENERGY RELEASE AND TRANSFER IN SOLAR FLARES: SIMULATIONS OF THREE-DIMENSIONAL RECONNECTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE MHD; Sun: corona; Sun: magnetic fields ID X-RAY SOURCES; MAGNETIC RECONNECTION; FLUX ROPES; CHROMOSPHERIC EVAPORATION; PARTICLE-ACCELERATION; EMISSION MEASURE; ACTIVE-REGION; ALFVEN WAVES; TEMPERATURE; EVOLUTION AB Using three-dimensional magnetohydrodynamic simulations we investigate energy release and transfer in a three-dimensional extension of the standard two-ribbon flare picture. In this scenario, reconnection is initiated in a thin current sheet (suggested to form below a departing coronal mass ejection) above a bipolar magnetic field. Two cases are contrasted: an initially force-free current sheet (low beta) and a finite-pressure current sheet (high beta), where beta represents the ratio between gas (plasma) and magnetic pressure. The energy conversion process from reconnection consists of incoming Poynting flux turned into up-and downgoing Poynting flux, enthalpy flux, and bulk kinetic energy flux. In the low-beta case, the outgoing Poynting flux is the dominant contribution, whereas the outgoing enthalpy flux dominates in the high-beta case. The bulk kinetic energy flux is only a minor contribution in the downward direction. The dominance of the downgoing Poynting flux in the low-beta case is consistent with an alternative to the thick target electron beam model for solar flare energy transport, suggested recently by Fletcher & Hudson, whereas the enthalpy flux may act as an alternative transport mechanism. For plausible characteristic parameters of the reconnecting field configuration, we obtain energy release timescales and energy output rates that compare favorably with those inferred from observations for the impulsive phase of flares. Significant enthalpy flux and heating are found even in the initially force-free case with very small background beta, resulting mostly from adiabatic compression rather than Ohmic dissipation. The energy conversion mechanism is most easily understood as a two-step process (although the two steps may occur essentially simultaneously): the first step is the acceleration of the plasma by Lorentz forces in layers akin to the slow shocks in the Petschek reconnection model, involving the conversion of magnetic energy to bulk kinetic energy. However, due to pressure gradient forces that oppose the Lorentz forces in approximate, or partial force balance, the accelerated plasma becomes slowed down and compressed, whereby the bulk kinetic energy is converted to heat, either locally deposited or transported away by enthalpy flux and deposited later. This mechanism is most relevant in the downflow region, which is more strongly governed by force balance; it is less important in the outflow above the reconnection site, where more energy remains in the form of fast bulk flow. C1 [Birn, J.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Fletcher, L.] Univ Glasgow, Glasgow G12 8QQ, Lanark, Scotland. [Hesse, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Neukirch, T.] Univ St Andrews, St Andrews KY16 9AJ, Fife, Scotland. RP Birn, J (reprint author), Los Alamos Natl Lab, POB 1663, Los Alamos, NM 87545 USA. EM jbirn@lanl.gov RI Neukirch, Thomas/C-1981-2009; Hesse, Michael/D-2031-2012; NASA MMS, Science Team/J-5393-2013 OI Neukirch, Thomas/0000-0002-7597-4980; NASA MMS, Science Team/0000-0002-9504-5214 FU US Department of Energy; NASA; UK STFC [ST/F002637]; European Commission [MTRNCT-2006-035484] FX This work was conducted under the auspices of the US Department of Energy, supported by NASA through its Heliophysic Theory, Living With a Star, and Supporting Research and Technology programs. L. F. and T.N. acknowledges support by the UK STFC under rolling grant ST/F002637 and by the European Commission through the SOLAIRE Network (MTRNCT-2006-035484). NR 45 TC 30 Z9 30 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2009 VL 695 IS 2 BP 1151 EP 1162 DI 10.1088/0004-637X/695/2/1151 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430VS UT WOS:000265018300034 ER PT J AU Vanzella, E Giavalisco, M Dickinson, M Cristiani, S Nonino, M Kuntschner, H Popesso, P Rosati, P Renzini, A Stern, D Cesarsky, C Ferguson, HC Fosbury, RAE AF Vanzella, E. Giavalisco, M. Dickinson, M. Cristiani, S. Nonino, M. Kuntschner, H. Popesso, P. Rosati, P. Renzini, A. Stern, D. Cesarsky, C. Ferguson, H. C. Fosbury, R. A. E. CA GOODS Team TI SPECTROSCOPIC OBSERVATIONS OF LYMAN BREAK GALAXIES AT REDSHIFTS similar to 4, 5, AND 6 IN THE GOODS-SOUTH FIELD SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: distances and redshifts; galaxies: evolution; galaxies: formation ID HUBBLE-SPACE-TELESCOPE; STAR-FORMING GALAXIES; ORIGINS DEEP SURVEY; LY-ALPHA EMISSION; REST-FRAME ULTRAVIOLET; FORMATION HISTORY; VLT/FORS2 SPECTROSCOPY; LUMINOSITY FUNCTIONS; STELLAR POPULATIONS; RADIATION TRANSFER AB We report on observations of Lyman break galaxies (LBGs) selected from the Great Observatories Origins Deep Survey at mean redshifts z similar to 4, 5, and 6 (B(435-), V(606-), and i(775)-band dropouts, respectively), obtained with the red-sensitive FORS2 spectrograph at the ESO VLT. This program has yielded spectroscopic identifications for 114 galaxies (similar to 60% of the targeted sample), of which 51 are at z similar to 4, 31 at z similar to 5, and 32 at z similar to 6. We demonstrate that the adopted selection criteria are effective, identifying galaxies at the expected redshift with minimal foreground contamination. Of the 10% interlopers, 83% turn out to be Galactic stars. Once selection effects are properly accounted for, the rest-frame ultraviolet (UV) spectra of the higher redshift LBGs appear to be similar to their counterparts at z similar to 3. As at z similar to 3, LBGs at z similar to 4 and z similar to 5 are observed with Ly alpha both in emission and in absorption; when in absorption, strong interstellar lines are also observed in the spectra. The stacked spectra of Lya absorbers and emitters also show that the former have redder UV spectra and stronger but narrower interstellar lines, a fact also observed at z similar to 2 and 3. At z similar to 6, sensitivity issues bias our sample toward galaxies with Ly alpha in emission; nevertheless, these spectra appear to be similar to their lower redshift counterparts. As in other studies at similar redshifts, we find clear evidence that brighter LBGs tend to have weaker Ly alpha emission lines. At fixed rest-frame UV luminosity, the equivalent width of the Ly alpha emission line is larger at higher redshifts. At all redshifts where the measurements can be reliably made, the redshift of the Ly alpha emission line turns out to be larger than that of the interstellar absorption lines (ISLs), with a median velocity difference Delta V similar to 400 km s(-1) at z similar to 4 and 5, consistent with results at lower redshifts. This shows that powerful, large-scale winds are common at high redshift. In general, there is no strong correlation between the morphology of the UV light and the spectroscopic properties. However, galaxies with deep ISLs and strong Ly alpha absorption appear to be more diffuse than galaxies with Ly alpha in emission. C1 [Vanzella, E.; Cristiani, S.; Nonino, M.] INAF Osservatorio Astron Trieste, I-40131 Trieste, Italy. [Giavalisco, M.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Dickinson, M.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Cristiani, S.] Natl Inst Nucl Phys, Ist Nazl Fis Nucl, I-34127 Trieste, Italy. [Kuntschner, H.; Fosbury, R. A. E.] ST EFC, D-85748 Garching, Germany. [Popesso, P.; Rosati, P.; Cesarsky, C.] ESO, D-85748 Garching, Germany. [Renzini, A.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy. [Stern, D.] CALTECH, JPL, Pasadena, CA 91109 USA. [Ferguson, H. C.] STScI, Baltimore, MD 21218 USA. RP Vanzella, E (reprint author), INAF Osservatorio Astron Trieste, Via GB Tiepolo 11, I-40131 Trieste, Italy. OI Fosbury, Robert/0000-0001-9975-8003; Cristiani, Stefano/0000-0002-2115-5234; Kuntschner, Harald/0000-0002-2768-1198 FU NASA; [ASI/COFIN I/016/07/0]; [PRIN INAF 2007] FX We are grateful to the ESO staff in Paranal and Garching who greatly helped in the development of this programme. We acknowledge financial contribution from contract ASI/COFIN I/016/07/0 and PRIN INAF 2007 "A Deep VLT and LBT view of the Early Universe." E. V. thanks STScI and NOAO for hospitality during a visit in which this paper was conceived and partially written. E. V. thanks F. Calura for useful discussions about the dust properties of high-redshift galaxies. The work of D. S. was carried out at Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 91 TC 134 Z9 134 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2009 VL 695 IS 2 BP 1163 EP 1182 DI 10.1088/0004-637X/695/2/1163 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430VS UT WOS:000265018300035 ER PT J AU Fukumura, K Kazanas, D Stephenson, G AF Fukumura, Keigo Kazanas, Demosthenes Stephenson, Gordon TI QUASI-PERIODIC OSCILLATIONS FROM RANDOM X-RAY BURSTS AROUND ROTATING BLACK HOLES SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; stars: oscillations; X-rays: galaxies ID ADVECTION-DOMINATED ACCRETION; ENERGY EXTRACTION; GRO J1655-40; BINARIES; PRECESSION; DISCOVERY; MODELS; PLASMA; FLOWS; DISK AB We continue our earlier studies of quasi-periodic oscillations (QPOs) in the power spectra of accreting, rapidly rotating black holes that originate from the geometric "light echoes" of X-ray flares occurring within the black hole ergosphere. Our present work extends our previous treatment to three-dimensional photon emission and orbits to allow for arbitrary latitudes in the positions of the distant observers and the X-ray sources in place of the mainly equatorial positions and photon orbits of the earlier consideration. Following the trajectories of a large number of photons, we calculate the response functions of a given geometry and use them to produce model light curves which we subsequently analyze to compute their power spectra and autocorrelation functions. In the case of an optically thin environment, relevant to advection-dominated accretion flows, we consistently find QPOs at frequencies on the order of similar to kHz for stellar-mass black hole candidates, while on the order of similar to mHz for typical active galactic nuclei (similar to 10(7)M(circle dot)) for a wide range of viewing angles (30 degrees-80 degrees) from X-ray sources predominantly concentrated toward the equator within the ergosphere. As in our previous treatment, here too, the QPO signal is produced by the frame-dragging of the photons by the rapidly rotating black hole, which results in photon "bunches" separated by constant time lags, the result of multiple photon orbits around the hole. Our model predicts for various source/observer configurations the robust presence of a new class of QPOs, which is inevitably generic to a curved spacetime structure in rotating black hole systems. C1 [Fukumura, Keigo] UMBC CRESST, Baltimore, MD 21250 USA. [Fukumura, Keigo; Kazanas, Demosthenes] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Stephenson, Gordon] Univ Calif San Diego, La Jolla, CA 92093 USA. RP Fukumura, K (reprint author), UMBC CRESST, Baltimore, MD 21250 USA. EM Keigo.Fukumura@nasa.gov NR 37 TC 5 Z9 5 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2009 VL 695 IS 2 BP 1199 EP 1209 DI 10.1088/0004-637X/695/2/1199 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430VS UT WOS:000265018300038 ER PT J AU Rawat, A Wadadekar, Y De Mello, D AF Rawat, Abhishek Wadadekar, Yogesh De Mello, Dulia TI REST-FRAME UV VERSUS OPTICAL MORPHOLOGIES OF GALAXIES USING SERSIC PROFILE FITTING: THE IMPORTANCE OF MORPHOLOGICAL K-CORRECTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: statistics ID STAR-FORMING GALAXIES; LYMAN-BREAK GALAXIES; ORIGINS DEEP SURVEY; MERGER RATE; FIELD; Z-SIMILAR-TO-3; PARALLELS; REDSHIFTS; EVOLUTION AB We show a comparison of the rest-frame UV morphologies of a sample of 162 intermediate-redshift (z(median) = 1.02) galaxies with their rest-frame optical morphologies. We select our sample from the deepest near-UV image obtained with the Hubble Space Telescope (HST) using the Wide Field Planetary Camera 2 (WFPC2; F300W) as part of the parallel observations of the Hubble Ultra Deep Field campaign overlapping with the HST/ACS Great Observatories Origins Deep Survey data set. We perform single-component Sersic fits in both WFPC2/F300W (rest-frame UV) and ACS/F850LP (rest-frame optical) bands and deduce that the Sersic index n is estimated to be smaller in the rest-frame UV compared to the rest-frame optical, leading to an overestimation of the number of merger candidates by similar to 40%-100% compared to the rest-frame optical depending upon the cutoff in n employed for identifying merger candidates. This effect seems to be dominated by galaxies with low values of n(F300W) <= 0.5 that have a value of n(F850LP) similar to 1.0. We argue that these objects are probably clumpy star-forming galaxies or minor mergers, both of which are essentially contaminants, if one is interested in identifying major mergers. In addition, we also find evidence that the axis ratio b/a is lower, i.e., ellipticity (1-b/a) is higher in rest-frame UV compared to the rest-frame optical. Moreover, we find that in the rest-frame UV, the number of high ellipticity (e >= 0.8) objects are higher by a factor of similar to 2.8 compared to the rest-frame optical. This indicates that the reported dominance of elongated morphologies among high-z Lyman Break Galaxies might just be a bias related to the use of rest-frame UV data sets in high-z studies. C1 [Rawat, Abhishek] Inter Univ Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. [Wadadekar, Yogesh] Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [De Mello, Dulia] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [De Mello, Dulia] Catholic Univ Amer, Washington, DC 20064 USA. [De Mello, Dulia] Johns Hopkins Univ, Baltimore, MD 21218 USA. RP Rawat, A (reprint author), Inter Univ Ctr Astron & Astrophys, Post Bag 4, Pune 411007, Maharashtra, India. EM rawat@iucaa.ernet.in NR 18 TC 7 Z9 7 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2009 VL 695 IS 2 BP 1315 EP 1326 DI 10.1088/0004-637X/695/2/1315 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430VS UT WOS:000265018300048 ER PT J AU Novak, G Dotson, JL Li, H AF Novak, G. Dotson, J. L. Li, H. TI DISPERSION OF OBSERVED POSITION ANGLES OF SUBMILLIMETER POLARIZATION IN MOLECULAR CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: magnetic fields; polarization; stars: formation; submillimeter ID MAGNETIC-FIELD STRENGTHS; FAR-INFRARED POLARIMETRY; STAR-FORMATION; DUST EMISSION; DARK CLOUDS; TURBULENCE; CORES; MODELS; SPARO; HERTZ AB One can estimate the characteristic magnetic field strength in Giant Molecular Clouds (GMCs) by comparing submillimeter polarimetric observations of these sources with simulated polarization maps developed using a range of different values for the assumed field strength. The point of comparison is the degree of order in the distribution of polarization position angles. In a recent paper by H. Li and collaborators, such a comparison was carried out using SPARO observations of two GMCs, and employing simulations by E. Ostriker and collaborators. Here, we re-examine this same question, using the same data set and the same simulations, but using an approach that differs in several respects. The most important difference is that we incorporate new, higher angular resolution observations for one of the clouds, obtained using the Hertz polarimeter. We conclude that the agreement between observations and simulations is best when the total magnetic energy (including both uniform and fluctuating field components) is at least as large as the turbulent kinetic energy. C1 [Novak, G.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Dotson, J. L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Li, H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Novak, G (reprint author), Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. EM g-novak@northwestern.edu FU SPARO [OPP-01-30389]; Hertz [AST-02-04886]; Caltech Submillimeter Observatory [AST-05-40882] FX This work has benefited from illuminating discussions with R. Hildebrand and A. Lazarian. We are also grateful to E. Ostriker for providing the unpublished simulation, to P. Calisse for operating SPARO, and to the N. S. F. for supporting SPARO (Award OPP-01-30389 to Northwestern University), Hertz (Award AST-02-04886 to the University of Chicago), and the Caltech Submillimeter Observatory (Award AST-05-40882 to Caltech). NR 30 TC 16 Z9 16 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2009 VL 695 IS 2 BP 1362 EP 1369 DI 10.1088/0004-637X/695/2/1362 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430VS UT WOS:000265018300053 ER PT J AU Leggett, SK Cushing, MC Saumon, D Marley, MS Roellig, TL Warren, SJ Burningham, B Jones, HRA Kirkpatrick, JD Lodieu, N Lucas, PW Mainzer, AK Martin, EL McCaughrean, MJ Pinfield, DJ Sloan, GC Smart, RL Tamura, M Van Cleve, J AF Leggett, S. K. Cushing, Michael C. Saumon, D. Marley, M. S. Roellig, T. L. Warren, S. J. Burningham, Ben Jones, H. R. A. Kirkpatrick, J. D. Lodieu, N. Lucas, P. W. Mainzer, A. K. Martin, E. L. McCaughrean, M. J. Pinfield, D. J. Sloan, G. C. Smart, R. L. Tamura, M. Van Cleve, J. TI THE PHYSICAL PROPERTIES OF FOUR similar to 600 K T DWARFS SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: atmospheres; stars: individual (ULAS J003402.77-005206.7, ULAS J133553.45+113005.2, 2MASS J09393548-2448279, CFBD J005910.82-011401.3); stars: low-mass, brown dwarfs ID SPITZER-SPACE-TELESCOPE; EXOPLANET HOST STAR; DIGITAL SKY SURVEY; BROWN DWARF; SPECTRAL CLASSIFICATION; CHEMICAL-EQUILIBRIUM; ULTRACOOL DWARFS; GLIESE 229B; PHOTOMETRY; 2MASS AB We present Spitzer 7.6-14.5 mu m spectra of ULAS J003402.77-005206.7 and ULAS J133553.45+113005.2, two T9 dwarfs with the latest spectral types currently known. We fit synthetic spectra and photometry to the near-through mid-infrared energy distributions of these dwarfs and that of the T8 dwarf 2MASS J09393548-2448279. We also analyze near-infrared data for another T9, CFBD J005910.82-011401.3. We find that the ratio of the mid-to near-infrared fluxes is very sensitive to effective temperature at these low temperatures, and that the 2.2 mu m and 4.5 mu m fluxes are sensitive to metallicity and gravity; increasing gravity has a similar effect to decreasing metallicity, and vice versa, and there is a degeneracy between these parameters. The 4.5 mu m and 10 mu m fluxes are also sensitive to vertical transport of gas through the atmosphere, which we find to be significant for these dwarfs. The full near-through mid-infrared spectral energy distribution allows us to constrain the effective temperature (K)/gravity (ms(2))/metallicity ([m/H] dex) of ULAS J0034-00 and ULAS J1335+11 to 550-600/100-300/0.0-0.3 and 500-550/100-300/0.0-0.3, respectively. These fits imply low masses and young ages for the dwarfs of 5-20 M(Jupiter) and 0.1-2 Gyr. The fits to 2MASS J0939-24 are in good agreement with the measured distance, the observational data, and the earlier T8 near-infrared spectral type if it is a slightly metal-poor 4-10 Gyr old system consisting of a 500 K and 700 K, similar to 25 M(Jupiter) and similar to 40 M(Jupiter), pair, although it is also possible that it is an identical pair of 600 K, 30 M(Jupiter), dwarfs. As no mid-infrared data are available for CFBD J0059-01 its properties are less well constrained; nevertheless it appears to be a 550-600 K dwarf with g = 300-2000 ms(-2) and [m/H] = 0-0.3 dex. These properties correspond to mass and age ranges of 10-50 M(Jupiter) and 0.5-10 Gyr for this dwarf. C1 [Leggett, S. K.] Gemini Observ, Hilo, HI 96720 USA. [Cushing, Michael C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Saumon, D.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Marley, M. S.; Roellig, T. L.] NASA, Ames Res Ctr, Moffett Field, CA 94305 USA. [Warren, S. J.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England. [Burningham, Ben; Jones, H. R. A.; Lucas, P. W.; Pinfield, D. J.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Kirkpatrick, J. D.] CALTECH, IPAC, Pasadena, CA 91125 USA. [Lodieu, N.; Martin, E. L.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain. [Mainzer, A. K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Martin, E. L.] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA. [McCaughrean, M. J.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Sloan, G. C.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Smart, R. L.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, TO, Italy. [Tamura, M.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Van Cleve, J.] Ball Aerosp & Technol Corp, Boulder, CO 80301 USA. RP Leggett, SK (reprint author), Gemini Observ, 670 N Aohoku Pl, Hilo, HI 96720 USA. EM sleggett@gemini.edu RI Marley, Mark/I-4704-2013; OI Burningham, Ben/0000-0003-4600-5627; Smart, Richard/0000-0002-4424-4766; Jones, Hugh/0000-0003-0433-3665 FU NASA; Association of Universities for Research in Astronomy, Inc; Spanish Ministry of Science [AYA2007-67458] FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. S.K.L.'s research is supported by the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., on behalf of the international Gemini partnership of Argentina, Australia, Brazil, Canada, Chile, the United Kingdom, and the United States of America. E.L.M.'s research is supported by The Spanish Ministry of Science via project AYA2007-67458. NR 45 TC 52 Z9 52 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2009 VL 695 IS 2 BP 1517 EP 1526 DI 10.1088/0004-637X/695/2/1517 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430VS UT WOS:000265018300066 ER PT J AU Ziurys, LM Tenenbaum, ED Pulliam, RL Woolf, NJ Milam, SN AF Ziurys, L. M. Tenenbaum, E. D. Pulliam, R. L. Woolf, N. J. Milam, S. N. TI CARBON CHEMISTRY IN THE ENVELOPE OF VY CANIS MAJORIS: IMPLICATIONS FOR OXYGEN-RICH EVOLVED STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; circumstellar matter; radio lines: stars; stars: AGB and post-AGB; supergiants ID GIANT BRANCH STARS; MASS-LOSS-RATE; CIRCUMSTELLAR ENVELOPES; BEARING MOLECULES; ROTATIONAL-EXCITATION; AGB STARS; O-RICH; SOLAR NEIGHBORHOOD; LINE EMISSION; 1ST DETECTION AB Observations of the carbon-bearing molecules CO, HCN, CS, HNC, CN, and HCO(+) have been conducted toward the circumstellar envelope of the oxygen-rich red supergiant star, VY Canis Majoris (VY CMa), using the Arizona Radio Observatory (ARO). CO and HCN were also observed toward the O-rich shells of NML Cyg, TX Cam, IK Tau, and W Hya. Rotational transitions of these species at 1 mm, 0.8 mm, and 0.4 mm were measured with the ARO Submillimeter Telescope, including the J = 6 -> 5 line of CO at 691 GHz toward TX Cam and W Hya. The ARO 12 m was used for 2 mm and 3 mm observations. Four transitions were observed for HCO+ in VY CMa, the first definitive identification of this ion in a circumstellar envelope. Molecular line profiles from VY CMa are complex, indicating three separate outflows: a roughly spherical flow and separate red- and blueshifted winds, as suggested by earlier observations. Spectra from the other sources appear to trace a single outflow component. The line data were modeled with a radiative transfer code to establish molecular abundances relative to H(2) and source distributions. Abundances for CO derived for these objects vary over an order of magnitude, f similar to 0.4-5 x 10(-4), with the lower values corresponding to the supergiants. For HCN, a similar range in abundance is found (f similar to 0.9- 9 x 10(-6)), with no obvious dependence on the mass-loss rate. In VY CMa, HCO+ is present in all three outflows with f similar to 0.4-1.6 x 10(-8) and a spatial extent similar to that of CO. HNC is found only in the red- and blueshifted components with [HCN]/[ HNC] similar to 150-190, while [CN]/[HCN] similar to 0.01 in the spherical flow. All three velocity components are traced in CS, which has a confined spatial distribution and f similar to 2-6 x 10(-7). These observations suggest that carbon-bearing molecules in O-rich shells are produced by a combination of photospheric shocks and photochemistry. Shocks may play a more prominent role in the supergiants because of their macroturbulent velocities. C1 [Ziurys, L. M.; Tenenbaum, E. D.; Pulliam, R. L.; Woolf, N. J.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Ziurys, L. M.; Tenenbaum, E. D.; Pulliam, R. L.; Woolf, N. J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Ziurys, L. M.; Tenenbaum, E. D.; Pulliam, R. L.] Univ Arizona, Dept Chem, Tucson, AZ 85721 USA. [Ziurys, L. M.] Univ Arizona, Arizona Radio Observ, Tucson, AZ 85721 USA. [Milam, S. N.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. RP Ziurys, LM (reprint author), Univ Arizona, Dept Astron, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM lziurys@as.arizona.edu; emilyt@as.arizona.edu; rpulliam@email.arizona.edu; nwoolf@as.arizona.edu; Stefanie.N.Milam@nasa.gov RI Milam, Stefanie/D-1092-2012 OI Milam, Stefanie/0000-0001-7694-4129 FU NSF [AST-06-07803]; NASA Astrobiology Institute [CAN-02-0SS02] FX This research is supported by NSF Grant AST-06-07803 and the NASA Astrobiology Institute under cooperative agreement CAN-02-0SS02 issued through the Office of Space Science. E. D. T. thanks the NSF for her graduate fellowship. The authors also thank the staff of the ARO for their assistance, and Eugene Lauria for his efforts in providing the newARO 0.4 mm receiver. NR 56 TC 30 Z9 30 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2009 VL 695 IS 2 BP 1604 EP 1613 DI 10.1088/0004-637X/695/2/1604 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430VS UT WOS:000265018300074 ER PT J AU Dodson-Robinson, SE Bodenheimer, P AF Dodson-Robinson, Sarah E. Bodenheimer, Peter TI DISCOVERING THE GROWTH HISTORIES OF EXOPLANETS: THE SATURN ANALOG HD 149026b SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE methods: analytical; planetary systems: formation; planetary systems: protoplanetary disks; planets and satellites: formation ID TRANSITING EXTRASOLAR PLANETS; GIANT PLANETS; CORE ACCRETION; PROTOSTELLAR DISKS; SOLAR NEBULA; JUPITER; MIGRATION; MODELS; STARS; GAS AB The transiting "hot Saturn" HD149026b, which has the highest mean density of any confirmed planet in the Neptune Jupiter mass range, has challenged theories of planet formation since its discovery in 2005. Previous investigations could not explain the origin of the planet's 45-110 Earth-mass solid core without invoking catastrophes such as gas giant collisions or heavy planetesimal bombardment launched by neighboring planets. Here we show that HD 149026b's large core can be successfully explained by the standard core accretion theory of planet formation. The keys to our reconstruction of HD 149026b are (1) applying a model of the solar nebula to describe the protoplanet nursery, (2) placing the planet initially on a long-period orbit at Saturn's heliocentric distance of 9.5 AU, and (3) adjusting the solid mass in the HD 149026 disk to twice that of the solar nebula in accordance with the star's heavy element enrichment. We show that the planet's migration into its current orbit at 0.042 AU is consistent with our formation model. Our study of HD 149026b demonstrates that it is possible to discover the growth history of any planet with a well-defined core mass that orbits a solar-type star. C1 [Dodson-Robinson, Sarah E.] CALTECH, Exoplanet Sci Inst, NASA, Pasadena, CA 91125 USA. [Bodenheimer, Peter] Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA. RP Dodson-Robinson, SE (reprint author), CALTECH, Exoplanet Sci Inst, NASA, 770 S Wilson Ave, Pasadena, CA 91125 USA. EM sdr@ipac.caltech.edu FU NASA Origins [NNX08AH82G] FX Support for S. D. R's work was provided by NASA through the Spitzer Space Telescope Fellowship Program. P. B. received support from the NASA Origins Grant NNX08AH82G. The authors thank Chas Beichman for helpful comments. NR 39 TC 9 Z9 9 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 20 PY 2009 VL 695 IS 2 BP L159 EP L162 DI 10.1088/0004-637X/695/2/L159 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 428TE UT WOS:000264872100008 ER PT J AU Gosling, JT McComas, DJ Roberts, DA Skoug, RM AF Gosling, J. T. McComas, D. J. Roberts, D. A. Skoug, R. M. TI A ONE-SIDED ASPECT OF ALFVENIC FLUCTUATIONS IN THE SOLAR WIND SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE magnetic fields; plasmas; solar wind; turbulence; waves ID TURBULENCE; WAVES; RECONNECTION; MODEL AB Using Advanced Composition Explorer (ACE) 64 s data at 1 AU we find that Alfvenic fluctuations propagating outward from the Sun along the magnetic field, B, in the solar wind often produce one-sided variations in one of the equatorial components of Band velocity, V. This is a natural consequence of the fact that the Alfvenic fluctuations are transverse fluctuations in which |B| remains nearly constant. Thus, fluctuations in the field component that defines the underlying background field direction are always relative to a base value rather than to an average value. This suggests that conclusions derived from statistical analyses of fluctuations in the solar wind that assume the fluctuations in all field components are relative to average values need to be re-examined. We also find that discrete, sunward-propagating Alfvenic fluctuations or rotational discontinuities are extremely rare in the pristine solar wind; thus far we have identified such discrete events in ACE data only in association with events identified as magnetic reconnection exhausts and/or in association with backstreaming ions from reverse shocks, including Earth's bow shock. C1 [Gosling, J. T.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA. [McComas, D. J.] SW Res Inst, San Antonio, TX 78228 USA. [Roberts, D. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Skoug, R. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RP Gosling, JT (reprint author), Univ Colorado, Atmospher & Space Phys Lab, 1234 Innovat Dr, Boulder, CO 80303 USA. EM jack.gosling@lasp.colorado.edu FU NASA [NNG06GC27G]; NASA/ACE program FX J. G. thanks A. Balogh, J. Borovsky, T. Horbury, B. Matthaeus, M. Neugebauer, C. Smith, and M. Velli, for a number of stimulating conversations on one or more of the topics of this paper, C. Smith for use of the magnetometer data, and M. Desai for providing energetic particle observations. This work has been supported by NASA grant NNG06GC27G and the SWEPAM portion of the NASA/ACE program. NR 19 TC 23 Z9 24 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 20 PY 2009 VL 695 IS 2 BP L213 EP L216 DI 10.1088/0004-637X/695/2/L213 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 428TE UT WOS:000264872100020 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 X-RAY SPECTRAL VARIATIONS IN THE YOUNGEST GALACTIC SUPERNOVA REMNANT G1.9+0.3 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: individual (G1.9+0.3); supernova remnants; X-rays: ISM ID SHOCK ACCELERATION; HIGH-ENERGY; GRAINS AB The discovery of the youngest Galactic supernova remnant (SNR) G1.9+0.3 has allowed a look at a stage of SNR evolution never before observed. We analyze the 50 ks Chandra observation with particular regard to spectral variations. The very high column density (N(H) similar to 6 x 10(22) cm(-2)) implies that dust scattering is important, and we use a simple scattering model in our spectral analysis. The integrated X-ray spectrum of G1.9+0.3 is well described by synchrotron emission from a power-law electron distribution with an exponential cutoff. Using our measured radio flux and including scattering effects, we find a rolloff frequency of 5.4(3.0, 10.2) x 10(17) Hz (h nu(roll) = 2.2 keV). Including scattering in a two-region model gives lower values of nu(roll) by over a factor of 2. Dividing G1.9+0.3 into six regions, we find a systematic pattern in which spectra are hardest (highest nu(roll)) in the bright southeast and northwest limbs of the shell. They steepen as one moves around the shell or into the interior. The extensions beyond the bright parts of the shell have the hardest spectra of all. We interpret the results in terms of dependence of shock acceleration properties on the obliquity angle theta(Bn) between the shock velocity and a fairly uniform upstream magnetic field. This interpretation probably requires a Type Ia event. If electron acceleration is limited by synchrotron losses, the spectral variations require obliquity-dependence of the acceleration rate independent of the magnetic-field strength. 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 FU NASA through Chandra General Observer Program [GO6- 7059X] FX This work was supported by NASA through Chandra General Observer Program grant GO6- 7059X. We thank A. Patil, D. Huard, and C. Fonnesbeck for creating and making available the PyMC package. NR 15 TC 21 Z9 21 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 20 PY 2009 VL 695 IS 2 BP L149 EP L153 DI 10.1088/0004-637X/695/2/L149 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 428TE UT WOS:000264872100006 ER PT J AU Gordley, LL Thompson, E McHugh, M Remsberg, E Russell, J Magill, B AF Gordley, Larry L. Thompson, Earl McHugh, Martin Remsberg, Ellis Russell, James, III Magill, Brian TI Accuracy of atmospheric trends inferred from the Halogen Occultation Experiment data SO JOURNAL OF APPLIED REMOTE SENSING LA English DT Article DE solar occultation; atmospheric trends; satellite remote sensing; radiometry ID STRATOSPHERIC WATER-VAPOR; UARS PLATFORM; VALIDATION; OZONE; PROFILES; QUALITY AB The Halogen Occultation Experiment (HALOE) operated in orbit for over 14 years, providing high quality measurements from the upper troposphere into the lower thermosphere. Since the quality of this data set depended on the long-term stability of the instrument, a series of analysis tests were designed to routinely monitor instrument performance. These tests evaluated possible changes in the gas cells, electronic gains, optical performance, and signal temperature dependencies. The gas cell stability was determined from an analysis of the Doppler shift signature in retrieved mixing ratios. Electronic gain stability was determined by instrument scans of the solar disk, each with different balance settings. Optical and tracking performance was also determined from solar scan data. The only statistically significant changes detected were: 1. a small methane gas cell change, causing less than 0.5% per decade change in retrieved methane, and 2. a small optical alignment change in the HF channel that only affects HF results below 25 kilometers. These detailed analyses indicate that the HALOE instrument remained stable throughout the mission, adding confidence to the long-term atmospheric trends deduced from HALOE products. C1 [Gordley, Larry L.; Thompson, Earl; McHugh, Martin] GATS Inc, Newport News, VA 23606 USA. [Remsberg, Ellis] NASA, Langley Res Ctr, Atmospher Sci Directorate, Hampton, VA 23681 USA. [Russell, James, III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. [Magill, Brian] SSAI, Hampton, VA 23666 USA. RP Gordley, LL (reprint author), GATS Inc, 11864 Canon Blvd,Suite 101, Newport News, VA 23606 USA. EM l.l.gordley@gats-inc.com; r.e.thompson@gats-inc.com; m.j.mchugh@gats-inc.com; e.e.remsberg@larc.nasa.gov; james.russell@hamptonu.edu; brian_magill@ssaihq.com FU NASA [NAS1-02058, NNG04GE42G] FX We would like to thank Jeff Tabor of SAIC, Inc. for supplying us with the DAC data and would also like to thank Janet Daniels of SAIC and John Wells of NASA Langley for helpful discussions and suggestions. This work was supported by NASA Contract No. NAS1-02058 and NASA Grant No. NNG04GE42G. NR 25 TC 8 Z9 8 U1 0 U2 1 PU SPIE-SOC PHOTOPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 1931-3195 J9 J APPL REMOTE SENS JI J. Appl. Remote Sens. PD APR 20 PY 2009 VL 3 AR 033526 DI 10.1117/1.3131722 PG 24 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 520WD UT WOS:000271879300001 ER PT J AU Wu, DL Austin, RT Deng, M Durden, SL Heymsfield, AJ Jiang, JH Lambert, A Li, JL Livesey, NJ McFarquhar, GM Pittman, JV Stephens, GL Tanelli, S Vane, DG Waliser, DE AF Wu, D. L. Austin, R. T. Deng, M. Durden, S. L. Heymsfield, A. J. Jiang, J. H. Lambert, A. Li, J. -L. Livesey, N. J. McFarquhar, G. M. Pittman, J. V. Stephens, G. L. Tanelli, S. Vane, D. G. Waliser, D. E. TI Comparisons of global cloud ice from MLS, CloudSat, and correlative data sets SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MILLIMETER-WAVE RADAR; VISIBLE OPTICAL DEPTH; PACIFIC WARM POOL; WATER-CONTENT; EOS MLS; RADIATIVE-TRANSFER; PROFILING RADAR; CIRRUS CLOUDS; RETRIEVALS; SATELLITE AB Aura Microwave Limb Sounder (MLS) version 2.2 (V2.2) and CloudSat R04 (release 4) ice water content (IWC) and partial-column ice water path (pIWP) measurements are analyzed and compared to other correlative data sets. The MLS IWC, representing an average over similar to 300 x 7 x 4 km(3) volume, is retrieved at 215-268 hPa with precision varying between 0.06 and 1 mg/m(3). The MLS pIWP products, representing the partial columns over similar to 100 x 7 km(2) area with the bottom at similar to 8, similar to 6, and similar to 11 km for 115, 240, and 640 GHz, have estimated precisions of 5, 1.5, and 0.8 g/m(2), respectively. CloudSat, on the other hand, shows a minimum detectable sensitivity of -31 dBZ in the reflectivity measurement at 94 GHz. CloudSat IWC is an average over similar to 1.8 x 1.4 x 0.5 km(3) volume, and its precision varies from 0.4 mg/m(3) at 8 km to 1.6 mg/m(3) at 12 km. The estimated single-profile precision for CloudSat IWP is similar to 9 g/m(2). However, these measurements are associated with relatively large systematic error, mostly due to uncertainties in the retrieval assumptions about microphysics, which lead to relatively poor accuracy compared to measurement precision. To characterize systematic differences among various observations and those derived from models, we employ the normalized probability density function (pdf) in the comparisons. CloudSat IWC shows generally consistent slopes of pdf distribution with in situ observations, particularly at similar to 12 km where the in situ data come mostly from long-leg flights. Despite similar IWC morphology found between MLS and CloudSat observations, CloudSat R04 IWC retrieval is higher compared to MLS, especially at 14-17 km where the MLS technique is not limited by sensitivity saturation. The MLS and CloudSat IWC pdf's agree well in the overlapped sensitivity range with relative difference <50%, but the difference appears to increase with IWC. MLS and CloudSat cloud ice measurements are compared with other data sets in terms of monthly map and pdf. Comparisons with European Center for Medium range Weather Forecasting (ECMWF) analyses show that grid box averages of monthly ECMWF IWC are much smaller (by similar to 5 x and similar to 20 x) than the same MLS and CloudSat averages. Comparisons of pIWP data from CloudSat and passive sensors reveal large uncertainties associated with passive techniques, such as penetration depth and sensitivity limitation. In particular, retrievals from Moderate Resolution Imaging Spectroradiometer (MODIS) and Advanced Microwave Sounding Unit-B (AMSU-B) differ largely in IWP pdf from the CloudSat R04 retrieval, showing CloudSat values generally lower (by similar to 5 x and similar to 8 x, respectively) at IWP = 10-500 g/m(2) but higher at IWP > 500 g/m(2). C1 [Wu, D. L.; Durden, S. L.; Jiang, J. H.; Lambert, A.; Li, J. -L.; Livesey, N. J.; Tanelli, S.; Vane, D. G.; Waliser, D. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Austin, R. T.; Stephens, G. L.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Deng, M.] Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82071 USA. [Heymsfield, A. J.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [McFarquhar, G. M.] Univ Illinois, Dept Atmospher Sci, Urbana, IL 61820 USA. [Pittman, J. V.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Wu, DL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM dong.l.wu.@jpl.nasa.gov RI Heymsfield, Andrew/E-7340-2011; Wu, Dong/D-5375-2012; OI McFarquhar, Greg/0000-0003-0950-0135 NR 65 TC 45 Z9 46 U1 0 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 APR 18 PY 2009 VL 114 AR D00A24 DI 10.1029/2008JD009946 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 435FO UT WOS:000265329500001 ER PT J AU Birn, J Hesse, M Schindler, K Zaharia, S AF Birn, J. Hesse, M. Schindler, K. Zaharia, S. TI Role of entropy in magnetotail dynamics SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID COLLISIONLESS MAGNETIC RECONNECTION; THIN CURRENT SHEETS; PLASMA SHEET; EARTHS MAGNETOTAIL; ELECTRON DISSIPATION; FLUX TUBES; CONVECTION; BUBBLES; BALANCE; FLOWS AB The role of entropy conservation and loss in magnetotail dynamics, particularly in relation to substorm phases, is discussed on the basis of MHD theory and simulations, using comparisons with particle-in-cell (PIC) simulations for validation. Entropy conservation appears to be a crucial element leading to the formation of thin embedded current sheets in the late substorm growth phase and the potential loss of equilibrium. Entropy conservation also governs the accessibility of final states of evolution and the amount of energy that may be released. Entropy loss (in the form of plasmoids) is essential in the earthward transport of flux tubes (bubbles, bursty bulk flows). Entropy loss also changes the tail stability properties and may render ballooning modes unstable and thus contribute to cross-tail variability. We illustrate these effects through results from theory and simulations. C1 [Birn, J.; Zaharia, S.] Los Alamos Natl Lab, Space Sci & Applicat Grp, Los Alamos, NM 87545 USA. [Hesse, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Schindler, K.] Ruhr Univ Bochum, Inst Theoret Phys, D-44780 Bochum, Germany. RP Birn, J (reprint author), Los Alamos Natl Lab, Space Sci & Applicat Grp, POB 1663, Los Alamos, NM 87545 USA. EM jbirn@lanl.gov RI Hesse, Michael/D-2031-2012; NASA MMS, Science Team/J-5393-2013 OI NASA MMS, Science Team/0000-0002-9504-5214 FU NASA Goddard Space Flight Center; NASA's Heliophysics Theory Program FX This work was performed under the auspices of the U. S. Department of Energy, supported by a grant from NASA Goddard Space Flight Center and by NASA's Heliophysics Theory Program.; Wolfgang Baumjohann thanks the reviewers for their assistance in evaluating this paper. NR 38 TC 41 Z9 42 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD APR 18 PY 2009 VL 114 AR A00D03 DI 10.1029/2008JA014015 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 435GN UT WOS:000265332200005 ER PT J AU Michael, M Tripathi, SN Borucki, WJ Whitten, RC AF Michael, Marykutty Tripathi, Sachchida Nand Borucki, W. J. Whitten, R. C. TI Highly charged cloud particles in the atmosphere of Venus SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID AEROSOL ATTACHMENT COEFFICIENTS; COSMIC-RAY IONIZATION; ELECTRICAL-CONDUCTIVITY; PLANETARY-ATMOSPHERES; NEGATIVE-IONS; NIGHT SIDE; MODEL; MICROPHYSICS; DUST; IONOSPHERE AB The accumulation of charges on cloud particles by the charge transfer of ions and attachment of electrons in the atmosphere of Venus is investigated in the present work. Three cloud layers between 45 and 70 km exist in the atmosphere of Venus. Ions and electrons are produced by the interaction of galactic cosmic rays with the neutral molecules. Ion to particle and electron to particle attachment coefficients are calculated. The charge balance equations include ion-ion recombination, ion-electron recombination, electron attachment to neutrals, electron detachment from negative ions, and attachment of electron and charge transfer from ions to particles. It is found that the ion concentrations are reduced by a maximum of a factor of 5 by charging of the particles, while the earlier studies showed a maximum reduction of about an order of magnitude due to the differences in the surface area of the particles. A similar result is observed in the calculation of electrical conductivity. Both monodisperse and polydisperse distribution of particles are considered. The conductivity was reduced by a factor of 3 when using the monodisperse distribution of particles, while the maximum reduction observed was a factor of 2 when using the polydisperse distribution. This result implies that the monodisperse particle distribution overestimates the effect of particles on the atmospheric conductivity. The ratio of negative to positive charges is found to be very large in the middle and upper cloud layers. The low abundance of the aerosols and high conductivity of the atmosphere appear to rule out lightning activity in the 40 to 70 km altitude region. C1 [Michael, Marykutty; Tripathi, Sachchida Nand] Indian Inst Technol, Dept Civil Engn, Kanpur 208016, Uttar Pradesh, India. [Borucki, W. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Whitten, R. C.] SETI Res Inst, Mountain View, CA 94043 USA. RP Michael, M (reprint author), Indian Inst Technol, Dept Civil Engn, Kanpur 208016, Uttar Pradesh, India. EM snt@iitk.ac.in RI Tripathi, Sachchida/J-4840-2016 NR 64 TC 17 Z9 17 U1 1 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD APR 17 PY 2009 VL 114 AR E04008 DI 10.1029/2008JE003258 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 435GF UT WOS:000265331200001 ER PT J AU Hakkinen, S Rhines, PB AF Hakkinen, Sirpa Rhines, Peter B. TI Shifting surface currents in the northern North Atlantic Ocean SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID SUBPOLAR GYRE; THERMOHALINE CIRCULATION; KINETIC-ENERGY; LABRADOR SEA; NORDIC SEAS; VARIABILITY; WATER; OSCILLATION; ALTIMETRY; PATHWAYS AB Analysis of surface drifter tracks in the North Atlantic Ocean from the time period 1990 to 2007 provides evidence that warm subtropical waters have recently increased their penetration toward the Nordic seas. Prior to 2000, the warm water branches of the North Atlantic Current fed by the Gulf Stream turned southeastward in the eastern North Atlantic. Since 2001, these paths have shifted toward the Rockall Trough, through which the most saline North Atlantic waters pass to the Nordic seas. These surface drifters are able to overcome the Ekman drift, which would force them southward under the westerly winds dominating the subpolar Atlantic, yet the changes in path cannot be accounted for by changes in Ekman drift. Eddy kinetic energy from satellite altimetry shows increased energy along the shifted drifter pathways across the Mid-Atlantic Ridge since 2001. These near-surface changes have occurred during continual weakening of the North Atlantic subpolar gyre, as seen by altimetry. They are also consistent with the observed increase in temperature and salinity of the waters flowing northward into the Nordic seas. These findings suggest the changes in the vertical structure of the northern North Atlantic Ocean, its dynamics, and exchanges with the higher latitudes. Wind stress and its curl changes are discussed as a possible forcing of the changes in the pathways of the subtropical waters. C1 [Hakkinen, Sirpa] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rhines, Peter B.] Univ Washington, Sch Oceanog, Seattle, WA 98195 USA. RP Hakkinen, S (reprint author), NASA, Goddard Space Flight Ctr, Code 614-2, Greenbelt, MD 20771 USA. EM sirpa.hakkinen@nasa.gov RI Hakkinen, Sirpa/E-1461-2012 FU NASA; OSTST Science Team FX S. H. gratefully acknowledges the support from NASA Headquarters Physical Oceanography Program for this work. P. B. R. is supported by NASA through the OSTST Science Team. We thank Denise Worthen for the invaluable technical assistance in data set analysis and graphics. NR 40 TC 85 Z9 86 U1 4 U2 35 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 APR 16 PY 2009 VL 114 AR C04005 DI 10.1029/2008JC004883 PG 12 WC Oceanography SC Oceanography GA 435FV UT WOS:000265330200001 ER PT J AU Zhou, D Semones, E Gaza, R Johnson, S Zapp, N Lee, K George, T AF Zhou, D. Semones, E. Gaza, R. Johnson, S. Zapp, N. Lee, K. George, T. TI Radiation measured during ISS-Expedition 13 with different dosimeters SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Space radiation; Cosmic rays; Active and passive dosimeters; LET spectra ID LOW-EARTH-ORBIT; HIGH-LET RADIATION; CR-39 DETECTORS; TRACK DETECTORS; DOSE-EQUIVALENT; COSMIC-RAYS; SPECTRA; ETCH AB Radiation in low Earth orbit (LEO) is mainly composed of galactic cosmic rays (GCR), solar energetic particles and particles in SAA (South Atlantic Anomaly). The biological impact of space radiation to astronauts depends strongly on the particles' linear energy transfer (LET) and is dominated by high LET radiation. It is important to measure the LET spectrum for the space radiation field and to investigate the influence of radiation oil astronauts. At present, the preferred active dosimeters sensitive to all LET are the tissue equivalent proportional counter (TEPC) and the silicon detectors in various configurations; the preferred passive dosimeters are CR-39 plastic nuclear track detectors (PNTDs) sensitive to high LET and thermoluminescence dosimeters (TLDs) as well as optically stimulated luminescence dosimeters (OSLDs) sensitive to low LET. The TEPC, CR-39 PNTDs, TLDs and OSLDs were used to investigate the radiation field for the ISS mission Expedition 13 (ISS-12S) in LEO. LET spectra and radiation quantities (fluence, absorbed dose, dose equivalent and quality factor) were measured for the space mission with different dosimeters. This paper introduces the role of high LET radiation in radiobiology, the operational principles for the different dosimeters, the LET spectrum method using CR-39 detectors, the method to combine the results measured with TLDs/OSLDs and CR-39 PNTDs, and presents the LET spectra and the radiation quantities measured and combined. Published by Elsevier Ltd on behalf of COSPAR. C1 [Zhou, D.; Semones, E.; Gaza, R.; Johnson, S.; Zapp, N.; Lee, K.; George, T.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Zhou, D.; Gaza, R.] Univ Space Res Assoc, Houston, TX 77058 USA. RP Zhou, D (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 Nasa Pkwy, Houston, TX 77058 USA. EM dazhuang.zhou-1@nasa.gov NR 35 TC 12 Z9 14 U1 0 U2 5 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 APR 15 PY 2009 VL 43 IS 8 BP 1212 EP 1219 DI 10.1016/j.asr.2009.02.003 PG 8 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 438OV UT WOS:000265565900006 ER PT J AU Bamsey, M Berinstain, A Auclair, S Battler, M Binsted, K Bywaters, K Harris, J Kobrick, R Mckay, C AF Bamsey, M. Berinstain, A. Auclair, S. Battler, M. Binsted, K. Bywaters, K. Harris, J. Kobrick, R. McKay, C. TI Four-month Moon and Mars crew water utilization study conducted at the Flashline Mars Arctic Research Station, Devon Island, Nunavut SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Space analogue studies; Space life support; Water utilization; Moon/Mars exploration AB A categorized water usage study was undertaken at the Flashline Mars Arctic Research Station on Devon Island, Nunavut in the High Canadian Arctic. This study was conducted as part of a long duration four-month Mars mission simulation during the summer of 2007. The study determined that the crew of seven averaged 82.07 L/day over the expedition (standard deviation 22.58 L/day). The study also incorporated a Mars Time Study phase which determined that an average of 12.12 L/sol of water was required for each crewmember. Drinking, food preparation, hand/face, oral, dish wash, clothes wash, shower, shaving, cleaning, engineering, science, plant growth and medical water were each individually monitored throughout the detailed study phases. It was determined that implementing the monitoring program itself resulted in an approximate water savings of 1.5 L/day per crewmember. The seven person crew averaged 202 distinct water draws a day (standard deviation 34) with high water use periods focusing around meal times. No statistically significant correlation was established between total water use and EVA or exercise duration. Study results suggest that current crew water utilization estimates for long duration planetary surface stays are more than two times greater than that required. Crown copyright (C) 2009 Published by Elsevier Ltd. on behalf of COSPAR. All rights reserved. C1 [Bamsey, M.; Berinstain, A.] Univ Guelph, Dept Environm Biol, Guelph, ON N1G 2W1, Canada. [Berinstain, A.] Canadian Space Agcy, Longueuil, PQ J3Y 8Y9, Canada. [Auclair, S.; Battler, M.] Univ Western Ontario, Dept Earth Sci, London, ON N6A 5B7, Canada. [Binsted, K.] Univ Hawaii, NASA, Astrobiol Inst, Informat & Comp Sci Dept, Honolulu, HI 96744 USA. [Bywaters, K.] Calif State Univ San Marcos, San Marcos, CA 92096 USA. [Harris, J.] Austin Community Coll, Dept Comp Informat Syst, Austin, TX 78724 USA. [Kobrick, R.] Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80303 USA. [McKay, C.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Bamsey, M (reprint author), Univ Guelph, Dept Environm Biol, 50 Stone Rd E, Guelph, ON N1G 2W1, Canada. EM mbamsey@uoguelph.ca RI Battler, Melissa/N-2591-2014 FU Polar Continental Shelf Project FX This work was carried out with the aid of a grant from the Canadian Space Agency, Longueuil, Quebec, Canada. Arctic logistics support was provided by the Polar Continental Shelf Project. Mars Society International and Mars Society Canada are acknowledged for overall project management and support of FMARS2007. Finally, Paul Graham provided technical aid for on-site monitoring system deployment. NR 22 TC 4 Z9 4 U1 5 U2 6 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 APR 15 PY 2009 VL 43 IS 8 BP 1256 EP 1274 DI 10.1016/j.asr.2009.01.009 PG 19 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 438OV UT WOS:000265565900013 ER PT J AU Murphy, KL Rygalov, VY Johnson, SB AF Murphy, K. L. Rygalov, V. Ye. Johnson, S. B. TI Minimal support technology and in situ resource utilization for risk management of planetary spaceflight missions SO ADVANCES IN SPACE RESEARCH LA English DT Article DE In situ resource utilization; System closure; Reliability; Interplanetary mission; System degradation; Risk mitigation ID SPACE STATION; SYSTEM; MARS; MAINTENANCE; EXPLORATION AB All artificial systems and components in space degrade at higher rates than oil Earth, depending in part oil environmental conditions, design approach, assembly technologies, and the materials used. This degradation involves not only the hardware and software systems but the humans that interact with those systems. All technological functions and systems can be expressed through functional dependence: [Function] similar to [ERU] * [RUIS] * [ISR]/[DR]: where [ERU] efficiency (rate) of environmental resource utilization [RUIS] resource utilization infrastructure [ISR] in situ resources [DR] degradation rate The limited resources of spaceflight and open space for autonomous missions require a high reliability (maximum possible, approaching 100%) for system functioning and operation, and must minimize the rate of any system degradation. To date, only a continuous human presence with a system in the spaceflight environment can absolutely mitigate those degradations. This mitigation is based on environmental amelioration for both the technology systems, as repair of data and spare parts, and the humans, as exercise and psychological support. Such maintenance now requires huge infrastructures, including research and development complexes and management agencies, which currently cannot move beyond the Earth. When considering what is required to move manned spaceflight from near Earth stations to remote locations such as Mars, what are the minimal technologies and infrastructures necessary for autonomous restoration of a degrading system in space? In all of the known system factors of a mission to Mars that reduce the mass load, increase the reliability, and reduce the mission's overall risk, the current common denominator is the use of undeveloped or untested technologies. None of the technologies required to significantly reduce the risk for critical systems are currently available at acceptable readiness levels. Long term interplanetary missions require that space programs produce a craft with all systems integrated so that they arc of the highest reliability. Right now, with current technologies, we cannot guarantee this reliability for a crew of six for 1000 days to Mars and back. Investigation of the technologies to answer this need and a focus of resources and research oil their advancement would significantly improve chances for a safe and successful mission. (C) 2008 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Murphy, K. L.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Rygalov, V. Ye.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA. [Johnson, S. B.] Univ Colorado Colorado Springs, Larkspur, CO 80118 USA. RP Murphy, KL (reprint author), NASA, George C Marshall Space Flight Ctr, Bldg 4600,Room 5318, Huntsville, AL 35812 USA. EM karen.l.murphy@nasa.gov NR 47 TC 2 Z9 2 U1 1 U2 3 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PD APR 15 PY 2009 VL 43 IS 8 BP 1275 EP 1284 DI 10.1016/j.asr.2008.12.010 PG 10 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 438OV UT WOS:000265565900014 ER PT J AU Laity, JE Bridges, NT AF Laity, Julie E. Bridges, Nathan T. TI Ventifacts on Earth and Mars: Analytical, field, and laboratory studies supporting sand abrasion and windward feature development SO GEOMORPHOLOGY LA English DT Article DE Aeolian geomorphology; Ventifacts; Aeolian abrasion; Wind erosion; Mars; Deserts ID PATHFINDER LANDING SITE; MERIDIANI-PLANUM; SEDIMENT-TRANSPORT; OPPORTUNITY ROVER; COACHELLA VALLEY; GUSEV CRATER; DRIVEN SAND; CALIFORNIA; EROSION; DUST AB Terrestrial ventifacts - rocks that have been abraded by windblown particles - are found in desert, periglacial, and coastal environments. On Mars, their abundance suggests that aeolian abrasion is one of the most significant erosional processes on the planet. There are several conflicting viewpoints concerning the efficacy of potential abrasive agents, principally sand and dust, and the relationships between wind direction and ventifact form. Our research, supported by a review of the literature, shows that sand, rather than dust or other materials, is the principle abrasive agent on Earth and Mars. Relative to dust, sand delivers about 1000x the energy onto rock surfaces on a per particle basis. Even multiple dust collisions will do little or no damage because the stress field from the impact is much smaller than the spacing of microflaws in the rock. The abrasion profiles of terrestrial ventifacts are consistent with a kinetic energy flux due to saltating sand, not airborne dust. Furthermore, Scanning Electron Microscope images reveal surfaces that are fractured and cleaved by sand grain impact. With respect to their distribution, ventifacts are found in regions that contain sand or did so in the past, but are not found where only dust activity occurs. Contrary to some published reports, our evidence from field studies, analytical models, and wind tunnel and other experiments indicates that windward, not leeward, abrasion is responsible for facet development and feature formation (pits, flutes, and grooves). Leeward abrasion is confined to fluvial conditions, in which the high viscosity and density of water are able to entrain sand-size material in vortices. Therefore, ventifacts and abraded terrain provide an unambiguous proxy for the direction of the highest velocity winds, and can be used to reconstruct palaeowind flow. (C) 2008 Elsevier B.V. All rights reserved. C1 [Laity, Julie E.] Calif State Univ Northridge, Dept Geog, Northridge, CA 91330 USA. [Bridges, Nathan T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Laity, JE (reprint author), Calif State Univ Northridge, Dept Geog, 18111 Nordhaff St, Northridge, CA 91330 USA. EM julie.laity@csun.edu; nathan.bridges@jpl.nasa.gov RI Bridges, Nathan/D-6341-2016 FU NASA's Planetary Geology and Geophysics Program FX We are grateful to A. Razdan and his research group at Arizona State University, who conducted the laser scans and made the derived models. We would also like to thank S.A.D'Agostino and M. Petkov at the jet Propulsion Laboratory for performing the SEM analyses. We would like to thank M. Banks, M. Benzit, and E.E. Eddlemon for assisting in the setup and interpretation of the high speed video experiments and J-P. Wiens for the filming and conversion of the HSV to MP4 files. David Deis of the Department of Geography at California State University Northridge drafted Fig. 13. Unofficial reviews from S.A. D'Agostino, M.P. Golombek, and BJ. Thomson improved this paper. S.A. D'Agostino, R. Greeley, and J.P, Marshall provided insight on rock elastic failure limits. N.T. Bridges'work on this project was supported by NASA's Planetary Geology and Geophysics Program. This paper benefited from reviews by two anonymous referees. NR 96 TC 31 Z9 34 U1 0 U2 12 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0169-555X EI 1872-695X J9 GEOMORPHOLOGY JI Geomorphology PD APR 15 PY 2009 VL 105 IS 3-4 BP 202 EP 217 DI 10.1016/j.geomorph.2008.09.014 PG 16 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 426XQ UT WOS:000264742100004 ER PT J AU Juarez, MD Marcus, S Dornbrack, A Schroder, TM Kivi, R Iijima, BA Hajj, GA Mannucci, AJ AF Juarez, M. de la Torre Marcus, S. Doernbrack, A. Schroder, T. M. Kivi, R. Iijima, B. A. Hajj, G. A. Mannucci, A. J. TI Detection of temperatures conducive to Arctic polar stratospheric clouds using CHAMP and SAC-C radio occultation data SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID GLOBAL POSITIONING SYSTEM; GRAVITY-WAVE ACTIVITY; GPS OCCULTATION; EARTHS ATMOSPHERE; DEPLETION; OZONE; WATER; DISTRIBUTIONS; METEOROLOGY; PARTICLES AB We use global positioning system radio occultation (GPSRO) data from the Challenging Mini-Satellite Payload for Geophysical Research and Application (CHAMP) and Satelite de Applicaciones Cientificas-C (SAC-C) low Earth orbiting satellites to investigate the occurrence of air with temperatures cold enough to allow the formation of polar stratospheric clouds (PSCs) during four successive Arctic winters spanning 2001 to 2005. The GPSRO data are validated and compared with analysis data from the European Centre for Medium-Range Weather Forecasts using a series of criteria designed to eliminate faulty soundings but retain profiles which do not differ too strongly from the model data. We find that GPSRO is able to detect more PSC-prone temperature profiles during winters with disturbed conditions (in particular during December 2001 and 2003) than the analysis, but that the model fully captures the extent of PSC-prone air in winters with strong, cold vortices (in particular December 2002 and January 2005). Examination of detailed profiles for December 2001 shows that this difference is due to the ability of GPSRO to detect short-vertical wavelength features which may represent either localized gravity or global-scale planetary waves. Since the GPSRO data are now being directly assimilated into operational analysis systems, the benefits of the higher vertical resolution retrievals it provides should become evident in future observational studies of PSC formation and ozone loss, particularly under the disturbed conditions noted in several recent winters. C1 [Juarez, M. de la Torre; Marcus, S.; Schroder, T. M.; Iijima, B. A.; Hajj, G. A.; Mannucci, A. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91189 USA. [Doernbrack, A.] DLR, Inst Atmospher Phys, D-82230 Oberpfaffenhofen, Germany. [Kivi, R.] FMI, Arctic Res Ctr, FI-99600 Sodankyla, Finland. [Schroder, T. M.] Natl Acad Sci, Natl Res Council, Washington, DC 20418 USA. RP Juarez, MD (reprint author), CALTECH, Jet Prop Lab, MS 169-237,4800 Oak Grove Dr, Pasadena, CA 91189 USA. EM mtj@jpl.nasa.gov OI Marcus, Steven/0000-0002-5763-6961 NR 47 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 EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD APR 15 PY 2009 VL 114 AR D07112 DI 10.1029/2008JD011261 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 435FH UT WOS:000265328800003 ER PT J AU Kaul, AB AF Kaul, Anupama B. TI Gas sensing with long, diffusively contacted single-walled carbon nanotubes SO NANOTECHNOLOGY LA English DT Article ID OHMIC CONTACTS; TRANSPORT; SENSORS; WIRES AB A carbon nanotube thermal-conductivity-based pressure or gas sensor is described, which utilizes 5-10 mu m long, diffusively contacted single-walled nanotubes (SWNTs). Low temperature electrical transport measurements for these tubes were suggestive of a thermally activated hopping mechanism for electron localization, where a hopping energy of similar to 39 meV was computed. A negative differential conductance regime was also detected in suspended tubes, released using critical point drying, at high bias voltages. The pressure or gas sensitivity increased more dramatically as the bias power was increased up to 14 mu W, which was interpreted in the context of the high optical phonon density in the suspended SWNTs. Such devices are promising for use as pressure sensors, as well as for the chemical identification of species having differing gas thermal conductivities. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kaul, AB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM anupama.b.kaul@jpl.nasa.gov FU Defense Advanced Research Project Agency [715839, NAS7-03001] FX We greatly acknowledge James Wishard for his assistance in the JPL Micro-Devices Laboratory, Dr Eric Wong for CNT growth and annealing, Dr Henry LeDuc for use of the low temperature electrical measurement facility, Dr. Harish Manohara for initial interest, and Mr Ron Ruiz for SEM imaging. This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration and was funded by a Defense Advanced Research Project Agency seedling fund (Task Order NMO# 715839 under NAS7-03001). NR 20 TC 9 Z9 9 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0957-4484 J9 NANOTECHNOLOGY JI Nanotechnology PD APR 15 PY 2009 VL 20 IS 15 AR 155501 DI 10.1088/0957-4484/20/15/155501 PG 6 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Science & Technology - Other Topics; Materials Science; Physics GA 424BD UT WOS:000264539600010 PM 19420548 ER PT J AU Calaway, MJ Stansbery, EK Keller, LP AF Calaway, Michael J. Stansbery, Eileen K. Keller, Lindsay P. TI Genesis capturing the sun: Solar wind irradiation at Lagrange 1 SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM INTERACTIONS WITH MATERIALS AND ATOMS LA English DT Article DE Irradiation damage; Radiation damage; NASA Genesis Mission; Solar wind; Space weathering; Silicon defects ID ION-IMPLANTED SILICON; AMORPHIZATION; RADIATION; MISSION; RATES; NEON AB Genesis, a member of NASAs Discovery Mission program, is the world's first sample return mission since the Apollo program to bring home solar matter in ultra-pure materials. Outside the protection of Earth's magnetosphere at the Earth-Sun Lagrange 1 point, the deployed sample collectors were directly exposed to solar wind irradiation. The natural process of solar wind ion implantation into a highly pure silicon (Si) bulk composition array collector has been measured by spectroscopic ellipsometry and scanning transmission electron microscopy (STEM). Ellipsometry results show that bulk solar wind ions composed of approximately 95% H(+), 4% He(+) and < 1% other elements physically altered the first 59-63 nm of crystalline silicon substrate during 852.8 days of solar exposure. STEM analysis confirms that the solar accelerated ions caused significant strain and visible structural defects to the silicon structure forming a 60-75 nm thick irradiation damage region directly below the surface SiO(2) native oxide layer. Monte Carlo simulations of solar wind H, He, C, O, Ne, Mg, Si and Fe ion collisions in the Si collector with fluences calculated from the Genesis and ACE spacecrafts were used to estimate the energy deposited and Si vacancies produced by nuclear stopping in a flight-like Si bulk array collector. The coupled deposited energy model with the flown Genesis Si in situ measurements provides new insight into the basic principles of solar wind diffusion and space weathering of materials outside Earth's magnetosphere. (c) 2009 Elsevier B.V. All rights reserved. C1 [Calaway, Michael J.] NASA, Lyndon B Johnson Space Ctr, Jacobs ESCG, Houston, TX 77058 USA. RP Calaway, MJ (reprint author), NASA, Lyndon B Johnson Space Ctr, Jacobs ESCG, Mail Code KT,2101 NASA Pkwy, Houston, TX 77058 USA. EM michael.calaway-1@nasa.gov NR 51 TC 3 Z9 3 U1 1 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-583X J9 NUCL INSTRUM METH B JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms PD APR 15 PY 2009 VL 267 IS 7 BP 1101 EP 1108 DI 10.1016/j.nimb.2009.01.132 PG 8 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 446XN UT WOS:000266155000012 ER PT J AU Aghara, SK Blattnig, SR Norbury, JW Singleterry, RC AF Aghara, S. K. Blattnig, S. R. Norbury, J. W. Singleterry, R. C. TI Monte Carlo analysis of pion contribution to absorbed dose from Galactic cosmic rays SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM INTERACTIONS WITH MATERIALS AND ATOMS LA English DT Article DE Pions; Mesons; Space radiation; Monte Carlo; Neutron flux; Photon flux; Absorbed dose; GCR; Space; Heavy ions ID RADIATION ENVIRONMENT; CODE; SIMULATIONS; TRANSPORT; ENERGY; MCNPX AB Accurate knowledge of the physics of interaction, particle production and transport is necessary to estimate the radiation damage to equipment used on spacecraft and the biological effects of space radiation. For long duration astronaut missions, both on the International Space Station and the planned manned missions to Moon and Mars, the shielding strategy must include a comprehensive knowledge of the secondary radiation environment. The distribution of absorbed dose and dose equivalent is a function of the type, energy and population of these secondary products. Galactic cosmic rays (GCR) comprised of protons and heavier nuclei have energies from a few MeV per nucleon to the ZeV region, with the spectra reaching flux maxima in the hundreds of MeV range. Therefore, the MeV-GeV region is most important for space radiation. Coincidentally, the pion production energy threshold is about 280 MeV. The question naturally arises as to how important these particles are with respect to space radiation problems. The space radiation transport code, HZETRN (High charge (Z) and Energy TRaNsport), currently used by NASA, performs neutron. proton and heavy ion transport explicitly, but it does not take into account the production and transport of mesons, photons and leptons. In this paper, we present results from the Monte Carlo code MCNPX (Monte Carlo N-Particle eXtended), showing the effect of leptons and mesons when they are produced and transported in a GCR environment. (c) 2009 Elsevier B.V. All rights reserved. C1 [Aghara, S. K.] Prairie View A&M Univ, Chem Engn Nucl Program, Prairie View, TX 77446 USA. [Blattnig, S. R.; Norbury, J. W.; Singleterry, R. C.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Aghara, SK (reprint author), Prairie View A&M Univ, Chem Engn Nucl Program, POB 519,MS 2505, Prairie View, TX 77446 USA. EM Sukesh.K.Aghara@nasa.gov FU NASA Administrator's Fellow Program (NAFP); United Negro College Funds Special Programs (UNCFSP) [003844] FX We thank Dr. Ryan Norman, Dr. Francis Badavi and Dr. Steven Walker for reviewing the manuscript. This research was supported by NASA Administrator's Fellow Program (NAFP) managed by United Negro College Funds Special Programs (UNCFSP), Grant No. 003844. NR 33 TC 19 Z9 19 U1 1 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-583X J9 NUCL INSTRUM METH B JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms PD APR 15 PY 2009 VL 267 IS 7 BP 1115 EP 1124 DI 10.1016/j.nimb.2009.01.136 PG 10 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 446XN UT WOS:000266155000014 ER PT J AU Norbury, JW AF Norbury, John W. TI Total cross section parameterizations for pion production in nucleon-nucleon collisions SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM INTERACTIONS WITH MATERIALS AND ATOMS LA English DT Article DE Cross section; Pion production; Nuclear reactions ID PP INTERACTIONS; CHARGED PIONS; GEV-C; GAMMA PRODUCTION; GEV/C; PARTICLE; MULTIPLICITIES; PROTONS AB Total cross section parameterizations for neutral and charged pion production in nucleon-nucleon collisions are compared to experimental data over the projectile momentum range from threshold to 300 GeV. Both proton-proton and proton-neutron reactions are considered. Overall excellent agreement between parameterizations and experiment is found, except for some disagreements near threshold. This gives much greater confidence to previously developed pion cross section formulas for nucleon-nucleon, proton-nucleus, and nucleus-nucleus reactions. These results are useful for particle transport. Published by Elsevier B.V. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Norbury, JW (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM john.w.norbury@nasa.gov NR 18 TC 2 Z9 2 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-583X EI 1872-9584 J9 NUCL INSTRUM METH B JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms PD APR 15 PY 2009 VL 267 IS 7 BP 1209 EP 1212 DI 10.1016/j.nimb.2009.02.067 PG 4 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 446XN UT WOS:000266155000030 ER PT J AU Baldridge, AM Hook, SJ Grove, CI Rivera, G AF Baldridge, A. M. Hook, S. J. Grove, C. I. Rivera, G. TI The ASTER spectral library version 2.0 SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE ASTER; Spectral library ID SPACEBORNE THERMAL EMISSION; REFLECTION RADIOMETER ASTER; NEVADA; IMAGES; MINERALS; CONTRAST; SPRINGS; SURFACE; FIELD AB The Advanced Spaceborne Thermal Emission Reflection Radiometer (ASTER) on NASA's Terra platform has been widely used in geological and other science studies. In support of ASTER studies, a library of natural and man-made materials was compiled as the ASTER Spectral Library v1.2 and made available from http://speclib.jpl.nasa.gov. The library is a collection of contributions in a standard format with ancillary data from the jet Propulsion Laboratory (JPL), Johns Hopkins University (JHU) and the United States Geological Survey (USGS). A new version of the library (v2.0) is now available online or via CD, which includes major additions to the mineral and rock spectra. The ASTER library provides a comprehensive collection of over 2300 spectra of a wide variety of materials covering the wavelength range 0.4-15.4 Pm. (C) 2008 Elsevier Inc. All rights reserved. C1 [Baldridge, A. M.; Hook, S. J.; Grove, C. I.; Rivera, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Baldridge, AM (reprint author), CALTECH, Jet Prop Lab, MS 183-501,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM alice.m.baldridge@jpl.nasa.gov FU California Institute of Technology, Government sponsorship FX The research described in this paper was carried out at the jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. (C) 2008 California Institute of Technology, Government sponsorship is acknowledged. NR 18 TC 415 Z9 431 U1 4 U2 43 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 APR 15 PY 2009 VL 113 IS 4 BP 711 EP 715 DI 10.1016/j.rse.2008.11.007 PG 5 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 423NQ UT WOS:000264503400002 ER PT J AU Zhang, QY Middleton, EM Margolis, HA Drolet, GG Barr, AA Black, TA AF Zhang, Qingyuan Middleton, Elizabeth M. Margolis, Hank A. Drolet, Guillaume G. Barr, Alan A. Black, T. Andrew TI Can a satellite-derived estimate of the fraction of PAR absorbed by chlorophyll (FAPAR(chl)) improve predictions of light-use efficiency and ecosystem photosynthesis for a boreal aspen forest? SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE MODIS; Aspen; Chlorophyll; Ecosystem flux; Gross primary production; Gross ecosystem production; Light use efficiency (LUE); LUEchl; FAPAR(chl); NDVI; LUEtower ID GROSS PRIMARY PRODUCTION; SURFACE PARAMETERIZATION SIB2; DECIDUOUS BROADLEAF FOREST; GLOBAL PRIMARY PRODUCTION; NET PRIMARY PRODUCTION; LEAF-AREA INDEX; PRODUCT VALIDATION; ATMOSPHERIC GCMS; MODIS DATA; MODEL AB We used daily MODerate resolution Imaging Spectroradiometer (MODIS) imagery obtained over a five-year period to analyze the seasonal and inter-annual variability of the fraction of absorbed photosynthetically active radiation (FAPAR) and photosynthetic light use efficiency (LUE) for the Southern Old Aspen (SOA) flux tower site located near the southern limit of the boreal forest in Saskatchewan, Canada. To obtain the spectral characteristics of a standardized land area to compare with tower measurements, we scaled up the nominal 500 m MODIS products to a 2.5 km x 2.5 kin area (5 x 5 MODIS 500 m grid cells). We then used the scaled-up MODIS products in a coupled canopy-leaf radiative transfer model, PROSAIL-2, to estimate the fraction of absorbed photosynthetically active radiation (APAR) by the part of the canopy dominated by chlorophyll (FAPAR(chl)) versus that by the whole canopy (FAPAR(canopy)). Using the additional information provided by flux tower-based measurements of gross ecosystem production (GEP) and incident PAR, we determined 90-minute averages for APAR and LUE (slope of GEP:APAR) for both the physiologically active foliage (APAR(chl), LUEchl) and for the entire canopy (APAR(canopy), LUEcanopy). The flux tower measurements of GEP were strongly related to the MODIS-derived estimates of APAR(chl), (r(2)=0.78) but only weakly related to APAR(canopy) (r(2)=0.33). Gross LUE between 2001 and 2005 for LUEchl was 0.0241 mu mol C mu mol(-1) PPFD whereas LUEcanopy 6% lower. Time series of the 5-year normalized difference vegetation index (NDVI) were used to estimate the average length of the core growing season as days of year 152-259. Inter-annual variability in the core growing season LUEchl (mu mol C mu mol(-1) PPFD) ranged from 0.0225 in 2003 to 0.0310 in 2004. The five-year time series of LUEchl corresponded well with both the seasonal phase and amplitude of LUE from the tower measurements but this was not the case for LUEcanopy. We conclude that LUE,h, derived from MODIS observations could provide a more physiologically realistic parameter than the more commonly used LUEcanopy as an input to large-scale photosynthesis models. (C) 2009 Elsevier Inc. All rights reserved. C1 [Zhang, Qingyuan; Middleton, Elizabeth M.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. [Zhang, Qingyuan] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Margolis, Hank A.; Drolet, Guillaume G.] Univ Laval, Fac Foresterie & Geomat, CEF, Quebec City, PQ G1K 7P4, Canada. [Barr, Alan A.] Meteorol Serv Canada, Atmospher Sci & Technol Directorate, Saskatoon, SK S7N 3H5, Canada. [Black, T. Andrew] Univ British Columbia, Biometeorol & Soil Phys Grp, Vancouver, BC V6T 1Z4, Canada. RP Zhang, QY (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Bldg 33,Room G321,Code 614-4, Greenbelt, MD 20771 USA. EM qyz72@yahoo.com FU NASA Carbon Cycle Science Program; North American Carbon Program; FCRN and BERMS programs through several Canadian funding sources (Environment Canada, the Canadian Forest Service, NSERC, CFCAS, BIOCAP, Action Plan 2000 and PERD) FX This project was supported by the NASA Carbon Cycle Science Program (Dr. Diane Wickland, Program Manager) under the auspices of the North American Carbon Program. Support was provided to the FCRN and BERMS programs through several Canadian funding sources (Environment Canada, the Canadian Forest Service, NSERC, CFCAS, BIOCAP, Action Plan 2000 and PERD). NR 45 TC 59 Z9 59 U1 3 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 APR 15 PY 2009 VL 113 IS 4 BP 880 EP 888 DI 10.1016/j.rse.2009.01.002 PG 9 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 423NQ UT WOS:000264503400016 ER PT J AU Balin, Y Kaul, B Kokhanenko, G Winker, D AF Balin, Yurii Kaul, Bruno Kokhanenko, Grigorii Winker, David TI Application of circularly polarized laser radiation for sensing of crystal clouds SO OPTICS EXPRESS LA English DT Article ID LIDAR; ORIENTATION; DEPOLARIZATION; PARTICLES AB The application of circularly polarized laser radiation and measurement of the fourth Stokes parameter of scattered radiation considerably reduce the probability of obtaining ambiguous results for radiation depolarization in laser sensing of crystal clouds. The uncertainty arises when cloud particles appear partially oriented by their large diameters along a certain azimuth direction. Approximately in 30% of all cases, the measured depolarization depends noticeably on the orientation of the lidar reference plane with respect to the particle orientation direction. In this case, the corridor of the most probable depolarization values is about 0.1-0.15, but in individual cases, it can be noticeably wider. The present article considers theoretical aspects of this phenomenon and configuration of a lidar capable of measuring the fourth Stokes parameter together with an algorithm of lidar signal processing in the presence of optically thin cloudiness when molecular scattering cannot be neglected. It is demonstrated that the element a(44) of the normalized backscattering phase matrix (BSPM) can be measured. Results of measurements are independent of the presence or absence of azimuthal particle orientation. For sensing in the zenith or nadir, this element characterizes the degree of horizontal orientation of long particle diameters under the action of aerodynamic forces arising during free fall of particles. (C) 2009 Optical Society of America C1 [Balin, Yurii; Kaul, Bruno; Kokhanenko, Grigorii] Russian Acad Sci, Siberian Branch, Inst Atmospher Opt, Tomsk 634055, Russia. [Winker, David] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Balin, Y (reprint author), Russian Acad Sci, Siberian Branch, Inst Atmospher Opt, Tomsk 634055, Russia. EM balin@iao.ru NR 19 TC 10 Z9 12 U1 0 U2 3 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 APR 13 PY 2009 VL 17 IS 8 BP 6849 EP 6859 DI 10.1364/OE.17.006849 PG 11 WC Optics SC Optics GA 432BQ UT WOS:000265108900103 PM 19365512 ER PT J AU Mitra, S Sengupta, AS Ray, S Saha, R Souradeep, T AF Mitra, Sanjit Sengupta, Anand S. Ray, Subharthi Saha, Rajib Souradeep, Tarun TI Cosmic microwave background power spectrum estimation with non-circular beam and incomplete sky coverage SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE cosmic microwave background ID PROBE WMAP OBSERVATIONS; PRIMORDIAL INHOMOGENEITY; STATISTICAL ISOTROPY; HARMONIC-ANALYSIS; 2003 FLIGHT; PYTHON-V; ANISOTROPY; POLARIZATION; MAPS; TEMPERATURE AB Over the last decade, measurements of the cosmic microwave background (CMB) anisotropy have spearheaded the remarkable transition of cosmology into a precision science. However, addressing the systematic effects in the increasingly sensitive, high-resolution, 'full' sky measurements from different CMB experiments poses a stiff challenge. The analysis techniques must not only be computationally fast to contend with the huge size of the data, but the higher sensitivity also limits the simplifying assumptions which can then be invoked to achieve the desired speed without compromising the final precision goals. While maximum likelihood is desirable, the enormous computational cost makes the suboptimal method of power spectrum estimation using pseudo-C-l unavoidable for high-resolution data. The debiasing of the pseudo-C-l needs account for non-circular beams, together with non-uniform sky coverage. We provide a (semi) analytic framework to estimate bias in the power spectrum due to the effect of beam non-circularity and non-uniform sky coverage, including incomplete/masked sky maps and scan strategy. The approach is perturbative in the distortion of the beam from non-circularity, allowing for rapid computations when the beam is mildly non-circular. We advocate that it is computationally advantageous to employ 'soft' azimuthally apodized masks whose spherical harmonic transform die down fast with m. We numerically implement our method for non-rotating beams. We present preliminary estimates of the computational cost to evaluate the bias for the upcoming CMB anisotropy probes (l(max) similar to 3000), with angular resolution comparable to the Planck surveyor mission. We further show that this implementation and estimate are applicable for rotating beams on equal declination scans, and can possibly be extended to simple approximations to other scan strategies. C1 [Mitra, Sanjit; Ray, Subharthi; Saha, Rajib; Souradeep, Tarun] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. [Mitra, Sanjit; Saha, Rajib] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Sengupta, Anand S.] CALTECH, LIGO Lab, Pasadena, CA 91125 USA. [Ray, Subharthi] Univ KwaZulu Natal, Sch Math Sci, Astrophys & Cosmol Res Unit, ZA-4000 Durban, South Africa. [Saha, Rajib] Indian Inst Technol, Kanpur 208016, Uttar Pradesh, India. RP Mitra, S (reprint author), Interuniv Ctr Astron & Astrophys, Post Bag 4, Pune 411007, Maharashtra, India. EM Sanjit.Mitra@jpl.nasa.gov FU Council of Scientific and Industrial Research (India) FX SM would like to thank Council of Scientific and Industrial Research (India) for supporting his research. Part of the writing of this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We thank Kris Gorski, Jeff Jewel and Ben Wandelt for providing the reference and a code for computing Wigner-d functions. We thank Olivier Dore and Mike Nolta for providing us with the data files of the non-circular beam correction estimated by the WMAP team. We acknowledge the fruitful discussions with Francois Bouchet, Simon Prunet and Charles Lawrence. Computations were carried out at the HPC facility available at IUCAA. NR 57 TC 8 Z9 8 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 11 PY 2009 VL 394 IS 3 BP 1419 EP 1439 DI 10.1111/j.1365-2966.2008.14277.x PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 428AP UT WOS:000264820500018 ER PT J AU Temi, P Brighenti, F Mathews, WG AF Temi, Pasquale Brighenti, Fabrizio Mathews, William G. TI EVIDENCE OF STAR FORMATION IN LOCAL S0 GALAXIES: Spitzer OBSERVATIONS OF THE SAURON SAMPLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: ISM; infrared: galaxies; infrared: ISM ID ELLIPTIC GALAXIES; LENTICULAR GALAXIES; PROJECT; EMISSION; KINEMATICS; COLORS; DUST AB We discuss infrared Spitzer observations of early-type galaxies in the SAURON sample at 24, 60, and 170 mu m. When compared with 2MASS K s band luminosities, lenticular (S0) galaxies exhibit a much wider range of mid-to-far-infrared luminosities than elliptical (E) galaxies. Mid- and far-infrared emission from E galaxies is a combination of circumstellar or interstellar emission from local mass-losing red giant stars, dust buoyantly transported from the galactic cores into distant hot interstellar gas and dust accreted from the environment. The source of mid- and far-IR emission in S0 galaxies is quite different and is consistent with low levels of star formation, 0.02-0.2 M(circle dot) yr(-1), in cold, dusty gaseous disks. The infrared 24 mu m-70 mu m color is systematically lower for (mostly S0) galaxies with known molecular disks. Our observations support the conjecture that cold dusty gas in some S0 galaxies is created by stellar mass loss at approximately the same rate that it is consumed by star formation, so the mass depletion of these disks by star formation will be slow. Unlike E galaxies, the infrared luminosities of S0 galaxies correlate with both the mass of molecular gas and the stellar H beta spectral index, and all are related to the recent star formation rate (SFR). However, star formation rates estimated from the H beta-emission-line luminosities L(H beta) in SAURON S0 galaxies are generally much smaller. Since L(H beta) does not correlate with 24 mu m emission from dust heated by young stars, optical emission lines appear to be a poor indicator of SFRs in SAURON S0 galaxies. The absence of H beta emission may be due to a relative absence of OB stars in the initial mass function or to dust absorption of H beta emission lines. C1 [Temi, Pasquale] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA. [Temi, Pasquale] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Brighenti, Fabrizio; Mathews, William G.] Univ Calif Santa Cruz, Board Studies Astron & Astrophys, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. [Brighenti, Fabrizio] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. RP Temi, P (reprint author), NASA, Ames Res Ctr, Astrophys Branch, MS 245-6, Moffett Field, CA 94035 USA. EM pasquale.temi@nasa.gov; fabrizio.brighenti@unibo.it; mathews@ucolick.org FU NASA [1407, RSA 1276023]; Spitzer Theory Grant; NSF FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. Support for this work was provided by NASA through Spitzer Guest Observer grant RSA 1276023. Studies of the evolution of hot gas in elliptical galaxies at UC Santa Cruz are supported by a Spitzer Theory Grant and an NSF grant for which we are very grateful. Finally we thank the referee for thoughtful remarks. NR 23 TC 43 Z9 43 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2009 VL 695 IS 1 BP 1 EP 11 DI 10.1088/0004-637X/695/1/1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 427KZ UT WOS:000264779500001 ER PT J AU Corbet, RHD Zand, JJMI Levine, AM Marshall, FE AF Corbet, R. H. D. Zand, J. J. M. In't Levine, A. M. Marshall, F. E. TI ROSSI X-RAY TIMING EXPLORER AND BeppoSAX OBSERVATIONS OF THE TRANSIENT X-RAY PULSAR XTE J1859+083 SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: individual (XTE J1859+083); stars: neutron; X-rays: binaries ID PROPORTIONAL COUNTER ARRAY; BINARY-SYSTEMS; CALIBRATION; ACCRETION; CATALOG AB We present observations of the 9.8 s X-ray pulsar XTE J1859+083 made with the All Sky Monitor (ASM) and Proportional Counter Array (PCA) on board the Rossi X-ray Timing Explorer, and the Wide Field Camera (WFC) on board BeppoSAX. The ASM data cover a 12 year time interval and show that an extended outburst occurred between approximately MJD 50,250 and 50,460 (1996 June 16 to 1997 January 12). The ASM data excluding this outburst interval suggest a possible modulation with a period of 60.65 +/- 0.08 days. Eighteen sets of PCA observations were obtained over an approximately one month interval in 1999. The flux variability measured with the PCA appears consistent with the possible period found with the ASM. The PCA measurements of the pulse period showed it to decrease nonmonotonically and then to increase significantly. Doppler shifts due to orbital motion rather than accretion torques appear to be better able to explain the pulse period changes. Observations with the WFC during the extended outburst give a position that is consistent with a previously determined PCA error box, but which has a significantly smaller error. The transient nature of XTE J1859+083 and the length of its pulse period are consistent with it being a Be/neutron star binary. The possible 60.65 day orbital period would be of the expected length for a Be star system with a 9.8 s pulse period. C1 [Corbet, R. H. D.] Univ Maryland, Baltimore, MD USA. [Corbet, R. H. D.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Zand, J. J. M. In't] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Zand, J. J. M. In't] Univ Utrecht, Astron Inst, NL-3508 GA Utrecht, Netherlands. [Levine, A. M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Corbet, RHD (reprint author), Univ Maryland, Baltimore, MD USA. EM corbet@umbc.edu; jeanz@sron.nl NR 17 TC 2 Z9 2 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2009 VL 695 IS 1 BP 30 EP 35 DI 10.1088/0004-637X/695/1/30 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 427KZ UT WOS:000264779500003 ER PT J AU Whittet, DCB Cook, AM Chiar, JE Pendleton, YJ Shenoy, SS Gerakines, PA AF Whittet, D. C. B. Cook, A. M. Chiar, J. E. Pendleton, Y. J. Shenoy, S. S. Gerakines, P. A. TI THE NATURE OF CARBON DIOXIDE BEARING ICES IN QUIESCENT MOLECULAR CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; infrared: ISM; ISM: lines and bands; ISM: molecules ID TAURUS DARK CLOUD; SPITZER-SPACE-TELESCOPE; YOUNG STELLAR OBJECTS; INFRARED SPECTROGRAPH; SPECTROSCOPIC SURVEY; GRAIN MANTLES; CO2 ICE; BACKGROUND STARS; INTERSTELLAR ICE; SWS OBSERVATIONS AB The properties of the ices that form in dense molecular clouds represent an important set of initial conditions in the evolution of interstellar and preplanetary matter in regions of active star formation. Of the various spectral features available for study, the bending mode of solid CO(2) near 15 mu m has proven to be a particularly sensitive probe of physical conditions, especially temperature. We present new observations of this absorption feature in the spectrum of Q21-1, a background field star located behind a dark filament in the Cocoon Nebula (IC 5146). We show the profile of the feature to be consistent with a two-component (polar + nonpolar) model for the ices, based on spectra of laboratory analogs with temperatures in the range 10-20 K. The polar component accounts for similar to 85% of the CO(2) in the line of sight. We compare for the first time 15 mu m profiles in three widely separated dark clouds (Taurus, Serpens, and IC 5146), and show that they are indistinguishable to within observational scatter. Systematic differences in the observed CO(2)/H(2)O ratio in the three clouds have little or no effect on the 15 mu m profile. The abundance of elemental oxygen in the ices appears to be a unifying factor, displaying consistent behavior in the three clouds. We conclude that the ice formation process is robust and uniformly efficient, notwithstanding compositional variations arising from differences in how the O is distributed between the primary species (H(2)O, CO(2), and CO) in the ices. C1 [Whittet, D. C. B.; Cook, A. M.] Rensselaer Polytech Inst, Dept Phys Appl Phys & Astron, Troy, NY 12180 USA. [Chiar, J. E.] SETI Inst, Mountain View, CA 94043 USA. [Pendleton, Y. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Shenoy, S. S.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Gerakines, P. A.] Univ Alabama, Dept Phys, Birmingham, AL 35294 USA. RP Whittet, DCB (reprint author), Rensselaer Polytech Inst, Dept Phys Appl Phys & Astron, 110 8th St, Troy, NY 12180 USA. RI Gerakines, Perry/B-9705-2009; Gerakines, Perry/D-2226-2012; OI Gerakines, Perry/0000-0002-9667-5904; Whittet, Douglas/0000-0001-8539-3891 FU NASA [NNX07AK38G, 1290823, 1266411, 1267778] FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. The authors acknowledge NASA support from grant NNX07AK38G and JPL/Caltech Support Agreement No. 1290823 (D. C. B. W.) and JPL/Caltech subcontracts 1266411 and 1267778 (J.E.C.). We are grateful to an anonymous referee for helpful comments that led to improvements to this paper. NR 46 TC 29 Z9 29 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2009 VL 695 IS 1 BP 94 EP 100 DI 10.1088/0004-637X/695/1/94 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 427KZ UT WOS:000264779500008 ER PT J AU Horan, D Acciari, VA Bradbury, SM Buckley, JH Bugaev, V Byrum, KL Cannon, A Celik, O Cesarini, A Chow, YCK Ciupik, L Cogan, P Falcone, AD Fegan, SJ Finley, JP Fortin, P Fortson, LF Gall, D Gillanders, GH Grube, J Gyuk, G Hanna, D Hays, E Kertzman, M Kildea, J Konopelko, A Krawczynski, H Krennrich, F Lang, MJ Lee, K Moriarty, P Nagai, T Niemiec, J Ong, RA Perkins, JS Pohl, M Quinn, J Reynolds, PT Rose, HJ Sembroski, GH Smith, AW Steele, D Swordy, SP Toner, JA Vassiliev, VV Wakely, SP Weekes, TC White, RJ Williams, DA Wood, MD Zitzer, B Aller, HD Aller, MF Baker, M Barnaby, D Carini, MT Charlot, P Dumm, JP Fields, NE Hovatta, T Jordan, B Kovalev, YA Kovalev, YY Krimm, HA Kurtanidze, OM Lahteenmaki, A Le Campion, JF Maune, J Montaruli, T Sadun, AC Smith, S Tornikoski, M Turunen, M Walters, R AF Horan, D. Acciari, V. A. Bradbury, S. M. Buckley, J. H. Bugaev, V. Byrum, K. L. Cannon, A. Celik, O. Cesarini, A. Chow, Y. C. K. Ciupik, L. Cogan, P. Falcone, A. D. Fegan, S. J. Finley, J. P. Fortin, P. Fortson, L. F. Gall, D. Gillanders, G. H. Grube, J. Gyuk, G. Hanna, D. Hays, E. Kertzman, M. Kildea, J. Konopelko, A. Krawczynski, H. Krennrich, F. Lang, M. J. Lee, K. Moriarty, P. Nagai, T. Niemiec, J. Ong, R. A. Perkins, J. S. Pohl, M. Quinn, J. Reynolds, P. T. Rose, H. J. Sembroski, G. H. Smith, A. W. Steele, D. Swordy, S. P. Toner, J. A. Vassiliev, V. V. Wakely, S. P. Weekes, T. C. White, R. J. Williams, D. A. Wood, M. D. Zitzer, B. Aller, H. D. Aller, M. F. Baker, M. Barnaby, D. Carini, M. T. Charlot, P. Dumm, J. P. Fields, N. E. Hovatta, T. Jordan, B. Kovalev, Y. A. Kovalev, Y. Y. Krimm, H. A. Kurtanidze, O. M. Lahteenmaki, A. Le Campion, J. F. Maune, J. Montaruli, T. Sadun, A. C. Smith, S. Tornikoski, M. Turunen, M. Walters, R. TI MULTIWAVELENGTH OBSERVATIONS OF MARKARIAN 421 IN 2005-2006 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: individual (Markarian 421); gamma rays: observations; X-rays: individual (Markarian 421) ID ACTIVE GALACTIC NUCLEI; BL-LACERTAE OBJECTS; GAMMA-RAY EMISSION; SPECTRAL SLOPE VARIABILITY; TEV BLAZAR MARKARIAN-421; X-RAY; LAC OBJECTS; CORRELATED VARIABILITY; TIMING EXPLORER; PROTON BLAZAR AB Since 2005 September, the Whipple 10 m Gamma-ray Telescope has been operated primarily as a blazar monitor. The five northern hemisphere blazars that have already been detected at the Whipple Observatory, Markarian 421 (Mrk 421), H1426+428, Mrk 501, 1ES 1959+650, and 1ES 2344+514, are monitored routinely each night that they are visible. We report on the Mrk 421 observations taken from 2005 November to 2006 June in the gamma-ray, X-ray, optical, and radio bands. During this time, Mrk 421 was found to be variable at all wavelengths probed. Both the variability and the correlations among different energy regimes are studied in detail here. A tentative correlation, with large spread, was measured between the X-ray and gamma-ray bands, while no clear correlation was evident among the other energy bands. In addition to this, the well-sampled spectral energy distribution of Mrk 421 (1101+384) is presented for three different activity levels. The observations of the other blazar targets will be reported separately. C1 [Horan, D.; Byrum, K. L.; Hays, E.; Smith, A. W.] Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60439 USA. [Acciari, V. A.; Moriarty, P.] Galway Mayo Inst Technol, Dept Phys & Life Sci, Galway, Ireland. [Acciari, V. A.; Kildea, J.; Perkins, J. S.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Bradbury, S. M.; Rose, H. J.; White, R. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Cannon, A.; Grube, J.; Quinn, J.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Cannon, A.; Grube, J.; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Celik, O.; Chow, Y. C. K.; Fegan, S. J.; Ong, R. A.; Vassiliev, V. V.; Wood, M. D.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Cesarini, A.; Gillanders, G. H.; Lang, M. J.; Toner, J. A.] Natl Univ Ireland, Sch Phys, Galway, Ireland. [Ciupik, L.; Fortson, L. F.; Gyuk, G.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cogan, P.; Hanna, D.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Falcone, A. D.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Finley, J. P.; Gall, D.; Sembroski, G. H.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Fortin, P.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Hays, E.; Swordy, S. P.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Hays, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Konopelko, A.] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA. [Krennrich, F.; Nagai, T.; Niemiec, J.; Pohl, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Niemiec, J.] Inst Fizyki Hadrowej PAN, PL-31342 Krakow, Poland. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Aller, H. D.; Aller, M. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Baker, M.; Dumm, J. P.; Fields, N. E.; Montaruli, T.] Univ Wisconsin, Madison, WI 53706 USA. [Barnaby, D.; Carini, M. T.; Maune, J.; Smith, S.; Walters, R.] Western Kentucky Univ, Bowling Green, KY 42104 USA. [Charlot, P.; Le Campion, J. F.] Univ Bordeaux, Observ Aquitain Sci Univ, F-33271 Floirac, France. [Charlot, P.; Le Campion, J. F.] CNRS, UMR 5804, Lab Astrophys Bordeaux, F-33271 Floirac, France. [Hovatta, T.; Lahteenmaki, A.; Tornikoski, M.; Turunen, M.] Helsinki Univ Technol, Metsahovi Radio Observ, Kylmala 02540, Finland. [Jordan, B.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 4, Ireland. [Kovalev, Y. A.; Kovalev, Y. Y.] Ctr Astro Space, PN Lebedev Phys Inst, Moscow 117997, Russia. [Kovalev, Y. Y.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Krimm, H. A.] CRESST, Greenbelt, MD 20771 USA. [Krimm, H. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Kurtanidze, O. M.] Abastumani Observ, Abastumani, GA USA. [Sadun, A. C.] Univ Colorado, Dept Phys, Denver, CO 80208 USA. RP Horan, D (reprint author), Argonne Natl Lab, Div High Energy Phys, 9700 S Cass Ave, Argonne, IL 60439 USA. EM deirdre.horan@gmail.com RI Kovalev, Yuri/J-5671-2013; Lahteenmaki, Anne/L-5987-2013; Hays, Elizabeth/D-3257-2012; Kurtanidze, Omar/J-6237-2014; Kovalev, Yuri/N-1053-2015 OI Kovalev, Yuri/0000-0001-9303-3263; NR 61 TC 35 Z9 35 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2009 VL 695 IS 1 BP 596 EP 618 DI 10.1088/0004-637X/695/1/596 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 427KZ UT WOS:000264779500050 ER PT J AU Vinko, J Sarneczky, K Balog, Z Immler, S Sugerman, BEK Brown, PJ Misselt, K Szabo, GM Csizmadia, S Kun, M Klagyivik, P Foley, RJ Filippenko, AV Csak, B Kiss, LL AF Vinko, J. Sarneczky, K. Balog, Z. Immler, S. Sugerman, B. E. K. Brown, P. J. Misselt, K. Szabo, Gy. M. Csizmadia, Sz. Kun, M. Klagyivik, P. Foley, R. J. Filippenko, A. V. Csak, B. Kiss, L. L. TI THE YOUNG, MASSIVE, STAR CLUSTER SANDAGE-96 AFTER THE EXPLOSION OF SUPERNOVA 2004dj IN NGC 2403 SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: individual (2004dj) ID RED SUPERGIANT PROGENITOR; EVOLUTIONARY SYNTHESIS MODELS; SPACE-TELESCOPE IMAGES; II-P SUPERNOVAE; STELLAR POPULATIONS; MAGELLANIC CLOUDS; NEARBY GALAXIES; AGB STARS; X-RAY; SWIFT AB The bright Type II-plateau supernova (SN) 2004dj occurred within the young, massive stellar cluster Sandage-96 in a spiral arm of NGC 2403. New multiwavelength observations obtained with several ground-based and space-based telescopes were combined to study the radiation from Sandage-96 after SN 2004dj faded away. Sandage-96 started to dominate the flux in the optical bands starting from 2006 September (similar to 800 days after explosion). The optical fluxes are equal to the pre-explosion ones within the observational uncertainties. An optical Keck spectrum obtained similar to 900 days after explosion shows the dominant blue continuum from the cluster stars shortward of 6000 angstrom as well as strong SN nebular emission lines redward. The integrated spectral energy distribution (SED) of the cluster has been extended into the ultraviolet region by archival XMM-Newton and new Swift observations, and compared with theoretical models. The outer parts of the cluster have been resolved by the Hubble Space Telescope, allowing the construction of a color-magnitude diagram (CMD). The fitting of the cluster SED with theoretical isochrones results in cluster ages distributed between 10 and 40 Myr, depending on the assumed metallicity and the theoretical model family. The isochrone fitting of the CMDs indicates that the resolved part of the cluster consists of stars having a bimodal age distribution: a younger population at similar to 10-16 Myr and an older one at similar to 32-100 Myr. The older population has an age distribution similar to that of the other nearby field stars. This may be explained with the hypothesis that the outskirts of Sandage-96 are contaminated by stars captured from the field during cluster formation. The young age of Sandage-96 and the comparison of its pre and postexplosion SEDs suggest 12 less than or similar to M-prog less than or similar to 20 M-circle dot as the most probable mass range for the progenitor of SN 2004dj. This is consistent with, but perhaps slightly higher than, most of the other Type II-plateau SN progenitor masses determined so far. C1 [Vinko, J.; Sarneczky, K.; Balog, Z.; Csak, B.] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary. [Vinko, J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Balog, Z.; Misselt, K.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Immler, S.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Xray Astrophys Lab Code 662, Greenbelt, MD 20771 USA. [Sugerman, B. E. K.] Goucher Coll, Dept Phys & Astron, Baltimore, MD 21204 USA. [Brown, P. J.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Szabo, Gy. M.] Univ Szeged, Dept Expt Phys, Szeged, Hungary. [Csizmadia, Sz.] German Aerosp Ctr, Inst Planetary Res, D-12489 Berlin, Germany. [Kun, M.] Hungarian Acad Sci, Konkoly Observ, Budapest, Hungary. [Klagyivik, P.] Eotvos Lorand Univ, Dept Astron, Budapest, Hungary. [Foley, R. J.; Filippenko, A. V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Foley, R. J.] Ctr Astrophys, Cambridge, MA 02138 USA. [Kiss, L. L.] Univ Sydney, Inst Astron, Sch Phys, Sydney, NSW 2006, Australia. RP Vinko, J (reprint author), Univ Szeged, Dept Opt & Quantum Elect, Dom ter 9, H-6720 Szeged, Hungary. EM vinko@physx.u-szeged.hu RI Kiss, Laszlo/A-2539-2008; Szabo, Gyula/A-8310-2012 FU NASA [NAS 5-26555, 1255094]; W. M. Keck Foundation; STScI [GO-10607, GO-10182]; NSF [AST-0607485, AST-0707769]; Texas Advanced Research Project grant [AST-0094]; Hungarian OTKA [TS049872]; Swift Science Center FX This work was based in part on observations made with the NASA/ESA HST, obtained from the Data Archive at the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. It is also based in part on data from the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. This work was partially supported by NASA through contract 1255094 issued by JPL/Caltech, by NASA/HST grants GO-10607 (B. S.) and GO-10182 (A. V. F.) from STScI, and by NSF grant AST-0607485 (A. V. F.). J. V. received support from NSF grant AST-0707769 and Texas Advanced Research Project grant AST-0094 to J. C. Wheeler, and from Hungarian OTKA grant TS049872.; We are grateful for the support received from the Swift Science Center. An anonymous referee provided many useful suggestions and advice that helped us extend and improve the paper. The SIMBAD database at CDS, the NASA ADS and NED, and the Canadian Astronomy Data Centre have been used to access data and references. NR 57 TC 28 Z9 28 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 APR 10 PY 2009 VL 695 IS 1 BP 619 EP 635 DI 10.1088/0004-637X/695/1/619 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 427KZ UT WOS:000264779500051 ER PT J AU Ogliore, RC Stone, EC Leske, RA Mewaldt, RA Wiedenbeck, ME Binns, WR Israel, MH von Rosenvinge, TT de Nolfo, GA Moskalenko, IV AF Ogliore, R. C. Stone, E. C. Leske, R. A. Mewaldt, R. A. Wiedenbeck, M. E. Binns, W. R. Israel, M. H. von Rosenvinge, T. T. de Nolfo, G. A. Moskalenko, I. V. TI THE PHOSPHORUS, SULFUR, ARGON, AND CALCIUM ISOTOPIC COMPOSITION OF THE GALACTIC COSMIC RAY SOURCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic rays; Galaxy: abundances; ISM: abundances; ISM: bubbles; supernovae: general ID SUPERBUBBLE ORIGIN; SUPERNOVA-REMNANTS; STELLAR EVOLUTION; ABUNDANCES; STARS; MODELS; DUST; NUCLEOSYNTHESIS; PROPAGATION; ELEMENTS AB Galactic cosmic ray (GCR) measurements of the phosphorus, sulfur, argon, and calcium isotopes made by the Cosmic Ray Isotope Spectrometer aboard the Advanced Composition Explorer are reported over the energy range from similar to 100 to similar to 400 MeV nucleon(-1). The propagation of cosmic rays through the Galaxy and heliosphere is modeled with constraints imposed by measurements. Isotopic source abundance ratios (31)P/(32)S, (34)S/(32)S, (38)Ar/(36)Ar, and (44)Ca/(40)Ca are deduced. The derived (31)P/(32)S ratio is 2.34 +/- 0.34 times larger than the solar system value, lending further credence to the suggestion that refractory elements are enriched in the GCRs due to the sputtering of ions off grains in the cores of superbubbles. By determining the GCR source abundances of argon (a noble gas) and calcium (a refractory), it is determined that material in grains is accelerated to GCR energies a factor of 6.4 +/- 0.3 more efficiently than gas-phase material in this charge range. With this information, the dust fraction of phosphorus and sulfur in the interstellar material that is mixed with stellar ejecta to form the GCR seed material is found to be consistent with astronomical observations. C1 [Wiedenbeck, M. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Binns, W. R.; Israel, M. H.] Washington Univ, St Louis, MO 63130 USA. [von Rosenvinge, T. T.; de Nolfo, G. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Moskalenko, I. V.] Stanford Univ, HEPL, Stanford, CA 94305 USA. [Moskalenko, I. V.] Stanford Univ, KIPAC, Stanford, CA 94305 USA. [Ogliore, R. C.; Stone, E. C.; Leske, R. A.; Mewaldt, R. A.] CALTECH, Pasadena, CA 91125 USA. RP Ogliore, RC (reprint author), Univ Calif Berkeley, Berkeley Space Sci Lab, 7 Gauss Way, Berkeley, CA 94704 USA. EM ogliore@ssl.berkeley.edu RI de Nolfo, Georgia/E-1500-2012; Moskalenko, Igor/A-1301-2007 OI Moskalenko, Igor/0000-0001-6141-458X FU NASA at the California Institute of Technology [NAG5-12929]; Jet Propulsion Laboratory; Goddard Space Flight Center; Washington University; APRA FX This work was supported by NASA at the California Institute of Technology (under grant NAG5-12929), the Jet Propulsion Laboratory, the Goddard Space Flight Center, and Washington University. I. V. M. acknowledges NASA and APRA grants for partial support. NR 65 TC 3 Z9 3 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2009 VL 695 IS 1 BP 666 EP 678 DI 10.1088/0004-637X/695/1/666 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 427KZ UT WOS:000264779500055 ER PT J AU Soummer, R Pueyo, L Ferrari, A Aime, C Sivaramakrishnan, A Yaitskova, N AF Soummer, Remi Pueyo, Laurent Ferrari, Andre Aime, Claude Sivaramakrishnan, Anand Yaitskova, Natalia TI APODIZED PUPIL LYOT CORONAGRAPHS FOR ARBITRARY APERTURES. II. THEORETICAL PROPERTIES AND APPLICATION TO EXTREMELY LARGE TELESCOPES SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation: high angular resolution ID SPHEROIDAL WAVE-FUNCTIONS; EXTRASOLAR GIANT PLANETS; PHASE-MASK CORONAGRAPH; STELLAR CORONAGRAPH; RECTANGULAR APERTURES; FOURIER-ANALYSIS; APODIZATION; PRINCIPLE AB We study the application of Lyot coronagraphy to future Extremely Large Telescopes (ELTs), showing that Apodized Pupil Lyot Coronagraphs enable high-contrast imaging for exoplanet detection and characterization with ELTs. We discuss the properties of the optimal pupil apodizers for this application (generalized prolate spheroidal functions). The case of a circular aperture telescope with a central obstruction is considered in detail, and we discuss the effects of primary mirror segmentation and secondary mirror support structures as a function of the occulting mask size. In most cases where inner working distance is critical, e. g., for exoplanet detection, these additional features do not alter the solutions derived with just the central obstruction, although certain applications such as quasar-host galaxy coronagraphic observations could benefit from designs that explicitly accomodate ELT spider geometries. We illustrate coronagraphic designs for several ELT geometries including ESO/OWL, the Thirty Mirror Telescope, the Giant Magellan Telescope, and describe numerical methods for generating these designs. C1 [Soummer, Remi] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Pueyo, Laurent] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ferrari, Andre; Aime, Claude] Univ Nice Sophia Antipolis, LUAN, F-06108 Nice, France. [Sivaramakrishnan, Anand] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [Yaitskova, Natalia] European So Observ, D-85748 Garching, Germany. EM lpueyo@jpl.nasa.gov; ferrari@unice.fr; aime@unice.fr; anand@amnh.org; nyaitsko@eso.org FU Michelson Postdoctoral Fellowship; NASA; AMNH Kalbfleisch; National Science Fundation [AST-0215793, AST-0334916]; National Science Foundation Science and Technology Center for Adaptive Optics, managed by the University of California at Santa Cruz [AST 98-76783] FX R. S. is supported by a Michelson Postdoctoral Fellowship, under contract to the Jet Propulsion Laboratory (JPL) funded by NASA. JPL is managed for NASA by the California Institute of Technology and partially supported by an AMNH Kalbfleisch Fellowship. This work is based upon work partially supported by the National Science Fundation: AST-0215793 and AST-0334916 and has also been partially supported by the National Science Foundation Science and Technology Center for Adaptive Optics, managed by the University of California at Santa Cruz under cooperative agreement AST 98-76783. NR 44 TC 29 Z9 29 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2009 VL 695 IS 1 BP 695 EP 706 DI 10.1088/0004-637X/695/1/695 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 427KZ UT WOS:000264779500057 ER PT J AU Godfrey, LEH Bicknell, GV Lovell, JEJ Jauncey, DL Gelbord, J Schwartz, DA Marshall, HL Birkinshaw, M Georganopoulos, M Murphy, DW Perlman, ES Worrall, DM AF Godfrey, L. E. H. Bicknell, G. V. Lovell, J. E. J. Jauncey, D. L. Gelbord, J. Schwartz, D. A. Marshall, H. L. Birkinshaw, M. Georganopoulos, M. Murphy, D. W. Perlman, E. S. Worrall, D. M. TI A MULTIWAVELENGTH STUDY OF THE HIGH SURFACE BRIGHTNESS HOT SPOT IN PKS 1421-490 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: jets; quasars: individual (PKS 1421-490) ID X-RAY-EMISSION; MAGNETOSONIC SHOCK-WAVES; POWERFUL RADIO GALAXIES; ACTIVE GALACTIC NUCLEI; PARTICLE-ACCELERATION; CYGNUS-A; CHANDRA OBSERVATIONS; PHYSICAL CONDITIONS; RELATIVISTIC JETS; OPTICAL-EMISSION AB Long Baseline Array imaging of the z = 0.663 broadline radio galaxy PKS 1421-490 reveals a 400 pc diameter high surface brightness hot spot at a projected distance of similar to 40 kpc from the active galactic nucleus. The isotropic X-ray luminosity of the hot spot, L2-10 (keV) = 3 x 10(44) ergs s(-1), is comparable to the isotropic X-ray luminosity of the entire X-ray jet of PKS 0637-752, and the peak radio surface brightness is hundreds of times greater than that of the brightest hot spot in Cygnus A. We model the radio to X-ray spectral energy distribution using a one-zone synchrotron self-Compton model with a near equipartition magnetic field strength of 3 mG. There is a strong brightness asymmetry between the approaching and receding hotspots and the hot spot spectrum remains flat (alpha approximate to 0.5) well beyond the predicted cooling break for a 3 mG magnetic field, indicating that the hotspot emission may be Doppler beamed. A high plasma velocity beyond the terminal jet shock could be the result of a dynamically important magnetic field in the jet. There is a change in the slope of the hotspot radio spectrum at GHz frequencies, which we model by incorporating a cutoff in the electron energy distribution at gamma(min) approximate to 650, with higher values implied if the hotspot emission is Doppler beamed. We show that a sharp decrease in the electron number density below a Lorentz factor of 650 would arise from the dissipation of bulk kinetic energy in an electron/proton jet with a Lorentz factor Gamma(jet) greater than or similar to 5. C1 [Godfrey, L. E. H.; Bicknell, G. V.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Godfrey, L. E. H.; Lovell, J. E. J.; Jauncey, D. L.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 2121, Australia. [Lovell, J. E. J.] CSIRO, Sydney, NSW 2070, Australia. [Lovell, J. E. J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. [Schwartz, D. A.; Birkinshaw, M.; Worrall, D. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marshall, H. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Birkinshaw, M.; Worrall, D. M.] Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. [Georganopoulos, M.; Perlman, E. S.] Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Dept Phys, Baltimore, MD 21250 USA. [Georganopoulos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Murphy, D. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Godfrey, LEH (reprint author), Australian Natl Univ, Res Sch Astron & Astrophys, Cotter Rd, Weston, ACT 2611, Australia. EM lgodfrey@mso.anu.edu.au RI Godfrey, Leith/B-5283-2013 FU Commonwealth of Australia for operation as a National Facility managed by CSIRO; National Aeronautics and Space Administration; National Science Foundation FX L. E. H. G. thanks John Kirk for very helpful discussions on the topic of particle acceleration, and Emil Lenc for supplying the cordump patch for DIFMAP. L. E. H. G. also thanks the Grote Reber Foundation for financial support. The Australia Telescope Compact Array and Long Baseline Array are part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. This paper includes data gathered with the 6.5 meter Magellan Telescopes located at Las Campanas Observatory, Chile. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 66 TC 26 Z9 26 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 APR 10 PY 2009 VL 695 IS 1 BP 707 EP 723 DI 10.1088/0004-637X/695/1/707 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 427KZ UT WOS:000264779500058 ER PT J AU Haas, M Willner, SP Heymann, F Ashby, MLN Fazio, GG Wilkes, BJ Chini, R Siebenmorgen, R Stern, D AF Haas, Martin Willner, S. P. Heymann, Frank Ashby, M. L. N. Fazio, G. G. Wilkes, Belinda J. Chini, Rolf Siebenmorgen, Ralf Stern, Daniel TI CLUSTERING OF RED GALAXIES AROUND THE z=1.53 QUASAR 3C 270.1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (3C270.1); infrared: galaxies; quasars: general ID SPITZER-SPACE-TELESCOPE; LYMAN-BREAK GALAXIES; RADIO GALAXIES; DISCOVERY; OBJECTS; IRAC; PROTOCLUSTER; OVERDENSITY; PHOTOMETRY; SOFTWARE AB In the paradigm of hierarchical galaxy formation, luminous radio galaxies mark mass assembly peaks that should contain clusters of galaxies. Observations of the z = 1.53 quasar 3C 270.1 with the Spitzer Space Telescope at 3.6-24 mu m and with the 6.5 m MMT in the z' and Y bands allow the detection of potential cluster members via photometric redshifts. Compared with nearby control fields, there is an excess of similar to 11 extremely red objects (EROs) at 1.33 <= z(phot) <= 1.73, consistent with a protocluster around the quasar. The spectral energy distributions of 3/4 of the EROs are better fitted with passive elliptical galaxies than with dust-reddened starbursts, and of four sources well detected on an archival Hubble Space Telescope (HST) snapshot image, all have undisturbed morphologies. However, one ERO, not covered by the HST image, is a double source with 0.'' 8 separation on the z' image and a marginal (2 sigma) 24 mu m detection indicating a dust-enshrouded starburst. The EROs are more luminous than L(star) (H = -23.6 AB mag at z approximate to 1.5). C1 [Haas, Martin; Heymann, Frank; Chini, Rolf] Ruhr Univ Bochum, Inst Astron, D-44801 Bochum, Germany. [Willner, S. P.; Ashby, M. L. N.; Fazio, G. G.; Wilkes, Belinda J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Heymann, Frank; Siebenmorgen, Ralf] European So Observ, D-85748 Garching, Germany. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Haas, M (reprint author), Ruhr Univ Bochum, Inst Astron, Univ Str 150, D-44801 Bochum, Germany. EM haas@astro.rub.de OI Wilkes, Belinda/0000-0003-1809-2364 FU NASA; Nordrhein-Westfalische Akademie der Wissenschaften FX This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory (JPL), Caltech under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. The ground-based observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. This research has made use of the NASA/IPAC Extragalactic Database (NED) and of the Sloan Digital Sky Survey (SDSS DR6). We thank Dominik Bomans and Hans Hippelein for valuable discussions and comments on the manuscript, and an anonymous referee for the constructive, critical report. M. H. is supported by the Nordrhein-Westfalische Akademie der Wissenschaften. NR 40 TC 4 Z9 4 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2009 VL 695 IS 1 BP 724 EP 731 DI 10.1088/0004-637X/695/1/724 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 427KZ UT WOS:000264779500059 ER PT J AU Abdo, AA Ackermann, M Atwood, WB Baldini, L Ballet, J Barbiellini, G Baring, MG Bastieri, D Baughman, BM Bechtol, K Bellazzini, R Berenji, B Bloom, ED Bonamente, E Borgland, AW Bregeon, J Brez, A Brigida, M Bruel, P Burnett, TH Caliandro, GA Cameron, RA Caraveo, PA Casandjian, JM Cecchi, C Charles, E Chekhtman, A Cheung, CC Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Cominsky, LR Conrad, J Dermer, CD de Angelis, A de Palma, F Digel, SW Donato, D Dormody, M Silva, EDE Drell, PS Dubois, R Dumora, D Edmonds, Y Farnier, C Favuzzi, C Fleury, P Focke, WB Frailis, M Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giebels, B Giglietto, N Giordano, F Glanzman, T Godfrey, G Grenier, IA Grondin, MH Grove, JE Guillemot, L Guiriec, S Harding, AK Hayashida, M Hays, E Hughes, RE Johannesson, G Johnson, AS Johnson, RP Johnson, TJ Johnson, WN Johnston, S Kamae, T Katagiri, H Kataoka, J Kawai, N Kerr, M Knodlseder, J Komin, N Kramer, M Kuehn, F Kuss, M Latronico, L Lee, SH Lemoine-Goumard, M Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Makeev, A Marelli, M Mazziotta, MN McConville, W McEnery, JE Meurer, C Michelson, PF Mitthumsiri, W Mizuno, T Moiseev, AA Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nolan, PL Nuss, E Ohsugi, T Omodei, N Orlando, E Ormes, JF Paneque, D Panetta, JH Parent, D Pepe, M Pesce-Rollins, M Piron, F Porter, TA Raino, S Rando, R Razzano, M Reimer, A Reimer, O Reposeur, T Ritz, S Rochester, LS Rodriguez, AY Romani, RW Roth, M Ryde, F Sadrozinski, HFW Sanchez, D Sander, A Parkinson, PMS Sgro, C Siskind, EJ Smith, DA Smith, PD Spandre, G Spinelli, P Starck, JL Strickman, MS Suson, DJ Tajima, H Takahashi, H Tanaka, T Thayer, JB Thayer, JG Thompson, DJ Thorsett, SE Tibaldo, L Torres, DF Tosti, G Tramacere, A Uchiyama, Y Usher, TL Van Etten, A Vilchez, N Vitale, V Waite, AP Watters, K Wood, KS Ylinen, T Ziegler, M Hobbs, G Keith, M Manchester, RN Weltevrede, P AF Abdo, A. A. Ackermann, M. Atwood, W. B. Baldini, L. Ballet, J. Barbiellini, G. Baring, M. G. Bastieri, D. Baughman, B. M. Bechtol, K. Bellazzini, R. Berenji, B. Bloom, E. D. Bonamente, E. Borgland, A. W. Bregeon, J. Brez, A. Brigida, M. Bruel, P. Burnett, T. H. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Casandjian, J. M. Cecchi, C. Charles, E. Chekhtman, A. Cheung, C. C. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Cominsky, L. R. Conrad, J. Dermer, C. D. de Angelis, A. de Palma, F. Digel, S. W. Donato, D. Dormody, M. do Couto e Silva, E. Drell, P. S. Dubois, R. Dumora, D. Edmonds, Y. Farnier, C. Favuzzi, C. Fleury, P. Focke, W. B. Frailis, M. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giebels, B. Giglietto, N. Giordano, F. Glanzman, T. Godfrey, G. Grenier, I. A. Grondin, M. -H. Grove, J. E. Guillemot, L. Guiriec, S. Harding, A. K. Hayashida, M. Hays, E. Hughes, R. E. Johannesson, G. Johnson, A. S. Johnson, R. P. Johnson, T. J. Johnson, W. N. Johnston, S. Kamae, T. Katagiri, H. Kataoka, J. Kawai, N. Kerr, M. Knoedlseder, J. Komin, N. Kramer, M. Kuehn, F. Kuss, M. Latronico, L. Lee, S. -H. Lemoine-Goumard, M. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Makeev, A. Marelli, M. Mazziotta, M. N. McConville, W. McEnery, J. E. Meurer, C. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nolan, P. L. Nuss, E. Ohsugi, T. Omodei, N. Orlando, E. Ormes, J. F. Paneque, D. Panetta, J. H. Parent, D. Pepe, M. Pesce-Rollins, M. Piron, F. Porter, T. A. Raino, S. Rando, R. Razzano, M. Reimer, A. Reimer, O. Reposeur, T. Ritz, S. Rochester, L. S. Rodriguez, A. Y. Romani, R. W. Roth, M. Ryde, F. Sadrozinski, H. F. -W. Sanchez, D. Sander, A. Parkinson, P. M. Saz Sgro, C. Siskind, E. J. Smith, D. A. Smith, P. D. Spandre, G. Spinelli, P. Starck, J. -L. Strickman, M. S. Suson, D. J. Tajima, H. Takahashi, H. Tanaka, T. Thayer, J. B. Thayer, J. G. Thompson, D. J. Thorsett, S. E. Tibaldo, L. Torres, D. F. Tosti, G. Tramacere, A. Uchiyama, Y. Usher, T. L. Van Etten, A. Vilchez, N. Vitale, V. Waite, A. P. Watters, K. Wood, K. S. Ylinen, T. Ziegler, M. Hobbs, G. Keith, M. Manchester, R. N. Weltevrede, P. TI DISCOVERY OF PULSED gamma-RAYS FROM THE YOUNG RADIO PULSAR PSR J1028-5819 WITH THE FERMI LARGE AREA TELESCOPE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE pulsars: general; stars: neutron ID TIME-DIFFERENCING TECHNIQUE; SPACE TELESCOPE; RADIATION; EMISSION; CATALOG; SEARCH; GAPS AB Radio pulsar PSR J1028-5819 was recently discovered in a high-frequency search (at 3.1 GHz) in the error circle of the Energetic Gamma-Ray Experiment Telescope (EGRET) source 3EG J1027-5817. The spin-down power of this young pulsar is great enough to make it very likely the counterpart for the EGRET source. We report here the discovery of gamma-ray pulsations from PSR J1028-5819 in early observations by the Large Area Telescope (LAT) on the Fermi Gamma-Ray Space Telescope. The gamma-ray light curve shows two sharp peaks having phase separation of 0.460 +/- 0.004, trailing the very narrow radio pulse by 0.200 +/- 0.003 in phase, very similar to that of other known gamma-ray pulsars. The measured gamma-ray flux gives an efficiency for the pulsar of similar to 10-20% (for outer magnetosphere beam models). No evidence of a surrounding pulsar wind nebula is seen in the current Fermi data but limits on associated emission are weak because the source lies in a crowded region with high background emission. However, the improved angular resolution afforded by the LAT enables the disentanglement of the previous COS-B and EGRET source detections into at least two distinct sources, one of which is now identified as PSR J1028-5819. C1 [Cheung, C. C.; Donato, D.; Gehrels, N.; Harding, A. K.; Hays, E.; Johnson, T. J.; McConville, W.; McEnery, J. E.; Ritz, S.; Thompson, D. J.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Abdo, A. A.; Chekhtman, A.; Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Makeev, A.; Strickman, M. S.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Ackermann, M.; Bechtol, K.; Berenji, B.; Bloom, E. D.; Borgland, A. W.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Edmonds, Y.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Lee, S. -H.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Paneque, D.; Panetta, J. H.; Reimer, A.; Reimer, O.; Rochester, L. S.; Romani, R. W.; Tajima, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Van Etten, A.; Waite, A. P.; Watters, K.] Stanford Univ, W W Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Ackermann, M.; Bechtol, K.; Berenji, B.; Bloom, E. D.; Borgland, A. W.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Edmonds, Y.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Lee, S. -H.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Paneque, D.; Panetta, J. H.; Reimer, A.; Reimer, O.; Rochester, L. S.; Romani, R. W.; Tajima, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Van Etten, A.; Waite, A. P.; Watters, K.] Stanford Univ, Stanford Linear Accelerator Ctr, Stanford, CA 94305 USA. [Atwood, W. B.; Dormody, M.; Johnson, R. P.; Porter, T. A.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Thorsett, S. E.; Ziegler, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Atwood, W. B.; Dormody, M.; Johnson, R. P.; Porter, T. A.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Thorsett, S. E.; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Brez, A.; Kuss, M.; Latronico, L.; Omodei, N.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Komin, N.; Starck, J. -L.] Univ Paris, CEA Saclay, Serv Astrophys, Lab AIM,CEA,IRFU,CNRS, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy. [Baring, M. G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA. [Bastieri, D.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Baughman, B. M.; Hughes, R. E.; Kuehn, F.; Sander, A.; Smith, P. D.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Brigida, M.; Caliandro, G. A.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; Caliandro, G. A.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fleury, P.; Giebels, B.; Sanchez, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Burnett, T. H.; Kerr, M.; Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Caraveo, P. A.; Marelli, M.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Chekhtman, A.; Makeev, A.] George Mason Univ, Fairfax, VA 22030 USA. [Cohen-Tanugi, J.; Farnier, C.; Guiriec, S.; Komin, N.; Nuss, E.; Piron, F.] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticules, Montpellier, France. [Cominsky, L. R.] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA. [Conrad, J.; Meurer, C.; Ryde, F.; Ylinen, T.] Oskar Klein Ctr Cosmo Particle Phys, SE-10691 Stockholm, Sweden. [Conrad, J.; Ryde, F.; Ylinen, T.] Royal Inst Technol, Dept Phys, KTH, SE-10691 Stockholm, Sweden. [Conrad, J.; Meurer, C.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [de Angelis, A.; Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.; Frailis, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. [Dumora, D.; Grondin, M. -H.; Guillemot, L.; Lemoine-Goumard, M.; Lott, B.; Parent, D.; Reposeur, T.; Smith, D. A.] CEN Bordeaux Gradignan, CNRS, IN2P3, UMR 5797, F-33175 Gradignan, France. [Dumora, D.; Grondin, M. -H.; Guillemot, L.; Lemoine-Goumard, M.; Lott, B.; Parent, D.; Reposeur, T.; Smith, D. A.] Univ Bordeaux, CEN Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France. [Fukazawa, Y.; Katagiri, H.; Mizuno, T.; Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima 7398526, Japan. [Fukazawa, Y.; Katagiri, H.; Mizuno, T.; Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima 7398526, Japan. [Gasparrini, D.] ASI, Sci Data Ctr, I-00044 Frascati, Roma, Italy. [Gehrels, N.; Johnson, T. J.; Ritz, S.] Univ Maryland, College Pk, MD 20742 USA. [Johnston, S.; Hobbs, G.; Keith, M.; Manchester, R. N.; Weltevrede, P.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Kataoka, J.; Kawai, N.] Tokyo Inst Technol, Dept Phys, Tokyo 1528551, Japan. [Kawai, N.] RIKEN, Inst Phys & Chem Res, Cosm Radiat Lab, Wako, Saitama 3510198, Japan. [Knoedlseder, J.; Vilchez, N.] CNR, SUPS 47, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. [Kramer, M.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Rodriguez, A. Y.; Torres, D. F.] CSIC, IEEC, Inst Ciencies Espai, Barcelona 08193, Spain. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Torres, D. F.] ICREA, Barcelona, Spain. [Tramacere, A.] CIFS, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Ylinen, T.] Univ Kalmar, Sch Pure & Appl Nat Sci, SE-39182 Kalmar, Sweden. RP Harding, AK (reprint author), NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. EM ahardingx@yahoo.com; Tyrel.J.Johnson@nasa.gov RI Nolan, Patrick/A-5582-2009; De Angelis, Alessandro/B-5372-2009; Starck, Jean-Luc/D-9467-2011; Thompson, David/D-2939-2012; Harding, Alice/D-3160-2012; Gehrels, Neil/D-2971-2012; McEnery, Julie/D-6612-2012; Baldini, Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Morselli, Aldo/G-6769-2011; Tosti, Gino/E-9976-2013; Rando, Riccardo/M-7179-2013; Komin, Nukri/J-6781-2015; Hays, Elizabeth/D-3257-2012; Johnson, Neil/G-3309-2014; Reimer, Olaf/A-3117-2013; Funk, Stefan/B-7629-2015; Johannesson, Gudlaugur/O-8741-2015; Gargano, Fabio/O-8934-2015; Loparco, Francesco/O-8847-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; OI Starck, Jean-Luc/0000-0003-2177-7794; Thompson, David/0000-0001-5217-9135; lubrano, pasquale/0000-0003-0221-4806; giglietto, nicola/0000-0002-9021-2888; Morselli, Aldo/0000-0002-7704-9553; Giordano, Francesco/0000-0002-8651-2394; Thorsett, Stephen/0000-0002-2025-9613; SPINELLI, Paolo/0000-0001-6688-8864; De Angelis, Alessandro/0000-0002-3288-2517; Frailis, Marco/0000-0002-7400-2135; Caraveo, Patrizia/0000-0003-2478-8018; Komin, Nukri/0000-0003-3280-0582; Reimer, Olaf/0000-0001-6953-1385; Funk, Stefan/0000-0002-2012-0080; Johannesson, Gudlaugur/0000-0003-1458-7036; Gargano, Fabio/0000-0002-5055-6395; Loparco, Francesco/0000-0002-1173-5673; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Torres, Diego/0000-0002-1522-9065; Rando, Riccardo/0000-0001-6992-818X; Sgro', Carmelo/0000-0001-5676-6214 FU Istituto Nazionale di Astrofisica in Italy; K. A. Wallenberg Foundation in Sweden FX Additional support for science analysis during the operations phase from the following agencies is also gratefully acknowledged: the Istituto Nazionale di Astrofisica in Italy and the K. A. Wallenberg Foundation in Sweden for providing a grant in support of a Royal Swedish Academy of Sciences Research fellowship for J.C.; The Parkes radio telescope is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by the CSIRO. NR 26 TC 30 Z9 31 U1 0 U2 1 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 APR 10 PY 2009 VL 695 IS 1 BP L72 EP L77 DI 10.1088/0004-637X/695/1/L72 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424BE UT WOS:000264539700016 ER PT J AU Catelan, M Grundahl, F Sweigart, AV Valcarce, AAR Cortes, C AF Catelan, M. Grundahl, F. Sweigart, A. V. Valcarce, A. A. R. Cortes, C. TI CONSTRAINTS ON HELIUM ENHANCEMENT IN THE GLOBULAR CLUSTER M3 (NGC 5272): THE HORIZONTAL BRANCH TEST SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE globular clusters: general; globular clusters: individual (M3=NGC 5272, M13=NGC 6205); Hertzsprung-Russell diagram; stars: abundances; stars: horizontal-branch ID MAIN-SEQUENCE STARS; METAL-POOR STARS; OMEGA-CENTAURI; RR-LYRAE; ABUNDANCES; METALLICITIES; SYSTEM; MASS; AGE; POPULATIONS AB It has recently been suggested that the presence of multiple populations showing various amounts of helium enhancement is the rule, rather than the exception, among globular star clusters. An important prediction of this helium enhancement scenario is that the helium-enhanced blue horizontal branch (HB) stars should be brighter than the red HB stars which are not helium enhanced. In this Letter, we test this prediction in the case of the Galactic globular cluster M3 (NGC 5272), for which the helium-enhancement scenario predicts helium enhancements of greater than or similar to 0.02 in virtually all blue HB stars. Using high-precision Stromgren photometry and spectroscopic gravities for blue HB stars, we find that any helium enhancement among most of the cluster's blue HB stars is very likely less than 0.01, thus ruling out the much higher helium enhancements that have been proposed in the literature. C1 [Catelan, M.; Valcarce, A. A. R.; Cortes, C.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 7820436, Chile. [Catelan, M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Grundahl, F.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus, Denmark. [Sweigart, A. V.] NASA, Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA. [Cortes, C.] Univ Fed Rio Grande do Norte, Dept Fis Teor Expt, BR-59072970 Natal, RN, Brazil. RP Catelan, M (reprint author), Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Av Vicuna Mackenna 4860, Santiago 7820436, Chile. FU Proyecto Basal [PFB-06/2007]; FONDAP Centro de Astrofisica [15010003]; Proyecto FONDECYT Regular [1071002]; John Simon Guggenheim Memorial Foundation Fellowship; Carlsberg Foundation; Danish AsteroSeismology Centre at Aarhus University; Danish National Research Council FX We thank an anonymous referee for some helpful comments, and D. A. VandenBerg and S. Moehler for some enlightening discussions. Support for M. C. is provided by Proyecto Basal PFB-06/2007, by FONDAP Centro de Astrofisica 15010003, by Proyecto FONDECYT Regular # 1071002, and by a John Simon Guggenheim Memorial Foundation Fellowship. F. G. acknowledges support from the Carlsberg Foundation and the Danish AsteroSeismology Centre at Aarhus University, and support from the Danish National Research Council to the Project "Stars: Central engines to the evolution of the Universe". NR 43 TC 34 Z9 34 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 10 PY 2009 VL 695 IS 1 BP L97 EP L102 DI 10.1088/0004-637X/695/1/L97 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424BE UT WOS:000264539700021 ER PT J AU Hamaguchi, K Corcoran, MF Ezoe, Y Townsley, L Broos, P Gruendl, R Vaidya, K White, SM Strohmayer, T Petre, R Chu, YH AF Hamaguchi, Kenji Corcoran, Michael F. Ezoe, Yuichiro Townsley, Leisa Broos, Patrick Gruendl, Robert Vaidya, Kaushar White, Stephen M. Strohmayer, Tod Petre, Rob Chu, You-Hua TI A SMOKING GUN IN THE CARINA NEBULA SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: bubbles; stars: evolution; stars: formation; stars: neutron; supernova remnants; X-rays: stars ID X-RAY EMISSION; ETA-CARINAE; XMM-NEWTON; MASSIVE STARS; NEUTRON-STAR; MAGNETIC-FIELDS; ORION NEBULA; SPECTROSCOPY; PROGENITOR; TELESCOPE AB The Carina Nebula is one of the youngest, most active sites of massive star formation in our Galaxy. In this nebula, we have discovered a bright X-ray source that has persisted for similar to 30 years. The soft X-ray spectrum, consistent with kT similar to 128 eV blackbody radiation with mild extinction, and no counterpart in the near- and mid-infrared wavelengths indicates that it is a similar to 10(6) year old neutron star housed in the Carina Nebula. Current star formation theory does not suggest that the progenitors of the neutron star and massive stars in the Carina Nebula, in particular. Car, are coeval. This result suggests that the Carina Nebula experienced at least two major episodes of massive star formation. The neutron star may be responsible for remnants of high-energy activity seen in multiple wavelengths. C1 [Hamaguchi, Kenji; Corcoran, Michael F.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Hamaguchi, Kenji; Corcoran, Michael F.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Hamaguchi, Kenji] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA. [Corcoran, Michael F.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Ezoe, Yuichiro] Tokyo Metropolitan Univ, Tokyo 1920397, Japan. [Townsley, Leisa; Broos, Patrick] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Gruendl, Robert; Vaidya, Kaushar; Chu, You-Hua] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [White, Stephen M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Strohmayer, Tod; Petre, Rob] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Hamaguchi, K (reprint author), NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. FU NASA's Astrobiology Institute [RTOP 344-53-51] FX We are grateful to T. R. Gull, K. E. Nielsen, S. Drake, K. Mukai, M. Ishida, C. Markwardt, and the anonymous referee for useful comments. This work was performed while K. H. was supported by NASA's Astrobiology Institute (RTOP 344-53-51) to the Goddard Center for Astrobiology. This research has made use of data and softwares obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center and Chandra X-ray Center (CXC). NR 45 TC 17 Z9 17 U1 0 U2 1 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 APR 10 PY 2009 VL 695 IS 1 BP L4 EP L9 DI 10.1088/0004-637X/695/1/L4 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424BE UT WOS:000264539700002 ER PT J AU Travnicek, PM Hellinger, P Schriver, D Hercik, D Slavin, JA Anderson, BJ AF Travnicek, Pavel M. Hellinger, Petr Schriver, David Hercik, David Slavin, James A. Anderson, Brian J. TI Kinetic instabilities in Mercury's magnetosphere: Three-dimensional simulation results SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MESSENGERS 1ST FLYBY; MAGNETIC-FIELD AB A self-consistent global three-dimensional kinetic study of Mercury's magnetosphere is carried out examining waves and instabilities generated by ion temperature anisotropy and plasma flow. The overall structure of Mercury's upstream bow shock and magnetosheath are qualitatively very similar to those of Earth. Beam-generated long-wavelength oscillations are present upstream of Mercury's quasi-parallel bow shock, whereas large-amplitude mirror waves develop downstream of the quasi-parallel bow shock in the magnetosheath. A train of mirror waves forms also downstream of the quasi-perpendicular bow shock. A velocity shear near the magnetopause can lead to formation of vortex-like structures. The magnetospheric cavity close to the planet's equatorial plane is filled with ions much hotter than the solar wind protons. A drift-driven plasma belt close to the equator is present in the model and contains plasma with high-temperature anisotropy, and the loss cone for charged particles in this region is large. The belt may cause diamagnetic effects superimposed on the planet's internal magnetic field and can interact with Mercury's magnetopause. Citation: Travnicek, P. M., P. Hellinger, D. Schriver, D. Hercik, J. A. Slavin, and B. J. Anderson (2009), Kinetic instabilities in Mercury's magnetosphere: Three-dimensional simulation results, Geophys. Res. Lett., 36, L07104, doi: 10.1029/2008GL036630. C1 [Travnicek, Pavel M.; Hellinger, Petr; Hercik, David] Acad Sci Czech Republic, Inst Atmospher Phys, Prague 14131 4, Czech Republic. [Slavin, James A.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Travnicek, Pavel M.; Schriver, David] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Anderson, Brian J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Travnicek, Pavel M.; Hellinger, Petr] Acad Sci Czech Republic, Astron Inst, Prague 14131 4, Czech Republic. RP Travnicek, PM (reprint author), Acad Sci Czech Republic, Inst Atmospher Phys, Bocni 2-1401, Prague 14131 4, Czech Republic. EM trav@ig.cas.cz; petr.hellinger@ig.cas.cz; dave@igpp.ucla.edu; james.a.slavin@nasa.gov; brian.j.anderson@jhuapl.edu RI Anderson, Brian/I-8615-2012; Slavin, James/H-3170-2012; Hellinger, Petr/F-5267-2014; Hercik, David/G-1224-2014; Travnicek, Pavel/G-8608-2014 OI Slavin, James/0000-0002-9206-724X; Hellinger, Petr/0000-0002-5608-0834; FU Academy of Sciences of the Czech Republic (ASCR) [300030805]; European Space Agency [98068]; NASA MESSENGER Participating Scientist [NNX07AR62G.]; Post Rouge, CNRS, France FX Authors acknowledge the support of contract 300030805 from the Grant Agency of the Academy of Sciences of the Czech Republic (ASCR), ESA PECS contract 98068 from the European Space Agency, and NASA MESSENGER Participating Scientist grant NNX07AR62G. This work has been performed on the Amalka supercomputing facility, Institute of Atmospheric Physics, ASCR. Part of this work has been supported by Post Rouge, CNRS, France, awarded to PT. NR 6 TC 24 Z9 24 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 APR 10 PY 2009 VL 36 AR L07104 DI 10.1029/2008GL036630 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 431YT UT WOS:000265101400001 ER PT J AU Tangborn, A Stajner, I Buchwitz, M Khlystova, I Pawson, S Burrows, J Hudman, R Nedelec, P AF Tangborn, Andrew Stajner, Ivanka Buchwitz, Michael Khlystova, Iryna Pawson, Steven Burrows, John Hudman, Rynda Nedelec, Philippe TI Assimilation of SCIAMACHY total column CO observations: Global and regional analysis of data impact SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID CARBON-MONOXIDE; MODEL; EMISSIONS; SATELLITE; CHEMISTRY; MOPITT; SYSTEM AB Carbon monoxide (CO) total column observations from the Scanning Imaging Absorption Spectrometer for Atmospheric Cartography (SCIAMACHY) on board Envisat-1 are assimilated into the Global Modeling and Assimilation Office constituent assimilation system for the period 1 April to 20 December 2004. The impact of the assimilation on CO distribution is evaluated using independent surface flask observations from the National Oceanic and Atmospheric Administration (NOAA)/ESRL global cooperative air sampling network and Measurement of Ozone and Water Vapor by Airbus In-Service Aircraft (MOZAIC) in situ CO profiles. Assimilation of SCIAMACHY data improves agreement of CO assimilation with both of these data sets on both global and regional scales compared to the free-running model. Regional comparisons with MOZAIC profiles made in western Europe, the northeastern United States, and the Arabian Peninsula show improvements at all three locations in the free troposphere and into the boundary layer over Arabia and the northeastern United States. Comparisons with NOAA Earth System Research Laboratory data improve at about two thirds of the surface observation sites. The systematic model errors related to the uncertainty of CO surface sources and the chemistry of CO losses are investigated through experiments with increased surface CO emissions over the Arabian Peninsula and/or globally reduced hydroxyl radical (OH) concentrations. Both model changes decrease mean CO errors at all altitudes in comparison to MOZAIC data over Dubai and Abu Dhabi. In contrast, errors in the assimilated CO are reduced by the increased emissions for pressures >= 800 hPa and by the reduced OH for pressures <= 600 hPa. Our analysis suggests that CO emissions over Dubai in 2004 are more than double those in the 1998 emissions inventory. C1 [Tangborn, Andrew; Stajner, Ivanka; Pawson, Steven] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Tangborn, Andrew] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. [Buchwitz, Michael; Khlystova, Iryna; Burrows, John] Univ Bremen, Inst Environm Phys, D-28334 Bremen, Germany. [Burrows, John] Ctr Ecol & Hydrol, Wallingford, Oxon, England. [Hudman, Rynda] Harvard Univ, Atmospher Chem Modeling Grp, Cambridge, MA 02138 USA. [Nedelec, Philippe] Univ Toulouse, CNRS, Lab Aerol, Observ Midi Pyrenees, F-31400 Toulouse, France. RP Tangborn, A (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610-1, Greenbelt, MD 20771 USA. EM andrew.v.tangborn@nasa.gov; ivanka.stajner@noblis.org; michael.buchwitz@iup.physik.uni-bremen.de; iryna.khlystova@iup.physik.unibremen.de; steven.pawson@nasa.gov; burrows@iup.physic.uni-bremen.de; hudman@berkeley.edu; philippe.nedelec@aero.obs-mip.fr RI Hudman, Rynda/C-6118-2009; Buchwitz, Michael/G-1510-2011; Stajner, Ivanka/B-5228-2009; Pawson, Steven/I-1865-2014; Burrows, John/B-6199-2014 OI Stajner, Ivanka/0000-0001-6103-3939; Pawson, Steven/0000-0003-0200-717X; Burrows, John/0000-0002-6821-5580 FU GMAO [NASA NRA-03-OES-02]; NASA Modeling Analysis and Prediction (MAP) grant FX This project was funded in the GMAO under NASA NRA-03-OES-02 (carbon cycle research) and a NASA Modeling Analysis and Prediction ( MAP) grant. Computing resources were provided by NASA's High-End Computing Program at GSFC. Funding for the University of Bremen came from DLR-Bonn ( grant 50EE0727), ESA ( PROMOTE), and the EU (AMFIC). The authors acknowledge the strong support of the European Communities, Airbus, and the airlines Lufthansa, Austrian, and Air France, who carry the MOZAIC equipment free of charge and have performed maintenance since 1994. We also gratefully acknowledge the contribution of Paul Novelli, who made available the CO flask data from the NOAA/ESRL global cooperative air sampling network. The comments from the three anonymous reviewers greatly helped to improve the quality of the manuscript. NR 31 TC 16 Z9 16 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 APR 10 PY 2009 VL 114 AR D07307 DI 10.1029/2008JD010781 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 431ZA UT WOS:000265102100003 ER PT J AU Mostl, C Farrugia, CJ Miklenic, C Temmer, M Galvin, AB Luhmann, JG Kilpua, EKJ Leitner, M Nieves-Chinchilla, T Veronig, A Biernat, HK AF Moestl, C. Farrugia, C. J. Miklenic, C. Temmer, M. Galvin, A. B. Luhmann, J. G. Kilpua, E. K. J. Leitner, M. Nieves-Chinchilla, T. Veronig, A. Biernat, H. K. TI Multispacecraft recovery of a magnetic cloud and its origin from magnetic reconnection on the Sun SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID CORONAL MASS EJECTIONS; FLUX ROPES; 2-RIBBON FLARE; CROSS-SECTION; CLUSTER DATA; SOLAR-WIND; FIELD; MODEL; RECONSTRUCTION; MAGNETOPAUSE AB Multipoint spacecraft observations of a magnetic cloud on 22 May 2007 have given us the opportunity to apply a multispacecraft technique to infer the structure of this large-scale magnetic flux rope in the solar wind. Combining WIND and STEREO-B magnetic field and plasma measurements, we construct a combined magnetic field map by integrating the Grad-Shafranov equation, this being one of the very first applications of this technique in the interplanetary context. From this we obtain robust results on the shape of the cross section, the orientation and magnetic fluxes of the cloud. The only slightly "flattened" shape is discussed with respect to its heliospheric environment and theoretical expectations. We also relate these results to observations of the solar source region and its associated two-ribbon flare on 19 May 2007, using Ha images from the Kanzelhohe observatory, SOHO/MDI magnetograms and SECCHI/EUVI 171 angstrom images. We find a close correspondence between the magnetic flux reconnected in the flare and the poloidal flux of the magnetic cloud. The axial flux of the cloud agrees with the prediction of a recent 3-D finite sheared arcade model to within a factor of 2, which is evidence for formation of at least half of the magnetic flux of the ejected flux rope during the eruption. We outline the relevance of this result to models of coronal mass ejection initiation, and find that to explain the solar and interplanetary observations elements from sheared arcade as well as erupting-flux-rope models are needed. C1 [Moestl, C.; Miklenic, C.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria. [Moestl, C.; Temmer, M.; Veronig, A.; Biernat, H. K.] Graz Univ, Inst Phys, A-8010 Graz, Austria. [Farrugia, C. J.; Galvin, A. B.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Farrugia, C. J.; Galvin, A. B.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [Luhmann, J. G.; Kilpua, E. K. J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Kilpua, E. K. J.] Univ Helsinki, Dept Phys, Div Theoret Phys, Helsinki, Finland. [Leitner, M.] Univ Innsbruck, Inst Astro & Particle Phys, A-6020 Innsbruck, Austria. [Nieves-Chinchilla, T.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. RP Mostl, C (reprint author), Austrian Acad Sci, Space Res Inst, Schmiedlstr 6, A-8042 Graz, Austria. EM moestlch@stud.uni-graz.at; charlie.farrugia@unh.edu RI Kilpua, Emilia/G-8994-2012; Galvin, Antoinette/A-6114-2013; Veronig, Astrid/B-8422-2009; Nieves-Chinchilla, Teresa/F-3482-2016; OI Nieves-Chinchilla, Teresa/0000-0003-0565-4890; Moestl, Christian/0000-0001-6868-4152; Temmer, Manuela/0000-0003-4867-7558 FU NASA WIND/SWE; MFI [NNG06GC75G, NNG06GD41G, NNX08AD11G]; University of California, Berkeley [NAS5-03131]; Austrian Fonds zur Forderung der wissenschaftlichen Forschung [P20145-N16, P20131-N16] FX C. M. is supported by the young researchers fund of the Steiermarkische Sparkasse. C.J.F. is a co-Investigator on STEREO/PLASTIC. This work is supported by NASA WIND/SWE and MFI grants NNG06GC75G, NNG06GD41G and NNX08AD11G. Work at the University of California, Berkeley, was supported from STEREO grant NAS5-03131. It is also supported by the Austrian Fonds zur Forderung der wissenschaftlichen Forschung under projects P20145-N16 and P20131-N16. M. Temmer acknowledges project APART 11262 of the Austrian Academy of Sciences. We also acknowledge the use of WIND data provided by the magnetometer and the solar wind experiment teams at GSFC. This research was supported in part by an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 68 TC 27 Z9 27 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD APR 10 PY 2009 VL 114 AR A04102 DI 10.1029/2008JA013657 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 432AD UT WOS:000265105000002 ER PT J AU Ponchak, GE Scardelletti, MC Jordan, JL AF Ponchak, G. E. Scardelletti, M. C. Jordan, J. L. TI 270 degrees C, 1 GHz oscillator-type active antenna SO ELECTRONICS LETTERS LA English DT Article AB Reported is the first demonstration of an active antenna operating at 1 GHz and at temperatures above 200 degrees C. A Clapp oscillator integrated with a slot-ring antenna generated and transmitted a 1 GHz signal from 25 to 270 degrees C. The oscillation frequency varied by less than 4% over the temperature range. RP Ponchak, GE (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM george.ponchak@ieee.org NR 7 TC 1 Z9 1 U1 0 U2 1 PU INST ENGINEERING TECHNOLOGY-IET PI HERTFORD PA MICHAEL FARADAY HOUSE SIX HILLS WAY STEVENAGE, HERTFORD SG1 2AY, ENGLAND SN 0013-5194 J9 ELECTRON LETT JI Electron. Lett. PD APR 9 PY 2009 VL 45 IS 8 BP 386 EP U9 DI 10.1049/el.2009.0615 PG 2 WC Engineering, Electrical & Electronic SC Engineering GA 433VO UT WOS:000265234100002 ER PT J AU Gautam, R Hsu, NC Lau, KM Tsay, SC Kafatos, M AF Gautam, R. Hsu, N. C. Lau, K. -M. Tsay, S. -C. Kafatos, M. TI Enhanced pre-monsoon warming over the Himalayan-Gangetic region from 1979 to 2007 SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ASIAN SUMMER MONSOON; BLACK CARBON AEROSOLS; TIBETAN PLATEAU; CLIMATE; EVOLUTION; IMPACTS; CLOUDS; TRENDS; RECORD AB Fundamental to the onset of the Indian Summer Monsoon is the land-sea thermal gradient from the Indian Ocean to the Himalayas-Tibetan Plateau (HTP). The timing of the onset is strongly controlled by the meridional tropospheric temperature gradient due to the rapid pre-monsoon heating of the HTP compared to the relatively cooler Indian Ocean. Analysis of tropospheric temperatures from the longest available record of microwave satellite measurements reveals widespread warming over the Himalayan-Gangetic region and consequent strengthening of the land-sea thermal gradient. This trend is most pronounced in the pre-monsoon season, resulting in a warming of 2.7 degrees C in the 29-year record (1979-2007), when this region is strongly influenced by dust aerosols at elevated altitudes. The enhanced tropospheric warming is accompanied by increased atmospheric loading of absorbing aerosols, particularly vertically extended dust aerosols, raising the possibility that aerosol solar heating has amplified the seasonal warming and in turn strengthened the land-sea gradient. Citation: Gautam, R., N. C. Hsu, K.-M. Lau, S.-C. Tsay, and M. Kafatos (2009), Enhanced pre-monsoon warming over the Himalayan-Gangetic region from 1979 to 2007, Geophys. Res. Lett., 36, L07704, doi:10.1029/2009GL037641. C1 [Gautam, R.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Gautam, R.; Hsu, N. C.; Lau, K. -M.; Tsay, S. -C.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Kafatos, M.] Chapman Univ, Schmid Coll Sci, Ctr Excellence Earth Observing, Orange, CA 92866 USA. RP Gautam, R (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, 5523 Res Pk Dr,Suite 320, Baltimore, MD 21228 USA. EM rgautam@umbc.edu RI Gautam, Ritesh/E-9776-2010; Hsu, N. Christina/H-3420-2013; Tsay, Si-Chee/J-1147-2014; Lau, William /E-1510-2012 OI Gautam, Ritesh/0000-0002-2177-9346; Lau, William /0000-0002-3587-3691 FU NASA EOS Program FX This work is supported by grant from the NASA EOS Program, managed by Hal Maring. We thank Colin Seftor for his help with the radiative transfer model. We are grateful to the anonymous reviewers and the associate Editor for providing constructive comments in improving an earlier version of the manuscript. NR 25 TC 91 Z9 92 U1 2 U2 10 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 APR 9 PY 2009 VL 36 AR L07704 DI 10.1029/2009GL037641 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 431YS UT WOS:000265101300003 ER PT J AU Devlin, MJ Ade, PAR Aretxaga, I Bock, JJ Chapin, EL Griffin, M Gundersen, JO Halpern, M Hargrave, PC Hughes, DH Klein, J Marsden, G Martin, PG Mauskopf, P Moncelsi, L Netterfield, CB Ngo, H Olmi, L Pascale, E Patanchon, G Rex, M Scott, D Semisch, C Thomas, N Truch, MDP Tucker, C Tucker, GS Viero, MP Wiebe, DV AF Devlin, Mark J. Ade, Peter A. R. Aretxaga, Itziar Bock, James J. Chapin, Edward L. Griffin, Matthew Gundersen, Joshua O. Halpern, Mark Hargrave, Peter C. Hughes, David H. Klein, Jeff Marsden, Gaelen Martin, Peter G. Mauskopf, Philip Moncelsi, Lorenzo Netterfield, Calvin B. Ngo, Henry Olmi, Luca Pascale, Enzo Patanchon, Guillaume Rex, Marie Scott, Douglas Semisch, Christopher Thomas, Nicholas Truch, Matthew D. P. Tucker, Carole Tucker, Gregory S. Viero, Marco P. Wiebe, Donald V. TI Over half of the far-infrared background light comes from galaxies at z >= 1.2 SO NATURE LA English DT Article ID DEGREE EXTRAGALACTIC SURVEY; DEEP SUBMILLIMETER SURVEY; FIELD-SOUTH SURVEY; NUMBER COUNTS; SOURCE CATALOGS; STAR-FORMATION; HIGH-REDSHIFT; LOCKMAN HOLE; SPITZER; CHANDRA AB Submillimetre surveys during the past decade have discovered a population of luminous, high-redshift, dusty starburst galaxies(1-8). In the redshift range 1 <= z <= 4, these massive submillimetre galaxies go through a phase characterized by optically obscured star formation at rates several hundred times that in the local Universe. Half of the starlight from this highly energetic process is absorbed and thermally re-radiated by clouds of dust at temperatures near 30 K with spectral energy distributions peaking at 100 mu m in the rest frame(9). At 1 <= z <= 4, the peak is redshifted to wavelengths between 200 and 500 mu m. The cumulative effect of these galaxies is to yield extragalactic optical and far-infrared backgrounds with approximately equal energy densities. Since the initial detection of the far-infrared background (FIRB)(10), higher-resolution experiments have sought to decompose this integrated radiation into the contributions from individual galaxies. Here we report the results of an extragalactic survey at 250, 350 and 500 mu m. Combining our results at 500 mu m with those at 24 mu m, we determine that all of the FIRB comes from individual galaxies, with galaxies at z >= 1.2 accounting for 70% of it. As expected, at the longest wavelengths the signal is dominated by ultraluminous galaxies at z > 1. C1 [Devlin, Mark J.; Klein, Jeff; Rex, Marie; Semisch, Christopher; Truch, Matthew D. P.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Ade, Peter A. R.; Griffin, Matthew; Hargrave, Peter C.; Mauskopf, Philip; Moncelsi, Lorenzo; Pascale, Enzo; Tucker, Carole] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Aretxaga, Itziar; Hughes, David H.] Inst Nacl Astrofis Opt & Electr, Puebla, Mexico. [Bock, James J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Chapin, Edward L.; Halpern, Mark; Marsden, Gaelen; Ngo, Henry; Scott, Douglas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Gundersen, Joshua O.; Thomas, Nicholas] Univ Miami, Dept Phys, Coral Gables, FL 33146 USA. [Martin, Peter G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Martin, Peter G.; Netterfield, Calvin B.; Viero, Marco P.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Netterfield, Calvin B.; Wiebe, Donald V.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Olmi, Luca] Univ Puerto Rico, Dept Phys, Rio Piedras, PR 00931 USA. [Olmi, Luca] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Patanchon, Guillaume] Univ Paris Diderot, Lab APC, F-75205 Paris, France. [Tucker, Gregory S.] Brown Univ, Dept Phys, Providence, RI 02912 USA. RP Devlin, MJ (reprint author), Univ Penn, Dept Phys & Astron, 209 S 33rd St, Philadelphia, PA 19104 USA. EM devlin@physics.upenn.edu RI Klein, Jeffrey/E-3295-2013; OI Scott, Douglas/0000-0002-6878-9840; Olmi, Luca/0000-0002-1162-7947; Ngo, Henry/0000-0001-5172-4859 FU NASAUS National Science Foundation Office; Canadian Space Agency; Natural Sciences and Engineering Research Council of Canada; UK Science and Technology Facilities Council FX We acknowledge the support of NASA, the US National Science Foundation Office of Polar Programs, the Canadian Space Agency, the Natural Sciences and Engineering Research Council of Canada and the UK Science and Technology Facilities Council. We are grateful to B. Magnelli for help with the FIDEL 24-mu m data. This research was enabled by the WestGrid computing resources and the SIMBAD and NASA/IPAC databases. We thank the Columbia Scientific Balloon Facility, Ken Borek Air Ltd and the mountaineers of McMurdo Station for their work. NR 28 TC 136 Z9 136 U1 0 U2 5 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 APR 9 PY 2009 VL 458 IS 7239 BP 737 EP 739 DI 10.1038/nature07918 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 433GZ UT WOS:000265193600034 PM 19360081 ER PT J AU Konhauser, KO Pecoits, E Lalonde, SV Papineau, D Nisbet, EG Barley, ME Arndt, NT Zahnle, K Kamber, BS AF Konhauser, Kurt O. Pecoits, Ernesto Lalonde, Stefan V. Papineau, Dominic Nisbet, Euan G. Barley, Mark E. Arndt, Nicholas T. Zahnle, Kevin Kamber, Balz S. TI Oceanic nickel depletion and a methanogen famine before the Great Oxidation Event SO NATURE LA English DT Article ID ATMOSPHERIC OXYGEN; METHANOBACTERIUM-THERMOAUTOTROPHICUM; RISE; NI; GEOCHEMISTRY; TECTONICS; CHEMISTRY; SULFUR; MANTLE; GROWTH AB It has been suggested that a decrease in atmospheric methane levels triggered the progressive rise of atmospheric oxygen, the so-called Great Oxidation Event, about 2.4 Gyr ago(1). Oxidative weathering of terrestrial sulphides, increased oceanic sulphate, and the ecological success of sulphate-reducing microorganisms over methanogens has been proposed as a possible cause for the methane collapse(1), but this explanation is difficult to reconcile with the rock record(2,3). Banded iron formations preserve a history of Precambrian oceanic elemental abundance and can provide insights into our understanding of early microbial life and its influence on the evolution of the Earth system(4,5). Here we report a decline in the molar nickel to iron ratio recorded in banded iron formations about 2.7 Gyr ago, which we attribute to a reduced flux of nickel to the oceans, a consequence of cooling upper-mantle temperatures and decreased eruption of nickel-rich ultramafic rocks at the time. We measured nickel partition coefficients between simulated Precambrian sea water and diverse iron hydroxides, and subsequently determined that dissolved nickel concentrations may have reached similar to 400nM throughout much of the Archaean eon, but dropped below similar to 200nM by 2.5 Gyr ago and to modern day values(6) (similar to 9 nM) by similar to 550 Myr ago. Nickel is a key metal cofactor in several enzymes of methanogens(7) and we propose that its decline would have stifled their activity in the ancient oceans and disrupted the supply of biogenic methane. A decline in biogenic methane production therefore could have occurred before increasing environmental oxygenation and not necessarily be related to it. The enzymatic reliance of methanogens on a diminishing supply of volcanic nickel links mantle evolution to the redox state of the atmosphere. C1 [Konhauser, Kurt O.; Pecoits, Ernesto; Lalonde, Stefan V.] Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2E3, Canada. [Papineau, Dominic] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA. [Nisbet, Euan G.] Royal Holloway Univ London, Dept Earth Sci, Egham TW20 0EX, Surrey, England. [Barley, Mark E.] Univ Western Australia, Sch Earth & Environm, Crawley, WA 6009, Australia. [Arndt, Nicholas T.] Univ Grenoble 1, Lab Geodynam Chaine Alpines Maison Geosci, F-38041 Grenoble, France. [Zahnle, Kevin] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Kamber, Balz S.] Laurentian Univ, Dept Earth Sci, Sudbury, ON P3E 2C6, Canada. RP Konhauser, KO (reprint author), Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2E3, Canada. EM kurtk@ualberta.ca RI Kamber, Balz/A-1823-2008; Lalonde, Stefan/I-8879-2014; OI Kamber, Balz/0000-0002-8720-0608; Lalonde, Stefan/0000-0003-1318-2280; Konhauser, Kurt/0000-0001-7722-7068 FU Natural Science and Engineering Research Council of Canada (NSERC); Australian Research Council (ARC) FX We thank M. Labbe for sample preparation, G. Chen and A. Simonetti for assistance with LA-ICP-MS analyses in the Radiogenic Isotope Facility at the University of Alberta, and S. Matveev for assistance with electron microprobe analyses. Field assistance by W. Mueller is acknowledged for Hunter Mine Group samples. Samples from the Loch Maree Group were provided by A. Wright. Funding was provided by the Natural Science and Engineering Research Council of Canada (NSERC) to K. O. K., the Canada Research Chairs Program to B. S. K., the Australian Research Council (ARC) to M. E. B., and NASA Exobiology and Evolutionary Biology Program individually to D. P. and K. Z. This manuscript was improved by discussions with R. Buick, J. Kasting and M. Lesher, and reviews by R. Frei and M. Saito. NR 40 TC 165 Z9 177 U1 9 U2 106 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 APR 9 PY 2009 VL 458 IS 7239 BP 750 EP U85 DI 10.1038/nature07858 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 433GZ UT WOS:000265193600038 PM 19360085 ER PT J AU Lovell, CS Wise, KE Kim, JW Lillehei, PT Harrison, JS Park, C AF Lovell, Conrad S. Wise, Kristopher E. Kim, Jae-Woo Lillehei, Peter T. Harrison, Joycelyn S. Park, Cheol TI Thermodynamic approach to enhanced dispersion and physical properties in a carbon nanotube/polypeptide nanocomposite SO POLYMER LA English DT Article DE Copolypeptide; Single wall carbon nanotube (SWCNT); Nanotube/polymer interactions ID DESIGNED AMPHIPHILIC PEPTIDE; NANOTUBE-POLYMER COMPOSITES; MECHANICAL-PROPERTIES; INFRARED SPECTRA; FUNCTIONALIZATION; POLYPEPTIDES; STIFFNESS; BLENDS; PHASE AB A high molecular weight synthetic polypeptide has been designed which exhibits favorable interactions with single wall carbon nanotubes (SWCNTs). The enthalpic and entropic penalties of mixing between these two molecules are reduced due to the polypeptide's aromatic sidechains and helical secondary structure, respectively. These enhanced interactions result in a well dispersed SWCNT/Poly (L-Leucineran-L-Phenylalanine) nanocomposite with enhanced mechanical and electrical properties using only shear mixing and sonication. At 0.5 wt% loading of SWCNT filler, the nanocomposite exhibits simultaneous increases in the Young's modulus, failure strain, and toughness of 8%, 120%, and 144%, respectively. At 1 kHz, the same nanotube loading level also enhances the dielectric constant from 2.95 to 22.81, while increasing the conductivity by four orders of magnitude. (c) 2009 Elsevier Ltd. All rights reserved. C1 [Lovell, Conrad S.; Wise, Kristopher E.; Kim, Jae-Woo; Park, Cheol] Natl Inst Aerosp, Hampton, VA 23666 USA. [Lovell, Conrad S.] Univ Virginia, Dept Mat Sci & Engn, Charlottesville, VA 22904 USA. [Wise, Kristopher E.; Lillehei, Peter T.; Harrison, Joycelyn S.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA. [Park, Cheol] Univ Virginia, Dept Mech & Aerosp Engn, Charlottesville, VA 22904 USA. RP Park, C (reprint author), Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA. EM cheol.park-1@nasa.gov RI Kim, Jae-Woo/A-8314-2008; Lillehei, Peter/C-9196-2009 OI Lillehei, Peter/0000-0001-8183-9980 FU NASA University Research, Engineering and Technology Institute on Bio Inspired Materials (BIMat) [NCC-1-02037] FX The authors thank Nancy M. Holloway for electroding the samples. They also acknowledge Timothy Deming, Galen Stucky and Edward Worthington for supplying the LFcopolypepticle. Lovell appreciates the guidance and discussion of Dr. James M. Fitz-Gerald at the University of Virginia. Park and Wise appreciate NASA University Research, Engineering and Technology Institute on Bio Inspired Materials (BIMat) under Award No. NCC-1-02037 for support in part. NR 53 TC 11 Z9 13 U1 0 U2 18 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0032-3861 J9 POLYMER JI Polymer PD APR 9 PY 2009 VL 50 IS 8 BP 1925 EP 1932 DI 10.1016/j.polymer.2009.02.016 PG 8 WC Polymer Science SC Polymer Science GA 431ER UT WOS:000265044600015 ER PT J AU Collilieux, X Altamimi, Z Ray, J van Dam, T Wu, X AF Collilieux, X. Altamimi, Z. Ray, J. van Dam, T. Wu, X. TI Effect of the satellite laser ranging network distribution on geocenter motion estimation SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID TERRESTRIAL REFERENCE FRAME; SURFACE MASS VARIATIONS; LOADING DATA; ENERGY BALANCES; TIME-SERIES; LAND WATER; EARTH; DEFORMATION; DORIS; DEFINITION AB SLR network translations estimated between a quasi-instantaneous station position set, theoretically expressed with respect to the center of mass of the Earth ( CM), and a secular reference frame are the signature of the motion of the CM with respect to the Earth crust. Geocenter motion is defined here to be the motion of the CM with respect to the geometric center of the solid Earth surface (CF). SLR translational variations cannot be rigorously interpreted as identical to geocenter motion due to the sparse and nonuniform distribution of the SLR network. Their difference is called the network effect, which should be dominated at subdecadal timescales by loading signals. We have computed translation time series of the SLR network using two independent geophysically based loading models. One is a displacement model estimated from surface fluid data ( Green's function approach), called forward model, and the other is a displacement model estimated from GPS and ocean bottom pressure (OBP) data, called inverse model. The translation models have been subtracted from their respective geocenter motion models computed from degree-1 mass load coefficients in order to evaluate their network effect biases. Scatter due to the SLR network effect is at the level of 1.5 mm RMS. It could slightly shift the phase of the annual SLR geocenter motion estimate by less than 1 month and could affect X and Z annual geocenter motion amplitudes at the 1-mm level, which is about one third of the expected signal. Two distinct methods are suggested to account for network effect when comparing SLR translations to geocenter motion models. The first is to add the network effect term predicted by a displacement model to the geocenter motion loading model. The second relies on an adequate combination of SLR and GPS products to estimate SLR translation that could be better compared with geocenter motion. C1 [Collilieux, X.; Altamimi, Z.] Inst Geog Natl, Lab Rech Geodesie, F-77455 Marne La Vallee 2, France. [Ray, J.] NOAA, Natl Geodet Survey, Silver Spring, MD 20910 USA. [van Dam, T.] Univ Luxembourg, Dept Phys & Mat Sci, L-1511 Luxembourg, Luxembourg. [Wu, X.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Collilieux, X (reprint author), Inst Geog Natl, Lab Rech Geodesie, 6-8 Ave Blaise Pascal, F-77455 Marne La Vallee 2, France. EM xavier.collilieux@ign.fr; tonie.vandam@uni.lu; Xiaoping.Wu@jpl.nasa.gov RI Altamimi, Zuheir/A-4168-2009 NR 48 TC 31 Z9 33 U1 1 U2 14 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 APR 7 PY 2009 VL 114 AR B04402 DI 10.1029/2008JB005727 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 431ZQ UT WOS:000265103700001 ER PT J AU Sangalli, L Knudsen, DJ Larsen, MF Zhan, T Pfaff, RF Rowland, D AF Sangalli, L. Knudsen, D. J. Larsen, M. F. Zhan, T. Pfaff, R. F. Rowland, D. TI Rocket-based measurements of ion velocity, neutral wind, and electric field in the collisional transition region of the auroral ionosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID FREQUENCY; TEMPERATURES; ANALYZER; EISCAT; RADAR AB The JOULE-II sounding rocket salvo was launched from Poker Flat Rocket Range into weak pulsating aurora following a moderate substorm at 0345 LT on 19 January 2007. We present in situ measurements of ion flow velocity and electric and magnetic fields combined with neutral wind observations derived from ground observations of in situ chemical tracers. Measured ion drifts in the 150-198 km and 92-105 km altitude ranges are consistent with (E) over right arrow X (B) over right arrow motion to within 16 m s(-1) rms and with neutral wind velocity to within 20 m s(-1), respectively. From these measurements we have calculated the ratio kappa of the ion cyclotron and ion collision frequencies, finding kappa = 1 at an altitude of 118 +/- 0.3 km. Using direct measurements of ion current, we calculate the Joule heating rate and Pedersen and Hall conductivity profiles for this moderately active event and find height-integrated values of 390 W km(-2) and 0.59 and 2.22 S, respectively. We also find that these values would have errors of up to tens of percent without coincident neutral wind measurements, and presumably more so during more active conditions. Ion flow vectors were measured at a rate of 125 s(-1); however, no significant fluctuations were observed at spatial/temporal scales below similar to 350 m and 0.5 s. Observational limits were 5.5 m and 0.016 s. C1 [Sangalli, L.; Knudsen, D. J.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Larsen, M. F.; Zhan, T.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. [Pfaff, R. F.; Rowland, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Sangalli, L (reprint author), Univ Calgary, Dept Phys & Astron, 2500 Univ Dr NW, Calgary, AB T2N 1N4, Canada. EM sangalli@phys.ucalgary.ca; knudsen@phys.ucalgary.ca; mlarsen@clemson.edu; Robert.F.Pfaff@nasa.gov; Douglas.E.Rowland@nasa.gov RI Rowland, Douglas/F-5589-2012; Larsen, Miguel/A-1079-2013; Pfaff, Robert/F-5703-2012 OI Rowland, Douglas/0000-0003-0948-6257; Pfaff, Robert/0000-0002-4881-9715 NR 17 TC 17 Z9 17 U1 1 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 APR 7 PY 2009 VL 114 AR A04306 DI 10.1029/2008JA013757 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 432AA UT WOS:000265104700001 ER PT J AU Glavin, DP Dworkin, JP AF Glavin, Daniel P. Dworkin, Jason P. TI Enrichment of the amino acid L-isovaline by aqueous alteration on CI and CM meteorite parent bodies SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE enantiomeric excess; homochirality; origin of life; carbonaceous chondrite ID STAR-FORMATION REGIONS; MURCHISON METEORITE; CARBONACEOUS CHONDRITES; ASYMMETRIC AUTOCATALYSIS; CIRCULAR-POLARIZATION; ORGANIC-COMPOUNDS; HOMOCHIRALITY; ORIGIN; AMPLIFICATION; MINERALOGY AB The distribution and enantiomeric composition of the 5-carbon (C(5)) amino acids found in CI-, CM-, and CR-type carbonaceous meteorites were investigated by using liquid chromatography fluorescence detection/TOF-MS coupled with o-phthaldialdehyde/N-acetyl- L-cysteine derivatization. A large L-enantiomeric excess (ee) of the alpha-methyl amino acid isovaline was found in the CM meteorite Murchison (L(ee) = 18.5 +/- 2.6%) and the CI meteorite Orgueil (L(ee) = 15.2 +/- 4.0%). The measured value for Murchison is the largest enantiomeric excess in any meteorite reported to date, and the Orgueil measurement of an isovaline excess has not been reported previously for this or any CI meteorite. The L-isovaline enrichments in these two carbonaceous meteorites cannot be the result of interference from other C(5) amino acid isomers present in the samples, analytical biases, or terrestrial amino acid contamination. We observed no L-isovaline enrichment for the most primitive unaltered Antarctic CR meteorites EET 92042 and QUE 99177. These results are inconsistent with UV circularly polarized light as the primary mechanism for L-isovaline enrichment and indicate that amplification of a small initial isovaline asymmetry in Murchison and Orgueil occurred during an extended aqueous alteration phase on the meteorite parent bodies. The large asymmetry in isovaline and other alpha-dialkyl amino acids found in altered CI and CM meteorites suggests that amino acids delivered by asteroids, comets, and their fragments would have biased the Earth's prebiotic organic inventory with left-handed molecules before the origin of life. C1 [Glavin, Daniel P.; Dworkin, Jason P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Glavin, DP (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM daniel.p.glavin@nasa.gov RI Glavin, Daniel/D-6194-2012; Dworkin, Jason/C-9417-2012 OI Glavin, Daniel/0000-0001-7779-7765; Dworkin, Jason/0000-0002-3961-8997 FU National Aeronautics and Space Administration Astrobiology Institute; National Aeronautics and Space Administration Cosmo-chemistry; Astrobiology: Exobiology and Evolutionary Biology programs FX We thank K. Righter, T. McCoy, L. Welzenbach, and P. Ehrenfreund for providing the meteorite samples used in this study; S. Pizzarello, S. Miller, S. Davies, R. Duke, and R. Hudson for several amino acid standards; A. Lewis for optimizing the LC analytical separation conditions; M. Martin for help optimizing the QqQ-MS conditions; C. Alexander and L. Chizmadia for helpful discussions; O. Botta for assistance with the meteorite extractions; and A. Schwartz and an anonymous reviewer for helpful comments. Funding support was received from the National Aeronautics and Space Administration Astrobiology Institute and the National Aeronautics and Space Administration Cosmo-chemistry and Astrobiology: Exobiology and Evolutionary Biology programs. NR 54 TC 133 Z9 137 U1 2 U2 39 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD APR 7 PY 2009 VL 106 IS 14 BP 5487 EP 5492 DI 10.1073/pnas.0811618106 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 430CX UT WOS:000264967500008 PM 19289826 ER PT J AU Hudman, RC Murray, LT Jacob, DJ Turquety, S Wu, S Millet, DB Avery, M Goldstein, AH Holloway, J AF Hudman, R. C. Murray, L. T. Jacob, D. J. Turquety, S. Wu, S. Millet, D. B. Avery, M. Goldstein, A. H. Holloway, J. TI North American influence on tropospheric ozone and the effects of recent emission reductions: Constraints from ICARTT observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID CARBON-MONOXIDE; SURFACE OZONE; POLLUTION; ATLANTIC; METEOROLOGY; MODEL AB We use observations from the International Consortium for Atmospheric Research on Transport and Transformation (ICARTT) campaign over eastern North America in summer 2004, interpreted with a global 3-D model of tropospheric chemistry (GEOS-Chem), to improve and update estimates of North American influence on global tropospheric ozone and the effect of recent U. S. anthropogenic reductions on surface ozone pollution. We find that the 50% decrease in U. S. stationary NOx sources since 1999 has decreased mean U. S. boundary layer ozone concentrations by 6-8 ppbv in the southeast and 4-6 ppbv in the Midwest. The observed dO(3)/dCO molar enhancement ratio in the U. S. boundary layer during ICARTT was 0.46 mol mol(-1), larger than the range of 0.3-0.4 from studies in the early 1990s, possibly reflecting the decrease in the NOx/CO emission ratio as well as an increase in the ozone production efficiency per unit NOx. North American NOx emissions during summer 2004 as constrained by the ICARTT observations (0.72 Tg N fossil fuel, 0.11 Tg N biomass burning, 0.28 Tg N lightning for 1 July to 15 August) enhanced the hemispheric tropospheric ozone burden by 12.4%, with comparable contributions from fossil fuel and lightning (5-6%), but only 1% from biomass burning emissions despite 2004 being a record fire year over Alaska and western Canada. C1 [Avery, M.] NASA, Langley Res Ctr, Div Atmospher Sci, Hampton, VA 23681 USA. [Goldstein, A. H.] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA. [Holloway, J.] NOAA, Earth Syst Res Lab, Boulder, CO 80305 USA. [Hudman, R. C.; Murray, L. T.; Jacob, D. J.; Turquety, S.; Wu, S.; Millet, D. B.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Hudman, R. C.; Murray, L. T.; Jacob, D. J.; Turquety, S.; Wu, S.; Millet, D. B.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Holloway, J.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. RP Hudman, RC (reprint author), Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA. EM hudman@berkeley.edu RI Hudman, Rynda/C-6118-2009; Goldstein, Allen/A-6857-2011; Millet, Dylan/G-5832-2012; Holloway, John/F-9911-2012; Murray, Lee/F-2296-2014; Chem, GEOS/C-5595-2014 OI Goldstein, Allen/0000-0003-4014-4896; Holloway, John/0000-0002-4585-9594; Murray, Lee/0000-0002-3447-3952; FU NASA Global Tropospheric Chemistry Program; NOAA Office of Global Programs FX This work was funded by the NASA Global Tropospheric Chemistry Program and by the NOAA Office of Global Programs. Aboard the NOAA WP-3D aircraft measurements were provided for ozone, NO, NO2 (Tom Ryerson, NOAA ESRL), acetonitrile (Joost De Gouw, CIRES/NOAA ESRL), HNO3 (Andy Neuman, NOAA CIRES/ESRL), and PAN (Frank Flocke and Aaron Swanson, NCAR) and aboard the NASA DC-8 aircraft for HCN and PAN (Hanwant Singh, NASA Ames), NO2 (Ron Cohen and Tim Bertram, University of California, Berkeley), and NO (Bill Brune and Xinrong Ren). NR 49 TC 31 Z9 31 U1 1 U2 24 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD APR 4 PY 2009 VL 114 AR D07302 DI 10.1029/2008JD010126 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 428QE UT WOS:000264863100001 ER PT J AU Yue, GK Fromm, MD Shettle, EP AF Yue, Glenn K. Fromm, Michael D. Shettle, Eric P. TI Intercomparison of aerosol extinction measured by Stratospheric Aerosol and Gas Experiment (SAGE) II and III SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID POAM-III; SATELLITE EXPERIMENTS; INTEGRAL PROPERTIES; SAM-II; SIMULATED EXTINCTION; SIZE DISTRIBUTIONS; POLAR OZONE; VALIDATION; INSTRUMENT; RETRIEVAL AB Stratospheric Aerosol and Gas Experiment (SAGE) II and SAGE III are two satellite experiments designed to monitor aerosol extinction and the concentration of trace gases in the atmosphere using the solar and/or lunar occultation technique. While SAGE III used nine aerosol channels, four of them were centered at wavelengths very close or equal to the four aerosol channels used by SAGE II. Since both satellites conducted measurements between 2002 and 2005, there are comparison opportunities when their measurement locations on the same day are nearly coincident. In this study, the coincidence events are identified, and the aerosol extinction coefficients, color ratios (ratio of the extinction at two wavelengths), and optical depths measured by both satellites are compared. It is found that in the main stratospheric aerosol layer, between about 18 and 26 km, the differences of extinction coefficients are generally within their measurement uncertainties and are less than about 30%. The discrepancy between the wavelength dependence of the aerosol extinction coefficient, color ratio, and optical depth measured by SAGE II and SAGE III is also discussed. In the main stratospheric aerosol layer, the SAGE III mode radius deduced from the color ratio is about 20 to 30% less than the SAGE II mode radius. Wavelength dependence biases of the aerosol extinction coefficient evident in prior releases of SAGE III data persist in version 4.00. C1 [Yue, Glenn K.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Fromm, Michael D.; Shettle, Eric P.] USN, Res Lab, Washington, DC 20375 USA. RP Yue, GK (reprint author), NASA, Langley Res Ctr, MS 475,100 NASA Rd, Hampton, VA 23681 USA. EM glenn.k.yue@nasa.gov RI Fromm, Michael/F-4639-2010 FU NASA Office of Earth Science; NRL internal funding (from the Office of Naval Research) FX M. D. F. and E. P. S. were supported in part by a grant from the NASA Office of Earth Science and in part by NRL internal funding (from the Office of Naval Research). NR 25 TC 1 Z9 1 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD APR 4 PY 2009 VL 114 AR D07205 DI 10.1029/2008JD010452 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 428QE UT WOS:000264863100002 ER PT J AU Clilverd, MA Seppala, A Rodger, CJ Mlynczak, MG Kozyra, JU AF Clilverd, Mark A. Seppala, Annika Rodger, Craig J. Mlynczak, Martin G. Kozyra, Janet U. TI Additional stratospheric NOx production by relativistic electron precipitation during the 2004 spring NOx descent event SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ODD NITROGEN; MIDDLE ATMOSPHERE; MODEL; THERMOSPHERE; CHEMISTRY AB We analyze in detail the February 2004 Global Ozone Monitoring by Occultation of Stars (GOMOS) NO2 observations in the northern polar latitudes during the springtime descent of NOx from the mesosphere into the stratosphere. We combine GOMOS observations with SABER-observed NO 5.3 mu m radiated power and an AARDDVARK-derived radio wave index (RWI) to describe the impact of the 11 February geomagnetic storm. Energetic electron precipitation generated some additional NOx, supplementing the original amounts that were already descending. At altitudes of 50-70 km, GOMOS observations of NO2 showed a delayed response to the geomagnetic storm, with NO2 being generated 3 days after the start of the storm. The delayed response and duration of NO2 production was found to be consistent with the increase in the flux of relativistic electrons measured by GOES at geostationary orbit and by POES through relativistic electron contamination of the >16 MeV proton channel. Using the Sodankyla Ion and Neutral Chemistry model (SIC), we found that a good fit to the observed NO2 mixing ratios at the peak of the geomagnetic storm effect was produced by a monoenergetic 1.25 MeV electron beam with a flux of similar to 0.3 x10(6) el cm(-2) sr(-1) s(-1) keV(-1) or with a "hard'' electron spectra taken from Gaines et al. (1995) but with fluxes enhanced by a factor of 15, i.e., 8 x 10(4) el cm(-2) sr(-1) s(-1) for 2-6 MeV. Prior to the storm the descending NO2 had average mixing ratio values of similar to 150 ppbv. The geomagnetic storm-induced relativistic electron precipitation event doubled the amount of NOx descending into the stratosphere to similar to 300 ppbv after the storm. C1 [Clilverd, Mark A.] British Antarctic Survey, NERC, Div Phys Sci, Cambridge CB3 0ET, England. [Kozyra, Janet U.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Coll Engn, Ann Arbor, MI 48109 USA. [Mlynczak, Martin G.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Rodger, Craig J.] Univ Otago, Dept Phys, Dunedin, New Zealand. [Seppala, Annika] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland. RP Clilverd, MA (reprint author), British Antarctic Survey, NERC, Div Phys Sci, High Cross,Madingley Rd, Cambridge CB3 0ET, England. EM macl@bas.ac.uk; annika.seppala@fmi.fi; crodger@physics.otago.ac.nz; martin.g.mlynczak@nasa.gov; jukozyra@umich.edu RI Mlynczak, Martin/K-3396-2012; Seppala, Annika/C-8031-2014; Rodger, Craig/A-1501-2011 OI Seppala, Annika/0000-0002-5028-8220; Rodger, Craig/0000-0002-6770-2707 FU Academy of Finland FX M. A. C. would like to thank Glenda Harden at BAS for her valuable support in the development of this work. A. S. thanks the Academy of Finland for their support though the EPPIC project. The authors would like to thank the SABER and GOMOS science teams for useful and informative discussions regarding this work. We are grateful to NASA and the National Oceanic and Atmospheric Administration (NOAA) for the observations provided by the Polar Operational Environmental Satellite (POES) and Geostationary Operational Environmental Satellite Program (GOES) programs. NR 43 TC 16 Z9 16 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD APR 3 PY 2009 VL 114 AR A04305 DI 10.1029/2008JA013472 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 428RE UT WOS:000264866100001 ER PT J AU Rath, C Morfill, GE Rossmanith, G Banday, AJ Gorski, KM AF Raeth, C. Morfill, G. E. Rossmanith, G. Banday, A. J. Gorski, K. M. TI Model-Independent Test for Scale-Dependent Non-Gaussianities in the Cosmic Microwave Background SO PHYSICAL REVIEW LETTERS LA English DT Article ID PROBE SKY MAPS; ANISOTROPY-PROBE; INFLATIONARY UNIVERSE; K-INFLATION; WMAP DATA; PERTURBATIONS; SIGNATURES; FLATNESS; ISOTROPY; HORIZON AB We present a model-independent method to test for scale-dependent non-Gaussianities in combination with scaling indices as test statistics. Therefore, surrogate data sets are generated, in which the power spectrum of the original data is preserved, while the higher order correlations are partly randomized by applying a scale-dependent shuffling procedure to the Fourier phases. We apply this method to the Wilkinson Microwave Anisotropy Probe data of the cosmic microwave background and find signatures for non-Gaussianities on large scales. Further tests are required to elucidate the origin of the detected anomalies. C1 [Raeth, C.; Morfill, G. E.; Rossmanith, G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Banday, A. J.] Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France. [Gorski, K. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Rath, C (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. FU LAMBDA; NASA Office of Space Science. FX We acknowledge the use of LAMBDA. Support for LAMBDA is provided by the NASA Office of Space Science. NR 29 TC 32 Z9 32 U1 0 U2 1 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 APR 3 PY 2009 VL 102 IS 13 AR 131301 DI 10.1103/PhysRevLett.102.131301 PG 4 WC Physics, Multidisciplinary SC Physics GA 428YS UT WOS:000264888600011 PM 19392345 ER PT J AU Meador, MAB Weber, AS Hindi, A Naumenko, M McCorkle, L Quade, D Vivod, SL Gould, GL White, S Deshpande, K AF Meador, Mary Ann B. Weber, Amanda S. Hindi, Alia Naumenko, Melanie McCorkle, Linda Quade, Derek Vivod, Stephanie L. Gould, George L. White, Shannon Deshpande, Kiranmayi TI Structure-Property Relationships in Porous 3D Nanostructures: Epoxy-Cross-Linked Silica Aerogels Produced Using Ethanol as the Solvent SO ACS APPLIED MATERIALS & INTERFACES LA English DT Article DE aerogel; polymer cross-linking; nanoporous materials; hybrid materials; sol-gel ID AMINE-MODIFIED SILICA; ORGANIC-INORGANIC MATERIALS; COMPOSITE AEROGELS; TRANSPARENT; SOL AB Cross-linking silica aerogels with organic groups has been shown to improve the strength over un-cross-linked aerogels by as much as 2 orders of magnitude. Previous cross-linking chemistry has been developed using solvents specifically chosen to dissolve the monomers and accommodate the reaction temperature. Because the process of making the aerogels requires so much solvent, it is of interest to consider less toxic solvents such as ethanol to increase safety and enhance scale up. To this end, two different epoxy precursors with suitable solubility in ethanol were evaluated as cross-linkers for silica gels prepared from (3-aminopropyl)triethoxysilane and tetraethylorthosilicate. In addition, 1,6-bis(trimethoxysilyl)hexane (BTMSH) was used as an additive in the underlying silica structure to add flexibility to the aerogels. it was found that the ethanol-derived aerogels exhibited more shrinkage than those prepared from other solvents but that including BTMSH in the aerogels significantly reduced this shrinkage. Inclusion of BTMSH also imparted the ability of the aerogel monoliths to recover elastically when compressed up to 50% strain. In addition, optimized cross-linked aerogels prepared in this study have mechanical properties comparable to those using other more undesirable solvents and cross-linkers. C1 [Meador, Mary Ann B.; Quade, Derek; Vivod, Stephanie L.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Gould, George L.; White, Shannon; Deshpande, Kiranmayi] Aspen Aerogels, Northborough, MA 01532 USA. RP Meador, MAB (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM maryann.meador@nasa.gov OI Meador, Mary Ann/0000-0003-2513-7372 FU NASA's Fundamental Aeronautics Program; Undergraduate Student Researcher Program FX we gratefully acknowledge financial support from NASA's Fundamental Aeronautics Program, NASA's Innovative Partnerships Program, and the Undergraduate Student Researcher Program. We thank Dr. Baochau N. Nguyen of the Ohio Aerospace Institute for running solid NMR and Anna Palczer for porosimetry measurements. NR 23 TC 51 Z9 54 U1 6 U2 66 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1944-8244 J9 ACS APPL MATER INTER JI ACS Appl. Mater. Interfaces PD APR PY 2009 VL 1 IS 4 BP 894 EP 906 DI 10.1021/am900014z PG 13 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Science & Technology - Other Topics; Materials Science GA 464VM UT WOS:000267536100022 PM 20356015 ER PT J AU Lin, Y Watson, KA Fallbach, MJ Ghose, S Smith, JG Delozier, DM Cao, W Crooks, RE Connell, JW AF Lin, Yi Watson, Kent A. Fallbach, Michael J. Ghose, Sayata Smith, Joseph G., Jr. Delozier, Donavon M. Cao, Wei Crooks, Roy E. Connell, John W. TI Rapid, Solventless, Bulk Preparation of Metal Nanoparticle-Decorated Carbon Nanotubes SO ACS NANO LA English DT Article DE carbon nanotubes; metal decoration; nanohybrids; solventless; bulk preparation ID GRAPHITE COMPOSITE ELECTRODES; SURFACE-ENHANCED RAMAN; THERMAL-DECOMPOSITION; PALLADIUM NANOPARTICLES; GOLD NANOPARTICLES; CHARGE-TRANSFER; FUEL-CELLS; SINGLE; SILVER; SPECTROSCOPY AB A rapid, solventless method is described for the decoration of carbon nanotubes with metal nanoparticles. The straightforward two-step process utilizes neither reducing agents nor electric current and involves the dry mixing of a precursor metal salt (e.g., a metal acetate) with carbon nanotubes (single- or multi-walled) followed by heating in an inert atmosphere. The procedure is scalable to multigram quantities and generally applicable to various other carbon substrates (e.g., carbon nanofiber, expanded graphite, and carbon black) and many metal salts (e.g., Ag, Au, Co, Ni, and Pd acetates). As a model system, Ag nanoparticle-decorated carbon nanotube samples were prepared under various mixing techniques, metal loading levels, thermal treatment temperatures, and nanotube oxidative acid treatments. These nanohybrids were characterized by a variety of microscopic and spectroscopic techniques. For example, X-ray diffraction and scanning electron microscopy indicated that the average size of the Ag nanoparticles has little to do with the thermal treatment temperature but can be easily controlled by varying the Ag loading. Raman spectroscopy illustrated both the metal-nanotube electronic interactions and the surface enhancement effect from the Ag nanoparticle attachment. High-resolution transmission electron microscopy captured the in situ salt-to-metal conversion events on the nanotube surface. The mechanistic implications from the characterization results are discussed. C1 [Watson, Kent A.; Ghose, Sayata; Delozier, Donavon M.; Crooks, Roy E.] Natl Inst Aerospace, Hampton, VA 23666 USA. [Smith, Joseph G., Jr.; Connell, John W.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA. [Cao, Wei] Old Dominion Univ, Appl Res Ctr, Newport News, VA 23606 USA. [Lin, Yi; Fallbach, Michael J.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Lin, Y (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM yi.lin-1@nasa.gov; john.w.connell@nasa.gov RI Cao, Wei/E-8950-2011 FU Oak Ridge Associated Universities [NNH06CC03B] FX Y.L. and MJ.F. were supported by appointments to the NASA Postdoctoral Program at the Langley Research Center, administered by Oak Ridge Associated Universities (through NASA contract NNH06CC03B) and the National Research Council, respectively. The authors thank D. Hartman for XRD experiments, T. Williams for assistance in sample preparation and particle size measurements, and Drs. P. Lillehei, A. Belcher, and C. Wohl for their valuable comments and suggestions. The authors are in debt to Prof. Y.-P. Sun and his research group at Clemson University for their generous help in microscopy and other experiments, and Dr. J. Hudson at Clemson University for XPS measurements. NR 83 TC 130 Z9 133 U1 3 U2 95 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1936-0851 J9 ACS NANO JI ACS Nano PD APR PY 2009 VL 3 IS 4 BP 871 EP 884 DI 10.1021/nn8009097 PG 14 WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Chemistry; Science & Technology - Other Topics; Materials Science GA 439HR UT WOS:000265618700019 PM 19278218 ER PT J AU Demoulin, P Pariat, E AF Demoulin, P. Pariat, E. TI Modelling and observations of photospheric magnetic helicity SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Magnetic fields; Magnetic helicity; Magneto-hydrodynamic; Photosphere; Corona; Coronal mass ejections ID SOLAR ACTIVE REGIONS; LOCAL CORRELATION TRACKING; CORONAL MASS EJECTION; MINIMUM ENERGY FIT; FLUX TUBES; INDUCTION EQUATION; VECTOR MAGNETOGRAMS; INVERSE CASCADE; INJECTION; FIELDS AB Mounting observational evidence of the emergence of twisted magnetic flux tubes through the photosphere have now been published. Such flux tubes, formed by the solar dynamo and transported through the convection zone, eventually reach the solar atmosphere. Their accumulation in the solar corona leads to flares and coronal mass ejections. Since reconnections occur during the evolution of the flux tubes, the concepts of twist and magnetic stress become inappropriate. Magnetic helicity, as a well preserved quantity, in particular in plasma with high magnetic Reynolds number, is a more suitable physical quantity to use, even if reconnection is involved. Only recently, it has been realized that the flux of magnetic helicity can be derived from magnetogram time series. This paper reviews the advances made in measuring the helicity injection rate at the photospheric level, mostly in active regions. It relates the observations to our present theoretical understanding of the emergence process. Most of the helicity injection is found during magnetic flux emergence, whereas the effect of differential rotation is small, and the long-term evolution of active regions is still puzzling. The photospheric maps of the injection of magnetic helicity provide new spatial information about the basic properties of the link between the solar activity and its sub-photospheric roots. Finally, the newest techniques to measure photospheric flows arc reviewed. (C) 2008 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Demoulin, P.] Observ Paris, LESIA, CNRS, UMR 8109, F-92195 Meudon, France. [Pariat, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Pariat, E.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. [Pariat, E.] USN, Res Lab, Washington, DC 20375 USA. RP Demoulin, P (reprint author), Observ Paris, LESIA, CNRS, UMR 8109, F-92195 Meudon, France. EM Pascal.Demoulin@obspm.fr; epariat@helio.gsfc.nasa.gov OI Demoulin, Pascal/0000-0001-8215-6532 NR 89 TC 46 Z9 46 U1 1 U2 4 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 APR 1 PY 2009 VL 43 IS 7 BP 1013 EP 1031 DI 10.1016/j.asr.2008.12.004 PG 19 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 430OW UT WOS:000264999400001 ER PT J AU Inman, JA Danehy, PM Alderfer, DW Buck, GM McCrea, A AF Inman, Jennifer A. Danehy, Paul M. Alderfer, David W. Buck, Gregory M. McCrea, Andrew TI Planar Fluorescence Imaging and Three-Dimensional Reconstructions of Capsule Reaction-Control-System Jets SO AIAA JOURNAL LA English DT Article ID LASER-INDUCED FLUORESCENCE; TEMPERATURE-MEASUREMENTS; STREAMWISE VORTICES; FLOW; VISUALIZATION; LAYER; NO AB Planar laser-induced-fluorescence flowfield visualization has been used to investigate reaction-control-system jet flows in the wake of hypersonic capsule reentry vehicles. Pitch, roll, and yaw reaction-control-system jets were all studied. Planar laser-induced fluorescence was used to obtain offbody How images at planar slices in these flowfields, which are not easily visualized by other techniques, owing to characteristically low gas density. When viewed individually, these slices are shown to provide spatially and temporally resolved information, including the locations and characteristics of turbulent How structures and the location of the jet flow relative to the vehicle. In addition, ensembles of slices acquired at multiple locations throughout the flowfield are combined using computer visualization techniques to reconstruct the three-dimensional shape of the flow. Collectively, the offbody flow-visualization data set acquired in these tests represents a valuable complement to surface measurements, especially as a basis for explaining otherwise perplexing discrepancies between such measurements and computational fluid dynamics results. The tests described herein were conducted in the 31-Inch Mach 10 Air Tunnel at NASA Langley Research Center. C1 [Inman, Jennifer A.; Danehy, Paul M.; Alderfer, David W.] NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, Hampton, VA 23681 USA. [McCrea, Andrew] Alliant Techsyst, Adv Sensing & Opt Measurement Branch, Space Div, Hampton, VA 23681 USA. [Buck, Gregory M.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA. RP Inman, JA (reprint author), NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, Mail Stop 493, Hampton, VA 23681 USA. FU NASA Fundamental Aeronautics Program's Hypersonics Project; NASA's Constellation Orion Crew Exploration Vehicle Aeroscience Program (CAP) FX We wish to acknowledge the contribution to this project from the NASA Langley Research Center 31-Inch Mach 10 Air Tunnel technicians and engineers, including Anthony Robbins, Kevin Hollingsworth, Sheila Wright, Paul Tucker, Henry Fitz Fitzgerald, Johnny Ellis, Stan Mason, and Doug Boggs. This work was Supported by the NASA Fundamental Aeronautics Program's Hypersonics Project as well as NASA's Constellation Orion Crew Exploration Vehicle Aeroscience Program (CAP). Thanks also to Richard Schwartz from Alliant Techsystems, Hampton, Virginia, for assisting with the computer visualizations of the data. NR 41 TC 7 Z9 7 U1 0 U2 1 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD APR PY 2009 VL 47 IS 4 BP 803 EP 812 DI 10.2514/1.37116 PG 10 WC Engineering, Aerospace SC Engineering GA 432SA UT WOS:000265153200002 ER PT J AU Watkins, AN Buck, GM Leighty, BD Lipford, WE Oglesby, DM AF Watkins, A. Neal Buck, Gregory M. Leighty, Bradley D. Lipford, William E. Oglesby, Donald M. TI Using Pressure- and Temperature-Sensitive Paint on the Aftbody of a Capsule Vehicle SO AIAA JOURNAL LA English DT Article ID HEAT-TRANSFER AB Pressure-sensitive and temperature-sensitive paint were used to visualize and quantify the surface interactions of reaction control system jets on the afthody of capsule reentry vehicle shapes. The first model tested was an Apollo-like configuration and was used to focus primarily on the effects of the forward facing roll and yaw jets. The second model tested was an early Orion crew module configuration blowing only out of its forward-most yaw jet, which was expected to have the most intense aerodynamic heating augmentation on the model surface. This paper will present the results from the experiments, which show that with proper system design, both pressure-sensitive and temperature-sensitive paint are effective tools for studying these types of interaction in hypersonic testing environments. C1 [Watkins, A. Neal; Leighty, Bradley D.; Lipford, William E.] NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, Hampton, VA 23681 USA. [Buck, Gregory M.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA. [Oglesby, Donald M.] ATK Aerospace Co, Hampton, VA 23681 USA. RP Watkins, AN (reprint author), NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, Mail Stop 493, Hampton, VA 23681 USA. NR 34 TC 5 Z9 5 U1 1 U2 6 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD APR PY 2009 VL 47 IS 4 BP 821 EP 829 DI 10.2514/1.37258 PG 9 WC Engineering, Aerospace SC Engineering GA 432SA UT WOS:000265153200004 ER PT J AU Mielke, AF Elam, KA Sung, CJ AF Mielke, Amy F. Elam, Kristie A. Sung, Chih-Jen TI Multiproperty Measurements at High Sampling Rates Using Rayleigh Scattering SO AIAA JOURNAL LA English DT Article ID BRILLOUIN-SCATTERING; TEMPERATURE; DENSITY; FLOWS; GAS; FLUCTUATIONS; THERMOMETRY; VELOCIMETRY AB A molecular Rayleigh scattering technique is developed to measure gas velocity, temperature, and density in unseeded gas flows at sampling rates up to 32 kHz. A high-power continuous-wave laser beam is focused at a point in an air flowfield, and Rayleigh scattered light is collected and fiber-optically transmitted to a Fabry-Perot interferometer for spectral analysis. Photomultiplier tubes operated in the photon-counting mode allow high-frequency sampling of the total signal level and the circular interference pattern to provide density, temperature, and velocity measurements. Mean and root-mean-square fluctuation measurements in both an electrically heated jet facility with a 10-mm-diam nozzle and in a hydrogen-combustor-heated-jet facility with a 50.8-mm-diam nozzle at NASA John H. Glenn Research Center at Lewis Field are presented. Measurements are compared with hot-wire anemometry, cold-wire thermometry, and temporally resolved particle image velocimetry to validate the Rayleigh technique. C1 [Mielke, Amy F.] NASA, John H Glenn Res Ctr Lewis Field, Opt Instrumentat & Nondestruct Evaluat Branch, Cleveland, OH 44135 USA. [Elam, Kristie A.] Jacobs Sverdrup, Cleveland, OH 44135 USA. [Sung, Chih-Jen] Case Western Reserve Univ, Dept Mech & Aerosp Engn, Cleveland, OH 44106 USA. RP Mielke, AF (reprint author), NASA, John H Glenn Res Ctr Lewis Field, Opt Instrumentat & Nondestruct Evaluat Branch, 21000 Brookpk Rd,Mail Stop 77-1, Cleveland, OH 44135 USA. NR 34 TC 7 Z9 7 U1 0 U2 1 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD APR PY 2009 VL 47 IS 4 BP 850 EP 862 DI 10.2514/1.37369 PG 13 WC Engineering, Aerospace SC Engineering GA 432SA UT WOS:000265153200007 ER PT J AU Rumsey, CL Spalart, PR AF Rumsey, Christopher L. Spalart, Philippe R. TI Turbulence Model Behavior in Low Reynolds Number Regions of Aerodynamic Flowfields SO AIAA JOURNAL LA English DT Article ID BOUNDARY-LAYERS; PREDICTING TRANSITION; UNSTRUCTURED GRIDS; AIRFOIL FLOWS; HIGH-LIFT; EQUATION AB The behaviors of the widely used Spalart-Allmaras and Menter shear-stress transport turbulence models at low Reynolds numbers and under conditions conducive to relaminarization are documented. The flows used in the investigation include 2-D zero-pressure-gradient flow over a flat plate from subsonic to hypersonic Mach numbers, 2- airfoil flow from subsonic to supersonic Mach numbers, 2-D subsonic sink flow, and 3-D subsonic flow over an infinite swept wing (particularly its leading-edge region). Both models exhibit a range over which they behave "transitionally" even with inflow values set to cause immediate growth of the turbulence quantities, in the sense that the flow is neither laminar nor fully turbulent, but these behaviors are different: the shear-stress transport model typically has a well-defined transition location, whereas the Spalart-Allmaras model does not. Both models are predisposed to delayed activation of turbulence with increasing freestream Mach number. Also, both models can be made to achieve earlier activation of turbulence by increasing their freestream levels, but too high a level can disturb the turbulent solution behavior. The technique of maintaining freestream levels of turbulence without decay in the shear-stress transport model, introduced elsewhere, is shown here to be useful in reducing grid dependence of the model's transitional behavior. Both models are demonstrated to be incapable of predicting relaminarization; eddy viscosities remain weakly turbulent in accelerating or laterally strained boundary layers for which experiment and direct simulations indicate turbulence suppression. The main conclusion is that these models are intended for fully turbulent high Reynolds number computations, and using them for transitional (e.g., low Reynolds number) or relaminarizing flows is not appropriate. Competing models which fare better in these areas have not been identified. C1 [Rumsey, Christopher L.] NASA, Langley Res Ctr, Computat Aerosci Branch, Hampton, VA 23681 USA. RP Rumsey, CL (reprint author), NASA, Langley Res Ctr, Computat Aerosci Branch, Mail Stop 128, Hampton, VA 23681 USA. NR 39 TC 23 Z9 24 U1 2 U2 7 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 APR PY 2009 VL 47 IS 4 BP 982 EP 993 DI 10.2514/1.39947 PG 12 WC Engineering, Aerospace SC Engineering GA 432SA UT WOS:000265153200020 ER PT J AU Smith, SM Gardner, KK Locke, J Zwart, SR AF Smith, Scott M. Gardner, Keri K. Locke, James Zwart, Sara R. TI Vitamin D supplementation during Antarctic winter SO AMERICAN JOURNAL OF CLINICAL NUTRITION LA English DT Article ID CELL-MEDIATED-IMMUNITY; SERUM-LEVELS; OLDER-ADULTS; D DEFICIENCY; 25-HYDROXYVITAMIN-D; DISEASE; OSTEOPOROSIS; POPULATION; PREVALENCE; WOMEN AB Background: Persons with limited exposure to ultraviolet B light, including space travelers, may not receive enough vitamin D. Recent studies indicate that optimal serum 25-hydroxyvitamin D [25(OH) D] should be >= 80 nmol/L. Objective: This study was designed to evaluate the effectiveness of 3 doses of vitamin D to raise and maintain 25(OH) D to a concentration.80 nmol/L in persons with limited ultraviolet B light exposure. Design: This was a 5-mo, prospective, randomized, double-blind study of vitamin D supplementation. It was conducted during winter in Antarctica at the McMurdo Station, when ultraviolet B radiation levels are essentially zero. The 55 subjects were randomly divided into 3 groups for vitamin D supplementation: 2000 IU/d (n = 18), 1000 IU/d (n = 19), and 400 IU/d (n = 18). An additional 7 subjects did not take supplements or took supplements of their own choosing. Blood samples were collected about every 2 mo during the winter. Results: About 5 mo after supplementation started, 25(OH)D increased to 71 +/- 23 nmol/L in the 2000-IU/d group, 63 +/- 25 nmol/L in the 1000-IU/d group, and 57 +/- 15 nmol/L in the 400-IU/d group and decreased to 34 +/- 12 nmol/L in the group not taking supplements. Conclusions: These data will enable us to provide space crews with evidence-based recommendations for vitamin D supplementation. The findings also have implications for other persons with limited ultraviolet light exposure, including polar workers and the elderly. Am J Clin Nutr 2009; 89:1092-8. C1 [Smith, Scott M.; Locke, James] NASA, Lyndon B Johnson Space Ctr, Space Life Sci Directorate, Houston, TX 77058 USA. [Gardner, Keri K.] Univ Calif Los Angeles, Sch Med, Los Angeles, CA USA. [Gardner, Keri K.] VA Greater Los Angeles Hlth Care Syst, Los Angeles, CA USA. [Zwart, Sara R.] Univ Space Res Assoc, Houston, TX USA. RP Smith, SM (reprint author), NASA, Lyndon B Johnson Space Ctr, Space Life Sci Directorate, Mail Code SK3,2101 NASA Pkwy, Houston, TX 77058 USA. EM scott.m.smith@nasa.gov FU NASA; National Science Foundation FX Supported by the NASA Human Research Program and made possible by the National Science Foundation. NR 46 TC 43 Z9 44 U1 0 U2 6 PU AMER SOC CLINICAL NUTRITION PI BETHESDA PA 9650 ROCKVILLE PIKE, SUBSCRIPTIONS, RM L-3300, BETHESDA, MD 20814-3998 USA SN 0002-9165 J9 AM J CLIN NUTR JI Am. J. Clin. Nutr. PD APR 1 PY 2009 VL 89 IS 4 BP 1092 EP 1098 DI 10.3945/ajcn.2008.27189 PG 7 WC Nutrition & Dietetics SC Nutrition & Dietetics GA 420WF UT WOS:000264319200016 PM 19225122 ER PT J AU Hurowitz, JA Tosca, NJ Dyar, MD AF Hurowitz, Joel A. Tosca, Nicholas J. Dyar, M. Darby TI Acid production by FeSO4 center dot nH(2)O dissolution and implications for terrestrial and martian aquatic systems SO AMERICAN MINERALOGIST LA English DT Article DE Mars; AMD; melanterite; pH; Mossbauer ID X-RAY SPECTROMETER; THERMODYNAMIC BEHAVIOR; THEORETICAL PREDICTION; AQUEOUS ELECTROLYTES; MERIDIANI-PLANUM; SULFATE MINERALS; HIGH PRESSURES; IRON MOUNTAIN; MARS; TEMPERATURES AB Combined experimental, modeling, and analytical results indicate that the rapid acidification of dilute waters in contact with nominally Fe2+-sulfate minerals (FeSO4 center dot nH(2)O) is caused by Fe3+ hydrolysis, which occurs when low levels (<1 mol%) of a contaminant Fe3+-sulfate phase are dissolved along with the FeSO4 center dot nH(2)O. This rapid acidification has previously been attributed to hydrolysis by Fe2+. However, dissolution experiments performed using ZnSO4 center dot nH(2)O, in which the Zn2+ cation has a higher hydrolysis constant (log K = -8.96) than Fe2+ (log K = -9.5), failed to produce significant changes in solution pH. We present the results of geochemical modeling simulations confirming that FeSO4 center dot nH(2)O dissolution alone cannot explain the experimentally observed change in pH from 5.65 to 3.50. Nor can the experimental observations be explained by oxidation of Fe2+ to Fe 31 in solution. Instead, our experimental results can be best explained by modeling the incorporation of <1 mol% Fe3+ contamination from any number of Fe3+ or mixed valence Fe-sulfate phases, including anhydrous Fe-2(3+)(SO4)(3), coquimbite, kornelite, romerite, bilinite, copiapite, or ferricopiapite, all of which are reasonable candidate phases for oxidative breakdown products of FeSO4 center dot nH(2)O. Laboratory Mossbauer spectra are consistent with Lip to 0.6 mol% of the total Fe in the sample to be present as Fe3+. Although the doublet has parameters that are not diagnostic of any specific Fe3+-sulfate, they do help constrain its identification. These results demonstrate that minor contamination of labile Fe2+ sulfates by Fe3+ can have dramatic effects on solution chemistry that should be considered when studying reactions relevant to acid mine drainage waste sites and other localities where Fe-sulfate minerals occur, such as the surface of Mars. C1 [Hurowitz, Joel A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Tosca, Nicholas J.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Dyar, M. Darby] Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA. RP Hurowitz, JA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM joel.a.hurowitz@jpl.nasa.gov FU Jet Propulsion Laboratory, California Institute of Technology; NASA [NNX06AB62G] FX This work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This work was also supported by NASA grant NNX06AB62G, and an Origins Initiative Postdoctoral Fellowship to N.J.T. We thank Albert Yen for the use oflaboratory facilities. and WilliamAbbey for assistance with XRD data collection. NR 35 TC 11 Z9 11 U1 2 U2 10 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X EI 1945-3027 J9 AM MINERAL JI Am. Miner. PD APR PY 2009 VL 94 IS 4 BP 409 EP 414 DI 10.2138/am.2009.3085 PG 6 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 432TL UT WOS:000265157000001 ER PT J AU Chiesl, TN Chu, WK Stockton, AM Amashukeli, X Grunthaner, F Mathies, RA AF Chiesl, Thomas N. Chu, Wai K. Stockton, Amanda M. Amashukeli, Xenia Grunthaner, Frank Mathies, Richard A. TI Enhanced Amine and Amino Acid Analysis Using Pacific Blue and the Mars Organic Analyzer Microchip Capillary Electrophoresis System SO ANALYTICAL CHEMISTRY LA English DT Article ID MURCHISON METEORITE; EXTRATERRESTRIAL EXPLORATION; CARBONACEOUS CHONDRITES; BIOMARKER DETECTION; PARENT BODY; SURFACE; CHROMATOGRAPHY; SEPARATIONS; MICRODEVICE; MICELLES AB The fluorescent amine reactive probe Pacific Blue succinimidyl ester (PB) is used for the detection of trace amounts of amines and amino acids by microchip capillary electrophoresis on the Mars Organic Analyzer (MOA). The spectral and chemical properties of PB provide a 200-fold increase in sensitivity and improved resolution compared to fluorescamine derivatization. With the use of cross injection and PB labeling, the MOA detected amino acids at concentrations as low as 75 pM (sub-parts-per-trillion). Micellar electrokinetic chromatograpy (MEKC) which separates PB-labeled amino acids by their hydro-phobicity is also demonstrated. The optimized MEKC conditions (45 mM CHAPSO, pH 6 at 5 degrees C) effectively separated amines and 25 amino acids with enantiomeric resolution of alanine, serine, and citrulline. Samples from the Yungay Hills region in the Atacama Desert, Chile and from the Murchison meteorite are successfully analyzed using both techniques, and amino acids are found in the parts-per-billion range. Abiotic amino acids such as beta-alanine and epsilon-aminocaprioc acid are detected along with several neutral and acidic amino acids in the Murchison sample. The Atacama Desert sample is found to contain homochiral L-alanine and L-serine indicating the presence of extant or recently extinct life. C1 [Chiesl, Thomas N.; Chu, Wai K.; Stockton, Amanda M.; Mathies, Richard A.] Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA. [Amashukeli, Xenia; Grunthaner, Frank] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mathies, RA (reprint author), Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA. EM ramathies@berkeley.edu RI Stockton, Amanda/C-1173-2012 FU NASA [NNG04GB75G, NNX08AR09G]; Jet Propulsion Laboratory at Cal Tech [1297596] FX We acknowledge the assistance of the international Urey Instrument Team as well as the ASAP participants in the course of this research. Microfabrication was carried out at the University of California, Berkeley, Microfabrication Laboratory. This research was supported by NASA Grants NNG04GB75G and NNX08AR09G and by the Jet Propulsion Laboratory at Cal Tech under contract no.1297596. NR 41 TC 50 Z9 51 U1 4 U2 27 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0003-2700 EI 1520-6882 J9 ANAL CHEM JI Anal. Chem. PD APR 1 PY 2009 VL 81 IS 7 BP 2537 EP 2544 DI 10.1021/ac8023334 PG 8 WC Chemistry, Analytical SC Chemistry GA 427DG UT WOS:000264759400017 PM 19245228 ER PT J AU Blum, JS Han, S Lanoil, B Saltikov, C Witte, B Tabita, FR Langley, S Beveridge, TJ Jahnke, L Oremland, RS AF Blum, Jodi Switzer Han, Sukkyun Lanoil, Brian Saltikov, Chad Witte, Brian Tabita, F. Robert Langley, Sean Beveridge, Terry J. Jahnke, Linda Oremland, Ronald S. TI Ecophysiology of "Halarsenatibacter silvermanii" Strain SLAS-1(T), gen. nov., sp nov., a Facultative Chemoautotrophic Arsenate Respirer from Salt-Saturated Searles Lake, California SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID 16S RIBOSOMAL-RNA; GRADIENT GEL-ELECTROPHORESIS; SULFATE-REDUCING BACTERIA; SODA LAKES; MONO LAKE; DISSIMILATORY ARSENATE; FATTY-ACIDS; MEMBRANE-LIPIDS; SEQUENCE DATA; REDUCTION AB Searles Lake occupies a closed basin harboring salt-saturated, alkaline brines that have exceptionally high concentrations of arsenic oxyanions. Strain SLAS-1(T) was previously isolated from Searles Lake (R. S. Orem-land, T. R. Kulp, J. Switzer Blum, S. E. Hoeft, S. Baesman, L. G. Miller, and J. F. Stolz, Science 308: 1305-1308, 2005). We now describe this extremophile with regard to its substrate affinities, its unusual mode of motility, sequenced arrABD gene cluster, cell envelope lipids, and its phylogenetic alignment within the order Halanaero-bacteriales, assigning it the name "Halarsenatibacter silvermanii" strain SLAS-1(T). We also report on the substrate dynamics of an anaerobic enrichment culture obtained from Searles Lake that grows under conditions of salt saturation and whose members include a novel sulfate reducer of the order Desulfovibriales, the archaeon Halorhabdus utahensis, as well as a close homolog of strain SLAS-1(T). C1 [Blum, Jodi Switzer; Oremland, Ronald S.] US Geol Survey, Menlo Pk, CA 94025 USA. [Han, Sukkyun] Univ Calif Riverside, Dept Environm Sci, Riverside, CA 92521 USA. [Lanoil, Brian] Univ Alberta, Dept Biol Sci, Edmonton, AB T6G 2E1, Canada. [Saltikov, Chad] Univ Calif Santa Cruz, Dept Microbiol & Environm Toxicol, Santa Cruz, CA 95064 USA. [Witte, Brian; Tabita, F. Robert] Ohio State Univ, Dept Microbiol, Columbus, OH 43210 USA. [Langley, Sean] Univ Ottawa, Dept Earth Sci, Ottawa, ON K1N 6N5, Canada. [Beveridge, Terry J.] Univ Guelph, Dept Mol & Cellular Biol, Guelph, ON N1G 2W1, Canada. [Jahnke, Linda] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Oremland, RS (reprint author), US Geol Survey, MS 480,345 Middlefield Rd, Menlo Pk, CA 94025 USA. EM roremlan@usgs.gov OI Lanoil, Brian/0000-0001-8603-8330 FU USGS FX This work was supported by the USGS National Research Program and by a NASA Exobiology grant. We are indebted to H. Truper with his help with the epithet.; We are grateful to J. Stolz, C. Pearce, and R. Sierra for constructive criticism of earlier drafts of the manuscript. The TEMs were conducted by S. L. and T. J. B. at the University of Guelph. NR 65 TC 22 Z9 24 U1 0 U2 16 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0099-2240 J9 APPL ENVIRON MICROB JI Appl. Environ. Microbiol. PD APR 1 PY 2009 VL 75 IS 7 BP 1950 EP 1960 DI 10.1128/AEM.02614-08 PG 11 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA 424EX UT WOS:000264549400019 PM 19218420 ER PT J AU Gatewood, AG Liebman, KA Vourc'h, G Bunikis, J Hamer, SA Cortinas, R Melton, F Cislo, P Kitron, U Tsao, J Barbour, AG Fish, D Diuk-Wasser, MA AF Gatewood, Anne G. Liebman, Kelly A. Vourc'h, Gwenael Bunikis, Jonas Hamer, Sarah A. Cortinas, Roberto Melton, Forrest Cislo, Paul Kitron, Uriel Tsao, Jean Barbour, Alan G. Fish, Durland Diuk-Wasser, Maria A. TI Climate and Tick Seasonality Are Predictors of Borrelia burgdorferi Genotype Distribution SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID IXODES-SCAPULARIS ACARI; EARLY LYME-DISEASE; SENSU-STRICTO STRAINS; MEDIUM-SIZED MAMMALS; WHITE-FOOTED MICE; SOUTHERN NEW-YORK; UNITED-STATES; HEMATOGENOUS DISSEMINATION; POPULATION-DYNAMICS; RABIES VIRUS AB The blacklegged tick, Ixodes scapularis, is of significant public health importance as a vector of Borrelia burgdorferi, the agent of Lyme borreliosis. The timing of seasonal activity of each immature I. scapularis life stage relative to the next is critical for the maintenance of B. burgdorferi because larvae must feed after an infected nymph to efficiently acquire the infection from reservoir hosts. Recent studies have shown that some strains of B. burgdorferi do not persist in the primary reservoir host for more than a few weeks, thereby shortening the window of opportunity between nymphal and larval feeding that sustains their enzootic maintenance. We tested the hypothesis that climate is predictive of geographic variation in the seasonal activity of I. scapularis, which in turn differentially influences the distribution of B. burgdorferi genotypes within the geographic range of I. scapularis. We analyzed the relationships between climate, seasonal activity of I. scapularis, and B. burgdorferi genotype frequency in 30 geographically diverse sites in the northeastern and midwestern United States. We found that the magnitude of the difference between summer and winter daily temperature maximums was positively correlated with the degree of seasonal synchrony of the two immature stages of I. scapularis. Genotyping revealed an enrichment of 16S-23S rRNA intergenic spacer restriction fragment length polymorphism sequence type 1 strains relative to others at sites with lower seasonal synchrony. We conclude that climate-associated variability in the timing of I. scapularis host seeking contributes to geographic heterogeneities in the frequencies of B. burgdorferi genotypes, with potential consequences for Lyme borreliosis morbidity. C1 [Gatewood, Anne G.; Liebman, Kelly A.; Cislo, Paul; Fish, Durland; Diuk-Wasser, Maria A.] Yale Univ, Sch Med, Dept Epidemiol & Publ Hlth, New Haven, CT 06520 USA. [Vourc'h, Gwenael] Natl Inst Agr Res, Anim Epidemiol UR346, F-63122 St Genes Champanelle, France. [Bunikis, Jonas; Barbour, Alan G.] Univ Calif Irvine, Dept Microbiol & Mol Genet, Irvine, CA 92697 USA. [Hamer, Sarah A.; Tsao, Jean] Michigan State Univ, Dept Fisheries & Wildlife, E Lansing, MI 48824 USA. [Cortinas, Roberto] Univ Nebraska, Dept Entomol, Lincoln, NE 68583 USA. [Melton, Forrest] Calif State Univ Monterey Bay, Div Sci & Environm Policy, Seaside, CA 93955 USA. [Melton, Forrest] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Kitron, Uriel] Emory Univ, Dept Environm Studies, Atlanta, GA 30322 USA. [Tsao, Jean] Michigan State Univ, Dept Large Anim Clin Sci, E Lansing, MI 48824 USA. RP Diuk-Wasser, MA (reprint author), 60 Coll St,POB 208034, New Haven, CT 06520 USA. EM maria.diuk@yale.edu RI Barbour, Alan/B-3160-2009 OI Barbour, Alan/0000-0002-0719-5248 FU U. S. Centers for Disease Control and Prevention (CDC) [5U01CI00 0171-04]; U. S. Department of Agriculture Agricultural Research Service [58-0790-5-068]; G. Harold and Leila Y. Mathers Foundation FX This research was supported by the U. S. Centers for Disease Control and Prevention (CDC) under cooperative agreement no. 5U01CI00 0171-04, the U. S. Department of Agriculture Agricultural Research Service under cooperative agreement no. 58-0790-5-068, and the G. Harold and Leila Y. Mathers Foundation. A. G. G. acknowledges support from the CDC Fellowship Training Program in Vector-Borne Diseases. NR 62 TC 79 Z9 81 U1 0 U2 41 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0099-2240 J9 APPL ENVIRON MICROB JI Appl. Environ. Microbiol. PD APR PY 2009 VL 75 IS 8 BP 2476 EP 2483 DI 10.1128/AEM.02633-08 PG 8 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA 429RC UT WOS:000264936800028 PM 19251900 ER PT J AU Nixon, CA Teanby, NA Calcutt, SB Aslam, S Jennings, DE Kunde, VG Flasar, FM Irwin, PGJ Taylor, FW Glenar, DA Smith, MD AF Nixon, Conor A. Teanby, Nicholas A. Calcutt, Simon B. Aslam, Shahid Jennings, Donald E. Kunde, Virgil G. Flasar, F. Michael Irwin, Patrick G. J. Taylor, Fredric W. Glenar, David A. Smith, Michael D. TI Infrared limb sounding of Titan with the Cassini Composite InfraRed Spectrometer: effects of the mid-IR detector spatial responses SO APPLIED OPTICS LA English DT Article ID ISOTOPIC-RATIOS; RADIATIVE-TRANSFER; ATMOSPHERE; CIRS; HC3N; HCN; HYDROCARBONS; STRATOSPHERE; PROFILES; SPECTRA AB The composite infrared spectrometer (CIRS) instrument on board the Cassini Saturn orbiter employs two 1 x 10 HgCdTe detector arrays for mid-infrared remote sensing of Titan's and Saturn's atmospheres. In this paper we show that the real detector spatial response functions, as measured in ground testing before launch, differ significantly from idealized "boxcar" responses. We further show that neglecting this true spatial response function when modeling CIRS spectra can have a significant effect on interpretation of the data, especially in limb-sounding mode, which is frequently used for Titan science. This result has implications not just for CIRS data analysis but for other similar instrumental applications. (C) 2009 Optical Society of America C1 [Nixon, Conor A.; Kunde, Virgil G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Nixon, Conor A.; Aslam, Shahid; Jennings, Donald E.; Kunde, Virgil G.; Flasar, F. Michael; Glenar, David A.; Smith, Michael D.] NASA, Goddard Space Flight Ctr, Planetary Syst Branch, Greenbelt, MD 20771 USA. [Teanby, Nicholas A.; Calcutt, Simon B.; Irwin, Patrick G. J.; Taylor, Fredric W.] Univ Oxford, Clarendon Lab, Subdept Atmospher Ocean & Planetary Phys, Oxford OX1 3PU, England. [Aslam, Shahid] MEI Technol Inc, Houston, TX 77058 USA. RP Nixon, CA (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM conor.a.nixon@nasa.gov RI Nixon, Conor/A-8531-2009; Flasar, F Michael/C-8509-2012; Smith, Michael/C-8875-2012; Aslam, Shahid/D-1099-2012; Jennings, Donald/D-7978-2012; OI Nixon, Conor/0000-0001-9540-9121; Calcutt, Simon/0000-0002-0102-3170; Teanby, Nicholas/0000-0003-3108-5775; Irwin, Patrick/0000-0002-6772-384X FU Particle Physics and Astronomy Research Council (PPARC); Science and Technology Facilities Council (STFC); NASA Cassini FX The work described in this paper-including original laboratory measurements and current analysis-was funded by the Particle Physics and Astronomy Research Council (PPARC) and its successor, the Science and Technology Facilities Council (STFC) for the UK component, and in the U.S. by the NASA Cassini project, through their support for the design, build, and operation of the CIRS instrument. We are grateful for the helpful comments provided to us by two anonymous referees. NR 22 TC 16 Z9 16 U1 0 U2 0 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 APR 1 PY 2009 VL 48 IS 10 BP 1912 EP 1925 DI 10.1364/AO.48.001912 PG 14 WC Optics SC Optics GA 436VH UT WOS:000265443700050 PM 19340146 ER PT J AU Schafer, J Lyons, W Tong, WG Danehy, PM AF Schafer, J. Lyons, W. Tong, W. G. Danehy, P. M. TI Kinetic temperature and electron density measurement in an inductively coupled plasma torch using degenerate four-wave mixing SO APPLIED PHYSICS B-LASERS AND OPTICS LA English DT Article ID ATMOSPHERIC-PRESSURE PLASMAS; SPECTROSCOPY; DIAGNOSTICS AB Laser wave mixing is presented as an effective technique for spatially resolved kinetic temperature measurements in an atmospheric-pressure radio-frequency inductively coupled plasma. Measurements are performed in a 1 kW, 27 MHz radio-frequency plasma using a continuous-wave, tunable 811.5 nm diode laser to excite the 4s(3)P(2)-> 4p(3)D(3) argon transition. Kinetic temperature measurements are made at five radial steps from the center of the torch and at four different torch heights. The kinetic temperature is determined by measuring simultaneously the line shape of the sub-Doppler backward phase-conjugate degenerate four-wave mixing and the Doppler broadened forward-scattering degenerate four-wave mixing. The temperature measurements result in a range of 3,500 to 14,000 +/- 150 K. Electron densities measured range from 6.1 (+/- 0.3)x10(15) cm(-3) to 10.1 (+/- 0.3)x10(15) cm(-3). The experimental spectra are analyzed using a perturbative treatment of the backward phase-conjugate and forward-geometry wave-mixing theory. The Stark width is determined from the collisional broadening measured in the phase-conjugate geometry. Electron density measurements are made based on the Stark width. The kinetic temperature of the plasma was found to be more than halved by adding deionized water through the nebulizer. C1 [Schafer, J.; Lyons, W.; Tong, W. G.] San Diego State Univ, Dept Chem & Biochem, San Diego, CA 92182 USA. [Danehy, P. M.] NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, Hampton, VA 23681 USA. RP Tong, WG (reprint author), San Diego State Univ, Dept Chem & Biochem, San Diego, CA 92182 USA. EM william.tong@sdsu.edu FU National Institute of General Medical Sciences, National Institutes of Health [5-R01-GM41032]; Varian, Inc FX We gratefully acknowledge partial support of this work from the National Institute of General Medical Sciences, National Institutes of Health under Grant No. 5-R01-GM41032, and Varian, Inc. NR 20 TC 2 Z9 2 U1 1 U2 4 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0946-2171 J9 APPL PHYS B-LASERS O JI Appl. Phys. B-Lasers Opt. PD APR PY 2009 VL 95 IS 1 BP 161 EP 168 DI 10.1007/s00340-009-3440-0 PG 8 WC Optics; Physics, Applied SC Optics; Physics GA 422XM UT WOS:000264461000022 ER PT J AU Poulet, F Beaty, DW Bibring, JP Bish, D Bishop, JL Dobrea, EN Mustard, JF Petit, S Roach, LH AF Poulet, Francois Beaty, David W. Bibring, Jean-Pierre Bish, David Bishop, Janice L. Dobrea, Eldar Noe Mustard, John F. Petit, Sabine Roach, Leah H. TI Key Scientific Questions and Key Investigations from the First International Conference on Martian Phyllosilicates SO ASTROBIOLOGY LA English DT Article DE Mars; Mineralogy; Space exploration; Phyllosilicates; Prebiotic chemistry ID MARS SOIL; REFLECTANCE SPECTROSCOPY; AQUEOUS ALTERATION; HOMOIONIC CLAYS; SMECTITE CLAYS; MINERALS; ENVIRONMENT; LIFE; MICROORGANISMS; NUCLEOTIDES AB Minerals and their occurrences can tell us about the chemistry, pressure, and temperatures of past environments on Mars and thus allow inferences about the potential for habitability. Thanks to recent space exploration, a new vision is emerging wherein Mars hosted environmental conditions of potential astrobiological relevance. This epoch is identified by the presence of phyllosilicate-bearing deposits, which are generally contained in very ancient basement rocks. In October 2008, over 100 planetary scientists representing 11 countries met in Paris to assess and discuss the relevance of martian phyllosilicates. The conference was structured to promote the discussion and debate of key scientific questions and key essential investigations. The purpose of this report is to document the current state of knowledge related to martian phyllosilicates and to ascertain which questions remain to be addressed: What are the basic characteristics of the phyllosilicate minerals on Mars? What are the genetic mechanisms by which phyllosilicate minerals have formed on Mars? What is the relationship between the phyllosilicate minerals observed in martian meteorites and those detected from orbit? What are the implications of phyllosilicate-bearing rocks for the development of prebiotic chemistry and the preservation of biosignatures? The most promising investigations to address these questions are presented. C1 [Poulet, Francois; Bibring, Jean-Pierre] Univ Paris 11, Inst Astrophys Spatiale, CNRS, F-91405 Orsay, France. [Beaty, David W.; Dobrea, Eldar Noe] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Bish, David] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA. [Bishop, Janice L.] NASA, Ames Res Ctr, SETI Inst, Mountain View, CA USA. [Mustard, John F.; Roach, Leah H.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Petit, Sabine] Univ Poitiers, CNRS, HYDRASA, Poitiers, France. RP Poulet, F (reprint author), Univ Paris 11, Inst Astrophys Spatiale, CNRS, Batiment 121, F-91405 Orsay, France. EM francois.poulet@ias.u-psud.fr NR 73 TC 11 Z9 11 U1 2 U2 5 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD APR PY 2009 VL 9 IS 3 BP 257 EP 267 DI 10.1089/ast.2009.0335 PG 11 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 457GC UT WOS:000266915500001 PM 19400732 ER PT J AU Brozovic, M Jacobson, RA AF Brozovic, M. Jacobson, R. A. TI THE ORBITS OF THE OUTER URANIAN SATELLITES SO ASTRONOMICAL JOURNAL LA English DT Article DE ephemerides; planets and satellites: general; planets and satellites: individual (Uranus) ID IRREGULAR SATELLITES; DISCOVERY; URANUS; ORIGIN; INCLINATION; PLANETS; CAPTURE AB We report on the numerically integrated orbits for the nine outer Uranian satellites. The orbits are calculated based on fits to the astrometric observations for the period from 1984 to 2006. The results include the state vectors, post-fit residuals, and mean orbital elements. We also assess the accuracy of the orbital fits and discuss the need for future measurements. C1 [Brozovic, M.; Jacobson, R. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Brozovic, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM marina.brozovic@jpl.nasa.gov FU Jet Propulsion Laboratory; California Institute of Technology; National Aeronautics and Space Administration FX The research described here was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The authors thank all of the astronomers who contributed with their measurements to this orbital calculation. NR 22 TC 5 Z9 5 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2009 VL 137 IS 4 BP 3834 EP 3842 DI 10.1088/0004-6256/137/4/3834 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 417AF UT WOS:000264046100010 ER PT J AU Mattioda, AL Ricca, A Tucker, J Bauschlicher, CW Allamandola, LJ AF Mattioda, A. L. Ricca, A. Tucker, J. Bauschlicher, C. W., Jr. Allamandola, L. J. TI FAR-INFRARED SPECTROSCOPY OF NEUTRAL CORONENE, OVALENE, AND DICORONYLENE SO ASTRONOMICAL JOURNAL LA English DT Article DE astrochemistry; infrared: ISM; ISM: molecules; methods: laboratory; methods: numerical; techniques: spectroscopic ID POLYCYCLIC AROMATIC-HYDROCARBONS; PAH MOLECULES; EMISSION BANDS; SPECTRA; DUST; GAS; IDENTIFICATION; FREQUENCIES; CATIONS; CARBON AB Here we report the first far-IR (FIR) matrix-isolated spectra of the neutral polycyclic aromatic hydrocarbon (PAH) molecules coronene, ovalene, and dicoronylene. The experimental spectra covered the 650-100 cm(-1) (15.385-100 mu m) range and the theoretical spectra covered the 650-10 cm(-1) (15.385-1000 mu m) range. The experimentally measured values are in excellent agreement with theoretical values. The fundamental differences between the skeletal or drumhead modes of the FIR and the group vibrational modes of the mid-IR are discussed and detailed descriptions of the FIR vibrational modes are given. C1 [Mattioda, A. L.; Ricca, A.; Bauschlicher, C. W., Jr.; Allamandola, L. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ricca, A.] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA. [Tucker, J.] Amherst Coll, Amherst, MA 01002 USA. RP Mattioda, AL (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Andrew.L.Mattioda@nasa.gov; Alessandra.Ricca-1@nasa.gov; Charles.W.Bauschlicher@nasa.gov; Louis.J.Allamandola@nasa.gov FU NASA's Astronomy and Physics Research and Analysis (APRA) [NNX07AH02G]; Astrobiology [811073]; Spitzer Archival; Herschel Laboratory Astrophysics Programs; SETI Institute Summer Research Experience for Undergraduates [AST-0552751] FX We acknowledge financial support from NASA's Astronomy and Physics Research and Analysis (APRA) (NNX07AH02G), Astrobiology (811073), Spitzer Archival, and Herschel Laboratory Astrophysics Programs. Jonathan Tucker acknowledges the support of the SETI Institute Summer Research Experience for Undergraduates (funded by NSF award AST-0552751). We are deeply indebted to Robert Walker for his outstanding technical support of all phases of the experimental work. NR 30 TC 28 Z9 28 U1 0 U2 14 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 APR PY 2009 VL 137 IS 4 BP 4054 EP 4060 DI 10.1088/0004-6256/137/4/4054 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 417AF UT WOS:000264046100031 ER PT J AU Miroshnichenko, AS Hofmann, KH Schertl, D Weigelt, G Kraus, S Manset, N Albert, L Balega, YY Klochkova, VG Rudy, RJ Lynch, DK Mazuk, S Venturini, CC Russell, RW Grankin, KN Puetter, RC Perry, RB AF Miroshnichenko, A. S. Hofmann, K. -H. Schertl, D. Weigelt, G. Kraus, S. Manset, N. Albert, L. Balega, Y. Y. Klochkova, V. G. Rudy, R. J. Lynch, D. K. Mazuk, S. Venturini, C. C. Russell, R. W. Grankin, K. N. Puetter, R. C. Perry, R. B. TI A new spectroscopic and interferometric study of the young stellar object V645 Cygni SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques: spectroscopic; techniques: interferometric; stars: early-type; stars: winds, outflows; circumstellar matter; stars: individual: V645 Cyg ID HERBIG-AE/BE STARS; INFRARED SKY SURVEY; 6.7 GHZ; MOLECULAR OUTFLOW; METHANOL MASERS; EMISSION; V645-CYGNI; ENVELOPES; ATLAS; DUST AB Aims. We present the results of high-resolution optical spectroscopy, low-resolution near-IR spectroscopy and near-infrared speckle interferometry of the massive young stellar object candidate V645 Cyg, acquired to refine its fundamental parameters and the properties of its circumstellar envelope. Methods. Speckle interferometry in the H- and K-bands and an optical spectrum in the range 5200-6680 angstrom with a spectral resolving power of R = 60 000 were obtained at the 6 m telescope of the Russian Academy of Sciences. Another optical spectrum in the range 4300-10 500 angstrom with R = 79 000 was obtained at the 3.6 m CFHT. Low-resolution spectra in the ranges 0.46-1.4 mu m and 1.4-2.5 mu m with R similar to 800 and similar to 700, respectively, were obtained at the 3 m Shane telescope of the Lick Observatory. Results. Using a novel kinematical method based on the non-linear modeling of the neutral hydrogen density profile in the direction toward the object, we propose a distance of D = 4.2 +/- 0.2 kpc. We also suggest a revised estimate of the star's effective temperature, T-eff similar to 25 000 K. We resolved the object in both H- and K-bands. Using a two-component ring fit, we derived a compact component size of 14 mas and 12 mas in the H- and K-band, respectively, which correspond to 29 and 26 AU at the revised distance. Analysis of our own and previously published data indicates a similar to 2 mag decrease in the near-infrared brightness of V645 Cyg at the beginning of the 1980's. At the same time, the cometary nebular condensation N1 appears to fade in this wavelength range with respect to the N0 object, representing the star with a nearly pole-on optically-thick disk and an optically-thin envelope. Conclusions. We conclude that V645 Cyg is a young, massive, main-sequence star, which recently emerged from its cocoon and has already experienced its protostellar accretion stage. The presence of accretion is not necessary to account for the high observed luminosity of (2-6) x 10(4) M-circle dot yr(-1). The receding part of a strong, mostly uniform outflow with a terminal velocity of similar to 800 km s(-1) is only blocked from view far from the star, where forbidden lines form. The near-infrared size of the source is consistent with the dust sublimation distance close to this hot and luminous star and is the largest among all young stellar objects observed interferometrically to-date. C1 [Miroshnichenko, A. S.; Hofmann, K. -H.; Schertl, D.; Weigelt, G.; Kraus, S.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Miroshnichenko, A. S.] Univ N Carolina, Dept Phys & Astron, Greensboro, NC 27402 USA. [Manset, N.; Albert, L.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Balega, Y. Y.; Klochkova, V. G.] Russian Acad Sci, Special Astrophys Observ, Nizhnyj Arkhyz 369167, Russia. [Rudy, R. J.; Lynch, D. K.; Mazuk, S.; Venturini, C. C.; Russell, R. W.] Aerosp Corp, Los Angeles, CA 90009 USA. [Grankin, K. N.] Crimean Astrophys Observ, UA-334413 Nauchnyi, Ukraine. [Puetter, R. C.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Perry, R. B.] NASA, Langley Res Ctr, Earth & Space Sci Support Off, Hampton, VA 23665 USA. RP Miroshnichenko, AS (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM a_mirosh@uncg.edu OI Grankin, Konstantin/0000-0001-5707-8448 NR 58 TC 4 Z9 5 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2009 VL 498 IS 1 BP 115 EP 126 DI 10.1051/0004-6361/200810936 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 440DL UT WOS:000265679500014 ER PT J AU van Kempen, TA van Dishoeck, EF Salter, DM Hogerheijde, MR Jorgensen, JK Boogert, ACA AF van Kempen, T. A. van Dishoeck, E. F. Salter, D. M. Hogerheijde, M. R. Jorgensen, J. K. Boogert, A. C. A. TI The nature of the Class I population in Ophiuchus as revealed through gas and dust mapping SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; circumstellar matter; stars: formation; submillimeter; ISM: clouds; ISM: molecules ID YOUNG STELLAR OBJECTS; LOW-MASS PROTOSTARS; SPECTRAL ENERGY-DISTRIBUTIONS; STAR-FORMING REGIONS; SUBMILLIMETER CONTINUUM OBSERVATIONS; 2-DIMENSIONAL RADIATIVE-TRANSFER; RHO-OPHIUCHI; PROTOSTELLAR ENVELOPES; DARK CLOUD; MOLECULAR CLOUD AB Context. The Ophiuchus clouds, in particular L 1688, are an excellent region to study the embedded phases of star formation, due to the relatively large number of protostars. However, the standard method of finding and characterizing embedded young stellar objects (YSOs) through just their infrared spectral slope does not yield a reliable sample. This may affect the age determinations, often derived from the statistics on the total number of embedded YSOs and pre-main sequence stars within a cloud. Aims. Our aim is to characterize the structure of protostellar envelopes on an individual basis and to correctly identify the embedded YSO population of L 1688. Methods. Spectral maps of the HCO(+) J = 4-3 and C(18)O J = 3-2 lines, using the HARP-B array on the James Clerk Maxwell Telescope and SCUBA 850 mu m dust maps, are obtained of all sources in the L 1688 region with infrared spectral slopes consistent with, or close to, that of embedded YSOs. Selected 350 mu m maps obtained with the Caltech Submillimeter Observatory are presented as well. The properties, extent and variation of dense gas, column density and dust up to 1' (similar to 7500 AU) are probed at 15 '' resolution. Using the spatial variation of the gas and dust, together with the intensity of the HCO(+) J = 4-3 line, we are able to accurately identify the truly embedded YSOs and determine their properties. Results. The protostellar envelopes range from 0.05 to 0.5 M(circle dot) in mass. The concentration of HCO(+) emission (similar to 0.5 to 0.9) is generally higher than that of the dust concentration. Combined with absolute intensities, HCO(+) proves to be a better tracer of protostellar envelopes than dust, which can contain disk and cloud contributions. Our total sample of 45 sources, including all previously classified Class I sources, several flat-spectrum sources and some known disks, was re-classified using the molecular emission. Of these, only 17 sources are definitely embedded YSOs. Four of these embedded YSOs have little (0.1-0.2 M(circle dot)) envelope material remaining and are likely at the interesting transitional stage from embedded YSO to T Tauri star. About half of the flat-spectrum sources are found to be embedded YSOs and about half are disks. Conclusions. The presented classification method is successful in separating embedded YSOs from edge-on disks and confused sources. The total embedded population of the Ophiuchus L 1688 cloud is found almost exclusively in Oph-A, Oph-B2 and the Ophiuchus ridge with only three embedded YSOs not related to these regions. The detailed characterization presented will be necessary to interpret deep interferometric ALMA and future Herschel observations. C1 [van Kempen, T. A.; van Dishoeck, E. F.; Salter, D. M.; Hogerheijde, M. R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Kempen, T. A.] Ctr Astrophys, Cambridge, MA 02138 USA. [van Dishoeck, E. F.] Max Planck Inst Extraterr Phys, MPE, D-85748 Garching, Germany. [Jorgensen, J. K.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Boogert, A. C. A.] NASA, Herschel Sci Ctr, Infrared Proc & Anal Ctr IPAC, Pasadena, CA 91125 USA. RP van Kempen, TA (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM tvankempen@cfa.harvard.edu RI Jorgensen, Jes Kristian/L-7936-2014 OI Jorgensen, Jes Kristian/0000-0001-9133-8047 NR 82 TC 50 Z9 50 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 APR PY 2009 VL 498 IS 1 BP 167 EP 194 DI 10.1051/0004-6361/200810445 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 440DL UT WOS:000265679500019 ER PT J AU Stute, M Sahai, R AF Stute, M. Sahai, R. TI Detection of X-rays from the jet-driving symbiotic star MWC 560 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; binaries: symbiotic; stars: individual: MWC 560 (V694 Mon); stars: white dwarfs; X-rays: stars ID PHOTON IMAGING CAMERA; SYSTEM CH-CYGNI; R-AQUARII; HYDRODYNAMICAL SIMULATIONS; XMM-NEWTON; CATACLYSMIC VARIABLES; EMISSION; MWC-560; SPECTRUM; RADIATION AB Aims. We report the detection of X-ray emission from the jet-driving symbiotic star MWC 560. Methods. We observed MWC 560 with XMM-Newton for 36 ks. We fitted the spectra from the EPIC pn, MOS1 and MOS2 instruments with XSPEC and examined the light curves with the package XRONOS. Results. The spectrum can be fitted with a highly absorbed hard X-ray component from an optically thin hot plasma, a Gaussian emission line with an energy of 6.1 keV and a less absorbed soft thermal component. The best fit is obtained with a model in which the hot component is produced by optically thin thermal emission from an isobaric cooling flow with a maximum temperature of 61 keV, which might be created inside an optically thin boundary layer on the surface of the accreting with dwarf. The derived parameters of the hard component detected from MWC 560 are in good agreement with similar objects such as CH Cyg, SS7317, RT Cru and T CrB, which all form a new sub-class of symbiotic stars emitting hard X-rays. Our previous numerical simulations of the jet of MWC 560 showed that it should produce detectable soft X-ray emission. We infer a temperature of 0.17 keV for the observed soft component, i.e. less than expected from our models. The total soft X-ray flux (i.e. at <3 keV) is more than a factor 100 less than predicted for the propagating jet soon after its birth (<0.3 yr), but consistent with the value expected due its decrease with age. The ROSAT upper limit is also consistent with such a decrease. We find aperiodic or quasi-periodic variability on timescales of minutes and hours, but no periodic rapid variability. Conclusions. All results are consistent with an accreting white dwarf powering the X-ray emission and the existence of an optically thin boundary layer around it. C1 [Stute, M.] Univ Athens, Dept Phys, IASA, Athens 15784, Greece. [Stute, M.] Univ Athens, Sect Astrophys Astron & Mech, Dept Phys, Athens 15784, Greece. [Sahai, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Stute, M (reprint author), Univ Athens, Dept Phys, IASA, Athens 15784, Greece. EM mstute@phys.uoa.gr NR 52 TC 9 Z9 9 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2009 VL 498 IS 1 BP 209 EP 215 DI 10.1051/0004-6361/200811176 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 440DL UT WOS:000265679500021 ER PT J AU Roccatagliata, V Henning, T Wolf, S Rodmann, J Corder, S Carpenter, JM Meyer, MR Dowell, D AF Roccatagliata, V. Henning, Th. Wolf, S. Rodmann, J. Corder, S. Carpenter, J. M. Meyer, M. R. Dowell, D. TI Long-wavelength observations of debris discs around sun-like stars SO ASTRONOMY & ASTROPHYSICS LA English DT Review DE circumstellar matter; planetary systems: formation; stars: late-type; Kuiper Belt ID SCORPIUS OB ASSOCIATION; MAIN-SEQUENCE STARS; TERRESTRIAL PLANET FORMATION; NEARBY YOUNG STARS; SOLAR-TYPE STARS; T-TAURI STARS; CIRCUMSTELLAR DISKS; DUSTY DEBRIS; UPPER LIMITS; COLLISIONAL CASCADES AB Context. Tracing the evolution of debris discs is essential for our understanding of the architecture of planetary system. Even though the evolution of their inner discs has been recently studied with the Spitzer Space Telescope at mid- to far-infrared wavelengths, the outer discs are best characterised by sensitive millimetre observations. Aims. The goal of our study is to understand the evolution timescale of circumstellar debris discs, and the physical mechanisms responsible for such evolution around solar-type stars. In addition, we make a detailed characterisation of the detected debris discs. Methods. Two deep surveys of circumstellar discs around solar-type stars at different ages were carried out at 350 mu m with the CSO and at 1.2 mm with the IRAM 30-m telescope. The dust disc masses were computed from the millimetre emission, where the discs are optically thin. Theoretically, the mass of the disc is expected to decrease with time. To test this hypothesis, we performed the generalised Kendall's tau correlation and three different two-sample tests. A characterisation of the detected debris discs has been obtained by computing the collision and Poynting-Robertson timescales and by modelling the spectral energy distribution. Results. The Kendall's tau correlation yields a probability of 76% that the mass of debris discs and their age are correlated. Similarly, the three two-sample tests give a probability between 70 and 83% that younger and older debris systems belong to different parent populations in terms of dust mass. We detected submillimetre/millimetre emission from six debris discs, enabling a detailed SED modelling. Conclusions. Our results on the correlation and evolution of dust mass as a function of age are conditioned by the sensitivity limit of our survey. Deeper millimetre observations are needed to confirm the evolution of debris material around solar-like stars. In the case of the detected discs, the comparison between collision and Poynting-Robertson timescales supports the hypothesis that these discs are dominated by collisions. All detected debris disc systems show the inner part evacuated from small micron-sized grains. C1 [Roccatagliata, V.; Henning, Th.; Wolf, S.] MPIA, D-69117 Heidelberg, Germany. [Wolf, S.] Univ Kiel, Inst Theoret Phys & Astrophys, D-24098 Kiel, Germany. [Rodmann, J.] Estec, ESA, Res & Sci Support Dept, NL-2201 AZ Noordwijk, Netherlands. [Corder, S.; Carpenter, J. M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Meyer, M. R.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Dowell, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Roccatagliata, V (reprint author), MPIA, Konigstuhl 17, D-69117 Heidelberg, Germany. EM roccata@mpia.de RI Roccatagliata, Veronica/Q-3421-2016 FU German Research Foundation (DFG) through the Emmy Noether [WO 857/2]; NASA Astrobiology Institute; National Science Foundation [AST-0540882] FX All the authors wish to thank the entire FEPS team for their work. V. R. thanks A. Sicilia-Aguilar for helpful discussions on the IRAM data reduction, E. Feigelson for his suggestions about the survival analysis, L. Hillenbrand for some details about the stellar ages, S. J. Kim for her suggestions about the FEPS sample, A. Pasquali and A. Martinez-Sansigre for reading the manuscript. S. W. was supported at the MPIA by the German Research Foundation (DFG) through the Emmy Noether grant WO 857/2. J. R. wishes to thank Jesus Falcon-Barroso for a helpful discussion on how to project 3-d isosurfaces to lower dimensions. M. R. M. thanks support provided through the LAPLACE node of the NASA Astrobiology Institute. Research at the Caltech Submillimetre Observatory is supported by grant AST-0540882 from the National Science Foundation. NR 101 TC 38 Z9 38 U1 2 U2 5 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 APR PY 2009 VL 497 IS 2 BP 409 EP 421 DI 10.1051/0004-6361/200811018 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 431XE UT WOS:000265097300011 ER PT J AU Ferrero, P Klose, S Kann, DA Savaglio, S Schulze, S Palazzi, E Maiorano, E Bohm, P Grupe, D Oates, SR Sanchez, SF Amati, L Greiner, J Hjorth, J Malesani, D Barthelmy, SD Gorosabel, J Masetti, N Roth, MM AF Ferrero, P. Klose, S. Kann, D. A. Savaglio, S. Schulze, S. Palazzi, E. Maiorano, E. Boehm, P. Grupe, D. Oates, S. R. Sanchez, S. F. Amati, L. Greiner, J. Hjorth, J. Malesani, D. Barthelmy, S. D. Gorosabel, J. Masetti, N. Roth, M. M. TI GRB 060605: multi-wavelength analysis of the first GRB observed using integral field spectroscopy SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma rays: bursts ID GAMMA-RAY BURSTS; AFTERGLOW LIGHT CURVES; SWIFT XRT DATA; POTSDAM MULTIAPERTURE SPECTROPHOTOMETER; X-RAY; OPTICAL AFTERGLOW; COMPREHENSIVE ANALYSIS; COLUMN DENSITY; TELESCOPE; PROGENITOR AB The long and relatively faint gamma-ray burst GRB 060605 detected by Swift/BAT lasted about 20 s. Its afterglow could be observed with Swift/XRT for nearly 1 day, while Swift/UVOT could detect the afterglow during the first 6 h after the event. Here, we report on integral field spectroscopy of its afterglow performed with PMAS/PPak mounted at the Calar Alto 3.5 m telescope. In addition, we report on a detailed analysis of XRT and UVOT data and on the results of deep late-time VLT observations that reveal the GRB host galaxy. We find that the burst occurred at a redshift of z = 3.773, possibly associated with a faint, RC = 26.4 +/- 0.3 host. Based on the optical and X-ray data, we deduce information on the SED of the afterglow, the position of the cooling frequency in the SED, the nature of the circumburst environment, its collimation factor, and its energetics. We find that the GRB fireball was expanding into a constant-density medium and that the explosion was collimated with a narrow half-opening angle of about 2.4 degrees. The initial Lorentz factor of the fireball was about 250; however, its beaming-corrected energy release in the gamma-ray band was comparably low. The optical, X-ray afterglow, on the other hand, was rather luminous. Finally, we find that the data are consistent within the error bars with an achromatic evolution of the afterglow during the suspected jet break time at about 0.27 days after the burst. C1 [Ferrero, P.; Klose, S.; Kann, D. A.; Schulze, S.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Savaglio, S.; Greiner, J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Palazzi, E.; Maiorano, E.; Amati, L.; Masetti, N.] INAF Ist Astrofis Spaziale & Fis Cosm Bologna, I-40129 Bologna, Italy. [Maiorano, E.] Univ Ferrara, Dipartimento Fis, I-44100 Ferrara, Italy. [Boehm, P.; Roth, M. M.] Inst Astrophys, D-14482 Potsdam, Germany. [Grupe, D.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Oates, S. R.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Sanchez, S. F.] Ctr Astron Hispano Aleman Calar Alto, Almeria 04004, Spain. [Hjorth, J.; Malesani, D.] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Barthelmy, S. D.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. [Gorosabel, J.] IAA CSIC, Inst Astrofis Andalucia, Granada 18080, Spain. RP Ferrero, P (reprint author), Thuringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, Germany. EM ferrero@tls-tautenburg.de RI Barthelmy, Scott/D-2943-2012; Hjorth, Jens/M-5787-2014; Palazzi, Eliana/N-4746-2015; Amati, Lorenzo/N-5586-2015; OI Schulze, Steve/0000-0001-6797-1889; Hjorth, Jens/0000-0002-4571-2306; Masetti, Nicola/0000-0001-9487-7740; Savaglio, Sandra/0000-0003-2354-3238; Amati, Lorenzo/0000-0001-5355-7388; Palazzi, Eliana/0000-0002-8691-7666 FU DFG [Kl 766/13-2]; German Academic Exchange Service (DAAD) [D/05/54048]; Spanish Ministry of Science and Education [AYA2004-01515, ESP2005-07714-C03-03]; NASA [NAS5-00136]; Danish National Research Foundation; ESO staff FX P. F., S. K. and D. A. K., acknowledge financial support by DFG grant Kl 766/13-2 and by the German Academic Exchange Service (DAAD) under grant No. D/05/54048. S. K. and S. S. thank Kim Page (Leicester) for useful discussions. The research activities of J. G. are supported by the Spanish Ministry of Science and Education through projects AYA2004-01515 and ESP2005-07714-C03-03. Swift is supported at PSU by NASA contract NAS5-00136. The Dark Cosmology Centre is funded by the Danish National Research Foundation. We thank the Calar Alto and the ESO staff for excellent support and the referee for a very careful reading of the manuscript and very helpful remarks. NR 81 TC 28 Z9 28 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 APR PY 2009 VL 497 IS 3 BP 729 EP 741 DI 10.1051/0004-6361/200809980 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 434ND UT WOS:000265280500009 ER PT J AU van Peet, JCA Costantini, E Mendez, M Paerels, FBS Cottam, J AF van Peet, J. C. A. Costantini, E. Mendez, M. Paerels, F. B. S. Cottam, J. TI Properties of the ionised plasma in the vicinity of the neutron-star X-ray binary EXO 0748-676 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE atomic processes; stars: binaries: general; X-rays: binaries; X-rays: individuals: EXO 0748-676 ID PHOTON IMAGING CAMERA; XMM-NEWTON; PHOTOIONIZED PLASMA; CIRCUMBINARY DISKS; ECLIPSE TIMINGS; ACCRETION DISK; LIGHT CURVES; EXO-0748-676; DISCOVERY; BURST AB Aims. We present the spectral analysis of a large set of XMM-Newton observations of EXO 0748-676, a bright dipping low-mass X-ray binary. In particular, we focus on the dipping phenomenon as a result of changes in the properties of the ionised gas close to the source. Methods. We analysed the high-resolution spectra collected with the reflection grating spectrometer on board XMM-Newton. We studied dipping and persistent spectra separately. We used the Epic data to constrain the broad-band continuum. We explored two simple geometrical scenarios for which we derived physical quantities of the absorbing material like the density, size, and mass. Results. We find that the continuum is absorbed by a neutral gas, and by both a collisionally (temperature T similar to 70 eV) and photoionised (ionisation parameter log xi similar to 2.5) absorbers. Emission lines from OVII and OVIII are also detected. This is the first time that evidence of a collisionally ionised absorber has been found in a low-mass X-ray binary. The collisionally ionised absorber may be in the form of dense (n > 10(14) cm(-3)) filaments, located at a distance r greater than or similar to 10(11) cm. During dips, the photoionised absorber significantly increases its column density (factor 2-4) while becoming less ionised. This strengthens the idea that the colder material of the accretion stream impinging the disc is passing on our line of sight during dips. In this scenario, we find that the distance from the neutron star to the impact region (similar to 5 x 10(10) cm) is similar to the size of the neutron star's Roche lobe. The gas observed during the persistent state may have a flattened geometry. Finally, we explore the possibility of the existence of material forming an initial, hotter portion of a circumbinary disc. C1 [van Peet, J. C. A.; Costantini, E.] Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Mendez, M.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Paerels, F. B. S.] Columbia Univ, Dept Astron, Columbia Astrophys Lab, New York, NY 10027 USA. [Cottam, J.] NASA, Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA. RP van Peet, JCA (reprint author), Netherlands Inst Space Res, SRON, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM e.costantini@sron.nl RI Mendez, Mariano/C-8011-2012 OI Mendez, Mariano/0000-0003-2187-2708 FU NWO, The Netherlands Organisation for Scientific Research FX The authors wish to thank the anonymous referee for his/her useful comments. The Space Research Organisation of the Netherlands is financially supported by NWO, The Netherlands Organisation for Scientific Research. NR 35 TC 10 Z9 10 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2009 VL 497 IS 3 BP 805 EP 813 DI 10.1051/0004-6361/200811181 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 434ND UT WOS:000265280500014 ER PT J AU Ibarra, A Kuulkers, E Osborne, JP Page, K Ness, JU Saxton, RD Baumgartner, W Beckmann, V Bode, MF Hernanz, M Mukai, K Orio, M Sala, G Starrfield, S Wynn, GA AF Ibarra, A. Kuulkers, E. Osborne, J. P. Page, K. Ness, J. U. Saxton, R. D. Baumgartner, W. Beckmann, V. Bode, M. F. Hernanz, M. Mukai, K. Orio, M. Sala, G. Starrfield, S. Wynn, G. A. TI Pre-nova X-ray observations of V2491 Cygni (Nova Cyg 2008b) SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays: binaries; novae, cataclysmic variables ID CATACLYSMIC VARIABLES; AM-HERCULIS; EMISSION; ROSAT; INTEGRAL/IBIS; TELESCOPE; BAT AB Classical novae are phenomena caused by explosive hydrogen burning onto an accreting white dwarf. Only one classical nova had been identified in X-rays before the actual optical outburst occurred (V2487 Oph). The recently discovered nova, V2491 Cyg, is one of the fastest (He/N) novae observed to date. Using archival ROSAT, XMM-Newton, and Swift data, we show that V2491 Cyg was a persistent X-ray source during its quiescent time before the optical outburst. We present the X-ray spectral characteristics and derive X-ray fluxes. The pre-outburst X-ray emission is variable, and, at least in one observation, it exhibits a soft X-ray source. C1 [Ibarra, A.; Kuulkers, E.; Ness, J. U.; Saxton, R. D.] ESAC, ESA, Madrid 28691, Spain. [Osborne, J. P.; Page, K.; Wynn, G. A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Baumgartner, W.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Beckmann, V.] ISDC Data Ctr Astrophys, CH-1290 Versoix, Switzerland. [Beckmann, V.] Univ Geneva, Astron Observ, CH-1290 Sauverny, Switzerland. [Bode, M. F.] Liverpool John Moores Univ, Astroph Res Inst, Birkenhead CH41 1LD7, Merseyside, England. [Hernanz, M.] CSIC, IEEC, Fac Ciencies, Bellaterra 08193, Spain. [Mukai, K.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Mukai, K.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Orio, M.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Orio, M.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Sala, G.] Univ Politecn Cataluna, Dept Fis & Engn Nucl, Grp Astron & Astrofis, Barcelona 08036, Spain. [Starrfield, S.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. EM Aitor.Ibarra@sciops.esa.int RI Hernanz, Margarita/K-1770-2014 OI Hernanz, Margarita/0000-0002-8651-7910 FU XMM-Newton; ESA Member States; USA (NASA); STFC; NSF FX We acknowledge the use of observations obtained with XMM-Newton, an ESA science mission with instrument and contributions directly funded by ESA Member States and the USA (NASA), as well as public data from the Swift data archive. J. O. and K. P. acknowledge the support of the STFC; S. S. acknowledges partial support from NASA and NSF grants to ASU. NR 47 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2009 VL 497 IS 1 BP L5 EP L8 DI 10.1051/0004-6361/200911710 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 429AG UT WOS:000264892600002 ER PT J AU Turyshev, VG AF Turyshev, V. G. TI Relativistic gravitational deflection of light and its impact on the modeling accuracy for the Space Interferometry Mission SO ASTRONOMY LETTERS-A JOURNAL OF ASTRONOMY AND SPACE ASTROPHYSICS LA English DT Article DE Interferometric astrometry; SIM; tests of general relativity; solar system ID POST-NEWTONIAN FORMALISM; GENERAL-RELATIVITY; 2ND-ORDER CONTRIBUTIONS; REFERENCE FRAME; TIME-DELAY; ASTROMETRY; GAIA; JUPITER; MASSES; GALAXY AB We study the impact of relativistic gravitational deflection of light on the accuracy of future Space Interferometry Mission (SIM). We estimate the deflection angles caused by the monopole, quadrupole and octupole components of gravitational fields for a number of celestial bodies in the solar system. We observe that, in many cases, the magnitude of the corresponding effects is significantly larger than the 1 A mu as accuracy expected from SIM. This fact argues for the development of a relativistic observational model for the mission that would account for the influence of both static and time-varying effects of gravity on light propagation. Results presented here are different from the ones obtained elsewhere by the fact that we specifically account for the differential nature of the future SIM astrometric measurements. We also obtain an estimate for the accuracy of possible determination of the Eddington's parameter gamma via SIM global astrometric campaign; we conclude that accuracy of similar to 7 x 10(-6) is achievable via measurements of deflection of light by solar gravity. C1 [Turyshev, V. G.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia. [Turyshev, V. G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Turyshev, VG (reprint author), Moscow MV Lomonosov State Univ, Sternberg Astron Inst, 13 Univ Pr, Moscow 119992, Russia. EM turyshev@sai.msu.ru NR 57 TC 5 Z9 5 U1 2 U2 3 PU MAIK NAUKA/INTERPERIODICA/SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013-1578 USA SN 1063-7737 EI 1562-6873 J9 ASTRON LETT+ JI Astron. Lett.-J. Astron. Space Astrophys. PD APR PY 2009 VL 35 IS 4 BP 215 EP 234 DI 10.1134/S106377370904001X PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 429LV UT WOS:000264922800001 ER PT J AU Scully, ST Stecker, FW AF Scully, S. T. Stecker, F. W. TI Lorentz invariance violation and the observed spectrum of ultrahigh energy cosmic rays SO ASTROPARTICLE PHYSICS LA English DT Article DE Cosmic rays; Lorentz invariance; Quantum gravity ID QUANTUM-GRAVITY; UNIVERSE; TESTS AB There has been much interest in possible violations of Lorentz invariance, particularly motivated by quantum gravity theories. It has been suggested that a small amount of Lorentz invariance violation (LIV) could turn off photomeson interactions of ultrahigh energy cosmic rays (UHECRs) with photons of the cosmic background radiation and thereby eliminate the resulting sharp steepening in the spectrum of the highest energy CRs predicted by Greisen Zatsepin and Kuzmin (GZK). Recent measurements of the UHECR spectrum reported by the HiRes and Auger collaborations, however, indicate the presence of the GZK effect. We present the results of a detailed calculation of the modification of the UHECR spectrum caused by LIV using the formalism of Coleman and Glashow. We then compare these results with the experimental UHECR data from Auger and HiRes. Based on these data, we find a best-fit amount of LIV of 4.5(-4.5)(+1.5) X 10(-23), 10(-23) consistent with an upper limit of 6 x 10(-23). This possible amount of LIV can lead to a recovery of the cosmic ray spectrum at higher energies than presently observed. Such an LIV recovery effect can be tested observationally using future detectors. (C) 2009 Elsevier B.V. All rights reserved. C1 [Stecker, F. W.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Scully, S. T.] James Madison Univ, Dept Phys & Astron, Harrisonburg, VA 22807 USA. RP Stecker, FW (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. EM stecker@lheapop.gsfc.nasa.gov RI Stecker, Floyd/D-3169-2012 FU Thomas F. and Kate Miller Jeffress Memorial Trust [J-805] FX STS gratefully acknowledges partial support from the Thomas F. and Kate Miller Jeffress Memorial Trust Grant No. J-805. NR 38 TC 26 Z9 26 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-6505 EI 1873-2852 J9 ASTROPART PHYS JI Astropart Phys. PD APR PY 2009 VL 31 IS 3 BP 220 EP 225 DI 10.1016/j.astropartphys.2009.01.002 PG 6 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 435HK UT WOS:000265334500007 ER PT J AU Collins, NR Kraemer, SB Crenshaw, DM Bruhweiler, FC Melendez, M AF Collins, N. R. Kraemer, S. B. Crenshaw, D. M. Bruhweiler, F. C. Melendez, M. TI PHYSICAL CONDITIONS IN THE NARROW-LINE REGION OF MARKARIAN 3. II. PHOTOIONIZATION MODELING RESULTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (Markarian 3); galaxies: Seyfert; line: formation ID ACTIVE GALACTIC NUCLEI; SEYFERT-2 GALAXY MARKARIAN-3; LARGE-MAGELLANIC-CLOUD; SPACE-TELESCOPE; EMISSION-LINE; NGC 4151; RESOLVED SPECTROSCOPY; ULTRAVIOLET ABSORBERS; INTERSTELLAR GRAINS; INFRARED-EMISSION AB We have examined the physical conditions in the narrow-line region (NLR) of the Seyfert 2 galaxy Markarian 3, using long-slit spectra obtained with the Hubble Space Telescope/Space Telescope Imaging Spectrograph, and photoionization models. We find three components of photoionized gas in the NLR. Two of these components, characterized by emission lines such as [Ne v]lambda 3426 and [O III]lambda 5007, lie within the envelope of the biconical region described in our previous kinematic study. A component of lower ionization gas, in which lines such as [O II]lambda 3727 arise, is found to lie outside the bicone. Each of these components is irradiated by a power-law continuum which is attenuated by intervening gas, presumably closer to the central source. The radiation incident upon the low-ionization gas, external to the bicone, is much more heavily absorbed. These absorbers are similar to the intrinsic UV and X-ray absorbers detected in many Seyfert 1 galaxies, which suggests that the collimation of the ionizing radiation occurs in a circumnuclear wind, rather than a thick, molecular torus. We estimate the mass for the observed NLR emitting gas to be 2 x 10(6) M(circle dot). It is likely that Markarian 3 acquired this gas through an ongoing interaction with the spiral galaxy UGC 3422. C1 [Collins, N. R.; Kraemer, S. B.; Bruhweiler, F. C.] Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Collins, N. R.; Kraemer, S. B.; Bruhweiler, F. C.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Crenshaw, D. M.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. RP Collins, NR (reprint author), Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. EM nicholas.collins@nasa.gov; steven.b.kraemer@nasa.gov; frederick.c.bruhweiler@nasa.gov; marcio@milkyway.gsfc.nasa.gov FU NASA [NAS-526555, NAG5-7584]; [NAG5-4103]; [NAG5-13109] FX We acknowledge the financial support of NAG5-4103 and NAG5-13109. NR 47 TC 12 Z9 12 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2009 VL 694 IS 2 BP 765 EP 788 DI 10.1088/0004-637X/694/2/765 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424AW UT WOS:000264538900005 ER PT J AU Marshall, PJ Hogg, DW Moustakas, LA Fassnacht, CD Bradac, M Schrabback, T Blandford, RD AF Marshall, Philip J. Hogg, David W. Moustakas, Leonidas A. Fassnacht, Christopher D. Bradac, Marusa Schrabback, Tim Blandford, Roger D. TI AUTOMATED DETECTION OF GALAXY-SCALE GRAVITATIONAL LENSES IN HIGH-RESOLUTION IMAGING DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; gravitational lensing; methods: data analysis; methods: statistical; surveys; techniques: miscellaneous ID LYMAN BREAK GALAXY; HUBBLE DEEP FIELD; ALL-SKY SURVEY; ACS SURVEY; CANDIDATE SELECTION; TIME DELAYS; EVOLUTION; SEARCH; QUASAR; SAMPLE AB We expect direct lens modeling to be the key to successful and meaningful automated strong galaxy-scale gravitational lens detection. We have implemented a lens-modeling "robot" that treats every bright red galaxy (BRG) in a large imaging survey as a potential gravitational lens system. Having optimized a simple model for "typical" galaxy-scale gravitational lenses, we generate four assessments of model quality that are then used in an automated classification. The robot infers from these four data the lens classification parameter H that a human would have assigned; the inference is performed using a probability distribution generated from a human-classified training set of candidates, including realistic simulated lenses and known false positives drawn from the Hubble Space Telescope (HST) Extended Groth Strip (EGS) survey. We compute the expected purity, completeness, and rejection rate, and find that these statistics can be optimized for a particular application by changing the prior probability distribution for H; this is equivalent to defining the robot's "character." Adopting a realistic prior based on expectations for the abundance of lenses, we find that a lens sample may be generated that is similar to 100% pure, but only similar to 20% complete. This shortfall is due primarily to the oversimplicity of the model of both the lens light and mass. With a more optimistic robot, similar to 90% completeness can be achieved while rejecting similar to 90% of the candidate objects. The remaining candidates must be classified by human inspectors. Displaying the images used and produced by the robot on a custom "one-click" web interface, we are able to inspect and classify lens candidates at a rate of a few seconds per system, suggesting that a future 1000 deg(2) imaging survey containing 10(7) BRGs, and some 10(4) lenses, could be successfully, and reproducibly, searched in a modest amount of time. We have verified our projected survey statistics, albeit at low significance, using the HST EGS data, discovering four new lens candidates in the process. C1 [Marshall, Philip J.; Blandford, Roger D.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93601 USA. [Marshall, Philip J.; Bradac, Marusa; Blandford, Roger D.] Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94309 USA. [Hogg, David W.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Moustakas, Leonidas A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Fassnacht, Christopher D.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Schrabback, Tim] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Schrabback, Tim] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands. RP Marshall, PJ (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93601 USA. EM pjm@physics.ucsb.edu OI Moustakas, Leonidas/0000-0003-3030-2360; Hogg, David/0000-0003-2866-9403 FU NASA [HST-AR-10676, NAS 5-26555]; Space Telescope Science Institute; U.S. Department of Energy, at the Stanford Linear Accelerator Center [DE-AC02-76SF00515]; TABASGO foundation; National Science Foundation; Netherlands Organization for Scientific Research (NWO); German Ministry for Science and Education (BMBF) FX We thank Raphael Gavazzi, Tommaso Treu, Eric Morganson, Elisabeth Newton, Marco Lombardi, Ole Moller, and Konrad Kuijken for useful discussions, Jean-Paul Kneib for much encouragement, and Cecile Faure for a careful reading of the manuscript. We also thank the anonymous referee for their thoughtful queries and comments. We are grateful to the EGS team for providing their high level science products at an early stage in the project. D. W. H. thanks the staff of the Spitzer Science Center for their hospitality during his visit when some of this work was carried out. We are very grateful to Stuart Marshall and Glenn Morris at KIPAC for providing computing support. Support for this work was provided by NASA through grant HST-AR-10676 (the HAGGLeS project) from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. The work of P.J.M., R. D. B., and M. B. was supported in part by the U.S. Department of Energy, under contract DE-AC02-76SF00515 at the Stanford Linear Accelerator Center. P.J.M. acknowledges support from the TABASGO foundation in the form of a research fellowship. The work of L. A. M. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. The work of R. D. B. was supported in part by a National Science Foundation grant, "Gravitational optics, dark matter, and the evolution of faint galaxies," and by a U. S. Department of Energy Computational Astrophysics Consortium grant, "3. supernovae, gamma-ray bursts, and nucleosynthesis." T. S. acknowledges financial support from the Netherlands Organization for Scientific Research (NWO) and the German Ministry for Science and Education (BMBF) through the TR33 "The Dark Universe." NR 63 TC 35 Z9 35 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2009 VL 694 IS 2 BP 924 EP 942 DI 10.1088/0004-637X/694/2/924 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424AW UT WOS:000264538900015 ER PT J AU Lin, YT Partridge, B Pober, JC El Bouchefry, K Burke, S Klein, JN Coish, JW Huffenberger, KM AF Lin, Yen-Ting Partridge, Bruce Pober, J. C. El Bouchefry, Khadija Burke, Sarah Klein, Jonathan N. Coish, Joseph W. Huffenberger, Kevin M. TI SPECTRAL ENERGY DISTRIBUTION OF RADIO SOURCES IN NEARBY CLUSTERS OF GALAXIES: IMPLICATIONS FOR SUNYAEV-ZEL'DOVICH EFFECT SURVEYS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: clusters: general; galaxies: elliptical and lenticular, cD; radio continuum: galaxies ID ATACAMA COSMOLOGY TELESCOPE; ABELL CLUSTERS; HIGH-FREQUENCY; VLA SURVEY; STATISTICAL-METHODS; ASTRONOMICAL DATA; SOURCE POPULATION; POINT SOURCES; UPPER LIMITS; 30 GHZ AB To explore the high-frequency radio spectra of galaxies in clusters, we used NRAO's Very Large Array at four frequencies, 4.9-43 GHz, to observe 139 galaxies in low redshift (z < 0.25), X-ray detected, clusters. The clusters were selected from the survey conducted by Ledlow and Owen, who provided redshifts and 1.4 GHz flux densities for all the radio sources. We find that more than half of the observed sources have steep microwave spectra as generally expected (alpha < -0.5, in the convention S alpha nu(alpha)). However, 60%-70% of the unresolved or barely resolved sources have flat or inverted spectra. Most of these show an upward turn in flux at nu > 22 GHz, implying a higher flux than would be expected from an extrapolation of the lower-frequency flux measurements. Our results quantify the need for careful source subtraction in increasingly sensitive measurements of the Sunyaev-Zel'dovich effect in clusters of galaxies (as currently being conducted by, for instance, the Atacama Cosmology Telescope and South Pole Telescope groups). C1 [Lin, Yen-Ting] Princeton Univ Observ, Princeton, NJ 08544 USA. [Lin, Yen-Ting] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago, Chile. [Partridge, Bruce; Pober, J. C.; El Bouchefry, Khadija; Burke, Sarah; Klein, Jonathan N.; Coish, Joseph W.] Haverford Coll, Dept Astron, Haverford, PA 19041 USA. [El Bouchefry, Khadija] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, Durban, South Africa. [Burke, Sarah] Swinburne Univ Technol, Hawthorn, Vic 3122, Australia. [Huffenberger, Kevin M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Huffenberger, Kevin M.] Univ Miami, Dept Phys, Coral Gables, FL 33146 USA. RP Lin, YT (reprint author), Univ Tokyo, Inst Phys & Math Universe, Tokyo 1138654, Japan. EM yen-ting.lin@ipmu.jp; bpartrid@haverford.edu OI Huffenberger, Kevin/0000-0001-7109-0099; Pober, Jonathan/0000-0002-3492-0433 FU Princeton-Catolica Fellowship; NSF [OISE-0530095, AST-0606975]; FONDAP-Andes; World Premier International Research Center Initiative, MEXT, Japan; NASA; Alfred P. Sloan Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX This research has made use of the NED and BAX databases, and the data products from the NVSS and GB6 surveys. NR 40 TC 39 Z9 39 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2009 VL 694 IS 2 BP 992 EP 1009 DI 10.1088/0004-637X/694/2/992 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424AW UT WOS:000264538900021 ER PT J AU Mroczkowski, T Bonamente, M Carlstrom, JE Culverhouse, TL Greer, C Hawkins, D Hennessy, R Joy, M Lamb, JW Leitch, EM Loh, M Maughan, B Marrone, DP Miller, A Muchovej, S Nagai, D Pryke, C Sharp, M Woody, D AF Mroczkowski, Tony Bonamente, Max Carlstrom, John E. Culverhouse, Thomas L. Greer, Christopher Hawkins, David Hennessy, Ryan Joy, Marshall Lamb, James W. Leitch, Erik M. Loh, Michael Maughan, Ben Marrone, Daniel P. Miller, Amber Muchovej, Stephen Nagai, Daisuke Pryke, Clem Sharp, Matthew Woody, David TI APPLICATION OF A SELF-SIMILAR PRESSURE PROFILE TO SUNYAEV-ZEL'DOVICH EFFECT DATA FROM GALAXY CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: clusters: individual (Abell 1835, Abell 1914, CL J1226.9+3332); X-rays: galaxies: clusters ID RAY-IMAGING-SPECTROSCOPY; COSMIC DISTANCE SCALE; X-RAY; XMM-NEWTON; TEMPERATURE PROFILES; HOT PLASMA; MASS; GAS; CONSTRAINTS; SAMPLE AB We investigate the utility of a new, self-similar pressure profile for fitting Sunyaev-Zel'dovich (SZ) effect observations of galaxy clusters. Current SZ imaging instruments-such as the Sunyaev-Zel'dovich Array (SZA)-are capable of probing clusters over a large range in a physical scale. A model is therefore required that can accurately describe a cluster's pressure profile over a broad range of radii from the core of the cluster out to a significant fraction of the virial radius. In the analysis presented here, we fit a radial pressure profile derived from simulations and detailed X-ray analysis of relaxed clusters to SZA observations of three clusters with exceptionally high-quality X-ray data: A1835, A1914, and CL J1226.9+3332. From the joint analysis of the SZ and X-ray data, we derive physical properties such as gas mass, total mass, gas fraction and the intrinsic, integrated Compton y-parameter. We find that parameters derived from the joint fit to the SZ and X-ray data agree well with a detailed, independent X-ray-only analysis of the same clusters. In particular, we find that, when combined with X-ray imaging data, this new pressure profile yields an independent electron radial temperature profile that is in good agreement with spectroscopic X-ray measurements. C1 [Mroczkowski, Tony; Miller, Amber] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Mroczkowski, Tony; Muchovej, Stephen] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Mroczkowski, Tony] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Bonamente, Max] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Bonamente, Max; Joy, Marshall] NASA, Dept Space Sci, George C Marshall Space Flight Ctr, Huntsville, AL 35899 USA. [Carlstrom, John E.; Culverhouse, Thomas L.; Greer, Christopher; Hennessy, Ryan; Leitch, Erik M.; Loh, Michael; Marrone, Daniel P.; Pryke, Clem; Sharp, Matthew] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Carlstrom, John E.; Culverhouse, Thomas L.; Greer, Christopher; Hennessy, Ryan; Leitch, Erik M.; Pryke, Clem] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Carlstrom, John E.; Marrone, Daniel P.; Pryke, Clem] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Carlstrom, John E.; Loh, Michael; Sharp, Matthew] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Hawkins, David; Lamb, James W.; Woody, David] CALTECH, Owens Valley Radio Observ, Big Pine, CA 93513 USA. [Maughan, Ben] Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. [Maughan, Ben] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Miller, Amber] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Nagai, Daisuke] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Nagai, Daisuke] Yale Univ, Yale Ctr Astron Astrophys, New Haven, CT 06520 USA. RP Mroczkowski, T (reprint author), Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. OI Marrone, Daniel/0000-0002-2367-1080; Mroczkowski, Tony/0000-0003-3816-5372 FU James S. McDonnell Foundation; National Science Foundation [AST-0604982, PHY-0114422, AST-0507545, AST-05-07161]; University of Chicago; Sloan Fellowship; NRAO Jansky Fellowship; Chandra Fellowship FX We thank John Cartwright, Ben Reddall, and Marcus Runyan for their significant contributions to the construction and commissioning of the SZA instrument. We thank Esra Bulbul and Nicole Hasler for their insights, comments, and help with Chandra X-ray Observatory (CXO) data reduction and figure production. We thank the staff of the Owens Valley Radio Observatory and CARMA for their outstanding support. We thank Samuel LaRoque for his help with the modeling code. We gratefully acknowledge the James S. McDonnell Foundation, the National Science Foundation and the University of Chicago for funding to construct the SZA. The operation of the SZA is supported by NSF Division of Astronomical Sciences through grant AST-0604982. Partial support is provided by NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, and by NSF grants AST-0507545 and AST-05-07161 to Columbia University. A. M. acknowledges support from a Sloan Fellowship, D. P. M. from an NRAO Jansky Fellowship, B. M. from a Chandra Fellowship, and C. G., S. M., and M. S. from NSF Graduate Research Fellowships. NR 52 TC 49 Z9 49 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2009 VL 694 IS 2 BP 1034 EP 1044 DI 10.1088/0004-637X/694/2/1034 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424AW UT WOS:000264538900024 ER PT J AU van Belle, GT von Braun, K AF van Belle, Gerard T. von Braun, Kaspar TI DIRECTLY DETERMINED LINEAR RADII AND EFFECTIVE TEMPERATURES OF EXOPLANET HOST STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: stars; stars: fundamental parameters; techniques: interferometric ID PALOMAR TESTBED INTERFEROMETER; CHARA ARRAY; ANGULAR DIAMETERS; M GIANTS; NEARBY STARS; COOL STARS; SUPERGIANTS; HIPPARCOS; CATALOG; SYSTEMS AB We present interferometric angular sizes for 12 stars with known planetary companions, for comparison with 28 additional main-sequence stars not known to host planets. For all objects we estimate bolometric fluxes and reddenings through spectral-energy distribution (SED) fits, and in conjunction with the angular sizes, measurements of effective temperature. The angular sizes of these stars are sufficiently small that the fundamental resolution limits of our primary instrument, the Palomar Testbed Interferometer, are investigated at the sub-milliarcsecond level and empirically established based upon known performance limits. We demonstrate that the effective temperature scale as a function of dereddened (V - K)(0) color is statistically identical for stars with and without planets. A useful byproduct of this investigation is a direct calibration of the T(EFF) scale for solarlike stars, as a function of both spectral type and (V - K)(0) color, with an precision of (Delta T) over bar ((V-K)0) = 138 K over the range (V - K)(0) = 0.0- 4.0 and (Delta T) over bar (SpType) = 105 K for the range F6V- G5V. Additionally, in an Appendix we provide SED fits for the 166 stars with known planets which have sufficient photometry available in the literature for such fits; this derived "XO-Rad" database includes homogeneous estimates of bolometric flux, reddening, and angular size. C1 [van Belle, Gerard T.] European So Observ, D-85748 Garching, Germany. [von Braun, Kaspar] NASA, CALTECH, Exoplanet Sci Inst, Pasadena, CA 91125 USA. RP van Belle, GT (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM gerard.van.belle@eso.org; kaspar@ipac.caltech.edu NR 45 TC 76 Z9 76 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2009 VL 694 IS 2 BP 1085 EP 1098 DI 10.1088/0004-637X/694/2/1085 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424AW UT WOS:000264538900029 ER PT J AU Reichardt, CL Ade, PAR Bock, JJ Bond, JR Brevik, JA Contaldi, CR Daub, MD Dempsey, JT Goldstein, JH Holzapfel, WL Kuo, CL Lange, AE Lueker, M Newcomb, M Peterson, JB Ruhl, J Runyan, MC Staniszewski, Z AF Reichardt, C. L. Ade, P. A. R. Bock, J. J. Bond, J. R. Brevik, J. A. Contaldi, C. R. Daub, M. D. Dempsey, J. T. Goldstein, J. H. Holzapfel, W. L. Kuo, C. L. Lange, A. E. Lueker, M. Newcomb, M. Peterson, J. B. Ruhl, J. Runyan, M. C. Staniszewski, Z. TI HIGH-RESOLUTION CMB POWER SPECTRUM FROM THE COMPLETE ACBAR DATA SET SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmology: observations ID COSMIC BACKGROUND IMAGER; PROBE WMAP OBSERVATIONS; HUBBLE-SPACE-TELESCOPE; NUMBER COUNTS; COSMOLOGICAL PARAMETERS; LOCKMAN HOLE; 2003 FLIGHT; SUBMILLIMETER MAPS; POINT SOURCES; DARK ENERGY AB In this paper, we present results from the complete set of cosmic microwave background (CMB) radiation temperature anisotropy observations made with the Arcminute Cosmology Bolometer Array Receiver (ACBAR) operating at 150 GHz. We include new data from the final 2005 observing season, expanding the number of detector hours by 210% and the sky coverage by 490% over that used for the previous ACBAR release. As a result, the band- power uncertainties have been reduced by more than a factor of two on angular scales encompassing the third to fifth acoustic peaks as well as the damping tail of the CMB power spectrum. The calibration uncertainty has been reduced from 6% to 2.1% in temperature through a direct comparison of the CMB anisotropy measured by ACBAR with that of the dipole-calibrated WMAP5 experiment. The measured power spectrum is consistent with a spatially flat, Lambda CDM cosmological model. We include the effects of weak lensing in the power spectrum model computations and find that this significantly improves the fits of the models to the combined ACBAR+WMAP5 power spectrum. The preferred strength of the lensing is consistent with theoretical expectations. On fine angular scales, there is weak evidence (1.1 sigma) for excess power above the level expected from primary anisotropies. We expect any excess power to be dominated by the combination of emission from dusty protogalaxies and the Sunyaev-Zel'dovich effect (SZE). However, the excess observed by ACBAR is significantly smaller than the excess power at l > 2000 reported by the CBI experiment operating at 30 GHz. Therefore, while it is unlikely that the CBI excess has a primordial origin; the combined ACBAR and CBI results are consistent with the source of the CBI excess being either the SZE or radio source contamination. C1 [Reichardt, C. L.; Bock, J. J.; Brevik, J. A.; Kuo, C. L.; Lange, A. E.; Runyan, M. C.] CALTECH, Pasadena, CA 91125 USA. [Ade, P. A. R.] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. [Bock, J. J.; Lange, A. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bond, J. R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Contaldi, C. R.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England. [Daub, M. D.; Holzapfel, W. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Dempsey, J. T.] Joint Astron Ctr, Hilo, HI 96720 USA. [Goldstein, J. H.; Ruhl, J.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA. [Goldstein, J. H.] Arete Associates, Arlington, VA 22202 USA. [Kuo, C. L.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Kuo, C. L.] Stanford Univ, KIPAC, Stanford, CA 94305 USA. [Newcomb, M.] Univ Chicago, Yerkes Observ, Williams Bay, WI 53191 USA. [Peterson, J. B.] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. RP Reichardt, CL (reprint author), CALTECH, MS 59-33, Pasadena, CA 91125 USA. RI Peterson, Jeffrey/O-4794-2014; Holzapfel, William/I-4836-2015; OI Peterson, Jeffrey/0000-0003-1340-818X; Reichardt, Christian/0000-0003-2226-9169 NR 65 TC 273 Z9 273 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2009 VL 694 IS 2 BP 1200 EP 1219 DI 10.1088/0004-637X/694/2/1200 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424AW UT WOS:000264538900038 ER PT J AU Madore, BF Freedman, WL Catanzarite, J Navarrete, M AF Madore, Barry F. Freedman, Wendy L. Catanzarite, Joseph Navarrete, Mauricio TI THE CEPHEID DISTANCE TO NGC 0247 SO ASTROPHYSICAL JOURNAL LA English DT Article DE Cepheids; galaxies: distances and redshifts; galaxies: individual (NGC 0247) ID BVRI CCD PHOTOMETRY; GALAXIES; FIELD; DISCOVERY; VARIABLES; PROJECT; NGC-300; PROGRAM; SCALE; STARS AB We report VRI CCD observations of nine Cepheids in the South Polar (Sculptor) Group spiral galaxy NGC 0247. Periods of these Cepheids range from 20 to 70 days. Over the past 20 years, the brightest Cepheid in our sample, NGC 0247:[MF09] C1, has decreased its period by 6%, faded by 0.8 mag in the V band, and become bluer by 0.23 mag in (V-I). A multiwavelength analysis of the Cepheid data yields a true distance modulus of mu(o) = 27.81 +/- 0.10 mag (3.65 +/- 0.17 Mpc) with a total line-of-sight reddening of E(V-I) = 0.07 +/- 0.04 mag, after adopting an LMC true distance modulus of 18.5 mag and reddening of E(B-V) = 0.10 mag. These results are in excellent agreement with other very recently published (Cepheid and tip of the red giant branch) distances to NGC 0247. Combining both Cepheid data sets gives mu(o) = 27.85 +/- 0.09 mag (3.72 +/- 0.15 Mpc) with E(V-I) = 0.11 +/- 0.03 mag. C1 [Madore, Barry F.; Freedman, Wendy L.] Carnegie Inst Washington, Pasadena, CA 91101 USA. [Catanzarite, Joseph] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Navarrete, Mauricio] Carnegie Inst Washington, Las Campanas Observ, La Serena, Chile. RP Madore, BF (reprint author), Carnegie Inst Washington, 813 Santa Barbara St, Pasadena, CA 91101 USA. EM barry@ociw.edu; wendy@ociw.edu; joseph.h.catanzarite@jpl.nasa.gov; mnavarrete@lco.cl NR 18 TC 4 Z9 4 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2009 VL 694 IS 2 BP 1237 EP 1249 DI 10.1088/0004-637X/694/2/1237 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424AW UT WOS:000264538900041 ER PT J AU Budavari, T Heinis, S Szalay, AS Nieto-Santisteban, M Gupchup, J Shiao, B Smith, M Chang, RX Kauffmann, G Morrissey, P Schiminovich, D Milliard, B Wyder, TK Martin, DC Barlow, TA Seibert, M Forster, K Bianchi, L Donas, J Friedman, PG Heckman, TM Lee, YW Madore, BF Neff, SG Rich, RM Welsh, BY AF Budavari, Tamas Heinis, Sebastien Szalay, Alexander S. Nieto-Santisteban, Maria Gupchup, Jayant Shiao, Bernie Smith, Myron Chang, Ruixiang Kauffmann, Guinevere Morrissey, Patrick Schiminovich, David Milliard, Bruno Wyder, Ted K. Martin, D. Christopher Barlow, Tom A. Seibert, Mark Forster, Karl Bianchi, Luciana Donas, Jose Friedman, Peter G. Heckman, Timothy M. Lee, Young-Wook Madore, Barry F. Neff, Susan G. Rich, R. Michael Welsh, Barry Y. TI GALEX-SDSS CATALOGS FOR STATISTICAL STUDIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; methods: statistical; surveys; ultraviolet: general ID DIGITAL SKY SURVEY; GALAXY-EVOLUTION-EXPLORER; FOOTPRINT SERVICES; REPRESENTATIONS; CLASSIFICATION; CALIBRATION; FITS AB We present a detailed study of the Galaxy Evolution Explorer's (GALEX) photometric catalogs with special focus on the statistical properties of the All-sky and Medium Imaging Surveys. We introduce the concept of primaries to resolve the issue of multiple detections and follow a geometric approach to define clean catalogs with well understood selection functions. We cross-identify the GALEX sources (GR2+3) with Sloan Digital Sky Survey (SDSS; DR6) observations, which indirectly provides an invaluable insight into the astrometric model of the UV sources and allows us to revise the band merging strategy. We derive the formal description of the GALEX footprints as well as their intersections with the SDSS coverage along with analytic calculations of their areal coverage. The crossmatch catalogs are made available for the public. We conclude by illustrating the implementation of typical selection criteria in SQL for catalog subsets geared toward statistical analyses, e. g., correlation and luminosity function studies. C1 [Budavari, Tamas; Heinis, Sebastien; Szalay, Alexander S.; Nieto-Santisteban, Maria; Bianchi, Luciana; Heckman, Timothy M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Gupchup, Jayant] Johns Hopkins Univ, Dept Comp Sci, Baltimore, MD 21218 USA. [Shiao, Bernie; Smith, Myron] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Chang, Ruixiang] Shanghai Astron Observ, Shanghai 200030, Peoples R China. [Kauffmann, Guinevere] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Morrissey, Patrick; Wyder, Ted K.; Martin, D. Christopher; Barlow, Tom A.; Forster, Karl; Friedman, Peter G.] CALTECH, Pasadena, CA 91125 USA. [Schiminovich, David] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Milliard, Bruno; Donas, Jose] Lab Astrophys Marseille, F-13376 Marseille 12, France. [Forster, Karl; Madore, Barry F.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Lee, Young-Wook] Yonsei Univ, Ctr Space Astrophys, Seoul 120749, South Korea. [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 Budavari, T (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3701 San Martin Dr, Baltimore, MD 21218 USA. EM budavari@jhu.edu FU NASA; National Science Foundation FX GALEX is a NASA Small Explorer. We acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. This research has made use of data obtained from and software provided by the US National Virtual Observatory, which is sponsored by the National Science Foundation. T. B. gratefully acknowledges support from the Gordon and Betty Moore Foundation via GBMF 554. NR 28 TC 40 Z9 41 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2009 VL 694 IS 2 BP 1281 EP 1292 DI 10.1088/0004-637X/694/2/1281 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424AW UT WOS:000264538900045 ER PT J AU Galametz, A Stern, D Eisenhardt, PRM Brodwin, M Brown, MJI Dey, A Gonzalez, AH Jannuzi, BT Moustakas, LA Stanford, SA AF Galametz, Audrey Stern, Daniel Eisenhardt, Peter R. M. Brodwin, Mark Brown, Michael J. I. Dey, Arjun Gonzalez, Anthony H. Jannuzi, Buell T. Moustakas, Leonidas A. Stanford, S. Adam TI THE COSMIC EVOLUTION OF ACTIVE GALACTIC NUCLEI IN GALAXY CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: clusters: general; galaxies: evolution; infrared: galaxies; radio continuum: galaxies; X-rays: galaxies ID DUST-OBSCURED GALAXIES; IRAC SHALLOW SURVEY; QSO REDSHIFT SURVEY; X-RAY SURVEY; LUMINOSITY FUNCTION; RADIO GALAXIES; ENERGY-DISTRIBUTIONS; LARGE POPULATION; SKY SURVEY; 1.4 GHZ AB We present the surface density of luminous active galactic nuclei (AGNs) associated with a uniformly selected galaxy cluster sample identified in the 8.5 deg(2) Bootes field of the NOAO Deep Wide-Field Survey. The clusters are distributed over a large range of redshift (0 < z < 1.5), and we identify AGN using three different selection criteria: mid-IR color, radio luminosity, and X-ray luminosity. Relative to the field, we note a clear overdensity of the number of AGNs within 0.5 Mpc of the cluster centers at z > 0.5. The amplitude of this AGN overdensity increases with redshift. Although there are significant differences between the AGN populations probed by each selection technique, the rise in cluster AGN surface density generally increases more steeply than that of field quasars. In particular, X-ray-selected AGNs are at least 3 times more prevalent in clusters at 1 < z < 1.5 compared to clusters at 0.5 < z < 1. This effect is stronger than can be explained by the evolving median richness of our cluster sample. We thus confirm the existence of a Butcher-Oemler-type effect for AGN in galaxy clusters, with the number of AGNs in clusters increasing with redshift. C1 [Galametz, Audrey; Stern, Daniel; Eisenhardt, Peter R. M.; Moustakas, Leonidas A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Galametz, Audrey] European So Observ, D-85748 Garching, Germany. [Galametz, Audrey] Observ Astron, F-67000 Strasbourg, France. [Brodwin, Mark; Dey, Arjun; Jannuzi, Buell T.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Brown, Michael J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Stanford, S. Adam] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. RP Galametz, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM agalamet@eso.org RI Brown, Michael/B-1181-2015; OI Brown, Michael/0000-0002-1207-9137; Moustakas, Leonidas/0000-0003-3030-2360 FU National Optical Astronomy Observatory (NOAO); National Science Foundation; NSF [AST-0708490]; University of California, Lawrence Livermore National Laboratory [W-7405-Eng-48] FX We thank the anonymous referee whose comments significantly improved this paper. We thank Joel Vernet and Carlos De Breuck for carefully reading the manuscript. This work is partly based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. This work made use of data products provided by the NOAO Deep Wide- Field Survey, which is supported by the National Optical Astronomy Observatory (NOAO). NOAO is operated by AURA, Inc., under a cooperative agreement with the National Science Foundation. A. H. G. acknowledges support from NSF grant AST-0708490. SAS's work was performed under the auspices of the U. S. Department of Energy, National Nuclear Security Administration by the University of California, Lawrence Livermore National Laboratory under contract No. W-7405-Eng-48. NR 59 TC 46 Z9 46 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2009 VL 694 IS 2 BP 1309 EP 1316 DI 10.1088/0004-637X/694/2/1309 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424AW UT WOS:000264538900047 ER PT J AU Daddi, E Dannerbauer, H Stern, D Dickinson, M Morrison, G Elbaz, D Giavalisco, M Mancini, C Pope, A Spinrad, H AF Daddi, E. Dannerbauer, H. Stern, D. Dickinson, M. Morrison, G. Elbaz, D. Giavalisco, M. Mancini, C. Pope, A. Spinrad, H. TI TWO BRIGHT SUBMILLIMETER GALAXIES IN A z=4.05 PROTOCLUSTER IN GOODS-NORTH, AND ACCURATE RADIO-INFRARED PHOTOMETRIC REDSHIFTS SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmology: observations; galaxies: formation; galaxies: high-redshift; galaxies: starburst; infrared: galaxies; submillimeter ID STAR-FORMING GALAXIES; HUBBLE-DEEP-FIELD; DEGREE EXTRAGALACTIC SURVEY; LYMAN-BREAK GALAXIES; SCUBA SUPER-MAP; MASSIVE GALAXIES; FORMATION HISTORY; ELLIPTIC GALAXIES; EVOLVED GALAXIES; PASSIVE GALAXIES AB We present the serendipitous discovery of molecular gas CO emission lines with the IRAM Plateau de Bure interferometer coincident with two luminous submillimeter galaxies (SMGs) in the Great Observatories Origins Deep Survey North (GOODS-N) field. The identification of the millimeter emission lines as CO[4-3] at z = 4.05 is based on the optical and near-IR photometric redshifts, radio-infrared photometric redshifts, and Keck+DEIMOS optical spectroscopy. These two galaxies include the brightest submillimeter source in the field (GN20; S-850 mu m = 20.3 mJy, z(CO) = 4.055 +/- 0.001) and its companion (GN20.2; S-850 mu m = 9.9 mJy, z(CO) = 4.051 +/- 0.003). These are among the most distant submillimeter-selected galaxies reliably identified through CO emission and also some of the most luminous known. GN20.2 has a possible additional counterpart and a luminous active galactic nucleus inside its primary counterpart revealed in the radio. Continuum emission of 0.3 mJy at 3.3 mm (0.65 mm in the rest frame) is detected at 5 sigma for GN20, the first dust continuum detection in an SMG at such long wavelength, unveiling a spectral energy distribution that is similar to local ultra luminous IR galaxies. In terms of CO to bolometric luminosities, stellar mass, and star formation rates (SFRs), these newly discovered z > 4 SMGs are similar to z similar to 2-3 SMGs studied to date. These z similar to 4 SMGs have much higher specific star formation rates than those of typical B-band dropout Lyman break galaxies at the same redshift. The stellar mass-SFR correlation for normal galaxies does not seem to evolve much further, between z similar to 2 and z similar to 4. A significant z = 4.05 spectroscopic redshift spike is observed in GOODS-N, and a strong spatial overdensity of B-band dropouts and IRAC selected z > 3.5 galaxies appears to be centered on the GN20 and GN20.2 galaxies. This suggests a protocluster structure with total mass similar to 10(14) M-circle dot. Using photometry at mid-IR ( 24 mu m), submillimeter (850 mu m), and radio (20 cm) wavelengths, we show that reliable photometric redshifts (Delta z/(1 + z) similar to 0.1) can be derived for SMGs over 1 less than or similar to z less than or similar to 4. This new photometric redshift technique has been used to provide a first estimate of the space density of 3.5 < z < 6 hyper-luminous starburst galaxies, and to show that they both contribute substantially to the SFR density at early epochs and that they can account for the presence of old galaxies at z similar to 2-3. Many of these high-redshift starbursts will be within reach of Herschel. We find that the criterion S-1.4 GHz greater than or similar to S-24 mu m, coupled to optical, near-IR and mid-IR photometry, can be used to select z > 3.5 starbursts, regardless of their submillimeter/millimeter emission. C1 [Daddi, E.; Elbaz, D.; Mancini, C.] Univ Paris Diderot, CNRS, Lab AIM, CEA,Irfu SAp, F-91191 Gif Sur Yvette, France. [Dannerbauer, H.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Dickinson, M.; Pope, A.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Morrison, G.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Morrison, G.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Giavalisco, M.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Mancini, C.] Univ Firenze, Dipartimento Astron, I-50100 Florence, Italy. [Spinrad, H.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Daddi, E (reprint author), Univ Paris Diderot, CNRS, Lab AIM, CEA,Irfu SAp, F-91191 Gif Sur Yvette, France. EM edaddi@cea.fr RI Daddi, Emanuele/D-1649-2012 OI Daddi, Emanuele/0000-0002-3331-9590 FU INSU/CNRS ( France); MPG ( Germany); IGN ( Spain); French ANR [ANR-07-BLAN-0228, ANR-08-JCJC0008]; NASA [1224666] FX This study is based on observations carried out with the IRAM Plateau de Bure Interferometer. IRAM is supported by INSU/CNRS ( France), MPG ( Germany), and IGN ( Spain). We are grateful to Grant Wilson for sharing with us unpublished information from the GOODS-N AzTEC supermap. We thank Arancha Castro- Carrizo for assistance with the reduction of the IRAM Plateau de Bure Interferometer data, and Ranga-Ram Chary for discussions. Comments by an anonymous referee helped improving the paper. We acknowledge the use of GILDAS software (http://www.iram.fr/IRAMFR/GILDAS). E. D., C. M., and D. E. acknowledge support from the French ANR grant numbers ANR-07-BLAN-0228 and ANR-08-JCJC0008. The work of D. S. was carried out at Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA, contract number 1224666 issued by the JPL, Caltech, under NASA contract 1407. NR 116 TC 215 Z9 216 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 APR 1 PY 2009 VL 694 IS 2 BP 1517 EP 1538 DI 10.1088/0004-637X/694/2/1517 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424AW UT WOS:000264538900065 ER PT J AU Kim, JH Wise, JH Abel, T AF Kim, Ji-Hoon Wise, John H. Abel, Tom TI GALAXY MERGERS WITH ADAPTIVE MESH REFINEMENT: STAR FORMATION AND HOT GAS OUTFLOW SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: formation; galaxies: interactions; galaxies: starburst; stars: formation ID SMOOTHED PARTICLE HYDRODYNAMICS; FORMING GALAXIES; INTERSTELLAR-MEDIUM; MULTIPHASE MODEL; MAJOR MERGERS; DISK GALAXIES; HOST GALAXIES; SIMULATIONS; FEEDBACK; GASDYNAMICS AB In hierarchical structure formation, merging of galaxies is frequent and known to dramatically affect their properties. To comprehend these interactions high-resolution simulations are indispensable because of the nonlinear coupling between pc and Mpc scales. To this end, we present the first adaptive mesh refinement (AMR) simulation of two merging, low mass, initially gas-rich galaxies (1.8 x 10(10) M(circle dot) each), including star formation and feedback. With galaxies resolved by similar to 2 x 10(7) total computational elements, we achieve unprecedented resolution of the multiphase interstellar medium, finding a widespread starburst in the merging galaxies via shock-induced star formation. The high dynamic range of AMR also allows us to follow the interplay between the galaxies and their embedding medium depicting how galactic outflows and a hot metal-rich halo form. These results demonstrate that AMR provides a powerful tool in understanding interacting galaxies. C1 [Kim, Ji-Hoon; Abel, Tom] Kavli Inst Particle Astrophys & Cosmol, SLAC Natl Accelerator Lab, Menlo Pk, CA USA. [Kim, Ji-Hoon; Abel, Tom] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Wise, John H.] NASA, Goddard Space Flight Ctr, Lab Astron & Cosmol, Greenbelt, MD 20771 USA. RP Kim, JH (reprint author), Kavli Inst Particle Astrophys & Cosmol, SLAC Natl Accelerator Lab, Menlo Pk, CA USA. EM mornkr@slac.stanford.edu FU NASA ATFP grant [NNX08AH26G]; NSF [AST-0807312] FX We thank Marcelo Alvarez, T. J. Cox, Andres Escala, Kristian Finlator, Yuexing Li, Changbom Park, Cecilia Scannapieco, Volker Springel, Elizabeth Tasker, Matthew Turk, Peng Wang, and Risa Wechsler for insightful comments and advice. J. K. was supported by William R. and Sara Hart Kimball Stanford Graduate Fellowship. J. H. W. was supported by an appointment to the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities. This work was partially supported by NASA ATFP grant NNX08AH26G and NSF AST-0807312. These calculations were performed on 32 processors of the Orange cluster at KIPAC. NR 44 TC 27 Z9 27 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 1 PY 2009 VL 694 IS 2 BP L123 EP L127 DI 10.1088/0004-637X/694/2/L123 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 419CL UT WOS:000264196600008 ER PT J AU Evans, NJ Dunham, MM Jorgensen, JK Enoch, ML Merin, B van Dishoeck, EF Alcala, JM Myers, PC Stapelfeldt, KR Huard, TL Allen, LE Harvey, PM van Kempen, T Blake, GA Koerner, DW Mundy, LG Padgett, DL Sargent, AI AF Evans, Neal J., II Dunham, Michael M. Jorgensen, Jes K. Enoch, Melissa L. Merin, Bruno van Dishoeck, Ewine F. Alcala, Juan M. Myers, Philip C. Stapelfeldt, Karl R. Huard, Tracy L. Allen, Lori E. Harvey, Paul M. van Kempen, Tim Blake, Geoffrey A. Koerner, David W. Mundy, Lee G. Padgett, Deborah L. Sargent, Anneila I. TI THE SPITZER c2d LEGACY RESULTS: STAR-FORMATION RATES AND EFFICIENCIES; EVOLUTION AND LIFETIMES SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Review DE dust, extinction; infrared: stars; ISM: clouds; stars: formation ID YOUNG STELLAR OBJECTS; INITIAL MASS FUNCTION; MAIN-SEQUENCE STARS; SPECTRAL ENERGY-DISTRIBUTIONS; AURIGA MOLECULAR CLOUD; II DARK CLOUD; T-TAURI STARS; SPACE-TELESCOPE OBSERVATIONS; DUST CONTINUUM EMISSION; RHO-OPHIUCHI CLOUD AB The c2d Spitzer Legacy project obtained images and photometry with both IRAC and MIPS instruments for five large, nearby molecular clouds. Three of the clouds were also mapped in dust continuum emission at 1.1 mm, and optical spectroscopy has been obtained for some clouds. This paper combines information drawn from studies of individual clouds into a combined and updated statistical analysis of star-formation rates and efficiencies, numbers and lifetimes for spectral energy distribution (SED) classes, and clustering properties. Current star-formation efficiencies range from 3% to 6%; if star formation continues at current rates for 10 Myr, efficiencies could reach 15-30%. Star-formation rates and rates per unit area vary from cloud to cloud; taken together, the five clouds are producing about 260 M(circle dot) of stars per Myr. The star-formation surface density is more than an order of magnitude larger than would be predicted from the Kennicutt relation used in extragalactic studies, reflecting the fact that those relations apply to larger scales, where more diffuse matter is included in the gas surface density. Measured against the dense gas probed by the maps of dust continuum emission, the efficiencies are much higher, with stellar masses similar to masses of dense gas, and the current stock of dense cores would be exhausted in 1.8 Myr on average. Nonetheless, star formation is still slow compared to that expected in a free-fall time, even in the dense cores. The derived lifetime for the Class I phase is 0.54 Myr, considerably longer than some estimates. Similarly, the lifetime for the Class 0 SED class, 0.16 Myr, with the notable exception of the Ophiuchus cloud, is longer than early estimates. If photometry is corrected for estimated extinction before calculating class indicators, the lifetimes drop to 0.44 Myr for Class I and to 0.10 for Class 0. These lifetimes assume a continuous flow through the Class II phase and should be considered median lifetimes or half-lives. Star formation is highly concentrated to regions of high extinction, and the youngest objects are very strongly associated with dense cores. The great majority (90%) of young stars lie within loose clusters with at least 35 members and a stellar density of 1 M(circle dot) pc(-3). Accretion at the sound speed from an isothermal sphere over the lifetime derived for the Class I phase could build a star of about 0.25 M(circle dot), given an efficiency of 0.3. Building larger mass stars by using higher mass accretion rates could be problematic, as our data confirm and aggravate the "luminosity problem" for protostars. At a given T(bol), the values for L(bol) are mostly less than predicted by standard infall models and scatter over several orders of magnitude. These results strongly suggest that accretion is time variable, with prolonged periods of very low accretion. Based on a very simple model and this sample of sources, half the mass of a star would be accreted during only 7% of the Class I lifetime, as represented by the eight most luminous objects. C1 [Evans, Neal J., II; Dunham, Michael M.; Harvey, Paul M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Jorgensen, Jes K.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Enoch, Melissa L.; Sargent, Anneila I.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Enoch, Melissa L.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Merin, Bruno; van Dishoeck, Ewine F.; van Kempen, Tim] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Merin, Bruno] European Space Technol Ctr, European Space Agcy, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. [van Dishoeck, Ewine F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Alcala, Juan M.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Myers, Philip C.; Huard, Tracy L.; Allen, Lori E.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stapelfeldt, Karl R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Huard, Tracy L.; Mundy, Lee G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Blake, Geoffrey A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Koerner, David W.] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. [Padgett, Deborah L.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RP Evans, NJ (reprint author), Univ Texas Austin, Dept Astron, 1 Univ Stn,C1400, Austin, TX 78712 USA. EM nje@astro.as.utexas.edu; mdunham@astro.as.utexas.edu; jes@astro.uni-bonn.de; bmerin@rssd.esa.int; ewine@strw.LeidenUniv.nl; alcala@oacn.inaf.it; pmyers@cfa.harvard.edu; krs@exoplanet.jpl.nasa.gov; thuard@astro.umd.edu; leallen@cfa.harvard.edu; pmh@astro.as.utexas.edu; gab@gps.caltech.edu; david.koerner@nau.edu; lgm@astro.umd.edu; dlp@ipac.caltech.edu; afs@astro.caltech.edu RI Stapelfeldt, Karl/D-2721-2012; OI Alcala, Juan Manuel/0000-0001-8657-095X; Merin, Bruno/0000-0002-8555-3012 FU NASA [1224608, 1230779, 1288658, 1288664, 1230782, 1407, NNG04GG24G, NNX07AJ72G]; NSF [NSF PHY05-51164]; NWO Spinoza; NOVA FX We thank the referee, Charles Lada, for a very thought-provoking report, which helped us to improve the clarity of the paper. We thank the Lorentz Center in Leiden for hosting several meetings that contributed to this paper. Part of the work was done while in residence at the Kavli Institute for Theoretical Physics in Santa Barbara, California. We thank M. Krumholz for enlightening discussions and derivations of the speed of star formation in dense gas and F. Comeron for drawing our attention to biases caused by low-mass objects dropping out of the sample as they age. We are also grateful to D. Ward-Thompson for helpful suggestions. Support for this work, part of the Spitzer Legacy Science Program, was provided by NASA through contracts 1224608, 1230779, 1288658, 1288664, and 1230782 issued by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. Additional support came from NASA Origins grants NNG04GG24G and NNX07AJ72G to N.J.E. While several coauthors were at the Kavli Institute, the research was supported in part by the NSF under Grant No. NSF PHY05-51164. M. L. E. acknowledges support of an NSF Graduate Research Fellowship and a Spitzer Space Telescope Postdoctoral Fellowship. Astrochemistry in Leiden is supported by a NWO Spinoza grant and a NOVA grant. NR 179 TC 649 Z9 651 U1 3 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD APR PY 2009 VL 181 IS 2 BP 321 EP 350 DI 10.1088/0067-0049/181/2/321 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 426ZF UT WOS:000264746700001 ER PT J AU Nielsen, KE Kober, GV Weis, K Gull, TR Stahl, O Bomans, DJ AF Nielsen, K. E. Kober, G. Vieira Weis, K. Gull, T. R. Stahl, O. Bomans, D. J. TI ETA CARINAE ACROSS THE 2003.5 MINIMUM: ANALYSIS IN THE VISIBLE AND NEAR-INFRARED SPECTRAL REGION SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE circumstellar matter; line: identification; stars: individual (eta Car) ID OSCILLATOR-STRENGTHS; HOMUNCULUS-NEBULA; FE-II; STELLAR EVOLUTION; EJECTA ABSORPTION; CAR CAMPAIGN; ULTRAVIOLET; SPECTROSCOPY; EMISSION; LINES AB We present an analysis of the visible through near-infrared spectrum of Eta Carinae (eta Car) and its ejecta obtained during the "eta Car Campaign with the Ultraviolet and Visual Echelle Spectrograph (UVES) at the ESO Very Large Telescope (VLT)." This is a part of larger effort to present a complete eta Car spectrum, and extends the previously presented analyses with the Hubble Space Telescope/Space Telescope Imaging Spectrograph (HST/STIS) in the UV (1240-3159 angstrom) to 10,430 angstrom. The spectrum in the mid- and near-UV is characterized by the ejecta absorption. At longer wavelengths, stellar wind features from the central source and narrow-emission lines from the Weigelt condensations dominate the spectrum. However, narrow absorption lines from the circumstellar shells are present. This paper provides a description of the spectrum between 3060 and 10,430 angstrom, including line identifications of the ejecta absorption spectrum, the emission spectrum from the Weigelt condensations and the P Cygni stellar wind features. The high spectral resolving power of VLT/UVES enables equivalent width measurements of atomic and molecular absorption lines for elements with no transitions at the shorter wavelengths. However, the ground-based seeing and contributions of nebular-scattered radiation prevent direct comparison of measured equivalent widths in the VLT/UVES and HST/STIS spectra. Fortunately, HST/STIS and VLT/UVES have a small overlap in wavelength coverage which allows us to compare and adjust for the difference in scattered radiation entering the instruments' apertures. This paper provides a complete online VLT/UVES spectrum with line identifications and a spectral comparison between HST/STIS and VLT/UVES between 3060 and 3160 angstrom. C1 [Nielsen, K. E.; Kober, G. Vieira] Catholic Univ Amer, Washington, DC 20064 USA. [Nielsen, K. E.; Kober, G. Vieira; Gull, T. R.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Weis, K.; Bomans, D. J.] Ruhr Univ Bochum, Astron Inst, D-44780 Bochum, Germany. [Stahl, O.] Heidelberg Univ, ZAH, Landessternwarte Konigstuhl, D-69117 Heidelberg, Germany. RP Nielsen, KE (reprint author), Catholic Univ Amer, Washington, DC 20064 USA. EM krister.nielsen@nasa.gov RI Gull, Theodore/D-2753-2012 OI Gull, Theodore/0000-0002-6851-5380 NR 63 TC 8 Z9 8 U1 0 U2 1 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 APR PY 2009 VL 181 IS 2 BP 473 EP 485 DI 10.1088/0067-0049/181/2/473 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 426ZF UT WOS:000264746700012 ER PT J AU Cheung, CC Healey, SE Landt, H Kleijn, GV Jordan, A AF Cheung, C. C. Healey, Stephen E. Landt, Hermine Kleijn, Gijs Verdoes Jordan, Andres TI FIRST "WINGED" AND X-SHAPED RADIO SOURCE CANDIDATES. II. NEW REDSHIFTS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: active; galaxies: distances and redshifts; quasars: general ID BL LACERTAE OBJECTS; REVISED 3C CATALOG; ABELL CLUSTERS; BLACK-HOLE; OPTICAL SPECTROSCOPY; SURFACE PHOTOMETRY; GALAXY NGC-326; SKY SURVEY; VLA SURVEY; EMISSION AB We report optical spectroscopic observations of X-shaped radio sources with the Hobby-Eberly Telescope and Multiple-Mirror Telescope, focused on the sample of candidates from the FIRST survey presented in a previous paper. A total of 27 redshifts were successfully obtained, 21 of which are new, including a newly identified candidate source of this type which is presented here. With these observations, the sample of candidates from the previous paper is over 50% spectroscopically identified. Two new broad emission-lined X-shaped radio sources are revealed, while no emission lines were detected in about one-third of the observed sources; a detailed study of the line properties is deferred to a future paper. Finally, to explore their relation to the Fanaroff Riley division, the radio luminosities and host galaxy absolute magnitudes of a spectroscopically identified sample of 50 X-shaped radio galaxies are calculated to determine their placement in the Owen-Ledlow plane. C1 [Cheung, C. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cheung, C. C.; Healey, Stephen E.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Healey, Stephen E.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Landt, Hermine; Jordan, Andres] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kleijn, Gijs Verdoes] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Jordan, Andres] European So Observ, D-85748 Garching, Germany. RP Cheung, CC (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. EM Teddy.Cheung@nasa.gov OI Jordan, Andres/0000-0002-5389-3944 FU National Science Foundation; NASA; DOE DE-AC03-76SF00515; University of Texas at Austin; Pennsylvania State University; Stanford University; Ludwig-Maximillians-Universitat Munchen; Georg-August-Universitat Gottingen; HET; Instituto de Astronomia de la Universidad Nacional Autonoma de Mexico FX C. C. C. was supported by the National Radio Astronomy Observatory (2004-2007), which is operated by Associated Universities, Inc. under a cooperative agreement with the National Science Foundation, and currently by an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. S. E. H. is supported by the Stanford Linear Accelerator Center under DOE contract DE-AC03-76SF00515. C. C. C. is grateful to the MMT staff, particularly Mike Alegria and Grant Williams for their assistance during the observing run, and Alessondra Springmann for her assistance during a clouded out MMT run in July 2006. The MMT is a facility operated jointly by the University of Arizona and the Smithsonian Institution.; The Hobby-Eberly Telescope is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximillians-Universitat Munchen, and Georg-August-Universitat Gottingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly. The Marcario Low-Resolution Spectrograph is named for Mike Marcario of High Lonesome Optics, who fabricated several optics for the instrument but died before its completion; it is a joint project of the HET partnership and the Instituto de Astronomia de la Universidad Nacional Autonoma de Mexico. This paper includes data taken with the Harlan J. Smith Telescope at the McDonald Observatory of the University of Texas at Austin.; This research has made use of NASA's Astrophysics Data System Abstract Service and the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 48 TC 12 Z9 12 U1 0 U2 1 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 APR PY 2009 VL 181 IS 2 BP 548 EP 556 DI 10.1088/0067-0049/181/2/548 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 426ZF UT WOS:000264746700016 ER PT J AU Brassington, NJ Fabbiano, G Kim, DW Zezas, A Zepf, S Kundu, A Angelini, L Davies, RL Gallagher, J Kalogera, V Fragos, T King, AR Pellegrini, S Trinchieri, G AF Brassington, N. J. Fabbiano, G. Kim, D. -W. Zezas, A. Zepf, S. Kundu, A. Angelini, L. Davies, R. L. Gallagher, J. Kalogera, V. Fragos, T. King, A. R. Pellegrini, S. Trinchieri, G. TI DEEP CHANDRA MONITORING OBSERVATIONS OF NGC 4278: CATALOG OF SOURCE PROPERTIES SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: individual (NGC 4278); X-rays: binaries; X-rays: galaxies ID X-RAY BINARIES; GLOBULAR-CLUSTER SYSTEMS; MULTIWAVELENGTH PROJECT; ELLIPTIC GALAXIES; LUMINOSITY FUNCTION; SOURCE POPULATION; NEARBY GALAXIES; POINT SOURCES; CENTAURUS-A; DISTANCES AB We present the properties of the discrete X-ray sources detected in our monitoring program of the globular cluster ( GC) rich elliptical galaxy, NGC 4278, observed with Chandra ACIS-S in six separate pointings, resulting in a co-added exposure of 458 ks. From this deep observation, 236 sources have been detected within the region overlapped by all observations, 180 of which lie within the D(25) ellipse of the galaxy. These 236 sources range in L(X) from 3.5 x 10(36) erg s(-1) ( with 3 sigma upper limit <= 1 x 10(37) erg s(-1)) to similar to 2 x 10(40) erg s(-1), including the central nuclear source which has been classified as a LINER. From optical data, 39 X-ray sources have been determined to be coincident with a GC, these sources tend to have high X-ray luminosity, with 10 of these sources exhibiting L(X) > 1 x 10(38) erg s(-1). From X-ray source photometry, it has been determined that the majority of the 236 point sources that have well-constrained colors have values that are consistent with typical low-mass X-ray binary spectra, with 29 of these sources expected to be background objects from the log N - log S relation. There are 103 sources in this population that exhibit long-term variability, indicating that they are accreting compact objects. Three of these sources have been identified as transient candidates, with a further three possible transients. Spectral variations have also been identified in the majority of the source population, where a diverse range of variability has been identified, indicating that there are many different source classes located within this galaxy. C1 [Brassington, N. J.; Fabbiano, G.; Kim, D. -W.; Zezas, A.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zepf, S.; Kundu, A.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Angelini, L.] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA. [Davies, R. L.] Univ Oxford, Sub Dept Astrophys, Oxford OX1 3RH, England. [Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Kalogera, V.; Fragos, T.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [King, A. R.] Univ Leicester, Theoret Astrophys Grp, Leicester LE1 7RH, Leics, England. [Pellegrini, S.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Trinchieri, G.] Osserv Astron Brera, INAF, I-20121 Milan, Italy. RP Brassington, NJ (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM nbrassington@head.cfa.harvard.edu RI Zezas, Andreas/C-7543-2011; Fragos, Tassos/A-3581-2016 OI Zezas, Andreas/0000-0001-8952-676X; Trinchieri, Ginevra/0000-0002-0227-502X; Fragos, Tassos/0000-0003-1474-1523 FU Chandra G0 [G06-7079A, G06-7079B]; NASA [NAS8-3907, NAG5-13056]; Italian Space Agency ASI (Agenzia Spaziale Italiana) [ASI-INAF I/023/05/0] FX We thank the CXC DS and SDS teams for their efforts in reducing the data and developing the software used for the reduction (SDP) and analysis (CIAO). We also thank the referee, Jimmy Irwin, for his helpful comments which have improved this paper. This work was supported by Chandra G0 grant G06-7079A (PI: Fabbiano) and subcontract G06-7079B (PI: Kalogera). We acknowledge partial support from NASA contract NAS8-39073 (CXC). A. Zezas acknowledges support from NASA LTSA grant NAG5-13056. S. Pellegrini acknowledges partial financial support from the Italian Space Agency ASI (Agenzia Spaziale Italiana) through grant ASI-INAF I/023/05/0. NR 40 TC 29 Z9 29 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD APR PY 2009 VL 181 IS 2 BP 605 EP 626 DI 10.1088/0067-0049/181/2/605 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 426ZF UT WOS:000264746700019 ER PT J AU Bufano, F Immler, S AF Bufano, Filomena Immler, Stefan TI Ultraviolet SN observations with Swift SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Conference on Network for Ultra Violet Astronomy CY JUN, 2007 CL Madrid, SPAIN DE Supernovae; Ultraviolet: general ID I SUPERNOVAE; TELESCOPE; MODELS; 2006JC; STAR AB Ultraviolet (UV) data are powerful tools to understand supernovae (SNe). Currently, the Swift satellite is the best suited telescope available for SN UV studies, due to its photometric and spectroscopic capabilities and its fast response. We present recent results obtained with the Swift SN program, demonstrating the importance of the UV emission, which provides fundamental information about SN explosion mechanism, its environment and progenitor structure. C1 [Bufano, Filomena] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Bufano, Filomena] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Bufano, Filomena; Immler, Stefan] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Swift Supernova Team, Greenbelt, MD 20771 USA. RP Bufano, F (reprint author), Univ Padua, Dipartimento Astron, Vicolo Osservatorio 2, I-35122 Padua, Italy. EM filomena.bufano@oapd.inaf.it NR 21 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD APR PY 2009 VL 320 IS 1-3 BP 173 EP 176 DI 10.1007/s10509-008-9791-x PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 418UK UT WOS:000264174700028 ER PT J AU Roming, PWA Gronwall, C Berk, DEV Page, MJ Boyd, PT AF Roming, P. W. A. Gronwall, C. Berk, D. E. Vanden Page, M. J. Boyd, P. T. TI The Swift Ultra-Violet/Optical Telescope: a view of today and tomorrow SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Conference on Network for Ultra Violet Astronomy CY JUN, 2007 CL Madrid, SPAIN DE Space vehicles: instruments; Ultraviolet: general; Gamma rays: bursts ID EARLY OPTICAL AFTERGLOWS; X-RAY; ULTRAVIOLET VARIABILITY; UVOT OBSERVATIONS; MISSION; SUPERNOVA; EVOLUTION; GALAXIES; REGIONS; BURSTS AB Currently there are four operating near-UV imaging space telescopes, one of which is the Swift Ultra-Violet/Optical Telescope (UVOT). Although the UVOT was primarily built for observations of gamma-ray bursts, it has become a powerful instrument for studying other types of UV and optical astronomical phenomena. Here we discuss the properties of the UVOT, summarize some of the science undertaken with the UVOT, and present other possible science goals for the UVOT that have not yet been pursued. We also discuss some lessons learned that apply to future UV telescopes. C1 [Roming, P. W. A.; Gronwall, C.; Berk, D. E. Vanden] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Page, M. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Boyd, P. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Roming, PWA (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. EM roming@astro.psu.edu RI Boyd, Patricia/D-3274-2012 NR 33 TC 3 Z9 3 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD APR PY 2009 VL 320 IS 1-3 BP 203 EP 206 DI 10.1007/s10509-008-9813-8 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 418UK UT WOS:000264174700034 ER PT J AU Carpenter, KG Schrijver, CJ Karovska, M AF Carpenter, Kenneth G. Schrijver, Carolus J. Karovska, Margarita TI The Stellar Imager (SI) project: a deep space UV/Optical Interferometer (UVOI) to observe the Universe at 0.1 milli-arcsec angular resolution SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Conference on Network for Ultra Violet Astronomy CY JUN, 2007 CL Madrid, SPAIN DE Observatories: space; Interferometry: space; Stars: surface features; Stars: interiors; Galaxies: AGN; Planets: Exo-Solar AB The Stellar Imager (SI) is a space-based, UV/Optical Interferometer (UVOI) designed to enable 0.1 milli-arcsecond (mas) spectral imaging of stellar surfaces and of the Universe in general. It will also probe via asteroseismology flows and structures in stellar interiors. SI's science focuses on the role of magnetism in the Universe and will revolutionize our understanding of the formation of planetary systems, of the habitability and climatology of distant planets, and of many magneto-hydrodynamically controlled processes, such as accretion, in the Universe. The ultra-sharp images of SI will revolutionize our view of many dynamic astrophysical processes by transforming point sources into extended sources, and snapshots into evolving views. SI is a "Flagship and Landmark Discovery Mission" in the 2005 Heliophysics Roadmap and a potential implementation of the UVOI in the 2006 Science Program for NASA's Astronomy and Physics Division. We present here the science goals of the SI Mission, a mission architecture that could meet those goals, and the technology development needed to en-able this mission. Additional information on SI can be found at: http://hires.gsfc.nasa.gov/si/. C1 [Carpenter, Kenneth G.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Schrijver, Carolus J.] Lockheed Martin Adv Technol Ctr, Palo Alto, CA 94304 USA. [Karovska, Margarita] SAO, Cambridge, MA 02138 USA. RP Carpenter, KG (reprint author), NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 20771 USA. EM Kenneth.G.Carpenter@nasa.gov RI Carpenter, Kenneth/D-4740-2012 NR 8 TC 11 Z9 11 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD APR PY 2009 VL 320 IS 1-3 BP 217 EP 223 DI 10.1007/s10509-008-9815-6 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 418UK UT WOS:000264174700036 ER PT J AU Yorks, JE Thompson, AM Joseph, E Miller, SK AF Yorks, John E. Thompson, Anne M. Joseph, Everette Miller, Sonya K. TI The variability of free tropospheric ozone over Beltsville, Maryland (39N, 77W) in the summers 2004-2007 SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Ozone; Ozonesonde; Vertical profile; Air quality model; Boundary layer pollution ID UNITED-STATES; EVOLUTION; MODEL AB Ozone profiles are often used to investigate day-to-day and year-to-year variability in origins of free tropospheric ozone. With this in mind, more than 50 ozonesonde launches were conducted in Beltsville, MD, during the summers of 2004 through 2007. Budgets of free tropospheric ozone were calculated for each ozone profile in the four summers using a laminar identification (LID) method and unusual episodes were analyzed with respect to meteorological variables. The laminar method showed that stratosphere-to-troposphere transport (ST) accounted for greater than 50% of the free tropospheric ozone column on 17% of days sampled, a more pronounced influence than regional convective and lightning (RCL) sources. The ST origins were confirmed with trajectories, and tracers (water vapor and potential vorticity). The amount of free tropospheric ozone from ST and RCL Sources varied from year-to-year (up to 13%) and can be explained by differences in mean meteorological patterns. On average, almost 30% of the free tropospheric Column was attributed to ST influence, about twice as much as RCL, although the LID method may not capture weeks-old lightning influences as in a chemical model. The prevalence of ST ozone in summertime Beltsville soundings was similar to six sounding sites in the IONS-04 campaign [Thompson, A.M., et al.. 2007b. Intercontinental Transport Experiment Ozonesonde Network Study (IONS, 2004): 1. Summertime upper tropospheric/lower stratosphere ozone over northeastern North America. J. Geophys. Res. 112, D12S12; Thompson, A.M., et al., 2007c. Intercontinental Transport Experiment Ozonesonde Network Study (IONS, 2004): 2. Tropospheric ozone budgets and variability over northeastern North America. J. Geophys. Res. 112, D12S13.] and to statistics from a 30 year climatology of European soundings [Collette, A., Ancellet, G., 2005. Impact of vertical transport processes on the tropospheric ozone layering above Europe. Part II: Climatological analysis of the past 30 years. Atmos. Environ. 39, 5423-5435]. The Beltsville record also demonstrated the value of soundings for air quality forecasting in an urban area. The 22 nighttime soundings collected over Beltsville in 2004-2007 can be divided into distinct Polluted and unpolluted Subsets, the former 20 ppbv higher in residual layer ozone (I km) than the latter. These distinctions propagated to daytime differences of 10 ppbv at the surface in the Washington, DC, area, with the high-ozone residual layers leading to non-attainment of the National Ambient Air Quality Standard for ozone. More frequent ozone observations aloft appear essential for better understanding ozone variability and for enabling air quality modelers to achieve more accurate ozone forecasts. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Yorks, John E.; Thompson, Anne M.; Miller, Sonya K.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. [Joseph, Everette] Howard Univ, Dept Phys & Astron, Washington, DC 20059 USA. RP Yorks, JE (reprint author), Sci Syst & Applicat Inc, NASA, Goddard Space Flight Ctr, Code 613-1, Greenbelt, MD USA. EM John.E.Yorks@nasa.gov; anne@meteo.psu.edu; ejosgm@gmail.com; smiller@meteo.psu.edu RI Thompson, Anne /C-3649-2014 OI Thompson, Anne /0000-0002-7829-0920 FU NASA; IONS; NCAS through NOAA's Educational Partnership Program Cooperative [NA17AF.1623]; Maryland Department of the Environment (MDE); Goddard Space Flight Center Directors Discretionary Fund; NASA's WAVES; MDE FX The Upper Atmosphere Research Program of NASA, NASA's Tropospheric Chemistry Program and Aura Validation funded this study and IONS (M. J. Kurylo, K. W. jucks, B. G. Doddridge, J. [I. Crawford). The Beltsville site and the Soundings are supported by NCAS through NOAA's Educational Partnership Program Cooperative Agreement No. NA17AF.1623 and Maryland Department of the Environment (MDE). The 2004 Soundings were funded from the Goddard Space Flight Center Directors Discretionary Fund; supplies in 2006 and 2007 were funded through NASA's WAVES (Water Vapor Validation Experiment for Satellites and Soundings), and MDE. Thanks to D. N. Whiteman (NASA/GSFC), W. F. Ryan (PSU), B.F. TaUbman (Appalachian State), W. R. Stockwell (Howard/NCAS) and numerous Students W110 Supported ozonesonde operations at Beltsville. NR 37 TC 20 Z9 22 U1 0 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 J9 ATMOS ENVIRON JI Atmos. Environ. PD APR PY 2009 VL 43 IS 11 BP 1827 EP 1838 DI 10.1016/j.atmosenv.2008.12.049 PG 12 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 421HF UT WOS:000264349300001 ER PT J AU Han, QY Brenguier, JL Kuo, KS Naeger, A AF Han, Qingyuan Brenguier, Jean-Louis Kuo, Kuo-Sen Naeger, Aaron TI A new IR technique for monitoring low cloud properties using geostationary satellite data SO ATMOSPHERIC SCIENCE LETTERS LA English DT Article DE low cloud; infrared; SEVIRI ID SYSTEM AB A new technique of using satellite infrared radiance data for retrieving cloud properties is developed and applied to SEVIRI data, which is based on direct radiative transfer calculations, not on the emissivity approximation as used by other satellite IR only techniques. Instantaneous atmospheric profiles are used in the new technique for improving the accuracy of retrievals. Comparison of the retrieved results with coincident observations of CloudSat and CALIPSO shows excellent agreement for low clouds. This study shows that, using only IR radiances, the single layer assumption would significantly underestimate cloud optical depth when multilayered cloud system is presented. Copyright (C) 2009 Royal Meteorological Society C1 [Han, Qingyuan; Naeger, Aaron] Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35899 USA. [Brenguier, Jean-Louis] GMEI, CNRM GAME, Toulouse, France. [Kuo, Kuo-Sen] Caelum Res Corp, Greenbelt, MD USA. [Kuo, Kuo-Sen] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Han, QY (reprint author), Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35899 USA. EM han@nsstc.uah.edu FU Atmospheric Radiation Measurement Program; Office of Science; U.S. Department of Energy [DE-FG02-08ER64669] FX We thank two anonymous reviewers for their very helpful comments and suggestions. A. Naeger is supported by the Atmospheric Radiation Measurement Program, Office of Science, U.S. Department of Energy, Grant No. DE-FG02-08ER64669. K. S. Kuo is supported by NASA TC4 program for this study. Thanks for the support of Meteo-France during Q. Han's sabbatical when the work was started. The SEVIRI data were kindly supplied by Marcel Derrien. NCEP reanalysis data provided by the NOAA/OAR/ESRL PSD, from URL http://www.cdc.noaa.gov are acknowledged. NR 13 TC 2 Z9 2 U1 1 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1530-261X J9 ATMOS SCI LETT JI Atmos. Sci. Lett. PD APR PY 2009 VL 10 IS 2 BP 115 EP 121 DI 10.1002/asl.218 PG 7 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 460QK UT WOS:000267202000008 ER PT J AU Berry, CA Hoffler, GW Jernigan, CA Kerwin, JP Mohler, SR AF Berry, Charles A. Hoffler, G. Wyckliffe Jernigan, Clarence A. Kerwin, Joseph P. Mohler, Stanley R. TI History of Space Medicine: The Formative Years at NASA SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE spaceflight; history AB Almost nothing was known about the effects of spaceflight on human physiology when, in May of 1961, President John F. Kennedy committed the United States to land a man on the Moon and return him safely to Earth within the decade. There were more questions than answers regarding the effects of acceleration, vibration, cabin pressure, CO(2) Concentration, and microgravity. There were known external threats to life, Such as solar and ultraviolet radiation, meteorites, and extreme temperatures as well as issues for which the physicians and scientists could not even formulate the questions. And there was no time for controlled experiments with the required numbers of animal or human subjects. Of necessity, risks were evaluated and mitigated or accepted based on minimal data. This article Summarizes presentations originally giver) as a panel at the 79(th) Annual Scientific Meeting of the Aerospace Medical Association in Boston in 2008. In it, five pioneers in space medicine at NASA looked back on the development of their field. The authors related personal anecdotes, discussed the roles of various people and presented examples of contributions to emerging U.S. initiatives for human spaceflight. Topics included the development of quarantine facilities for returning Apollo astronauts, the struggles between operational medicine and research personnel, and observations from the first U.S. medical officer to experience weightlessness on orbit. Brief biographies of the authors are appended to document their participation in these historic events. C1 [Berry, Charles A.] UTMB, Galveston, TX USA. [Berry, Charles A.; Kerwin, Joseph P.] Lyndon B Johnson Space Ctr, Houston, TX USA. [Berry, Charles A.] NASA Headquarters, Washington, DC USA. [Hoffler, G. Wyckliffe] Virginia Commonwealth Univ Med Coll Virginia, Richmond, VA USA. [Hoffler, G. Wyckliffe] Med Coll Georgia, Augusta, GA 30912 USA. [Hoffler, G. Wyckliffe] Ohio State Univ, Columbus, OH 43210 USA. [Hoffler, G. Wyckliffe; Jernigan, Clarence A.] NASA, Manned Spacecraft Ctr, Washington, DC USA. [Jernigan, Clarence A.] Galveston Cty Community Hlth Serv, Galveston Cty, TX USA. [Mohler, Stanley R.] NIH, Ctr Aging Res, Bethesda, MD 20892 USA. [Mohler, Stanley R.] FAA Headquarters, Civil Aviat Med Res Inst, Washington, DC USA. [Mohler, Stanley R.] FAA Headquarters, Aeromed Applicat Div, Washington, DC USA. [Mohler, Stanley R.] Wright State Univ, Aerosp Med Residency Program, Dayton, OH 45435 USA. FU Space Medicine Association FX This panel was sponsored by the Space Medicine Association, a constituent organization of the AsMA. This summary was edited by E. A. Bopp. The Space Medicine Association intends this to be the first of an annual series of panels on Space Medicine History. NR 0 TC 3 Z9 4 U1 1 U2 7 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 APR PY 2009 VL 80 IS 4 BP 345 EP 352 DI 10.3357/ASEM.2463.2009 PG 8 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 427LL UT WOS:000264780700001 PM 19378903 ER PT J AU Kamine, TH Bendrick, GA AF Kamine, Tovy Haber Bendrick, Gregg A. TI Visual Display Angles of Conventional and a Remotely Piloted Aircraft SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE remotely piloted aircraft; display separation; human factors; instrument panel; information access cost; uninhabited aerial vehicle ID OPERATIONS AB Introduction: Instrument display separation and proximity are important human factor elements used in the design and grouping of aircraft instrument displays. To assess display proximity in practical operations, the viewing visual angles of various displays in several conventional aircraft and in a remotely piloted vehicle were assessed. Methods: The horizontal and vertical instrument display visual angles from the pilot's eye position were measured in 12 different types of conventional aircraft, and in the ground control station (GCS) of a remotely piloted air craft (RPA). A total of 18 categories of instrument display were measured and compared. Results: In conventional aircraft almost all of the vertical and horizontal visual display angles lay within a "cone of easy eye movement" (CEEM). Mission-critical instruments particular to specific aircraft types sometimes displaced less important instruments outside the CEEM. For the RPA, all horizontal visual angles lay within the CEEM, but most vertical visual angles lay Outside this cone. Discussion: Most instrument displays in conventional aircraft were consistent with display proximity principles, but several RPA displays lay outside the CEEM in the vertical plane. Awareness of this fact by RPA operators may be helpful in minimizing information access cost, and in optimizing RPA operations. C1 Univ Penn, Sch Med, Philadelphia, PA 19104 USA. NASA, Dryden Flight Res Ctr, Edwards AFB, CA USA. RP Kamine, TH (reprint author), 523 W 6th St,Ste 546, Los Angeles, CA 90014 USA. EM tovy.kamine@gmail.com NR 19 TC 0 Z9 0 U1 1 U2 4 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD APR PY 2009 VL 80 IS 4 BP 409 EP 413 DI 10.3357/ASEM.2337.2009 PG 5 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 427LL UT WOS:000264780700013 PM 19378915 ER PT J AU Tao, WK Chern, JD Atlas, R Randall, D Khairoutdinov, M Li, JL Waliser, DE Hou, A Lin, X Peters-Lidard, C Lau, W Jiang, J Simpson, J AF Tao, Wei-Kuo Chern, Jiun-Dar Atlas, Robert Randall, David Khairoutdinov, Marat Li, Jui-Lin Waliser, Duane E. Hou, Arthur Lin, Xin Peters-Lidard, Christa Lau, William Jiang, Jonathan Simpson, Joanne TI A MULTISCALE MODELING SYSTEM Developments, Applications, and Critical Issues SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID CLOUD-RESOLVING MODEL; CONVECTION PARAMETERIZATION CRCP; COMMUNITY CLIMATE MODEL; MEASURING MISSION TRMM; DIURNAL CYCLE; SINGLE-COLUMN; NUMERICAL-SIMULATION; MESOSCALE PROCESSES; MOMENTUM TRANSPORT; HYDROLOGIC-CYCLE AB A multiscale modeling framework (MMF), which replaces the conventional cloud parameterizations with a cloud-resolving model (CRM) in each grid column of a GCM, constitutes a new and promising approach for climate modeling. The MMF can provide for global coverage and two-way interactions between the CRMs and their parent GCM. The CRM allows for explicit simulation of cloud processes and their interactions with radiation and surface processes, and the GCM allows for global coverage. A new MMF has been developed that is based on the NASA Goddard Space Flight Center (GSFC) finite-volume GCM (fvGCM) and the Goddard Cumulus Ensemble (GCE) model. This Goddard MMF produces many features that are similar to another MMF that was developed at Colorado State University (CSU), such as an improved surface precipitation pattern, better cloudiness, improved diurnal variability over both oceans and continents, and a stronger propagating Madden-Julian oscillation (MJO) compared to their parent GCMs using traditional cloud parameterizations. Both MMFs also produce a large and positive precipitation bias in the Indian Ocean and western Pacific during the Northern Hemisphere summer. However, there are also notable differences between the two MMFs. For example, the CSU MMF simulates less rainfall over land than its parent GCM. This is why the CSU MMF simulated less overall global rainfall than its parent GCM. The Goddard MMF simulates more global rainfall than its parent GCM because of the high contribution from the oceanic component. A number of critical issues (i.e., the CRM's physical processes and its configuration) involving the Goddard MMF are discussed in this paper. C1 [Tao, Wei-Kuo; Chern, Jiun-Dar; Lau, William; Simpson, Joanne] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Chern, Jiun-Dar; Lin, Xin] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Atlas, Robert] NOAA Atlantic Oceanog & Meteorol Lab, Miami, FL USA. [Khairoutdinov, Marat] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Li, Jui-Lin; Waliser, Duane E.; Jiang, Jonathan] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Hou, Arthur; Lin, Xin] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Peters-Lidard, Christa] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. RP Tao, WK (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 613-1, Greenbelt, MD 20771 USA. EM Wei-Kuo.Tao-I@nasa.gov RI Atlas, Robert/A-5963-2011; Randall, David/E-6113-2011; Hou, Arthur/D-8578-2012; Peters-Lidard, Christa/E-1429-2012; Lau, William /E-1510-2012 OI Atlas, Robert/0000-0002-0706-3560; Randall, David/0000-0001-6935-4112; Peters-Lidard, Christa/0000-0003-1255-2876; Lau, William /0000-0002-3587-3691 NR 84 TC 65 Z9 65 U1 0 U2 16 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 EI 1520-0477 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD APR PY 2009 VL 90 IS 4 BP 515 EP + DI 10.1175/2008BAMS2542.1 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 445FI UT WOS:000266035100010 ER PT J AU Nelson, R Boudreau, J Gregoire, TG Margolis, H Naesset, E Gobakken, T Stahl, G AF Nelson, Ross Boudreau, Jonathan Gregoire, Timothy G. Margolis, Hank Naesset, Erik Gobakken, Terje Stahl, Goran TI Estimating Quebec provincial forest resources using ICESat/GLAS SO CANADIAN JOURNAL OF FOREST RESEARCH-REVUE CANADIENNE DE RECHERCHE FORESTIERE LA English DT Article ID BRAZILIAN AMAZON; CARBON SINK; BIOMASS; LASER; AIRBORNE; DEFORESTATION; INVENTORY; REGROWTH AB Ground plots, airborne profiling and space lidar (light detection and ranging) measurements of canopy height and crown closure, space radar topographic data, a Landsat cover type map, and a vegetation zone map were used in a model-assisted, two-phase sampling design to estimate the aboveground biomass and carbon resources of Quebec. It was determined that a simple random sampling estimator, with covariance terms added, could be used to quantify the variability of regional Geoscience Laser Altimeter System (GLAS) biomass estimates where interorbit distances are, on average, 15 km apart. Prediction error increased standard errors, on average, 24.4%, 4.6%, and 2.8% at the cover type, vegetation zone, and provincial levels, respectively. Inclusion of the covariance term in the calculation of grouped cover type variances increased the vegetation zone standard errors up to 3.7 times and the provincial standard errors 15.6 times. In the southern commercial forests of Quebec, GLAS underestimated ground-based biomass values by 7.3% (stratified linear model) and 10.2% (nonstratified linear model). Quebec forests support 2.57 +/- 0.33 gigatonnes of carbon (nonstratified linear model). Approximately 25% of that carbon was found to be located in two southern vegetation zones (northern hardwood and mixedwood), another 25% in two northern vegetation zones (taiga and treed tundra), and the remaining 50% in the boreal zone. C1 [Nelson, Ross] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. [Boudreau, Jonathan] Univ Laval, CEF, Dept Sci Bois & Foret, Quebec City, PQ G1K 7P4, Canada. [Gregoire, Timothy G.] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA. [Margolis, Hank] Univ Laval, Fac Foresterie & Geomat, CEF, Ste Foy, PQ G1K 7P4, Canada. [Naesset, Erik; Gobakken, Terje] Norwegian Univ Life Sci, Dept Ecol & Nat Resource Management, NO-1432 As, Norway. [Stahl, Goran] Swedish Univ Agr Sci, Dept Forest Resource Management & Geomat, S-90183 Umea, Sweden. RP Nelson, R (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Code 614-4, Greenbelt, MD 20771 USA. EM Ross.F.Nelson@nasa.gov NR 38 TC 35 Z9 37 U1 1 U2 12 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 1200 MONTREAL ROAD, BUILDING M-55, OTTAWA, ON K1A 0R6, CANADA SN 0045-5067 EI 1208-6037 J9 CAN J FOREST RES JI Can. J. For. Res.-Rev. Can. Rech. For. PD APR PY 2009 VL 39 IS 4 BP 862 EP 881 DI 10.1139/X09-002 PG 20 WC Forestry SC Forestry GA 468IJ UT WOS:000267810400016 ER PT J AU Middleton, EM Cheng, YB Hilker, T Black, TA Krishnan, P Coops, NC Huemmrich, KF AF Middleton, Elizabeth M. Cheng, Yen-Ben Hilker, Thomas Black, T. Andrew Krishnan, Praveena Coops, Nicholas C. Huemmrich, Karl Fred TI Linking foliage spectral responses to canopy-level ecosystem photosynthetic light-use efficiency at a Douglas-fir forest in Canada SO CANADIAN JOURNAL OF REMOTE SENSING LA English DT Review ID PHOTOCHEMICAL REFLECTANCE INDEX; RADIATION-USE-EFFICIENCY; GROSS PRIMARY PRODUCTION; BOREAL ASPEN FOREST; THERMAL-ENERGY DISSIPATION; EDDY COVARIANCE TECHNIQUE; NET PRIMARY PRODUCTION; CARBON-DIOXIDE FLUXES; LEAF-AREA INDEX; CHLOROPHYLL FLUORESCENCE AB The light-use efficiency (LUE) of a mature Canadian Douglas-fir forest (DF49) was studied using high-resolution in situ temporal, spatial, and spectral measurements in conjunction with fluxes acquired from an instrumented tower. We examined the photochemical reflectance index (PRI), a spectral index responsive to high light conditions that alters reflectance at 531 nm, in combination with several alternative reference bands at 551, 570, and 488 nm. These indices were derived from directional reflectance spectra acquired by a hyperspectral radiometer system mounted on the DF49 tower, viewing the canopy through almost 360 rotations multiple times an hour daily throughout the 2006 growing season. From canopy structure information, three foliage sectors within the canopy were delineated according to instantaneous illumination conditions (sunlit, shaded, and mixed shaded-sunlit). On sunny days, the PRI indices for the sunlit foliage sector captured high light-induced stress responses, expressed as significantly different PRI values for sunlit versus shaded foliage. This difference was not observed on highly diffuse or overcast days. PRIs on sunny days tracked the diurnal photoregulation responses throughout the growing season in concert with illumination intensity. We computed the effective instantaneous LUE for the three foliage groups (LUEfoliage) using modeled and measured information. We provide convincing evidence that LUEfoliage can be well described and strongly related to all variations of the PRI within this coniferous forest under relatively clear skies (0.59 > r(2) > 0.80, P < 0.0001). LUEfoliage varied through the growing season between 0.015 and 0.075 mu mol C mu mol(-1) absorbed photosynthetically active radiation (APAR), and the lowest daily values were associated with the sunlit foliage group. The mixed sunlit-shaded foliage was the only group to exhibit monthly averages close to the maximum ecosystem LUE parameter (epsilon(max)) used in LUE models for evergreen needle forests (0.0196 mu mol C mu mol(-1) APAR). Implications for remote sensing of carbon uptake dynamics and the interaction of canopy structure and physiology are discussed. C1 [Middleton, Elizabeth M.; Cheng, Yen-Ben] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. [Hilker, Thomas; Coops, Nicholas C.] Univ British Columbia, Fac Forest Resources Management, Vancouver, BC V6T 1Z4, Canada. [Black, T. Andrew; Krishnan, Praveena] Univ British Columbia, Fac Land & Food Syst, Vancouver, BC V6T 1Z4, Canada. [Krishnan, Praveena] Natl Ocean & Atmospher Adm, Atmospher Turbulence & Diffus Div, Oak Ridge, TN 37830 USA. [Huemmrich, Karl Fred] Univ Maryland, Joint Ctr Earth Syst Technol, Catonsville, MD 21228 USA. RP Middleton, EM (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. EM Elizabeth.M.Middleton@nasa.gov RI Krishnan, Praveena/F-8169-2010; Cheng, Yen-Ben/G-1311-2012; Coops, Nicholas/J-1543-2012 OI Coops, Nicholas/0000-0002-0151-9037 FU National Aeronautics and Space Administration (NASA); German Academic Exchange Service (DAAD); Natural Sciences and Engineering Research Council of Canada (NSERC) FX This research was supported by National Aeronautics and Space Administration (NASA) Research Opportunities in Space and Earth Sciences (ROSES) funding through the Carbon Cycle Science Program (Diane Wickland, Manager). Yen-Ben Cheng was supported through the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities. Thomas Hilker was partially funded by a postgraduate scholarship of the German Academic Exchange Service (DAAD), a Natural Sciences and Engineering Research Council of Canada (NSERC) Discovery Grant to Nicholas Coops, and funds provided to the University of British Columbia (UBC) from the Comprehensive Community Plan (CCP), NSERC, and BIOCAP. We acknowledge the following people for their assistance in technical design, installation, and maintenance of the radiometer platform: Zoran Nesic, Dominic Lessard, Rick Ketler, and Andrew Sauter from UBC Faculty of Land and Food Systems (LFS). NR 116 TC 47 Z9 47 U1 1 U2 22 PU CANADIAN AERONAUTICS SPACE INST PI KANATA PA 350 TERRY FOX DR, STE 104, KANATA, ON K2K 2W5, CANADA SN 1712-7971 J9 CAN J REMOTE SENS JI Can. J. Remote Sens. PD APR PY 2009 VL 35 IS 2 BP 166 EP 188 PG 23 WC Remote Sensing SC Remote Sensing GA 455BC UT WOS:000266729300007 ER PT J AU Pitjeva, EV Standish, EM AF Pitjeva, E. V. Standish, E. M. TI Proposals for the masses of the three largest asteroids, the Moon-Earth mass ratio and the Astronomical Unit SO CELESTIAL MECHANICS & DYNAMICAL ASTRONOMY LA English DT Article DE Ceres mass; DE ephemerides; EPM ephemerides; Pallas mass; Vesta mass; Moon-Earth mass ratio; Astronomical Unit ID 1 CERES; 4 VESTA; EPHEMERIS; PERTURBATIONS; PALLAS; MARS AB We propose to the NSFA (the IAU Working Group on Numerical Standards for Fundamental Astronomy) the following representative values and realistic uncertainties for the masses of the three largest asteroids (Ceres, Pallas, Vesta), to be used as the current best estimates: M(Cres)/M(circle dot) = 4.72 . 10(-10), M(Pallas)/M(circle dot) = 1.03 . 10(-10), M(Vesta)/M(circle dot) = 1.35 . 10(-10). Unlike the values previously adopted in the Astronomical Almanac, these are consistent with nearly all of the twenty or so modern accurate determinations from various authors. We also have proposed the following values for the Moon-Earth mass ratio and the astronomical unit in meters obtained from the ephemeris improvement processes at JPL in Pasadena and at IAA RAS in St.Petersburg: M(Moon)/M(Earth) = 0.0123000371(4) and AU = 149597870700(3) m. The numerical value of the AU in meters is identical in both the TDB-based and the TCB-based systems of units if one uses the conversion proposed by Irwin and Fukushima, Brumberg and Groten, Brumberg and Simon. C1 [Pitjeva, E. V.] Russian Acad Sci, Inst Appl Astron, St Petersburg 191187, Russia. [Standish, E. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Pitjeva, EV (reprint author), Russian Acad Sci, Inst Appl Astron, Kutuzov Quay 10, St Petersburg 191187, Russia. EM evp@ipa.nw.ru; ems@jpl.nasa.gov FU Institute of Applied Astronomy of Russian Academy of Sciences; Jet Propulsion Laboratory, California Institute of Technology FX The work described in this paper was carried out at the Institute of Applied Astronomy of Russian Academy of Sciences and at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 35 TC 32 Z9 35 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0923-2958 J9 CELEST MECH DYN ASTR JI Celest. Mech. Dyn. Astron. PD APR PY 2009 VL 103 IS 4 BP 365 EP 372 DI 10.1007/s10569-009-9203-8 PG 8 WC Astronomy & Astrophysics; Mathematics, Interdisciplinary Applications SC Astronomy & Astrophysics; Mathematics GA 431BP UT WOS:000265036600005 ER PT J AU Pavlick, MM Johnson, WS Jensen, B Weiser, E AF Pavlick, M. M. Johnson, W. S. Jensen, Brian Weiser, Erik TI Evaluation of mechanical properties of advanced polymers for composite cryotank applications SO COMPOSITES PART A-APPLIED SCIENCE AND MANUFACTURING LA English DT Article DE Polymers; Fracture toughness; Strength; Mechanical testing AB Composite materials are actively being used in the aerospace industry as a means of reducing weight. In particular, polymer matrix composites (PMC) are good candidates due to their high strength-to-weight and stiffness-to-weight ratios. A fundamental step to understand how a PMC will behave in a cryotank's extreme environmental is to first understand how the constituents (namely, the polymer matrix) behave in that same environment. Therefore, both stress-based and fracture-based experiments were conducted to evaluate four candidate polymers supplied by NASA Langley Research Center. Each type of test was conducted at approximately -196 degrees C (-320 degrees F), 24 degrees C (76 degrees F), and 160 degrees C (320 degrees F). Based on the results of the four polymer systems, a recommendation as to the best candidate for polymer matrix and adhesive bonding for Reusable Launch Vehicle's (RLV's) composite cryotanks is made. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Johnson, W. S.] Georgia Inst Technol, Sch Mat Sci & Engn, Atlanta, GA 30332 USA. [Pavlick, M. M.; Johnson, W. S.] Georgia Inst Technol, George W Woodruff Sch Mech Engn, Atlanta, GA 30332 USA. [Jensen, Brian; Weiser, Erik] NASA LaRC, Adv Mat & Proc Branch, Hampton, VA 23662 USA. RP Johnson, WS (reprint author), Georgia Inst Technol, Sch Mat Sci & Engn, Atlanta, GA 30332 USA. EM steve.johnson@mse.gatech.edu FU NASA Langley Research Center in Hampton, VA under NASA [NAG-1-02003] FX This research was sponsored by NASA Langley Research Center in Hampton, VA under NASA Grant NAG-1-02003. The authors thank Dr. C.P. Wong (MSE/Georgia Tech) for his time invested during TMA analysis. NR 12 TC 5 Z9 5 U1 1 U2 4 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1359-835X J9 COMPOS PART A-APPL S JI Compos. Pt. A-Appl. Sci. Manuf. PD APR PY 2009 VL 40 IS 4 BP 359 EP 367 DI 10.1016/j.compositesa.2008.12.009 PG 9 WC Engineering, Manufacturing; Materials Science, Composites SC Engineering; Materials Science GA 437BD UT WOS:000265459800006 ER PT J AU Narock, TW Szabo, A Merka, J AF Narock, T. W. Szabo, A. Merka, J. TI Using semantics to extend the space physics data environment SO COMPUTERS & GEOSCIENCES 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 Virtual observatory; Ontology; Registry; Search and retrieval; Data processing; Web services AB The space physics data environment is evolving with the advent of virtual observatories. With the primary function of most virtual observatories being data search and retrieval, an emphasis has been placed on providing value-added data processing services. That is, creating web services that take discovered data and provide common and routine processing such as coordinate transformations and data sub-setting. As these services proliferate, finding, accessing and using them no longer becomes a trivial task. This paper discusses a semantic registry that enables the searching of these services via ontology. We discuss the benefits of such a registry and illustrate how the web and application programming interfaces benefit the space physics community. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Narock, T. W.; Merka, J.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21250 USA. [Narock, T. W.; Szabo, A.; Merka, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Narock, TW (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, 1000 Hilltop Circle, Baltimore, MD 21250 USA. EM Thomas.W.Narock@nasa.gov OI Narock, Tom/0000-0002-9785-4496 NR 10 TC 1 Z9 1 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0098-3004 J9 COMPUT GEOSCI-UK JI Comput. Geosci. PD APR PY 2009 VL 35 IS 4 BP 791 EP 797 DI 10.1016/j.cageo.2007.12.010 PG 7 WC Computer Science, Interdisciplinary Applications; Geosciences, Multidisciplinary SC Computer Science; Geology GA 437GS UT WOS:000265475500011 ER PT J AU Nieves-Chinchilla, T Vinas, AF Hidalgo, M AF Nieves-Chinchilla, T. Vinas, A. -F. Hidalgo, M. A. TI Magnetic Field Profiles Within Magnetic Clouds: A Model-Approach SO EARTH MOON AND PLANETS LA English DT Article; Proceedings Paper CT European General Assembly on International Heliophysics Year CY JUN, 2007 CL Torino, ITALY DE Magnetic cloud; The cross-section distortion and expansion ID CROSS-SECTION; TOPOLOGY; WIND AB The model of Hidalgo (J. Geophys. Res. 108(A8):1320, 2003) has meant one more step in the understanding of the magnetic cloud events. We have modified a physical assumption over the y-components of the current density, have developed an algorithm which is able to resolve the elliptic integrals and have incorporated constrains over the parameters. This article is a new contribution for the improvement of the fitting procedure. C1 [Nieves-Chinchilla, T.; Vinas, A. -F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hidalgo, M. A.] Univ Alcala de Henares, Space Res Grp, Alcala De Henares, Spain. RP Nieves-Chinchilla, T (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd,Bld 21, Greenbelt, MD 20771 USA. EM Teresa.Nieves@nasa.gov RI Nieves-Chinchilla, Teresa/F-3482-2016; Hidalgo, Miguel/L-5826-2014 OI Nieves-Chinchilla, Teresa/0000-0003-0565-4890; Hidalgo, Miguel/0000-0003-1617-2037 NR 7 TC 2 Z9 2 U1 0 U2 4 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-9295 EI 1573-0794 J9 EARTH MOON PLANETS JI Earth Moon Planets PD APR PY 2009 VL 104 IS 1-4 BP 109 EP 113 DI 10.1007/s11038-008-9252-0 PG 5 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 414MX UT WOS:000263869300024 ER PT J AU Verdini, A Velli, M Buchlin, E AF Verdini, A. Velli, M. Buchlin, E. TI Reflection Driven MHD Turbulence in the Solar Atmosphere and Wind SO EARTH MOON AND PLANETS LA English DT Article; Proceedings Paper CT European General Assembly on International Heliophysics Year CY JUN, 2007 CL Torino, ITALY DE MHD; Waves; Turbulence; Sun: solar wind ID ALFVEN WAVES; LOW-FREQUENCY; SHELL-MODEL; ACCELERATION; PROPAGATION; REGION; SUN AB Alfv,nic turbulence is usually invoked and used in many solar wind models (Isenberg and Hollweg, 1982, J. Geophys. Res. 87:5023; Tu et al. 1984, J. Geophys. Res. 89:9695; Hu et al. 2000, J. Geophys. Res. 105:5093; Li 2003, Astron. Astrphys. 406:345; Isenberg 2004, J. Geophys. Res. 109:3101) as a process responsible for the transfer of energy, released at large scale in the photosphere, towards small scale in the corona, where it is dissipated. Usually an initial spectrum is prescribed since the closest constraint to the spectrum is given by Helios measurements at 0.3 AU. With this work we intend to study the efficiency of the reflection as a driver for the nonlinear interactions of Alfv,n waves, the development of a turbulent spectrum and its evolution in the highly stratified solar atmosphere inside coronal holes. Our main finding is that the perpendicular spectral slope changes substantially at the transition region because of the steep density gradient. As a result a strong turbulent heating occurs, just above the transition region, as requested by current solar wind models. C1 [Verdini, A.] Royal Observ Belgium, SIDC, Brussels, Belgium. [Verdini, A.; Velli, M.] Univ Florence, Dept Astron, Florence, Italy. [Velli, M.] JPL, Pasadena, CA USA. [Buchlin, E.] Univ London Imperial Coll Sci Technol & Med, London, England. RP Verdini, A (reprint author), Royal Observ Belgium, SIDC, Brussels, Belgium. EM verdini@oma.be OI Buchlin, Eric/0000-0003-4290-1897 NR 16 TC 4 Z9 5 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-9295 EI 1573-0794 J9 EARTH MOON PLANETS JI Earth Moon Planets PD APR PY 2009 VL 104 IS 1-4 BP 121 EP 125 DI 10.1007/s11038-008-9250-2 PG 5 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 414MX UT WOS:000263869300026 ER PT J AU Zimbardo, G Greco, A Veltri, P Voros, Z Amata, E Taktakishvili, A Carbone, V Sorriso-Valvo, L Guerra, I AF Zimbardo, G. Greco, A. Veltri, P. Voros, Z. Amata, E. Taktakishvili, A. L. Carbone, V. Sorriso-Valvo, L. Guerra, I. TI Solar-Terrestrial Relations: Magnetic Turbulence in the Earth's Magnetosphere and Geomagnetic Activity SO EARTH MOON AND PLANETS LA English DT Article; Proceedings Paper CT European General Assembly on International Heliophysics Year CY JUN, 2007 CL Torino, ITALY DE Magnetic turbulence; Magnetosphere; Transport; Solar wind ID ELECTRON WHISTLER INTERACTION; DISTANT MAGNETOTAIL; PLASMA SHEET; BOW SHOCK; DYNAMICS AB Recent spacecraft observations of magnetic turbulence in the ion foreshock, in the magnetosheath, in the polar cusp regions, and in the magnetotail will be reviewed. Turbulence features like the fluctuation level, the spectral power law index, the turbulence anisotropy and intermittency, and the turbulence driver will be addressed. C1 [Zimbardo, G.; Greco, A.; Veltri, P.; Carbone, V.; Sorriso-Valvo, L.; Guerra, I.] Univ Calabria, I-87036 Cosenza, Italy. [Voros, Z.] Inst Atmospher Res, Prague, Czech Republic. [Amata, E.] Ist Fis Spazio Interplanetario, INAF, Rome, Italy. [Taktakishvili, A. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Taktakishvili, A. L.] Abastumani Astrophys Observ, Tbilisi, Rep of Georgia. RP Zimbardo, G (reprint author), Univ Calabria, I-87036 Cosenza, Italy. EM zimbardo@fis.unical.it RI Sorriso-Valvo, Luca/A-9355-2008; Veltri, Pierluigi/J-1348-2014; OI Sorriso-Valvo, Luca/0000-0002-5981-7758; Veltri, Pierluigi/0000-0002-7412-1660; Voros, Zoltan/0000-0001-7597-238X; Zimbardo, Gaetano/0000-0002-9207-2647; CARBONE, Vincenzo/0000-0002-3182-6679 NR 15 TC 1 Z9 1 U1 0 U2 6 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-9295 J9 EARTH MOON PLANETS JI Earth Moon Planets PD APR PY 2009 VL 104 IS 1-4 BP 127 EP 129 DI 10.1007/s11038-008-9251-1 PG 3 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 414MX UT WOS:000263869300027 ER PT J AU Bettarini, L Landi, S Velli, M Londrillo, P AF Bettarini, L. Landi, S. Velli, M. Londrillo, P. TI Magnetic and Velocity Shear Driven Instabilities in the Heliospheric Plasma SO EARTH MOON AND PLANETS LA English DT Article; Proceedings Paper CT European General Assembly on International Heliophysics Year CY JUN, 2007 CL Torino, ITALY DE Solar wind; Ideal and resistive instabilities Magnetic reconnection; 3D MHD numerical simulations Introduction AB We have addressed the problem of combined magnetic and velocity shear driven instabilities in the context of the heliospheric plasma. New high-order numerical methods have been used to analyze the instability dynamics of the heliospheric current-sheet interacting with the structure determined by the slow component of the solar wind on the solar equatorial plane above the helmet streamers. Preliminary results are presented. C1 [Bettarini, L.; Landi, S.; Velli, M.] Univ Florence, Dipartimento Astron & Sci Spazio, I-50125 Florence, Italy. [Velli, M.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Londrillo, P.] INAF Osservatorio Astronom Bologna, Bologna, Italy. RP Bettarini, L (reprint author), Univ Florence, Dipartimento Astron & Sci Spazio, I-50125 Florence, Italy. EM lapo.bettarini@wis.kuleuven.be RI Landi, Simone/G-7282-2015 OI Landi, Simone/0000-0002-1322-8712 NR 8 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-9295 J9 EARTH MOON PLANETS JI Earth Moon Planets PD APR PY 2009 VL 104 IS 1-4 BP 135 EP 137 DI 10.1007/s11038-008-9270-y PG 3 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 414MX UT WOS:000263869300029 ER PT J AU Gopalswamy, N Eichhorn, G Sakurai, T Haubold, H AF Gopalswamy, N. Eichhorn, G. Sakurai, T. Haubold, H. J. TI Preface to the Proceedings of the European General Assembly and the United Nations Workshop SO EARTH MOON AND PLANETS LA English DT Editorial Material C1 [Gopalswamy, N.; Eichhorn, G.; Sakurai, T.; Haubold, H. J.] Vienna Int Ctr, UN Off Outer Space Affairs, A-1400 Vienna, Austria. [Gopalswamy, N.] NASA, Goddard Space Flight Ctr, Code 695, Greenbelt, MD 20771 USA. [Eichhorn, G.] Springer, Abstracting & Indexing, Norwell, MA 02061 USA. [Sakurai, T.] Natl Astron Observ, Tokyo 181, Japan. RP Haubold, H (reprint author), Vienna Int Ctr, UN Off Outer Space Affairs, Wagramerstr 5,POB 500, A-1400 Vienna, Austria. EM hans.haubold@unvienna.org RI Eichhorn, Guenther/C-9480-2009; Gopalswamy, Nat/D-3659-2012 OI Eichhorn, Guenther/0000-0002-3032-1978; NR 0 TC 0 Z9 0 U1 0 U2 4 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-9295 J9 EARTH MOON PLANETS JI Earth Moon Planets PD APR PY 2009 VL 104 IS 1-4 BP 139 EP 140 DI 10.1007/s11038-008-9278-3 PG 2 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 414MX UT WOS:000263869300030 ER PT J AU Gopalswamy, N Yashiro, S Michalek, G Stenborg, G Vourlidas, A Freeland, S Howard, R AF Gopalswamy, N. Yashiro, S. Michalek, G. Stenborg, G. Vourlidas, A. Freeland, S. Howard, R. TI The SOHO/LASCO CME Catalog SO EARTH MOON AND PLANETS LA English DT Article; Proceedings Paper CT European General Assembly on International Heliophysics Year CY JUN, 2007 CL Torino, ITALY DE Coronal mass ejections; Flares; Geomagnetic storms; Solar energetic particle events ID CORONAL MASS EJECTIONS; MAGNETIC CLOUDS; RADIO; SOLAR-CYCLE-23 AB Coronal mass ejections (CMEs) are routinely identified in the images of the solar corona obtained by the Solar and Heliospheric Observatory (SOHO) mission's Large Angle and Spectrometric Coronagraph (LASCO) since 1996. The identified CMEs are measured and their basic attributes are cataloged in a data base known as the SOHO/LASCO CME Catalog. The Catalog also contains digital data, movies, and plots for each CME, so detailed scientific investigations can be performed on CMEs and the related phenomena such as flares, radio bursts, solar energetic particle events, and geomagnetic storms. This paper provides a brief description of the Catalog and summarizes the statistical properties of CMEs obtained using the Catalog. Data products relevant to space weather research and some CME issues that can be addressed using the Catalog are discussed. The URL of the Catalog is: http://cdaw.gsfc.nasa.gov/CME_list. C1 [Yashiro, S.; Michalek, G.; Stenborg, G.] Catholic Univ Amer, Washington, DC 20064 USA. [Vourlidas, A.; Howard, R.] USN, Res Lab, Washington, DC 20375 USA. [Freeland, S.] Lockheed Martin Adv Technol Ctr, Palo Alto, CA USA. [Gopalswamy, N.] NASA, Goddard Space Flight Ctr, Code 695, Greenbelt, MD 20771 USA. RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Code 695, Greenbelt, MD 20771 USA. EM nat.gopalswamy@nasa.gov; seiji.yashiro@nasa.gov; freeland@lmsal.com; russ.howard@nrl.navy.mil RI Vourlidas, Angelos/C-8231-2009; Gopalswamy, Nat/D-3659-2012 OI Vourlidas, Angelos/0000-0002-8164-5948; NR 33 TC 159 Z9 160 U1 1 U2 7 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-9295 J9 EARTH MOON PLANETS JI Earth Moon Planets PD APR PY 2009 VL 104 IS 1-4 BP 295 EP 313 DI 10.1007/s11038-008-9282-7 PG 19 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 414MX UT WOS:000263869300045 ER PT J AU Hill, F Martens, P Yoshimura, K Gurman, J Hourcle, J Dimitoglou, G Suarez-Sola, I Wampler, S Reardon, K Davey, A Bogart, R Tian, K AF Hill, Frank Martens, Piet Yoshimura, Keji Gurman, Joseph Hourcle, Joseph Dimitoglou, George Suarez-Sola, Igor Wampler, Steve Reardon, Kevin Davey, Alisdair Bogart, Richard S. Tian, Karen Q. TI The Virtual Solar Observatory-A Resource for International Heliophysics Research SO EARTH MOON AND PLANETS LA English DT Article; Proceedings Paper CT European General Assembly on International Heliophysics Year CY JUN, 2007 CL Torino, ITALY DE Data management; Virtual observatories; Solar physics; Distributed archives ID SYSTEM AB The Virtual Solar Observatory (VSO) has been developed to allow researchers, educators, and the general public to access data and images from the major sources of on-line solar data. The VSO substantially reduces the effort required to locate disparate data sets, and removes the need for the user to locate the data and learn multiple interfaces. The VSO provides a single interface to about 60 geographically distributed data sets including space- and ground-based sources. These data sets incorporate several physical variables including magnetic field, intensity, Doppler velocity, etc., and all wavelengths from X-ray to radio. All layers of the sun, from the interior to the corona, are included. In this paper we describe the system and present the interface that the user will encounter. We also discuss future enhancements planned for the system. C1 [Hill, Frank; Suarez-Sola, Igor; Wampler, Steve] Natl Solar Observ, Tucson, AZ 85719 USA. [Martens, Piet; Yoshimura, Keji] Montana State Univ, Bozeman, MT 59717 USA. [Gurman, Joseph; Hourcle, Joseph; Dimitoglou, George] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Reardon, Kevin] Osservatorio Arcetri, Florence, Italy. [Davey, Alisdair] SW Res Inst, Boulder, CO USA. [Bogart, Richard S.; Tian, Karen Q.] Stanford Univ, Stanford, CA 94305 USA. RP Hill, F (reprint author), Natl Solar Observ, 950 N Cherry Ave, Tucson, AZ 85719 USA. EM fhill@noao.edu OI Hourcle, Joe/0000-0002-0713-594X NR 10 TC 5 Z9 5 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-9295 EI 1573-0794 J9 EARTH MOON PLANETS JI Earth Moon Planets PD APR PY 2009 VL 104 IS 1-4 BP 315 EP 330 DI 10.1007/s11038-008-9274-7 PG 16 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 414MX UT WOS:000263869300046 ER PT J AU Lee, JSF Berejikian, BA AF Lee, Jonathan S. F. Berejikian, Barry A. TI Structural complexity in relation to the habitat preferences, territoriality, and hatchery rearing of juvenile China rockfish (Sebastes nebulosus) SO ENVIRONMENTAL BIOLOGY OF FISHES LA English DT Article DE Stock enhancement; Conservation hatchery; Predation risk; Rearing effects ID CORAL-REEF FISH; BODY-SIZE; DOMINANCE; SETTLEMENT; ECOLOGY; COMMUNITIES; SURVIVAL; BEHAVIOR; GROWTH; SALMON AB Conservation efforts require an understanding of the basic behavior and ecology of target species. However, limited information exists for a wide range of taxa, including declining species of rockfish (genus Sebastes). First, we observed captive juvenile China rockfish (S. nebulosus) to determine how they interact with their environment and conspecifics. Juveniles exhibited site fidelity and territoriality. These aggressive interactions occurred within the context of size-biased dominance, centered on competition for structurally complex habitat. Given the apparent importance of structure and the absence of structure in typical hatchery environments, we then asked how the absence of structure affects future behavior. When barren-reared and structure-reared juveniles were combined into a structurally complex aquarium, barren-reared fish displayed less structure use and less site fidelity than structure-reared fish. However, after 1 to 2 weeks, barren-reared fish began to use structure and showed site fidelity that eventually equaled that of structure-reared juveniles, showing that those behavioral effects of the rearing environment were not permanent. Though these short-term effects may still impact survival after hatchery release, we were unable to detect significant effects on vulnerability to a predator (lingcod, Ophiodon elongatus) in laboratory trials. C1 [Lee, Jonathan S. F.; Berejikian, Barry A.] NW Fisheries Sci Ctr, Manchester Res Stn, Natl Marine Fisheries Serv, Resource Enhancement & Utilizat Technol Div, Manchester, WA 98353 USA. RP Lee, JSF (reprint author), NW Fisheries Sci Ctr, Manchester Res Stn, Natl Marine Fisheries Serv, Resource Enhancement & Utilizat Technol Div, POB 130, Manchester, WA 98353 USA. EM jon.lee@noaa.gov RI Bizzarro, Joseph/A-2988-2012 FU NOAA Fisheries; Science Consortium for Ocean Replenishment (SCORE) FX We thank Ken Massee (National Oceanic and Atmospheric Administration-NOAA), Mike Rust (NOAA), Tom Waite (University of Idaho), and the Seattle Aquarium for providing the juvenile China rockfish. We also appreciate help from Jeff Atkins in preparing the flume and aquaria, and Tom Flagg and Walt Dickhoff for reviewing the manuscript. This study was funded by a NOAA Fisheries funded research consortium - the Science Consortium for Ocean Replenishment (SCORE). The views expressed are those of the authors and do not necessarily reflect those of the funding agency. NR 31 TC 4 Z9 4 U1 3 U2 12 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0378-1909 J9 ENVIRON BIOL FISH JI Environ. Biol. Fishes PD APR PY 2009 VL 84 IS 4 BP 411 EP 419 DI 10.1007/s10641-009-9450-2 PG 9 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 420BG UT WOS:000264262800011 ER PT J AU Ross, KW Brown, ME Verdin, JP Underwood, LW AF Ross, K. W. Brown, M. E. Verdin, J. P. Underwood, L. W. TI Review of FEWS NET biophysical monitoring requirements SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Review DE applied remote sensing; requirements definition; Earth observations; early warning ID SPOT-VEGETATION; MODIS; RAINFALL; AFRICA; AVHRR AB The Famine Early Warning System Network (FEWS NET) provides monitoring and early warning support to decision makers responsible for responding to famine and food insecurity. FEWS NET transforms satellite remote sensing data into rainfall and vegetation information that can be used by these decision makers. The National Aeronautics and Space Administration has recently funded activities to enhance remote sensing inputs to FEWS NET. To elicit Earth observation requirements, a professional review questionnaire was disseminated to FEWS NET expert end-users; it focused upon operational requirements to determine additional useful remote sensing data and, subsequently, to assess whether such data would be beneficial as FEWS NET biophysical supplementary inputs. The review was completed by over 40 experts from around the world. Reviewers were asked to evaluate the relative importance of environmental variables and spatio-temporal requirements for Earth science data products, in particular for rainfall and vegetation products. The results showed that spatio-temporal resolution requirements are complex and need to vary according to place, time, and hazard; that high resolution remote sensing products continue to be in demand; and that rainfall and vegetation products are valued as data that provide actionable food security information. C1 [Ross, K. W.; Underwood, L. W.] Sci Syst & Applicat Inc, Poplarville, MS 39470 USA. [Brown, M. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Verdin, J. P.] NOAA, ESRL, US Geol Survey, Boulder, CO 80305 USA. RP Ross, KW (reprint author), Sci Syst & Applicat Inc, 411 W Michigan St, Poplarville, MS 39470 USA. EM kenton_ross@ssaihq.com; molly.brown@nasa.gov; verdin@usgs.gov; lauren_underwood@ssaihq.com RI Brown, Molly/E-2724-2010; Brown, Molly/M-5146-2013; OI Brown, Molly/0000-0001-7384-3314; Brown, Molly/0000-0001-7384-3314; Ross, Kenton/0000-0002-6381-5894 FU NASA [NNS06AA60I, NNG06HU01G] FX The USGS directs this work with funding provided through NASA Interagency Purchase Request NNS06AA60I. K Ross, M Brown, and L Underwood participate under NASA Grant NNG06HU01G. NR 17 TC 5 Z9 5 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1748-9326 J9 ENVIRON RES LETT JI Environ. Res. Lett. PD APR-JUN PY 2009 VL 4 IS 2 AR 024009 DI 10.1088/1748-9326/4/2/024009 PG 10 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 470QD UT WOS:000267991900010 ER PT J AU Priester, JH Stoimenov, PK Mielke, RE Webb, SM Ehrhardt, C Zhang, JP Stucky, GD Holden, PA AF Priester, John H. Stoimenov, Peter K. Mielke, Randall E. Webb, Samuel M. Ehrhardt, Christopher Zhang, Jin Ping Stucky, Galen D. Holden, Patricia A. TI Effects of Soluble Cadmium Salts Versus CdSe Quantum Dots on the Growth of Planktonic Pseudomonas aeruginosa SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID ESCHERICHIA-COLI; OXIDATIVE STRESS; ANTIMICROBIAL ACTIVITY; SILVER NANOPARTICLES; UNSATURATED BIOFILMS; CYTOTOXICITY; BACTERIA; MECHANISMS; COMMUNITY; TOXICITY AB With their increased use, engineered nanomaterials (ENMs) will enter the environment where they maybe altered by bacteria and affect bacterial processes. Metallic ENMs, such as CdSe quantum dots (QDs), are toxic due to the release of dissolved heavy metals, but the effects of cadmium ions versus intact QDs are mostly unknown. Here, planktonic Pseudomonas aeruginosa PG201 bacteria were cultured with similar total cadmium concentrations as either fully dissolved cadmium acetate (Cd(CH3COO)(2)) or ligand capped CdSe QDs, and cellular morphology, growth parameters, intracellular reactive oxygen species (ROS), along with the metal and metalloid fates were measured. QDs dissolved partially in growth media, but dissolution was less in biotic cultures compared to sterile controls. Dose-dependent growth effects were similar for low concentrations of either cadmium salts or QDs, but effects differed above a concentration threshold of 50 mg/L(total cadmium basis) where (1) the growth of QD-treated cells was more impaired, (2) the membranes of QD-grown cells were damaged, and (3) CID-grown cells contained QD-sized CdSe cytoplasmic inclusions in addition to Se-0 and dissolved cadmium. For most concentrations, intracellular ROS were higher for QD-versus cadmium salts-grown bacteria. Taken together, QDs were more toxic to this opportunistic pathogen than cadmium ions, and were affected by cells through QD extracellular stabilization, intracellular enrichment, and cell-associated decay. C1 [Priester, John H.; Holden, Patricia A.] Univ Calif Santa Barbara, Donald Bren Sch Environm Sci & Management, Santa Barbara, CA 93106 USA. [Stoimenov, Peter K.; Stucky, Galen D.] Univ Calif Santa Barbara, Dept Chem & Biochem, Santa Barbara, CA 93106 USA. [Mielke, Randall E.] CALTECH, Jet Prop Lab, Ctr Life Detect, Pasadena, CA 91109 USA. [Webb, Samuel M.] Stanford Linear Accelerator Ctr, Stanford Synchrotron Radiat Lab, Menlo Pk, CA 94025 USA. RP Holden, PA (reprint author), Univ Calif Santa Barbara, Donald Bren Sch Environm Sci & Management, Santa Barbara, CA 93106 USA. EM holden@bren.ucsb.edu RI Webb, Samuel/D-4778-2009; OI Webb, Samuel/0000-0003-1188-0464; Ehrhardt, Christopher/0000-0002-4909-0532 FU U.S. EPA STAR [R831712, R833323]; University of California Toxic Substances Research and Training Program; Office of Science (BER), U.S. Department of Energy [DE-FG02-05ER63949]; National Science Foundation [DMR05-20415]; Environmental Protection Agency [EF 0830117] FX This research was supported by the U.S. EPA STAR Awards R831712 and R833323, by the University of California Toxic Substances Research and Training Program: Lead Campus program in Nanotoxicology, and by the Office of Science (BER), U.S. Department of Energy, Grant DE-FG02-05ER63949. Publication of this material is Supported by the National Science Foundation and the Environmental Protection Agency under Cooperative Agreement EF 0830117. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the National Science Foundation or the Environmental Protection Agency. This work has not been subjected to EPA review and no official endorsement should be infer-red. This work made use of UCSB MRL Central Facilities supported by the MRSEC Program of the National Science Foundation under award DMR05-20415. Portions of this research were carried out at the Stanford Synchrotron Radiation Laboratory, a national user facility operated by Stanford University on behalf of the U.S. Department of Energy, Office of Basic Energy Sciences. NR 51 TC 90 Z9 93 U1 1 U2 54 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD APR 1 PY 2009 VL 43 IS 7 BP 2589 EP 2594 DI 10.1021/es802806n PG 6 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 427DI UT WOS:000264759600072 PM 19452921 ER PT J AU Tseng, CC Voytovych, DM Kulatilaka, WD Bhuiyan, AH Lucht, RP Merkle, CL Hulka, JR Jones, GW AF Tseng, C. C. Voytovych, D. M. Kulatilaka, W. D. Bhuiyan, A. H. Lucht, R. P. Merkle, C. L. Hulka, J. R. Jones, G. W. TI Structure and mixing of a transient flow of helium injected into an established flow of nitrogen: two dimensional measurement and simulation SO EXPERIMENTS IN FLUIDS LA English DT Article ID INDUCED FLUORESCENCE MEASUREMENTS; TURBULENT; LAYERS; INSTABILITIES; TRANSITION; FRACTION; FLAMES; NO AB The transient injection and mixing between nitrogen and helium in a confined chamber at atmospheric pressure is studied experimentally. The 2D injector and mixing chamber contained a middle injection slot for nitrogen flanked by a pair of outer slots for helium. Experiments were conducted by introducing the helium streams into a previously established quasi-steady flow of nitrogen. The nitrogen stream was seeded with nitric oxide (NO) that served as a source for quantitative, planar laser-induced fluorescence (PLIF) imaging of the transient mixing process. PLIF images were acquired by triggering an Nd:YAG laser system at selected times following helium valve actuation. The observed flow structures and extent of mixing between the two streams proved to be highly unsteady and irregular with the helium/nitrogen jets frequently deviating from the centerline toward the confining walls. Representative unsteady CFD solutions also show this same absence of symmetry and the same general flow structures as the measurements, however, they predict somewhat higher helium concentration in recirculation regions than were observed in the measurements. C1 [Voytovych, D. M.; Merkle, C. L.] Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA. [Tseng, C. C.; Voytovych, D. M.; Kulatilaka, W. D.; Bhuiyan, A. H.; Lucht, R. P.; Merkle, C. L.] Purdue Univ, Sch Mech Engn, W Lafayette, IN 47907 USA. [Hulka, J. R.] Jacobs ESTS Grp, Huntsville, AL 35812 USA. [Jones, G. W.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Voytovych, DM (reprint author), Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA. EM dvoyt@purdue.edu; lucht@purdue.edu; merkle@purdue.edu FU NASA Constellation University Institutes Project (CUIP) [NCC8-200]; Ms. Claudia Meyer and Dr. Jeff Rybak of Glenn Research Center; NASA Combustion Devices Injector Technology (CDIT) Program; LabVIEW program FX This project is supported by the NASA Constellation University Institutes Project (CUIP) Program under Grant NCC8-200 with Ms. Claudia Meyer and Dr. Jeff Rybak of Glenn Research Center as contract monitors. The funding for the fabrication of the injector assembly and for the initial measurements was provided by the NASA Combustion Devices Injector Technology (CDIT) Program. The substantial efforts of Dr. James Sisco and Dr. William Anderson (Purdue) in designing the injector, and of Dr. Thomas Anderson (Purdue) in developing the LabVIEW program are gratefully acknowledged. NR 23 TC 4 Z9 4 U1 1 U2 4 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0723-4864 J9 EXP FLUIDS JI Exp. Fluids PD APR PY 2009 VL 46 IS 4 BP 559 EP 575 DI 10.1007/s00348-008-0581-6 PG 17 WC Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA 431RQ UT WOS:000265081300001 ER PT J AU Evans, JM Ayanampudi, V Howarth, M Moore, F Patwardhan, A Knapp, C AF Evans, Joyce McClendon Ayanampudi, Vijaya Howarth, Mark Moore, Fritz Patwardhan, Abjihit Knapp, Charles TI Cardiovascular Regulation During Artificial Gravity Stress SO FASEB JOURNAL LA English DT Meeting Abstract C1 [Evans, Joyce McClendon; Ayanampudi, Vijaya; Howarth, Mark; Patwardhan, Abjihit; Knapp, Charles] Univ Kentucky, Lexington, KY USA. [Moore, Fritz] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU FEDERATION AMER SOC EXP BIOL PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA SN 0892-6638 J9 FASEB J JI Faseb J. PD APR PY 2009 VL 23 MA 1035.3 PG 1 WC Biochemistry & Molecular Biology; Biology; Cell Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics; Cell Biology GA V27OC UT WOS:000208621505525 ER PT J AU Evans, JM Meng, M Patwardhan, A Stenger, M Feiveson, A Knapp, C AF Evans, Joyce McClendon Meng, Martha Patwardhan, Abjihit Stenger, Michael Feiveson, Alan Knapp, Charles TI Prediction of Changes in Orthostatic Tolerance after Head down Bed Rest With and Without Artificial gravity Training SO FASEB JOURNAL LA English DT Meeting Abstract C1 [Evans, Joyce McClendon; Meng, Martha; Patwardhan, Abjihit; Knapp, Charles] Univ Kentucky, Ctr Biomed Engn, Lexington, KY 40506 USA. [Stenger, Michael] Wyle Labs, Houston, TX USA. [Feiveson, Alan] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU FEDERATION AMER SOC EXP BIOL PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA SN 0892-6638 J9 FASEB J JI Faseb J. PD APR PY 2009 VL 23 MA 1035.2 PG 1 WC Biochemistry & Molecular Biology; Biology; Cell Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics; Cell Biology GA V27OC UT WOS:000208621505262 ER PT J AU Dillon, JG Miller, S Bebout, B Hullar, M Pinel, N Stahl, DA AF Dillon, Jesse G. Miller, Scott Bebout, Brad Hullar, Meredith Pinel, Nicolas Stahl, David A. TI Spatial and temporal variability in a stratified hypersaline microbial mat community SO FEMS MICROBIOLOGY ECOLOGY LA English DT Article DE microbial mat; hypersaline; T-RFLP; migration; cyanobacteria; Guerrero Negro ID SALINS-DE-GIRAUD; SULFATE-REDUCING BACTERIA; SOLAR LAKE SINAI; CYANOBACTERIAL MATS; MEDITERRANEAN SALTERNS; VISIBLE IRRADIANCE; VERTICAL MIGRATION; GUERRERO NEGRO; DIVERSITY; PHOTOSYNTHESIS AB Hypersaline microbial mat communities have recently been shown to be more diverse than once thought. The variability in community composition of hypersaline mats, both in terms of spatial and temporal dimensions, is still poorly understood. Because this information is essential to understanding the complex biotic and abiotic interactions within these communities, terminal restriction fragment analysis and 16S rRNA gene sequencing were used to characterize the near-surface community of a hypersaline microbial mat in Guerrero Negro, Mexico. Core samples were analyzed to assay community variability over large regional scales (centimeter to kilometer) and to track depth-related changes in population distribution at 250-mu m intervals over a diel period. Significant changes in total species diversity were observed at increasing distances across the mat surface; however, key species (e.g. Microcoleus sp.) were identified throughout the mat. The vertical position and abundance of > 50% of the 60 peaks detected varied dramatically over a diel cycle, including Beggiatoa sp., cyanobacteria, Chloroflexus sp., Halochromatium sp., Bacteroidetes sp. and several as-yet-identified bacteria. Many of these migrations correlated strongly with diel changes in redox conditions within the mat, contributing to strong day-night community structure differences. C1 [Dillon, Jesse G.; Pinel, Nicolas] Univ Washington, Dept Microbiol, Seattle, WA 98195 USA. [Dillon, Jesse G.; Hullar, Meredith; Pinel, Nicolas; Stahl, David A.] Univ Washington, NASA Astrobiol Inst, Seattle, WA 98195 USA. [Miller, Scott] Univ Montana, Div Biol Sci, Missoula, MT 59812 USA. [Bebout, Brad] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Hullar, Meredith; Stahl, David A.] Univ Washington, Dept Civil & Environm Engn, Seattle, WA 98195 USA. RP Dillon, JG (reprint author), Calif State Univ Long Beach, Dept Biol Sci, Long Beach, CA 90840 USA. EM jdillon@csulb.edu FU NSF-IGERT [DGE-9870713]; NSF [DEB-0213186]; NASA NAI [NCC2-1273] FX This work was supported by NSF-IGERT grant (DGE-9870713) funding to J.G.D. and NSF grant (DEB-0213186) and NASA NAI grant (NCC2-1273) support to D.A.S. and J.G.D. We would like to thank Dr David Des Marais and all of the NASA Ames EMERG group for logistical support and field assistance on this project. We would like to thank the Mexican government and the Exportadora de Sal, SA, for granting permission to perform research in the salt ponds. We would like to thank Michael Rothrock and Dr Ferran Garcia-Pichel for assistance with experimental design and sampling. We would also like to thank Drs Jennifer Glick and Joseph Beavo for the use of the cryotome. Dr Ann Bernhard is gratefully acknowledged for her assistance in using PC-ORD. NR 51 TC 27 Z9 27 U1 1 U2 26 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0168-6496 J9 FEMS MICROBIOL ECOL JI FEMS Microbiol. Ecol. PD APR PY 2009 VL 68 IS 1 BP 46 EP 58 DI 10.1111/j.1574-6941.2009.00647.x PG 13 WC Microbiology SC Microbiology GA 415BN UT WOS:000263909400005 PM 19175677 ER PT J AU Sewall, FF Rodgveller, CJ AF Sewall, Fletcher F. Rodgveller, Cara J. TI Changes in body composition and fatty acid profile during embryogenesis of quillback rockfish (Sebastes maliger) SO FISHERY BULLETIN LA English DT Article ID EMBRYONIC-DEVELOPMENT; YELLOWTAIL ROCKFISH; MARINE FISH; LIPIDS; METABOLISM; SCHLEGELI; DYNAMICS; MELANOPS AB We investigated developmental changes in the body compositions and fatty acid (FA) profiles of embryos and preparturition larvae of the quillback rockfish (Sebastes maliger). Comparisons of proximate composition data from early-stage embryos with data from hatched preparturition larvae taken from wild-caught gravid females indicated that embryos gain over one-third their weight in moisture while consuming 20% of their dry tissue mass for energy as they develop into larvae. Lipid contributed 60% of the energy consumed and was depleted more rapidly than protein, indicating a protein-sparing effect. Oil globule volume was strongly correlated with lipid levels, affirming its utility as an indicator of energetic status. FA profiles of early embryos differed significantly from those of hatched larvae. Differences in the relative abundances of FAs between early embryos and hatched larvae indicated different FA depletion rates during embryonic development. We conclude that some metabolically important FAs may prove useful in assessing the condition of embryos and preparturition larvae, particularly 20:4n-6, which cannot be synthesized by many marine fish and which is conserved during embryogenesis. Variability in body composition and energy use among rockfish species should be considered when interpreting any measures of condition. C1 [Sewall, Fletcher F.; Rodgveller, Cara J.] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Labs,Ted Stevens Marine Res Inst, Juneau, AK 99801 USA. RP Sewall, FF (reprint author), NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Labs,Ted Stevens Marine Res Inst, 17109 Pt Lena Loop Rd, Juneau, AK 99801 USA. EM Fletcher.Sewall@noaa.gov NR 30 TC 6 Z9 6 U1 0 U2 2 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 APR PY 2009 VL 107 IS 2 BP 207 EP 220 PG 14 WC Fisheries SC Fisheries GA 435VG UT WOS:000265370800008 ER PT J AU Akkerman, V Ivanov, M Bychkov, V AF Akkerman, V'yacheslav Ivanov, Mikhail Bychkov, Vitaly TI Turbulent Flow Produced by Piston Motion in a Spark-ignition Engine SO FLOW TURBULENCE AND COMBUSTION LA English DT Article DE Spark-ignition (SI) engine; Piston motion; Direct numerical simulations ID BURNING VELOCITY; PREMIXED FLAMES; LENGTH SCALES; PROPAGATION; COMBUSTION; DISSIPATION; INSTABILITY; SIMULATION; EQUATION; MODEL AB Turbulence produced by the piston motion in spark-ignition engines is studied by 2D axisymmetric numerical simulations in the cylindrical geometry as in the theoretical and experimental work by Breuer et al. (Flow Turbul Combust 74:145, 2005). The simulations are based on the Navier-Stokes gas-dynamic equations including viscosity, thermal conduction and non-slip at the walls. Piston motion is taken into account as a boundary condition. The turbulent flow is investigated for a wide range of the engine speed, 1,000-4,000 rpm, assuming both zero and non-zero initial turbulence. The turbulent rms-velocity and the integral length scale are investigated in axial and radial directions. The rms-turbulent velocity is typically an order-of-magnitude smaller than the piston speed. In the case of zero initial turbulence, the flow at the top-dead-center may be described as a combination of two large-scale vortex rings of a size determined by the engine geometry. When initial turbulence is strong, then the integral turbulent length demonstrates self-similar properties in a large range of crank angles. The results obtained agree with the experimental observations of Breuer et al. (Flow Turbul Combust 74:145, 2005). C1 [Akkerman, V'yacheslav; Ivanov, Mikhail; Bychkov, Vitaly] Umea Univ, Dept Phys, S-90187 Umea, Sweden. [Akkerman, V'yacheslav; Ivanov, Mikhail] Russian Acad Sci, Nucl Safety Inst, Moscow 115191, Russia. [Akkerman, V'yacheslav; Ivanov, Mikhail] Moscow Inst Phys & Technol, Dept Phys & Power Engn, Dolgoprudnyi 141700, Moscow Region, Russia. RP Akkerman, V (reprint author), Stanford Univ, NASA, Ames Res Ctr, 488 Escondido Mall, Stanford, CA 94305 USA. EM akkerman@stanford.edu RI Akkerman, V'yacheslav/H-7982-2012 FU Swedish Research Council (VR); Kempe Foundation FX The authors are grateful to Martin Oberlack for the data of paper [1] reproduced in Figs. 8, 9b, c. We also thank Mikhail Modestov for useful discussions. This work has been supported by the Swedish Research Council (VR) and by the Kempe Foundation. NR 45 TC 3 Z9 4 U1 0 U2 8 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1386-6184 EI 1573-1987 J9 FLOW TURBUL COMBUST JI Flow Turbul. Combust. PD APR PY 2009 VL 82 IS 3 BP 317 EP 337 DI 10.1007/s10494-008-9179-6 PG 21 WC Thermodynamics; Mechanics SC Thermodynamics; Mechanics GA 423TZ UT WOS:000264519900002 ER PT J AU Park, J Garrison, DH Bogard, DD AF Park, Jisun Garrison, Daniel H. Bogard, Donald D. TI Ar-39-Ar-40 ages of martian nakhlites SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID BASALTIC SHERGOTTITES; NOBLE-GASES; PARENT BODY; METEORITES; MARS; PETROLOGY; PETROGENESIS; AR-40-AR-39; ATMOSPHERE; MIL-03346 AB We report Ar-39-Ar-40 ages of whole rock (WR) and plagioclase and pyroxene mineral separates of nakhlites MIL 03346 and Y-000593, and of WR samples of nakhlites NWA 998 and Nakhla. All age spectra are complex and indicate variable degrees of Ar-39 recoil and variable amounts of trapped Ar-40 in the samples. Thus, we examine possible Ar-Ar ages in several ways. From consideration of both limited plateau ages and isochron ages, we prefer Ar-Ar ages of NWA 998 = 1334 +/- 11 Ma, MIL 03346 = 1368 +/- 83 Ma (mesostasis) and 1334 +/- 54 Ma (pyroxene), Y-000593 = 1367 +/- 7 Ma, and Nakhla = 1357 +/- 11 Ma, (2 sigma errors). For NWA 998 and MIL 03346 the Ar-Ar ages are within uncertainties of preliminary Rb-Sr isochron ages reported in the literature. These Ar-Ar ages for Y-000593 and Nakhla are several Ma older than Sm-Nd ages reported in the literature. We conclude that the major factor in producing Ar-Ar ages slightly too old is the presence of small amounts of trapped martian or terrestrial Ar-40 on weathered grain surfaces that was degassed along with the first several percent of Ar-39. A total K-Ar-40 isochron for WR and mineral data from five nakhlites analyzed by us, plus Lafayette data in the literature, gives an isochron age of 1325 +/- 18 Ma (2 sigma). We emphasize the precision of this isochron over the value of the isochron age. Our Ar-Ar data are consistent with a common formation age for nakhlites. The cosmic-ray exposure (CRE) age for NWA 998 of similar to 12 Ma is also similar to CRE ages for other nakhlites. (c) Published by Elsevier Ltd. C1 [Park, Jisun; Garrison, Daniel H.; Bogard, Donald D.] NASA, Lyndon B Johnson Space Ctr, ARES, Code KR, Houston, TX 77058 USA. [Garrison, Daniel H.] ESCD Barrios, JE23, Houston, TX 77058 USA. RP Bogard, DD (reprint author), NASA, Lyndon B Johnson Space Ctr, ARES, Code KR, Houston, TX 77058 USA. EM donald.d.bogard@nasa.gov NR 54 TC 12 Z9 13 U1 1 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD APR 1 PY 2009 VL 73 IS 7 BP 2177 EP 2189 DI 10.1016/j.gca.2008.12.027 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 423TL UT WOS:000264518500024 ER PT J AU Ellis, JT Morrison, RF Priest, BH AF Ellis, Jean T. Morrison, Rebecca F. Priest, Barry H. TI Detecting impacts of sand grains with a microphone system in field conditions SO GEOMORPHOLOGY LA English DT Article; Proceedings Paper CT 6th International Conference on Aeolian Research (ICAR VI) CY JUL 24-28, 2006 CL Univ Guelph, Guelph, CANADA HO Univ Guelph DE Wind blown sediment; Miniphone; Saltation transport; Coastal geomorphology; Aeolian geomorphology ID AEOLIAN TRANSPORT; TRAP DESIGN; SALTATION; WIND; BEACH; LAYER AB This paper describes the "miniplione," an instrument to measure aeolian saltation. This instrument is a modified electret microphone that detects the impacts of individual grains. The unidirectional miniphone is inexpensive (approximately US$10), small, and poses minimal disruption to the wind field. It can be sampled at rates up to 44,100 Hz using commonly available Sound card technology or it can be interfaced with a data acquisition system. Data from deployments on beaches on Marco Island, FL, USA and near Shoalhaven Heads, NSW, Australia using sample rates of 44,100 Hz and 6000 Hz, are presented. An algorithm for identifying discrete impacts of grains is described. The number of saltation impacts was not reduced when sub-sampling a record from 44,100 Hz to 6000 Hz. The most immediate use for the miniphone is for short-term deployments to detect unsteadiness in the saltation field. (C) 2008 Elsevier B.V. All rights reserved. C1 [Ellis, Jean T.; Priest, Barry H.] Texas A&M Univ, Dept Geog, College Stn, TX 77843 USA. [Morrison, Rebecca F.] Texas A&M Univ, Dept Elect Engn, College Stn, TX 77843 USA. RP Ellis, JT (reprint author), NASA, Div Sci & Technol, Stennis Space Ctr, MS 39529 USA. EM jean.t.ellis@nasa.gov NR 34 TC 31 Z9 33 U1 1 U2 11 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0169-555X EI 1872-695X J9 GEOMORPHOLOGY JI Geomorphology PD APR 1 PY 2009 VL 105 IS 1-2 SI SI BP 87 EP 94 DI 10.1016/j.geomorph.2008.02.017 PG 8 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 414LZ UT WOS:000263866600010 ER PT J AU Hu, SW Kim, MHY McClellan, GE Cucinotta, FA AF Hu, Shaowen Kim, Myung-Hee Y. McClellan, Gene E. Cucinotta, Francis A. TI MODELING THE ACUTE HEALTH EFFECTS OF ASTRONAUTS FROM EXPOSURE TO LARGE SOLAR PARTICLE EVENTS SO HEALTH PHYSICS LA English DT Article DE analysis; risk; computer calculations; health effects; radiation risk ID GALACTIC COSMIC-RAYS; SPACE RADIATION; LETHALITY; DOSIMETRY; HUMANS; ISSUES; RISK; RBE; GY AB Radiation exposure from Solar Particle Events (SPE) presents a significant health concern for astronauts for exploration missions outside the protection of the Earth's magnetic field, which could impair their performance and result in the possibility of failure of the mission. Assessing the potential for early radiation effects under such adverse conditions is of prime importance. Here we apply a biologically based mathematical model that describes the dose- and time-dependent early human responses that constitute the prodromal syndromes to consider acute risks from SPEs. We examine the possible early effects on crews from exposure to some historically large solar events on lunar and/or Mars missions. The doses and dose rates of specific organs were calculated using the Baryon radiation transport (BRYNTRN) code and a computerized anatomical man model, while the hazard of the early radiation effects and performance reduction were calculated using the Radiation-Induced Performance Decrement (RIPD) code. Based on model assumptions we show that exposure to these historical events would cause moderate early health effects to crew members inside a typical spacecraft or during extra-vehicular activities, if effective shielding and medical countermeasure tactics were not provided. We also calculate possible even worse cases (double intensity, multiple occurrences in a short period of time, etc.) to estimate the severity, onset and duration of various types of early illness. Uncertainties in the calculation due to limited data on relative biological effectiveness and dose-rate modifying factors for protons and secondary radiation, and the identification of sensitive sites in critical organs are discussed. Health Phys. 96(4):465-476; 2009 C1 [Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Hu, Shaowen; Kim, Myung-Hee Y.] Univ Space Res Assoc, Div Space Life Sci, Houston, TX 77058 USA. [McClellan, Gene E.] Appl Res Associates Inc, Arlington, VA 22203 USA. RP Cucinotta, FA (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA. EM Shaowen.Hu-1@nasa.gov; Francis.A.Cuciniotta@NASA.gov FU Defense Threat Reduction Agency [DTRA01-03-D-0014-0015] FX We wish to extend a note of gratitude to John Moulder for discussions on models of acute risks. Funding for this study was provided by the NASA Space Radiation Program, Risk Assessment Project. One of the authors (GEM) participated with support from the Defense Threat Reduction Agency, Contract DTRA01-03-D-0014-0015. NR 38 TC 37 Z9 38 U1 6 U2 12 PU LIPPINCOTT WILLIAMS & WILKINS PI PHILADELPHIA PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA SN 0017-9078 EI 1538-5159 J9 HEALTH PHYS JI Health Phys. PD APR PY 2009 VL 96 IS 4 BP 465 EP 476 PG 12 WC Environmental Sciences; Public, Environmental & Occupational Health; Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health; Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging GA 420BX UT WOS:000264264500006 PM 19276707 ER PT J AU Thompson, WT AF Thompson, W. T. TI 3D triangulation of a Sun-grazing comet SO ICARUS LA English DT Article DE Comets, dynamics; Data reduction techniques ID SUNGRAZING COMETS; STEREO; SOLAR; MISSION; SECCHI AB The bright Kreutz Comet C/2007 L3 (SOHO) entered the fields of view of the twin Solar Terrestrial Relations Observatory (STEREO) COR1 telescopes oil 7-8 June 2007. The 12 degrees separation between the two spacecraft at the time afforded the opportunity to derive the position of the comet's tail in three-dimensional space using direct triangulation. The track of the comet's orbit is compared against more traditional orbital calculations using observations from the STEREO COR2 telescopes, and from the Large Angle and Spectrometric Coronagraph (LASCO) aboard the Solar and Heliospheric Observatory (SOHO). The shape of the comet's tail shows that it is composed of dust particles released when the comet was between 18 and 22 solar radii, with no significant dust production after that. The comet did not survive perihelion passage, but a rare faint remnant of the comet tail persisted for several hours after the break-up, and was seen by both the SOHO and STEREO coronagraphs to drift slowly away from the Sun. This tail remnant was found to be composed of particles far back from the head of the comet, The motion of the tail remnant shows a loss of angular momentum during the passage through the solar corona. Atmospheric drag is estimated to account for a significant fraction of this change in angular momentum. but indications are that other mechanisms may be required to completely account for the total amount of change. (C) 2008 Elsevier Inc. All rights reserved. C1 NASA, Goddard Space Flight Ctr, Adnet Syst Inc, Greenbelt, MD 20771 USA. RP Thompson, WT (reprint author), NASA, Goddard Space Flight Ctr, Adnet Syst Inc, Code 671, Greenbelt, MD 20771 USA. EM William.T.Thompson@nasa.gov RI Thompson, William/D-7376-2012 FU NASA [NNG06EB68C] FX The author would like to thank Karl Battams for his many helpful comments, and to the anonymous reviewer who suggested the approach resulting in Eq. (4). This work was Supported by NASA grant NNG06EB68C. NR 16 TC 23 Z9 23 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 APR PY 2009 VL 200 IS 2 BP 351 EP 357 DI 10.1016/j.icarus.2008.12.011 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424NH UT WOS:000264572900001 ER PT J AU Williams, KE Toon, OB Heldmann, JL Mellon, MT AF Williams, K. E. Toon, O. B. Heldmann, J. L. Mellon, M. T. TI Ancient melting of mid-latitude snowpacks on Mars as a water source for gullies SO ICARUS LA English DT Article DE Ices; Mars, surface ID POTENTIAL FORMATION MECHANISMS; MARTIAN GULLIES; VALLEY FORMATION; SUMMIT SNOWPACK; CARBON-DIOXIDE; SURFACE RUNOFF; DEPOSITS; FEATURES; ORIGIN; CONSTRAINTS AB We hypothesize that during past epochs of high obliquity seasonal snowfields at mid-latitudes melted to produce springtime sediment-rich surface flows resulting in gully formation. Significant seasonal mid-latitude snowfall does not occur on Mars today. General Circulation Model (GCM) results, however, suggest that under past climate conditions there may have been centimeters of seasonal mid-latitude snowfall [Mischna, M.A., Richardson, M.I., Wilson, R.J., McCleese, D.J., 2003. J. Geophys. Res. Planets 108, doi:10.1029/2003JE002051. 5062). Gully locations have been tabulated by several researchers (e.g. [Heldmann, J.L., Mellon, M.T., 2004. Icarus 168, 285-304; Heldmann, J.L., Carlsson, E., johansson, H., Mellon, M.T., Toon, O.B., 2007. Icarus 188, 324-344; Malin, M.C., Edgett, K.S., 2000. Science 288, 233023351) and found to cot-respond to mid-latitude bands. A natural question is whether the latitudinal bands where the gullies are located correspond to areas where the ancient snowfalls may have melted, producing runoff which may have incised gullies. In this study we model thin snowpacks with thicknesses similar to those predicted by [Mischna, M.A., Richardson, M.I., Wilson, R.J., McCleese, D.J., 2003. J. Geophys. Res. Planets 108, doi:10.1029/2003JE002051. 50621. We model these snowpacks under past climate regimes in order to determine whether snowmelt runoff could have occurred, and whether significant amounts of warm soil (T > 273 K) existed on both poleward and equatorward slopes in the regions where gullies exist. Both warm soil and water amounts are modeled because soil and water may have mixed to form a sediment-rich flow. We begin by applying the snowpack model of Williams et al. [Williams, K.E., Toon, O.B., Heldmann, J.E., Mellon, M., 2008. Icarus 196, 565-5771 to past climate regimes characterized by obliquities of 35 degrees (600 ka before present) and 45 degrees (5.5 ma before present), and to all latitudes between 70 degrees N and 70 degrees S. We find that the regions containing significant snowmelt runoff correspond to the regions identified by Heldmann and Mellon [Heldmann, j.L., Mellon, M.T., 2004. Icarus 168, 285-304], Heldmann et al. [Heldmann, J.L, Carlsson, E., johansson, H., Mellon, M.T., Toon, O.B., 2007. Icarus 188, 324-344] and Malin and Edgett [Malin, M.C., Edgett, K.S., 2000. Science 288, 2330-2335] as containing large numbers of gullies. We find that the snowmelt runoff (>1 mm, with equivalent rainfall rates of 0.25 mm/h) and warm soil (>1 cm depth) would have occurred on slopes within the gullied latitudinal bands. The snowfall amounts modeled are predicted to be seasonal [Mischna, M.A., Richardson, M.I., Wilson, Rj., McCleese, D.J., 2003. J. Geophys. Res. Planets 108, doi: 10.1029/2003JE002051. 5062 1, and our modeling finds that under the previous climate regimes there would have been meltwater present on the slopes in question for brief periods of time, on the order of days, each year. Our model provides a simple explanation for the latitudinal distribution of the gullies, and also suggests that the gullies date to times when water migrated away from the present poles to the mid-latitudes. (C) 2008 Elsevier Inc. All rights reserved. C1 [Williams, K. E.; Toon, O. B.; Mellon, M. T.] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA. [Heldmann, J. L.] NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Moffett Field, CA 94035 USA. [Williams, K. E.; Mellon, M. T.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. RP Williams, KE (reprint author), NASA Ames, Mail Stop 245, Moffett Field, CA 94035 USA. EM kaj.e.williams@nasa.gov RI Mellon, Michael/C-3456-2016 NR 32 TC 54 Z9 54 U1 2 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 APR PY 2009 VL 200 IS 2 BP 418 EP 425 DI 10.1016/j.icarus.2008.12.013 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424NH UT WOS:000264572900007 ER PT J AU Janchen, J Morris, RV Bish, DL Janssen, M Hellwig, U AF Jaenchen, Jochen Morris, Richard V. Bish, David L. Janssen, Mareike Hellwig, Udo TI The H2O and CO2 adsorption properties of phyllosilicate-poor palagonitic dust and smectites under martian environmental conditions SO ICARUS LA English DT Article DE Mars, surface; Mineralogy ID MARS; INSTRUMENT; REGOLITH; MINERALS; ANALOG AB The recent detection of up to similar to 10 wt% water-equivalent H heterogeneously distributed in the upper meter of the equatorial regions of the martian surface and the presence of the 3-mu m hydrations feature across the entire planet raises the question whether martian surficial dust can account for this water-equivalent H. We have investigated the H2O and CO2 adsorption properties of palagonitic dust (<5 mu m size fraction of phyllosilicate-poor palagonitic tephra HWMK919) as a martian dust analog and two smectites under simulated martian equatorial surface conditions. Our results show that the palagonitic dust, which contains hydrated and hydroxylated volcanic glass of basaltic composition, accommodates significantly more H2O under comparable humidity and temperature conditions than do the smectites nontronite and montmorillonite. (C) 2008 Elsevier Inc. All rights reserved. C1 [Jaenchen, Jochen] ZeoSolar eV, TFH Wildau, D-12489 Berlin, Germany. [Jaenchen, Jochen; Janssen, Mareike; Hellwig, Udo] Univ Appl Sci, TFH Wildau, D-15745 Wildau, Germany. [Morris, Richard V.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Bish, David L.] Indiana Univ, Bloomington, IN 47405 USA. RP Janchen, J (reprint author), ZeoSolar eV, TFH Wildau, Volmerstr 13, D-12489 Berlin, Germany. EM j.e.jaenchen@t-online.de FU International Space Science Institute Bern, Switzerland; NASA Mars Fundamental Research Program; NASA Mars Exploration Rover Project; NASA Mars Reconnaissance Orbiter CRISM Program; NASA CRISM-OMEGA Collaboration; NASA Johnson Space Center FX Support by the International Space Science Institute Bern, Switzerland, is acknowledged. D.L.B. gratefully acknowledges support by the NASA Mars Fundamental Research Program. R.V.M. acknowledges support of the NASA Mars Exploration Rover Project, the NASA Mars Reconnaissance Orbiter CRISM Program, the NASA CRISM-OMEGA Collaboration, and the NASA Johnson Space Center. NR 21 TC 21 Z9 21 U1 0 U2 7 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD APR PY 2009 VL 200 IS 2 BP 463 EP 467 DI 10.1016/j.icarus.2008.12.006 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424NH UT WOS:000264572900011 ER PT J AU Cui, J Yelle, RV Vuitton, V Waite, JH Kasprzak, WT Gell, DA Niemann, HB Muller-Wodarg, ICF Borggren, N Fletcher, GG Patrick, EL Raaen, E Magee, BA AF Cui, J. Yelle, R. V. Vuitton, V. Waite, J. H., Jr. Kasprzak, W. T. Gell, D. A. Niemann, H. B. Mueller-Wodarg, I. C. F. Borggren, N. Fletcher, G. G. Patrick, E. L. Raaen, E. Magee, B. A. TI Analysis of Titan's neutral upper atmosphere from Cassini Ion Neutral Mass Spectrometer measurements SO ICARUS LA English DT Article DE Atmospheres, composition; Atmospheres, structure; Titan ID COUPLING PHOTOCHEMISTRY; VOYAGER-1 ENCOUNTER; HAZE FORMATION; IONOSPHERE; NITROGEN; MODEL; THERMOSPHERE; CHEMISTRY; HC3N; HCN AB In this paper we present all in-depth study of the distributions of various neutral species in Titan's upper atmosphere, between 950 and 1500 km for abundant species (N-2, CH4, H-2) and between 950 and 1200 km for other minor species. Our analysis is based on a large sample of Cassini/INMS (Ion Neutral Mass Spectrometer) measurements in the CSN (Closed Source Neutral) mode, obtained during 15 close flybys of Titan. To untangle the overlapping cracking patterns, we adopt singular Value Decomposition (SVD) to determine simultaneously the densities of different species. Except for N-2, CH4, H-2 and Ar-40 (as well as their isotopes), all species present density enhancements measured during the outbound legs. This can be interpreted as a result of wall effects, which Could be either adsorption/desorption of these molecules or heterogeneous surface chemistry of the associated radicals on the chamber walls. In this paper, we provide both direct inbound measurements assuming ram pressure enhancement only and abundances corrected for wall adsorption/desorption based on a simple model to reproduce the observed time behavior. Among all minor species of photochemical interest, we have firm detections of C2H2, C2H4. C2H6, CH3C2H, C4H2, C6H6, CH3CN, HC3N, C2N2 and NH3 in Titan's upper atmosphere. Upper limits are given for other minor species. The globally averaged distributions of N-2, CH4 and H-2 are each modeled with the diffusion approximation. The N-2 profile Suggests all average thermospheric temperature of 151 K. The CH4 and H-2 profiles constrain their fluxes to be 2.6 x 10(9) cm(2) s (1) and 1.1 x 10(10) cm (2) S (1), referred to Titan's surface. Both fluxes are significantly higher than the jeans escape values. The INMs data also suggest horizontal/diurnal variations of temperature and neutral gas distribution in Titan's thermosphere. The equatorial region, the ramside, as well as the nightside hemisphere of Titan appear to be warmer and present some evidence for the depletion of light species such as CH4. Meridional variations of some heavy species are also Observed, with a trend of depletion toward the north pole. Though some of the above variations might be interpreted by either the solar-driven models or auroral-driven models, a physical scenario that reconciles all the observed horizontal/diurnal variations in a consistent way is still missing. With a careful evaluation of the effect of restricted sampling, some of the features shown in the INMS data are more likely to be observational biases. (C) 2008 Elsevier Inc. All rights reserved. C1 [Cui, J.; Mueller-Wodarg, I. C. F.] Univ London Imperial Coll Sci Technol & Med, Space & Atmospher Phys Grp, London SW7 2BW, England. [Cui, J.; Yelle, R. V.; Borggren, N.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Vuitton, V.] Univ Grenoble 1, CNRS, Lab Planetol Grenoble, Grenoble 9, France. [Waite, J. H., Jr.; Gell, D. A.; Fletcher, G. G.; Magee, B. A.] SW Res Inst, San Antonio, TX 78228 USA. [Kasprzak, W. T.; Niemann, H. B.; Patrick, E. L.; Raaen, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Cui, J (reprint author), Univ London Imperial Coll Sci Technol & Med, Space & Atmospher Phys Grp, London SW7 2BW, England. EM jcui@imperial.ac.uk RI Mueller-Wodarg, Ingo/M-9945-2014 OI Mueller-Wodarg, Ingo/0000-0001-6308-7826 NR 66 TC 120 Z9 120 U1 2 U2 31 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 APR PY 2009 VL 200 IS 2 BP 581 EP 615 DI 10.1016/j.icarus.2008.12.005 PG 35 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424NH UT WOS:000264572900021 ER PT J AU Dodson-Robinson, SE Willacy, K Bodenheimer, P Turner, NJ Beichman, CA AF Dodson-Robinson, Sarah E. Willacy, Karen Bodenheimer, Peter Turner, Neal J. Beichman, Charles A. TI Ice lines, planetesimal composition and solid surface density in the solar nebula SO ICARUS LA English DT Article DE Solar nebula; Planetary formation; Ices ID TURBULENT PROTOPLANETARY DISKS; SPECTRAL ENERGY-DISTRIBUTIONS; MOLECULAR-HYDROGEN FORMATION; INTER-STELLAR CLOUDS; GAS-GRAIN CHEMISTRY; ACCRETION DISKS; GIANT PLANETS; INTERSTELLAR CLOUDS; T-TAURI; PROTOSTELLAR DISKS AB To date, there is no core accretion simulation that can Successfully account for the formation of Uranus or Neptune within the observed 2-3 Myr lifetimes of protoplanetary disks. Since solid accretion rate is directly proportional to the available planetesimal surface density, one way to speed up planet formation is to take a full accounting of all the planetesimal-forming solids present in the solar nebula. By combining a viscously evolving protostellar disk with a kinetic model of ice formation, which includes not just water but methane, ammonia, CO and 54 minor ices, we calculate the solid surface density of a possible giant planet-forming solar nebula as a function of heliocentric distance and time. Our results can be used to provide the starting planetesimal surface density and evolving solar nebula conditions for core accretion simulations, or to predict the composition of planetesimals as a function of radius. We find three effects that favor giant planet formation by the core accretion mechanism: (1) a decretion flow that brings mass from the inner solar nebula to the giant planet-forming region, (2) the fact that the ammonia and water ice lines should coincide, according to recent lab results from Collings et A [Collings, M.P., Anderson, M.A., Chen, R., Dever, J.W., Viti, S., Williams, D.A., McCoustra, M.R.S., 2004. Mon. Not. R. Astron. Soc. 354, 1133-1140], and (3) the presence of a substantial amount of methane ice in the trans-saturnian region. Our results show higher solid Surface densities than assumed in the core accretion models of Pollack et al. [Pollack, J.B., Hubickyj, O., Bodenheimer, P., Lissauer, J.J., Podolak, M., Greenzweig, Y., 1996. Icarus 124, 62-85] by a factor of 3-4 throughout the trans-saturnian region. We also discuss the location of ice lines and their movement through the solar nebula, and provide new constraints on the possible initial disk configurations from gravitational stability arguments. (c) 2008 Elsevier Inc. All rights reserved. C1 [Dodson-Robinson, Sarah E.; Beichman, Charles A.] CALTECH, NASA, Exoplaret Sci Inst, Pasadena, CA 91125 USA. [Willacy, Karen; Turner, Neal J.; Beichman, Charles A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bodenheimer, Peter] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Dodson-Robinson, SE (reprint author), CALTECH, NASA, Exoplaret Sci Inst, MC 100-22, Pasadena, CA 91125 USA. EM sdr@ipac.caltech.edu OI Turner, Neal/0000-0001-8292-1943 FU NSF Graduate Research Fellowship [AST-0507424]; College Scientists Foundation; JPL Research and Technology Development Program; NASA [NNX08AH82G]; Jet Propulsion Laboratory, California Institute of Technology; National Aeronautics and Space Administration FX We thank Julie Moses, Mark Marley and Doug Lin for helpful discussions about the project design. S.D.R. was supported by grants from the NSF Graduate Research Fellowship program and the Achievement Rewards for College Scientists Foundation. K.W. and N.T. were supported by the JPL Research and Technology Development Program. P.B. received funding from NSF Grant AST-0507424 and NASA Origins Grant NNX08AH82G. The work of K.W. and N.T. was carried out at the Jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautics and Space Administration, with funding provided by the JPL Research and Technology Development Program. NR 94 TC 54 Z9 54 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD APR PY 2009 VL 200 IS 2 BP 672 EP 693 DI 10.1016/j.icarus.2008.11.023 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424NH UT WOS:000264572900026 ER PT J AU Webster, J AF Webster, Jeffery TI The Auditors Are Coming: A Practical Guide for Engineering Projects SO IEEE AEROSPACE AND ELECTRONIC SYSTEMS MAGAZINE LA English DT Article AB When management informs you that internal or external auditors are on their way to conduct an audit of your project, you may have many questions and, at times, few answers: Why are the auditors coming? Why now? What are they looking for? How long will the audit take? What can we do to prepare? What help will the project receive in responding to the auditors? This presents a description of the typical audit process, a list of do's and don'ts for projects undergoing an audit, how to design basic audit preparations into the project's design, and resources for, further information on auditing issues. C1 CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Webster, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA USA. FU National Aeronautics and Space Administration FX The work described herein was performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 3 TC 0 Z9 0 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0885-8985 J9 IEEE AERO EL SYS MAG JI IEEE Aerosp. Electron. Syst. Mag. PD APR PY 2009 VL 24 IS 4 BP 9 EP 16 PG 8 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA 435WO UT WOS:000265374200003 ER PT J AU Jansma, PA AF Jansma, P. A. Trisha TI Got Software? What Managers and Engineers Need To Know SO IEEE AEROSPACE AND ELECTRONIC SYSTEMS MAGAZINE LA English DT Article AB As part of a JPL-wide software quality initiative aimed at addressing the challenges of developing, managing, and acquiring software, a team fit JPL generated a detailed Software Training Plan for both managers and engineers. The team took the approach of treating the software training program as though it were a system development task and went through all the typical phases of system development including requirements, design, and implementation. During the requirements collection phase, the team conducted dozens; of interviews and identified the specific skills needed. The skills fell into categories such as software management, software engineering, systems engineering, and other technical areas. However, an equally important finding was that several "soft" skills were deemed critical for the successful and timely management and implementation of software-intensive systems. This discusses JPL's approach and "lessons learned" from planning and delivering a software training program. in an engineering and scientific environment. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU National Aeronautics and Space Administration (NASA) FX The work described herein was performed at the Jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautics and Space Administration (NASA). Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not constitute or imply its endorsement by the United States Government, NASA, or the Jet Propulsion Laboratory, California Institute of Technology. NR 10 TC 0 Z9 0 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0885-8985 J9 IEEE AERO EL SYS MAG JI IEEE Aerosp. Electron. Syst. Mag. PD APR PY 2009 VL 24 IS 4 BP 25 EP 35 PG 11 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA 435WO UT WOS:000265374200005 ER PT J AU Acker, J Lyon, P Hoge, F Shen, S Roffer, M Gawlikowski, G AF Acker, James Lyon, Paul Hoge, Frank Shen, Suhung Roffer, Mitchell Gawlikowski, Greg TI Interaction of Hurricane Katrina With Optically Complex Water in the Gulf of Mexico: Interpretation Using Satellite-Derived Inherent Optical Properties and Chlorophyll Concentration SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Chlorophyll; dissolved organic matter; marine vegetation; optics; plankton; remote sensing; sea coast; sea surface ID UPPER OCEAN RESPONSE; DISSOLVED ORGANIC-MATTER; SOUTHERN STRAITS; MATRIX-INVERSION; RADIANCE MODEL; RETRIEVAL; RESUSPENSION; VARIABILITY; ABSORPTION; FLORIDA AB When Hurricane Katrina passed over southern Florida, Florida Bay and the West Florida Shelf, and into the Gulf of Mexico, empirically derived chl a increases were observed in the Tortugas Gyre circulation feature, and in adjacent waters. Analysis of the empirically derived chl a increase within the gyre has been primarily attributed to initiation of a phytoplankton bloom promoted by nutrients upwelled by Katrina's winds. Detailed analysis of inherent optical properties derived from remotely sensed radiances, however, indicated the interaction of Katrina with shallow coastal and shelf waters likely entrained waters with higher concentrations of chromophoric dissolved organic matter (CDOM) into the gyre circulation, augmenting the chl a signa. Storm-induced upwelling would also transport optically active CDOM to the surface. Increases in empirically derived chl a in the Florida coastal waters influenced by Katrina's winds were therefore partly due to increased absorption by CDOM. This analysis indicates that elevated empirically derived chl a in hurricane-influenced waters should not be unambiguously attributed to increased phytoplankton productivity, particularly in an optically complex coastal environment. C1 [Acker, James] NASA, Goddard Space Flight Ctr, Goddard Earth Sci Data & Informat Serv Ctr Wyle I, Greenbelt, MD 20771 USA. [Lyon, Paul] USN, Res Lab, Ocean Opt Sect 7333, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA. [Hoge, Frank] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Ocean Sci Branch,Hydrospher & Biospher Sci Lab, Wallops Isl, VA 23337 USA. [Shen, Suhung] George Mason Univ, Goddard Earth Sci Data & Informat Serv Ctr, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Roffer, Mitchell; Gawlikowski, Greg] Roffers Ocean Fishing Forecasting Serv Inc, Miami, FL 33155 USA. RP Acker, J (reprint author), NASA, Goddard Space Flight Ctr, Goddard Earth Sci Data & Informat Serv Ctr Wyle I, Greenbelt, MD 20771 USA. EM jim.acker@nasa.gov NR 32 TC 9 Z9 9 U1 1 U2 25 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1545-598X EI 1558-0571 J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD APR PY 2009 VL 6 IS 2 BP 209 EP 213 DI 10.1109/LGRS.2008.2007658 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 435XG UT WOS:000265376000007 ER PT J AU Dinnat, EP Abraham, S Le Vine, DM de Matthaeis, P Jacob, D AF Dinnat, Emmanuel Philippe Abraham, Saji Le Vine, David M. de Matthaeis, Paolo Jacob, Daniel TI Effect of Emission From the Moon on Remote Sensing of Sea Surface Salinity: An Example With the Aquarius Radiometer SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Microwave remote sensing; ocean salinity; radiation from Moon ID L-BAND; SPACE; RADIATION; MISSION; WAVES; RADAR AB This letter describes the effect of thermal emission from the Moon on remote sensing of sea surface salinity from space. In most cases, radiation from the Moon is negligible; however, at several times during the lunar cycle, it is possible for radiation to be reflected from the Earth's surface into the main beam of the radiometer antennas. The signal in such cases can be important because of the high radiometric accuracy required to monitor salinity. Examples are presented using the Aquarius orbit and antennas for both smooth and rough ocean surfaces. C1 [Dinnat, Emmanuel Philippe; de Matthaeis, Paolo; Jacob, Daniel] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Abraham, Saji; Le Vine, David M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Dinnat, EP (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. EM David.M.Levine@nasa.gov RI Dinnat, Emmanuel/D-7064-2012 OI Dinnat, Emmanuel/0000-0001-9003-1182 NR 21 TC 3 Z9 3 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1545-598X J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD APR PY 2009 VL 6 IS 2 BP 239 EP 243 DI 10.1109/LGRS.2008.2008822 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 435XG UT WOS:000265376000013 ER PT J AU Karam, LJ Ebrahimi, T Hemami, SS Pappas, TN Safranek, RJ Wang, Z Watson, AB AF Karam, Lina J. Ebrahimi, Touradj Hemami, Sheila S. Pappas, Thrasyvoulos N. Safranek, Robert J. Wang, Zhou Watson, Andrew B. TI Introduction to the Issue on Visual Media Quality Assessment SO IEEE JOURNAL OF SELECTED TOPICS IN SIGNAL PROCESSING LA English DT Editorial Material C1 [Karam, Lina J.] Arizona State Univ, Tempe, AZ 85287 USA. [Ebrahimi, Touradj] LTSI, ITS, STI, EPFL, CH-1015 Lausanne, Switzerland. [Ebrahimi, Touradj] Q2S NTNU, N-7034 Trondheim, Norway. [Hemami, Sheila S.] Cornell Univ, Ithaca, NY 14853 USA. [Pappas, Thrasyvoulos N.] Northwestern Univ, Evanston, IL 60208 USA. [Safranek, Robert J.] Benevue Inc, Warren, NJ 07059 USA. [Wang, Zhou] Univ Waterloo, Waterloo, ON N2L 3G1, Canada. [Watson, Andrew B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Karam, LJ (reprint author), Arizona State Univ, Tempe, AZ 85287 USA. RI Pappas, Thrasyvoulos/B-7261-2009; Pappas, Thrasyvoulos/D-5054-2013 NR 0 TC 22 Z9 22 U1 0 U2 7 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1932-4553 J9 IEEE J-STSP JI IEEE J. Sel. Top. Signal Process. PD APR PY 2009 VL 3 IS 2 BP 189 EP 192 DI 10.1109/JSTSP.2009.2015485 PG 4 WC Engineering, Electrical & Electronic SC Engineering GA 439TH UT WOS:000265649400001 ER PT J AU Siegel, PH AF Siegel, Peter H. TI Sir Jagadis Chunder Bose: Traversing the Interdisciplinary Gap Between Physics and Biology SO IEEE MICROWAVE MAGAZINE LA English DT Biographical-Item C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Siegel, PH (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 1 TC 1 Z9 1 U1 1 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1527-3342 J9 IEEE MICROW MAG JI IEEE Microw. Mag. PD APR PY 2009 VL 10 IS 2 BP 119 EP 121 DI 10.1109/MMM.2009.932241 PG 3 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 420MJ UT WOS:000264293600015 ER PT J AU Kennedy, TF Fink, PW Chu, AW Champagne, NJ Lin, GY Khayat, MA AF Kennedy, Timothy F. Fink, Patrick W. Chu, Andrew W. Champagne, Nathan J., II Lin, Gregory Y. Khayat, Michael A. TI Body-Worn E-Textile Antennas: The Good, the Low-Mass, and the Conformal SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION LA English DT Article DE Antenna arrays; beamforming; conformal antennas; diversity methods; e-textile antennas ID 2.45 GHZ AB Support of ever increasing applications for wireless data and communications on a body-centric platform requires novel antenna systems that can be integrated with the body-worn environment, while maintaining free-range of movement and minimal mass impact. E-textile antennas show great promise due to their ease of integration with other textile materials, and they are inherently low-mass and flexible relative to conventional antenna materials. Much attention has been given recently to multiple-antenna communication systems due to the increased performance compared to conventional single-antenna systems. For body-centric applications, the low-mass, flexibility, and integration simplicity of e-textile antennas can enable multiple-antenna systems, which otherwise would be precluded by the rigidity and mass of conventional antenna materials. Several examples of this are considered here with e-textile antennas in an array environment. A conventional microstrip array constructed with e-textiles is shown to have robust performance with moderate amounts of bending, similar to that which might be seen with body-worn arrays. In addition to the conventional array, a wide-band multiple-antenna system to support a variety of wireless communication protocols, while maintaining polarization diversity and excellent coverage over a majority of the radian sphere is demonstrated. C1 [Kennedy, Timothy F.; Fink, Patrick W.; Chu, Andrew W.; Champagne, Nathan J., II; Lin, Gregory Y.; Khayat, Michael A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Kennedy, TF (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM timothy.f.kennedy@nasa.gov NR 29 TC 72 Z9 73 U1 1 U2 17 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-926X J9 IEEE T ANTENN PROPAG JI IEEE Trans. Antennas Propag. PD APR PY 2009 VL 57 IS 4 BP 910 EP 918 DI 10.1109/TAP.2009.2014602 PG 9 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 436TC UT WOS:000265438000010 ER PT J AU Pan, B Li, Y Ponchak, GE Papapolymerou, J Tentzeris, MM AF Pan, Bo Li, Yuan Ponchak, George E. Papapolymerou, John Tentzeris, Manos M. TI A 60-GHz CPW-Fed High-Gain and Broadband Integrated Horn Antenna SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION LA English DT Article DE Coplanar waveguide; integrated horn; micromachining; millimeter wave; V-band ID SUBMILLIMETER-WAVE APPLICATIONS; MILLIMETER-WAVE; FRONT-END; GUIDE; GHZ AB An integrated horn antenna is presented for 60-GHz WPAN applications. Compared with other types of antenna for 60-GHz WPAN applications, an integrated horn antenna features wide bandwidth and high gain. This integrated H-plane horn is elevated on the top of the substrate using CMOS-compatible microfabrication steps. Antenna efficiency is greatly improved after eliminating dielectric loss. This antenna is excited using an integrated vertical current probe connected with a coplanar-wave-guide (CPW) by surface micromachining technologies. The lower part of the horn is constructed by rows of metallized pillars. The upper part and the top wall are built by stacking two layers of micromachined silicon wafers. The horn bottom is formed by metalizing the substrate's top surface. A prototype antenna is designed, fabricated, and characterized. Simulation and measurement results have shown wide input matching bandwidth and radiation bandwidth. The measured radiation pattern agrees well with the simulated one, demonstrating a gain as high as 14.6 dBi. C1 [Li, Yuan; Papapolymerou, John; Tentzeris, Manos M.] Georgia Inst Technol, GEDC, Atlanta, GA 30332 USA. [Ponchak, George E.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Pan, B (reprint author), Wion Res, Realtek Semicond, Irvine, CA 92618 USA. EM bo.pan@ieee.org; papapol@ece.gatech.edu NR 23 TC 46 Z9 46 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-926X J9 IEEE T ANTENN PROPAG JI IEEE Trans. Antennas Propag. PD APR PY 2009 VL 57 IS 4 BP 1050 EP 1056 DI 10.1109/TAP.2009.2015815 PG 7 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 463BU UT WOS:000267404200005 ER PT J AU Kerola, DX Bruegge, CJ Gross, HN Helmlinger, MC AF Kerola, Dana Xavier Bruegge, Carol J. Gross, Harry N. Helmlinger, Mark C. TI On-Orbit Calibration of the EO-1 Hyperion and Advanced Land Imager (ALI) Sensors Using the LED Spectrometer (LSpec) Automated Facility SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Atmospheric measurements; calibration; remote sensing ID ANGLE IMAGING SPECTRORADIOMETER; MISR AB Vicarious calibration (VC) technology, developed in the mid-1980s, has been employed to establish the absolute radiometric calibration of Earth-viewing sensors aboard satellites and aircraft. This method has heretofore required special visits by a field team to collect surface and atmospheric measurements, at specific times necessarily coincident with a sensor overflight. With the recent creation of an autonomous calibration facility, VC data can now be made available to the sensor community without the need for each research group to deploy its own field team. Beginning in mid-November 2006, there have been ongoing efforts to expand the data processing capabilities of the Jet Propulsion Laboratory-operated LED Spectrometer (LSpec) automatic facility, which has been making continual measurements of surface reflectances and atmospheric transmittances since that time. The facility is located at Frenchman Flat, within the Nevada Test Site. Data are used to support the VC of sensors which make observations at visible and near-infrared wavelengths. An array of eight LSpecs performs the autonomous function of recording surface reflectances at 5-min intervals, thereby permitting accurate and continual real-time adjustments to high-resolution Analytical Spectral Devices spectrometer measurements, acquired every several months during on-site visits. Moreover, resident at the LSpec site is a Cimel sunphotometer, used to make atmospheric transmittance measurements. The Cimel is part of the Aerosol Robotic Network (AERONET). Measurements made by the LSpec Cimel are used by AERONET to derive values of aerosol optical depths. From continuous in situ measurement of spectral reflectance of the playa surface, along with acquired aerosol optical depths and ozone optical depths (obtained from the Ozone Mapping Instrument), an LSpec database is being produced and is available via a web-based interface. To highlight the viability of making use of LSpec-derived data, we have executed a few distinct multiple scattering radiative transfer codes in order to perform VCs of the Earth Observing-1 (EO-1) Hyperion and EO-1 Advanced Land Imager sensors. C1 [Kerola, Dana Xavier] Skillstorm Govt Integrated Serv, Pasadena, CA 91107 USA. [Bruegge, Carol J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gross, Harry N.] Integrity Applicat Inc, Chantilly, VA 20151 USA. [Helmlinger, Mark C.] Northrop Grumman Space Technol, Redondo Beach, CA 90278 USA. RP Kerola, DX (reprint author), Skillstorm Govt Integrated Serv, Pasadena, CA 91107 USA. EM Dina.X.Kerola@Jpl.Nasa.Gov; Carol.J.Bruegge@Jpl.Nasa.Gov; hgross@integrity-apps.com; Mark.Helmlinger@ngc.com NR 13 TC 15 Z9 17 U1 1 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD APR PY 2009 VL 47 IS 4 BP 1244 EP 1255 DI 10.1109/TGRS.2008.2008904 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 425IM UT WOS:000264630200024 ER PT J AU Wolff, R Bhaduri, K Kargupta, H AF Wolff, Ran Bhaduri, Kanishka Kargupta, Hillol TI A Generic Local Algorithm for Mining Data Streams in Large Distributed Systems SO IEEE TRANSACTIONS ON KNOWLEDGE AND DATA ENGINEERING LA English DT Article DE Distributed data mining; peer-to-peer; local algorithms AB In a large network of computers or wireless sensors, each of the components (henceforth, peers) has some data about the global state of the system. Much of the system's functionality such as message routing, information retrieval, and load sharing relies on modeling the global state. We refer to the outcome of the function (e. g., the load experienced by each peer) as the model of the system. Since the state of the system is constantly changing, it is necessary to keep the models up to date. Computing global data mining models, e. g., decision trees, k-means clustering in large distributed systems may be very costly due to the scale of the system and due to communication cost, which may be high. The cost further increases in a dynamic scenario when the data changes rapidly. In this paper, we describe a two-step approach for dealing with these costs. First, we describe a highly efficient local algorithm that can be used to monitor a wide class of data mining models. Then, we use this algorithm as a feedback loop for the monitoring of complex functions of the data such as its k-means clustering. The theoretical claims are corroborated with a thorough experimental analysis. C1 [Wolff, Ran] Univ Haifa, Dept Management Informat Syst, IL-31905 Haifa, Israel. [Bhaduri, Kanishka] NASA, Ames Res Ctr, Mission Crit Technol Inc, IDU Grp, Moffett Field, CA 94035 USA. [Kargupta, Hillol] Univ Maryland, Dept Comp Sci & Elect Engn, Baltimore, MD 21250 USA. [Kargupta, Hillol] AGNIK LLC, Columbia, MD 21045 USA. RP Wolff, R (reprint author), Univ Haifa, Dept Management Informat Syst, IL-31905 Haifa, Israel. EM rwolff@mis.haifa.il; kbhaduri@mail.arc.nasa.gov; hillol@cs.umbc.edu FU US National Science Foundation CAREER Award [IIS-0093353]; NASA [NNX07AV70G] FX A preliminary version of this work was published in the Proceedings of the 2006 SIAM Data Mining Conference (SDM '06). This work was done when Kanishka Bhaduri was at UMBC. This research was supported by the US National Science Foundation CAREER Award IIS-0093353 and NASA Grant NNX07AV70G. NR 25 TC 17 Z9 18 U1 0 U2 10 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA SN 1041-4347 EI 1558-2191 J9 IEEE T KNOWL DATA EN JI IEEE Trans. Knowl. Data Eng. PD APR PY 2009 VL 21 IS 4 BP 465 EP 478 DI 10.1109/TKDE.2008.169 PG 14 WC Computer Science, Artificial Intelligence; Computer Science, Information Systems; Engineering, Electrical & Electronic SC Computer Science; Engineering GA 407WG UT WOS:000263394400001 ER PT J AU Berg, MD Label, KA Kim, H Friendlich, M Phan, A Perez, C AF Berg, Melanie D. LaBel, Kenneth A. Kim, Hak Friendlich, Mark Phan, Anthony Perez, Christopher TI A Comprehensive Methodology for Complex Field Programmable Gate Array Single Event Effects Test and Evaluation SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article DE Evaluation; FPGA; scrubbing; Triple Mode Redundancy (TMR) AB A methodology for evaluating various types of FPGAs targeted for space missions is presented. The premise is to supply unambiguous SEE information so that flight-projects may insert the optimal device for their application. C1 [Berg, Melanie D.; LaBel, Kenneth A.; Kim, Hak; Friendlich, Mark; Phan, Anthony; Perez, Christopher] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kim, Hak; Friendlich, Mark; Phan, Anthony; Perez, Christopher] MEI Technol, Lanham, MD 20706 USA. RP Berg, MD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM mdberg@pop500.gsfc.nasa.gov; kenneth.a.label@nasa.gov; hak.s.kim@nasa.gov; mark.r.friendlich@nasa.gov; anthony.m.phan@nasa.gov; christopher.e.perez@nasa.gov NR 16 TC 9 Z9 9 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD APR PY 2009 VL 56 IS 2 BP 366 EP 374 DI 10.1109/TNS.2009.2013857 PG 9 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 435WZ UT WOS:000265375300001 ER PT J AU Sanmartin, JR Charro, M Lorenzini, EC Garrett, HB Bombardelli, C Bramanti, C AF Sanmartin, Juan R. Charro, Mario Lorenzini, Enrico C. Garrett, Henry B. Bombardelli, Claudio Bramanti, Cristina TI Electrodynamic Tether at Jupiter-II: Fast Moon Tour After Capture SO IEEE TRANSACTIONS ON PLASMA SCIENCE LA English DT Article DE Electrodynamic bare tether; Jovian mission design; planetary exploration; propellantless space propulsion and power AB An electrodynamic bare-tether mission to Jupiter, following the capture of a spacecraft (SC) into an equatorial highly elliptical orbit with perijove at about 1.3 times the Jovian radius, is discussed. Repeated applications of the propellantless Lorentz drag on a spinning tether, at the perijove vicinity, can progressively lower the apojove at constant perijove, for a tour of Galilean moons. Electrical energy is generated and stored as the SC moves from an orbit at 1: 1 resonance with a moon, down to resonance with the next moon; switching tether current off, stored power is then used as the SC makes a number of flybys of each moon. Radiation dose is calculated throughout the mission, during capture, flybys and moves between moons. The tour mission is limited by both power needs and accumulated dose. The three-stage apojove lowering down to Ganymede, Io, and Europa resonances would total less than 14 weeks, while 4 Ganymede, 20 Europa, and 16 Io flybys would add up to 18 weeks, with the entire mission taking just over seven months and the accumulated radiation dose keeping under 3 Mrad (Si) at 10-mm Al shield thickness. C1 [Sanmartin, Juan R.; Charro, Mario] Univ Politecn Madrid, Dept Appl Phys, Sch Aeronaut Engn, E-28040 Madrid, Spain. [Lorenzini, Enrico C.] Univ Padua, Dept Mech Engn, I-35100 Padua, Italy. [Garrett, Henry B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bombardelli, Claudio; Bramanti, Cristina] European Space Agcy, Adv Concepts Team, European Space Res & Technol Ctr, NL-2200 AG Noordwijk, Netherlands. RP Sanmartin, JR (reprint author), Univ Politecn Madrid, Dept Appl Phys, Sch Aeronaut Engn, E-28040 Madrid, Spain. EM juanr.sanmartin@upm.es; mario.charro@upm.es; enrico.lorenzini@unipd.it FU European Space Agency [19696/06]; Spanish Ministry of Science and Technology [ESP2004-0151] FX The works of J. R. Sanmartin and M. Charro were supported in part by the European Space Agency under Contract 19696/06 and by the Spanish Ministry of Science and Technology under Grant ESP2004-0151 NR 10 TC 13 Z9 13 U1 1 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0093-3813 EI 1939-9375 J9 IEEE T PLASMA SCI JI IEEE Trans. Plasma Sci. PD APR PY 2009 VL 37 IS 4 BP 620 EP 626 DI 10.1109/TPS.2009.2013955 PN 2 PG 7 WC Physics, Fluids & Plasmas SC Physics GA 435XK UT WOS:000265376400013 ER PT J AU Mourikis, AI Trawny, N Roumeliotis, SI Johnson, AE Ansar, A Matthies, L AF Mourikis, Anastasios I. Trawny, Nikolas Roumeliotis, Stergios I. Johnson, Andrew E. Ansar, Adrian Matthies, Larry TI Vision-Aided Inertial Navigation for Spacecraft Entry, Descent, and Landing SO IEEE TRANSACTIONS ON ROBOTICS LA English DT Article; Proceedings Paper CT Conference on Robotics - Science and Systems CY JUN 26-30, 2007 CL Atlanta, GA DE Descent and landing (EDL); entry; localization; sensor fusion; space robotics; vision-aided inertial navigation ID POSE ESTIMATION AB In this paper, we present the vision-aided inertial navigation (VISINAV) algorithm that enables precision planetary landing. The vision front-end of the VISINAV system extracts 2-D-to-3-D correspondences between descent images and a surface map (mapped landmarks), as well as 2-D-to-2-D feature tracks through a sequence of descent images (opportunistic features). An extended Kalman filter (EKF) tightly integrates both types of visual feature observations with measurements from an inertial measurement unit. The filter computes accurate estimates of the lander's terrain-relative position, attitude, and velocity, in a resource-adaptive and hence real-time capable fashion. In addition to the technical analysis of the algorithm, the paper presents validation results from a sounding-rocket test flight, showing estimation errors of only 0.16 m/s for velocity and 6.4 m for position at touchdown. These results vastly improve current state of the art for terminal descent navigation without visual updates, and meet the requirements of future planetary exploration missions. C1 [Mourikis, Anastasios I.] Univ Calif Riverside, Dept Elect Engn, Riverside, CA 92521 USA. [Trawny, Nikolas; Roumeliotis, Stergios I.] Univ Minnesota, Dept Comp Sci & Engn, Minneapolis, MN 55455 USA. [Johnson, Andrew E.; Ansar, Adrian; Matthies, Larry] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Mourikis, AI (reprint author), Univ Calif Riverside, Dept Elect Engn, Riverside, CA 92521 USA. EM mourikis@ee.ucr.edu; trawny@cs.umn.edu; stergios@cs.umn.edu; aej@jpl.nasa.gov; ansar@jpl.nasa.gov; lhm@jpl.nasa.gov NR 48 TC 99 Z9 110 U1 3 U2 28 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1552-3098 EI 1941-0468 J9 IEEE T ROBOT JI IEEE Trans. Robot. PD APR PY 2009 VL 25 IS 2 BP 264 EP 280 DI 10.1109/TRO.2008.2012342 PG 17 WC Robotics SC Robotics GA 435WA UT WOS:000265372800005 ER PT J AU Vasavada, S Sun, X Ishii, M Duval, W AF Vasavada, S. Sun, X. Ishii, M. Duval, W. TI Benchmarking of the one-dimensional one-group interfacial area transport equation for reduced-gravity bubbly flows SO INTERNATIONAL JOURNAL OF MULTIPHASE FLOW LA English DT Article DE Liquid-liquid flow; Reduced gravity; Interfacial area; Coalescence; Disintegration; Two-phase flow ID BUOYANCY-DRIVEN MOTION; GAS-LIQUID FLOW; 2-PHASE FLOW; MICROGRAVITY CONDITIONS; QUIESCENT LIQUID; VOID FRACTION; SLUG FLOW; COALESCENCE; VELOCITY; MODEL AB In order to properly design and safely operate two-phase flow systems, especially those deployed on future space missions, it is necessary to have accurate predictive capabilities. The application of a novel predictive method, the interfacial area transport equation (IATE), to dynamically predict the change of interfacial area concentration for reduced-gravity two-phase flows is described in this paper. Fluid particle interaction mechanisms such as coalescence and breakup that are present in reduced-gravity two-phase flows have been studied experimentally as reported in a previous paper by the current authors [Vasavada et al., 2007]. These mechanisms represent the source and sink terms in the IATE and their mechanistic models are benchmarked using experimental data obtained in a 25 mm inner diameter ground-based test section wherein reduced-gravity conditions were simulated. The comparison of the predictions from the model against experimental data shows good agreement. It has been found that, in contrast to the hypothesis extended in the literature, the wake entrainment based coalescence mechanism is present in reduced-gravity two-phase flows and in some cases is more important than coalescence due to random collision. Physics based arguments are extended to support this conclusion. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Vasavada, S.; Ishii, M.] Purdue Univ, Sch Nucl Engn, W Lafayette, IN 47907 USA. [Sun, X.] Ohio State Univ, Dept Mech Engn, Columbus, OH 43210 USA. [Duval, W.] NASA, Glenn Res Ctr, Fluid Phys & Transport Branch, Cleveland, OH 44135 USA. RP Vasavada, S (reprint author), Energy Res Inc, 6189 Execut Blvd, Rockville, MD 20852 USA. EM vasavad@purdue.edu; sxv@eri-world.com; ishii@purdue.edu; Walter.M.Duval@grc.nasa.gov RI Sun, Xiaodong/F-3752-2015 OI Sun, Xiaodong/0000-0002-9852-160X FU National Aeronautics and Space Administration (NASA); Office of Biological and Physical Research [NNC04GA26G]; NASA Glenn Research Center, Cleveland, OH; En'urga Inc.; West Lafayette, IN FX This work was supported by the National Aeronautics and Space Administration (NASA), Office of Biological and Physical Research under grant NNC04GA26G administered by the NASA Glenn Research Center, Cleveland, OH. The authors thank Dr. Fran Chiaramonte of the NASA Glenn Reserach Center for his support of this work. The authors also acknowledge Dr. Y. Mi of En'urga Inc., West Lafayette, IN for his help with the instrumentation. NR 43 TC 4 Z9 4 U1 0 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0301-9322 J9 INT J MULTIPHAS FLOW JI Int. J. Multiph. Flow PD APR PY 2009 VL 35 IS 4 BP 323 EP 334 DI 10.1016/j.ijmultiphaseflow.2009.01.006 PG 12 WC Mechanics SC Mechanics GA 435DH UT WOS:000265323400003 ER PT J AU Gaidos, E Marteinsson, V Thorsteinsson, T Johannesson, T Runarsson, AR Stefansson, A Glazer, B Lanoil, B Skidmore, M Han, S Miller, M Rusch, A Foo, W AF Gaidos, Eric Marteinsson, Viggo Thorsteinsson, Thorsteinn Johannesson, Tomas Runarsson, Arni Rafn Stefansson, Andri Glazer, Brian Lanoil, Brian Skidmore, Mark Han, Sukkyun Miller, Mary Rusch, Antje Foo, Wilson TI An oligarchic microbial assemblage in the anoxic bottom waters of a volcanic subglacial lake SO ISME JOURNAL LA English DT Article DE acetogenesis; anoxia; extreme environments; microbial diversity; psychrophily; sulfide oxidation ID RIBOSOMAL-RNA SEQUENCES; SP-NOV.; OLIGONUCLEOTIDE PROBES; GEN. NOV.; PHYLOGENETIC ANALYSIS; SULFATE REDUCTION; ONLINE RESOURCE; COMB. NOV; DEEP-SEA; COMMUNITY AB In 2006, we sampled the anoxic bottom waters of a volcanic lake beneath the Vatnajokull ice cap (Iceland). The sample contained 5 x 10(5) cells per ml, and whole-cell fluorescent in situ hybridization (FISH) and PCR with domain-specific probes showed these to be essentially all bacteria, with no detectable archaea. Pyrosequencing of the V6 hypervariable region of the 16S ribosomal RNA gene, Sanger sequencing of a clone library and FISH-based enumeration of four major phylotypes revealed that the assemblage was dominated by a few groups of putative chemotrophic bacteria whose closest cultivated relatives use sulfide, sulfur or hydrogen as electron donors, and oxygen, sulfate or CO(2) as electron acceptors. Hundreds of other phylotypes are present at lower abundance in our V6 tag libraries and a rarefaction analysis indicates that sampling did not reach saturation, but FISH data limit the remaining biome to < 10-20% of all cells. The composition of this oligarchy can be understood in the context of the chemical disequilibrium created by the mixing of sulfidic lake water and oxygenated glacial meltwater. C1 [Gaidos, Eric; Rusch, Antje] Univ Hawaii Manoa, Dept Geol & Geophys, Honolulu, HI 96822 USA. [Gaidos, Eric] NASA, Astrobiol Inst, Mountain View, CA USA. [Marteinsson, Viggo; Runarsson, Arni Rafn] MATIS Prokaria, Reykjavik, Iceland. [Thorsteinsson, Thorsteinn] Natl Energy Author, Hydrol Serv, Reykjavik, Iceland. [Johannesson, Tomas] Iceland Meteorol Off, Reykjavik, Iceland. [Stefansson, Andri] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Glazer, Brian] Univ Hawaii, Dept Oceanog, Honolulu, HI 96822 USA. [Lanoil, Brian; Han, Sukkyun; Foo, Wilson] Univ Calif Riverside, Dept Environm Sci, Riverside, CA 92521 USA. [Skidmore, Mark] Montana State Univ, Dept Earth Sci, Bozeman, MT 59717 USA. [Miller, Mary] Univ Texas Med Branch, Dept Microbiol & Immunol, Galveston, TX USA. RP Gaidos, E (reprint author), Univ Hawaii Manoa, Dept Geol & Geophys, 1680 East West Rd, Honolulu, HI 96822 USA. EM gaidos@hawaii.edu RI Glazer, Brian/C-2248-2011; OI Rusch, Antje/0000-0001-8686-9433; Lanoil, Brian/0000-0001-8603-8330 FU National Aeronautics and Space Administration [NNA04CC08A]; Icelandic Centre for Research FX This material is based upon work supported by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under Cooperative Agreement no. NNA04CC08A issued through the Office of Space Science and by the Icelandic Centre for Research. The Icelandic National Energy Authority, National Power Company and Public Roads Administration provided logistical support. Members of the Icelandic Glaciological Society assisted in the field campaign on Vatnajokull. The NAI lead team at the Marine Biological Laboratory performed pyrosequencing, and Mitch Sogin, Hilary Morrison and Sue Huse assisted with procedures and analysis. Ruth Richardson provided an enrichment culture for FISH. Brian Popp and Terri Rust measured POM. NR 70 TC 22 Z9 23 U1 1 U2 24 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1751-7362 J9 ISME J JI ISME J. PD APR PY 2009 VL 3 IS 4 BP 486 EP 497 DI 10.1038/ismej.2008.124 PG 12 WC Ecology; Microbiology SC Environmental Sciences & Ecology; Microbiology GA 427LP UT WOS:000264781100010 PM 19092861 ER PT J AU Fleurial, JP AF Fleurial, Jean-Pierre TI Thermoelectric Power Generation Materials: Technology and Application Opportunities SO JOM LA English DT Article ID THERMAL-CONDUCTIVITY; EFFICIENCY; DEVICES; ALLOYS AB Thermoelectric power sources have consistently demonstrated their extraordinary reliability and longevity for deep space missions (67 missions to date, more than 30 years of life) as well as terrestrial applications where unattended operation in remote locations is required. The development of new, more efficient materials and devices is the key to improving existing space power technology and expanding the range of terrestrial applications. The NASA Jet Propulsion Laboratory is leading collaborative research and development on novel advanced bulk materials capable of long-term operation at temperatures up to 1,300 K at more than 20% conversion efficiency. The research areas include refractory rare earth compounds and bulk three-dimensional nanostructures that emulate results obtained on low dimensional superlattices through "force engineering" and "self-assembling" techniques. Recent experimental results will be highlighted, and progress in transitioning thermoelectric technology to a more flexible, lower-cost modular array configuration suitable for various application opportunities will be discussed. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Fleurial, JP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 277-207, Pasadena, CA 91109 USA. EM jean-pierre.fleurial@jpl.nasa.gov NR 29 TC 34 Z9 34 U1 5 U2 26 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1047-4838 EI 1543-1851 J9 JOM-US JI JOM PD APR PY 2009 VL 61 IS 4 BP 79 EP 85 PG 7 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering; Mineralogy; Mining & Mineral Processing SC Materials Science; Metallurgy & Metallurgical Engineering; Mineralogy; Mining & Mineral Processing GA 445GK UT WOS:000266038200014 ER PT J AU Dresselhaus, MS Chen, G Ren, ZF Dresselhaus, G Henry, A Fleurial, JP AF Dresselhaus, M. S. Chen, G. Ren, Z. F. Dresselhaus, G. Henry, A. Fleurial, J. -P. TI New Composite Thermoelectric Materials for Energy Harvesting Applications SO JOM LA English DT Article ID BULK ALLOYS; PERFORMANCE; FIGURE; MERIT AB The concept of using nanostructured composite materials to enhance the dimensionless thermoelectric figure of merit ZT relative to that for their counterpart homogeneous alloyed bulk crystalline materials of similar chemical composition is presented in general terms. Specific applications are made to the Si-Ge and Bi (2-x)Sb(x)Te(3) systems for use in high-temperature power generation and cooling applications. The scientific advantages of the nanocomposite approach for the simultaneous increase in the power factor and decrease in the thermal conductivity are emphasized insofar as their simultaneous occurrence is enabled by the independent control of these physical properties through the special properties of their nanostructures. Also emphasized are the practical advantages of using such bulk samples both for thermoelectric property measurements and for providing a straightforward path to scaling up the materials synthesis and integration of such nanostructured materials into practical thermoelectric power-generation and cooling modules and devices. C1 [Dresselhaus, M. S.; Chen, G.; Dresselhaus, G.; Henry, A.] MIT, Cambridge, MA 02139 USA. [Ren, Z. F.] Boston Coll, Chestnut Hill, MA 02467 USA. [Fleurial, J. -P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Dresselhaus, MS (reprint author), MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM millie@mgm.mit.edu RI Ren, Zhifeng/B-4275-2014; Chen, Gang/J-1325-2014 OI Chen, Gang/0000-0002-3968-8530 FU U.S. Department of Energy [DE-FG02-08ER46516] FX The authors gratefully acknowledge the assistance of Mario Hofmann for help with the preparation of the figures. MSD, GC, and ZR acknowledge support for this work under U.S. Department of Energy BES Grant DE-FG02-08ER46516. Part of this work was performed at the Jet Propulsion Laboratory/California Institute of Technology under contract with NASA. NR 15 TC 29 Z9 29 U1 4 U2 38 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1047-4838 J9 JOM-US JI JOM PD APR PY 2009 VL 61 IS 4 BP 86 EP 90 PG 5 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering; Mineralogy; Mining & Mineral Processing SC Materials Science; Metallurgy & Metallurgical Engineering; Mineralogy; Mining & Mineral Processing GA 445GK UT WOS:000266038200015 ER PT J AU Miele, A Ciarcia, M Weeks, MW AF Miele, A. Ciarcia, M. Weeks, M. W. TI Rendezvous Guidance Trajectories via Multiple-Subarc Sequential Gradient-Restoration Algorithm SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Article AB We consider the three-dimensional rendezvous between a target spacecraft in a circular orbit and a chaser spacecraft with an initial separation distance and an initial separation velocity. We assume that the chaser spacecraft has variable mass and that its trajectory is governed by three controls, one determining the thrust magnitude and two determining the thrust direction. We employ the Clohessy-Wiltshire equations, describing the relative motion of the chaser vis-a-vis the target, and the multiple-subarc sequential gradient-restoration algorithm to produce first optimal trajectories and then guidance trajectories for the following problems: P1-minimum time, fuel free; P2-minimum fuel, time free; P3-minimum time, fuel given; P4-minimum fuel, time given; and P5-minimum timexfuel, time and fuel free. Clearly, P1 and P2 are basic problems, while P3, P4, and P5 are compromise problems. Problem P1 leads to a two-subarc solution including a max-thrust subarc followed by another max-thrust subarc. Problem P2 leads to a four-subarc solution including two coasting subarcs alternating with two max-thrust subarcs. Problems P5 leads to a three-subarc solution including two max-thrust subarcs alternating with one coasting subarc. Problems P3 and P4 include P1, P2, and P5 as particular cases and lead to two-, three-, or four-subarcs solutions depending on the prescribed value of fuel or time. For all problems, the thrust magnitude control is saturated at one of its extreme values: in optimization studies, we determine the best thrust direction controls; in guidance studies, we force the thrust direction controls to be constant in each subarc and determine the best thrust direction parameters. Of course, the time lengths of all the subarcs must also be determined. The computational results show that, for Problems P1-P5, the performance index of the multiple-subarc guidance trajectory approximates well the performance index of the multiple-subarc optimal trajectory: the pairwise relative differences in performance index are less than 1/100 in all cases. To sum up, the produced guidance trajectories are highly efficient and yet quite simple in implementation. C1 [Miele, A.; Ciarcia, M.] Rice Univ, Houston, TX 77005 USA. [Weeks, M. W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77005 USA. RP Miele, A (reprint author), Rice Univ, Houston, TX 77005 USA. EM michael.w.weeks@nasa.gov; ciarcia@rice.edu; michael.w.weeks@nasa.gov NR 11 TC 0 Z9 0 U1 1 U2 2 PU ASCE-AMER SOC CIVIL ENGINEERS PI RESTON PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA SN 0893-1321 J9 J AEROSPACE ENG JI J. Aerosp. Eng. PD APR PY 2009 VL 22 IS 2 BP 160 EP 172 DI 10.1061/(ASCE)0893-1321(2009)22:2(160) PG 13 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA 418MK UT WOS:000264152100007 ER PT J AU Liao, L Meneghini, R AF Liao, Liang Meneghini, Robert TI Validation of TRMM Precipitation Radar through Comparison of Its Multiyear Measurements with Ground-Based Radar SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID MEASURING MISSION TRMM; SIZE; SATELLITE; PARAMETERS; MODEL; SHAPE; SITE AB A procedure to accurately resample spaceborne and ground-based radar data is described and then is applied to the measurements taken from the Tropical Rainfall Measuring Mission (TRMM) precipitation radar (PR) and the ground-based Weather Surveillance Radar-1988 Doppler (WSR-88D or WSR) for the validation of the PR measurements and estimates. Through comparisons with the well-calibrated, non-attenuated WSR at Melbourne, Florida, for the period 1998-2007, the calibration of the PR aboard the TRMM satellite is checked using measurements near the storm top. Analysis of the results indicates that the PR, after taking into account differences in radar reflectivity factors between the PR and WSR, has a small positive bias of 0.8 dB relative to the WSR, implying a soundness of the PR calibration in view of the uncertainties involved in the comparisons. Comparisons between the PR and WSR reflectivities are also made near the surface for evaluation of the attenuation-correction procedures used in the PR algorithms. It is found that the PR attenuation is accurately corrected in stratiform rain but is underestimated in convective rain, particularly in heavy rain. Tests of the PR estimates of rainfall rate are conducted through comparisons in the overlap area between the TRMM overpass and WSR scan. Analyses of the data are made both on a conditional basis, in which the instantaneous rain rates are compared only at those pixels at which both the PR and WSR detect rain, and an unconditional basis, in which the area-averaged rain rates are estimated independently for the PR and WSR. Results of the conditional rain comparisons show that the PR-derived rain is about 9% greater and 19% less than the WSR estimates for stratiform and convective storms, respectively. Overall, the PR tends to underestimate the conditional mean rain rate by 8% for all rain categories, a finding that conforms to the results of the area-averaged rain (unconditional) comparisons. C1 [Liao, Liang] UMBC, Goddard Earth Sci & Technol Ctr, Greenbelt, MD 20771 USA. [Meneghini, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Liao, L (reprint author), UMBC, Goddard Earth Sci & Technol Ctr, Code 614-6, Greenbelt, MD 20771 USA. EM liang.liao-1@nasa.gov FU NASA's Precipitation Measurement Mission (PMM) [NNH06ZDA001N-PMM] FX We thank David Wolff, David Marks, and the Goddard Space Flight Center TRMM office for providing ground-based WSR data. This work is supported by Dr. R. Kakar of NASA Headquarters under NASA's Precipitation Measurement Mission (PMM) Grant NNH06ZDA001N-PMM. NR 28 TC 20 Z9 21 U1 0 U2 0 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 APR PY 2009 VL 48 IS 4 BP 804 EP 817 DI 10.1175/2008JAMC1974.1 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 443EQ UT WOS:000265893400008 ER PT J AU Nehrir, AR Repasky, KS Carlsten, JL Obland, MD Shaw, JA AF Nehrir, Amin R. Repasky, Kevin S. Carlsten, John L. Obland, Michael D. Shaw, Joseph A. TI Water Vapor Profiling Using a Widely Tunable, Amplified Diode-Laser-Based Differential Absorption Lidar (DIAL) SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID RAMAN LIDAR; DYE-LASER; TEMPERATURE; AIRBORNE; PERFORMANCE; RESOLUTION; AEROSOL AB A differential absorption lidar (DIAL) instrument for automated profiling of water vapor in the lower troposphere has been designed, tested, and is in routine operation at Montana State University. The laser transmitter for the DIAL instrument uses a widely tunable external cavity diode laser (ECDL) to injection seed two cascaded semiconductor optical amplifiers (SOAs) to produce a laser transmitter that accesses the 824-841-nm spectral range. The DIAL receiver utilizes a 28-cm-diameter Schmidt-Cassegrain telescope; an avalanche photodiode (APD) detector; and a narrowband optical filter to collect, discriminate, and measure the scattered light. A technique of correcting for the wavelength-dependent incident angle upon the narrowband optical filter as a function of range has been developed to allow accurate water vapor profiles to be measured down to 225 m above the surface. Data comparisons using the DIAL instrument and collocated radiosonde measurements are presented demonstrating the capabilities of the DIAL instrument. C1 [Nehrir, Amin R.; Repasky, Kevin S.; Shaw, Joseph A.] Montana State Univ, Dept Elect & Comp Engn, Bozeman, MT 59717 USA. [Carlsten, John L.; Obland, Michael D.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Obland, Michael D.] NASA, Langley Res Ctr, SSAI, Hampton, VA 23665 USA. RP Repasky, KS (reprint author), Montana State Univ, Dept Elect & Comp Engn, Cobleigh Hall,Room 610, Bozeman, MT 59717 USA. EM repasky@ece.montana.edu FU NASA [NNX06AD11G] FX This work was supported by NASA Grant NNX06AD11G. Partial support was also provided by the NASA Graduate Student Researchers Program (GSRP). NR 32 TC 19 Z9 19 U1 0 U2 2 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD APR PY 2009 VL 26 IS 4 BP 733 EP 745 DI 10.1175/2008JTECHA1201.1 PG 13 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 443ZN UT WOS:000265949400005 ER PT J AU Willis, JK Lyman, JM Johnson, GC Gilson, J AF Willis, Josh K. Lyman, John M. Johnson, Gregory C. Gilson, John TI In Situ Data Biases and Recent Ocean Heat Content Variability SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID T-5 EXPENDABLE BATHYTHERMOGRAPH; SEA-LEVEL RISE; ALTIMETRIC HEIGHT; STERIC HEIGHT; FALL-RATE; TOPEX/POSEIDON; TEMPERATURE; CIRCULATION; EQUATION; PACIFIC AB Two significant instrument biases have been identified in the in situ profile data used to estimate globally integrated upper-ocean heat content. A large cold bias was discovered in a small fraction of Argo floats along with a smaller but more prevalent warm bias in expendable bathythermograph (XBT) data. These biases appear to have caused the bulk of the upper-ocean cooling signal reported by Lyman et al. between 2003 and 2005. These systematic data errors are significantly larger than sampling errors in recent years and are the dominant sources of error in recent estimates of globally integrated upper-ocean heat content variability. The bias in the XBT data is found to be consistent with errors in the fall-rate equations, suggesting a physical explanation for that bias. With biased profiles discarded, no significant warming or cooling is observed in upper-ocean heat content between 2003 and 2006. C1 [Willis, Josh K.] CALTECH, Jet Prop Lab, Pasadena, CA 90034 USA. [Lyman, John M.; Johnson, Gregory C.] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA. [Lyman, John M.] Univ Hawaii Manoa, JIMAR, Honolulu, HI 96822 USA. [Gilson, John] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. RP Willis, JK (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 300-323, Pasadena, CA 90034 USA. EM joshua.k.willis@jpl.nasa.gov RI Johnson, Gregory/I-6559-2012 OI Johnson, Gregory/0000-0002-8023-4020 NR 21 TC 42 Z9 43 U1 0 U2 8 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD APR PY 2009 VL 26 IS 4 BP 846 EP 852 DI 10.1175/2008JTECHO608.1 PG 7 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 443ZN UT WOS:000265949400015 ER PT J AU Liu, P Kajikawa, Y Wang, B Kitoh, A Yasunari, T Li, T Annamalai, H Fu, XH Kikuchi, K Mizuta, R Rajendran, K Waliser, DE Kim, D AF Liu, Ping Kajikawa, Yoshiyuki Wang, Bin Kitoh, Akio Yasunari, Tetsuzo Li, Tim Annamalai, H. Fu, Xiouhua Kikuchi, Kazuyoshi Mizuta, Ryo Rajendran, Kavirajan Waliser, Duane E. Kim, Daehyun TI Tropical Intraseasonal Variability in the MRI-20km60L AGCM SO JOURNAL OF CLIMATE LA English DT Article ID MADDEN-JULIAN OSCILLATION; GENERAL-CIRCULATION MODELS; ASIAN SUMMER MONSOON; LARGE-SCALE MODELS; CONVECTION PARAMETERIZATION; VERTICAL STRUCTURE; LIFE-CYCLE; PART II; SCHEME; SIMULATION AB This study documents the detailed characteristics of the tropical intraseasonal variability (TISV) in the MRI-20km60L AGCM that uses a variant of the Arakawa-Schubert cumulus parameterization. Mean states, power spectra, propagation features, leading EOF modes, horizontal and vertical structures, and seasonality associated with the TISV are analyzed. Results show that the model reproduces the mean states in winds realistically and in convection comparable to that of the observations. However, the simulated TISV is less realistic. It shows low amplitudes in convection and low-level winds in the 30-60-day band. Filtered anomalies have standing structures. Power spectra and lag correlation of the signals do not propagate dominantly either in the eastward direction during boreal winter or in the northward direction during boreal summer. A combined EOF (CEOF) analysis shows that winds and convection have a loose coupling that cannot sustain the simulated TISV as realistically as that observed. In the composited mature phase of the simulated MJO, the low-level convergence does not lead convection clearly so that the moisture anomalies do not tilt westward in the vertical, indicating that the low-level convergence does not favor the eastward propagation. The less realistic TISV suggests that the representation of cumulus convection needs to be improved in this model. C1 [Liu, Ping; Kajikawa, Yoshiyuki; Wang, Bin; Li, Tim; Annamalai, H.; Fu, Xiouhua; Kikuchi, Kazuyoshi] Univ Hawaii Manoa, Int Pacific Res Ctr, SOEST, Honolulu, HI 96822 USA. [Kitoh, Akio] Met Res Inst, Tsukuba, Ibaraki, Japan. [Yasunari, Tetsuzo] Japan Agcy Marine Earth Sci & Technol, Frontier Res Ctr Global Change, Kanagawa, Japan. [Mizuta, Ryo] Meteorol Res Inst, Adv Earth Sci & Technol Org, Tsukuba, Ibaraki 305, Japan. [Rajendran, Kavirajan] Natl Aerosp Labs, Ctr Math Modelling & Comp Simulat, Bangalore, Karnataka, India. [Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Kim, Daehyun] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul, South Korea. RP Liu, P (reprint author), Univ Hawaii Manoa, Int Pacific Res Ctr, SOEST, 1680 East West Rd, Honolulu, HI 96822 USA. EM pliu@hawaii.edu RI Rajendran, Kavirajan/C-3334-2009; CMMACS, CSIR/A-2491-2011; Kikuchi, Kazuyoshi/C-2744-2009; Kajikawa, Yoshiyuki/C-2807-2009 OI Rajendran, Kavirajan/0000-0002-9437-4729; Kikuchi, Kazuyoshi/0000-0002-6200-0968; FU Japan Agency of Marine Science and Technology (JAMESTEC); NASA [NNX07AG53G]; International Pacific Research Center (IPRC); Jet Propulsion Laboratory; National Aeronautics and Space Administration FX This study is supported by the Japan Agency of Marine Science and Technology (JAMESTEC) and NASA Grant NNX07AG53G through their sponsorship of the International Pacific Research Center (IPRC). D. Waliser was supported by the Jet Propulsion Laboratory under a contract with the National Aeronautics and Space Administration. We thank the U. S. CLIVAR MJO Working Group for providing the software package. We also thank Diane Henderson and three reviewers for their comments. NR 57 TC 12 Z9 13 U1 0 U2 3 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 J9 J CLIMATE JI J. Clim. PD APR PY 2009 VL 22 IS 8 BP 2006 EP 2022 DI 10.1175/2008JCLI2406.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 444TH UT WOS:000266002800008 ER PT J AU Wu, MLC Schubert, SD Suarez, MJ Huang, NE AF Wu, Man-Li C. Schubert, Siegfried D. Suarez, Max J. Huang, Norden E. TI An Analysis of Moisture Fluxes into the Gulf of California SO JOURNAL OF CLIMATE LA English DT Article ID NORTH-AMERICAN-MONSOON; PACIFIC TROPICAL CYCLOGENESIS; SOUTHWESTERN UNITED-STATES; MADDEN-JULIAN OSCILLATION; EASTERN PACIFIC; HILBERT SPECTRUM; ARIZONA MONSOON; SURGES; WAVES; SUMMER AB This study examines the nature of episodes of enhanced warm-season moisture flux into the Gulf of California. Both spatial structure and primary time scales of the fluxes are examined using the 40-yr ECMWF Re-Analysis data for the period 1980-2001. The analysis approach consists of a compositing technique that is keyed on the low-level moisture fluxes into the Gulf of California. The results show that the fluxes have a rich spectrum of temporal variability, with periods of enhanced transport over the gulf linked to African easterly waves on subweekly (3-8 day) time scales, the Madden-Julian oscillation (MJO) at intraseasonal time scales (20-90 day), and intermediate (10-15 day) time-scale disturbances that appear to originate primarily in the Caribbean Sea-western Atlantic Ocean. In the case of the MJO, enhanced low-level westerlies and large-scale rising motion provide an environment that favors large-scale cyclonic development near the west coast of Central America that, over the course of about 2 weeks, expands northward along the coast eventually reaching the mouth of the Gulf of California where it acts to enhance the southerly moisture flux in that region. On a larger scale, the development includes a northward shift in the eastern Pacific ITCZ, enhanced precipitation over much of Mexico and the southwestern United States, and enhanced southerly/southeasterly fluxes from the Gulf of Mexico into Mexico and the southwestern and central United States. In the case of the easterly waves, the systems that reach Mexico appear to redevelop/ reorganize on the Pacific coast and then move rapidly to the northwest to contribute to the moisture flux into the Gulf of California. The most intense fluxes into the gulf on these time scales appear to be synchronized with a midlatitude short-wave trough over the U. S. West Coast and enhanced low-level southerly fluxes over the U. S. Great Plains. The intermediate (10-15 day) time-scale systems have zonal wavelengths roughly twice that of the easterly waves, and their initiation appears to be linked to an extratropical U. S. East Coast ridge and associated northeasterly winds that extend well into the Caribbean Sea during their development phase. The short (3-8 day) and, to a lesser extent, the intermediate (10-15 day) time-scale fluxes tend to be enhanced when the convectively active phase of the MJO is situated over the Americas. C1 [Wu, Man-Li C.; Schubert, Siegfried D.; Suarez, Max J.; Huang, Norden E.] NASA, Goddard Space Flight Ctr, Earth Sci Directorate, Greenbelt, MD 20771 USA. RP Huang, NE (reprint author), NASA GSFC GMAO, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM man-li.c.wu@nasa.gov FU National Research Council, Taiwan [95-2119-M-008-031-MY3] FX This work was supported by the NASA Earth Science Enterprises' Global Modeling and Analysis Program. However, Dr. Norden E. Huang is supported in part by a grant from National Research Council, Taiwan ( NSC 95-2119-M-008-031-MY3). NR 39 TC 10 Z9 12 U1 0 U2 3 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 J9 J CLIMATE JI J. Clim. PD APR PY 2009 VL 22 IS 8 BP 2216 EP 2239 DI 10.1175/2008JCLI2525.1 PG 24 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 444TH UT WOS:000266002800020 ER PT J AU Volz, MP Mazuruk, K Aggarwal, MD Croll, A AF Volz, M. P. Mazuruk, K. Aggarwal, M. D. Croell, A. TI Interface shape control using localized heating during Bridgman growth SO JOURNAL OF CRYSTAL GROWTH LA English DT Article DE Computer simulation; Convection; Heat transfer; Interfaces; Bridgman technique ID CRYSTAL-GROWTH; STOCKBARGER TECHNIQUE; CONFIGURATION; FURNACE AB Numerical calculations were performed to assess the effect of localized radial heating on the melt-crystal interface shape during vertical Bridgman growth. System parameters examined include the ampoule, melt and crystal thermal conductivities, the magnitude and width of localized heating, and the latent heat of crystallization. Concave interface shapes, typical of semiconductor systems, could be flattened or made convex with localized heating. Although localized heating caused shallower thermal gradients ahead of the interface, the magnitude of the localized heating required for convexity was less than that which resulted in a thermal inversion ahead of the interface. A convex interface shape was most readily achieved with ampoules of lower thermal conductivity. Increasing melt convection tended to flatten the interface, but the amount of radial heating required to achieve a convex interface was essentially independent of the convection intensity. (C) 2009 Elsevier B.V. All rights reserved. C1 [Volz, M. P.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Mazuruk, K.] Univ Alabama, Huntsville, AL 35899 USA. [Aggarwal, M. D.] Alabama A&M Univ, Dept Phys, Normal, AL 35762 USA. [Croell, A.] Univ Freiburg, Inst Kristallog, D-79104 Freiburg, Germany. RP Volz, MP (reprint author), NASA, George C Marshall Space Flight Ctr, EM30, Huntsville, AL 35812 USA. EM Martin.Volz@nasa.gov RI Croell, Arne/A-2480-2013 OI Croell, Arne/0000-0002-8673-9994 NR 12 TC 8 Z9 8 U1 0 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0248 J9 J CRYST GROWTH JI J. Cryst. Growth PD APR 1 PY 2009 VL 311 IS 8 BP 2321 EP 2326 DI 10.1016/j.jcrysgro.2009.02.019 PG 6 WC Crystallography; Materials Science, Multidisciplinary; Physics, Applied SC Crystallography; Materials Science; Physics GA 449SZ UT WOS:000266351600016 ER PT J AU Fong, T Nagatani, K Wettergreen, D AF Fong, Terrence Nagatani, Keiji Wettergreen, David TI EDITORIAL: Space Robotics, Part II SO JOURNAL OF FIELD ROBOTICS LA English DT Editorial Material C1 [Fong, Terrence] NASA, Ames Res Ctr, Washington, DC 20546 USA. [Nagatani, Keiji] Tohoku Univ, Sendai, Miyagi 980, Japan. [Wettergreen, David] Carnegie Mellon Univ, Pittsburgh, PA 15213 USA. RP Fong, T (reprint author), NASA, Ames Res Ctr, Washington, DC 20546 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU JOHN WILEY & SONS INC PI HOBOKEN PA 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 1556-4959 J9 J FIELD ROBOT JI J. Field Robot. PD APR PY 2009 VL 26 IS 4 BP 335 EP 336 DI 10.1002/rob.20298 PG 2 WC Robotics SC Robotics GA 421HH UT WOS:000264349500001 ER PT J AU Carsten, J Rankin, A Ferguson, D Stentz, A AF Carsten, Joseph Rankin, Arturo Ferguson, Dave Stentz, Anthony TI Global Planning on the Mars Exploration Rovers: Software Integration and Surface Testing SO JOURNAL OF FIELD ROBOTICS LA English DT Article AB In January 2004, NASA!s twin Mars Exploration Rovers (MERs), Spirit and Opportunity, began searching the surface of Mars for evidence of past water activity. To locatize and approach scientifically interesting targets, the rovers employ an onboard navigation system. Given the latency in sending commands from Earth to the Martian rovers (and in receiving return data), a high level of navigational autonomy is desirable. Autonomous navigation with hazard avoidance (AutoNav) is currently performed using a local path planner called GESTALT (grid-based estimation of surface traversability applied to local terrain) that incorporates terrain and obstacle information generated from stereo cameras. GESTALT works well at guiding the rovers around narrow and isolated hazards; however, it is susceptible to failure when clusters of closely spaced, non traversable rocks form extended obstacles. In May 2005, a new technology task was initiated at the jet Propulsion Laboratory to address this limitation. Specifically, a version of the Field D* global path planner was integrated into MER flight software, enabling simultaneous local and global planning during AutoNav. A revised version of AutoNav was then uploaded to the rovers during the summer of 2006. In this paper we describe how this integration of global planning into the MER flight software was performed and provide results from both the MER surface system test bed rover and five fully autonomous runs by Opportunity on Mars. (C) 2009 Wiley Periodicals, Inc. C1 [Carsten, Joseph; Rankin, Arturo] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ferguson, Dave] Intel Res Pittsburgh, Pittsburgh, PA 15213 USA. [Stentz, Anthony] Carnegie Mellon Univ, Inst Robot, Pittsburgh, PA 15213 USA. RP Carsten, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM joseph.carsten@jpl.nasa.gov; arturo.rankin@jpl.nasa.gov; dave.ferguson@intel.com; tony@cmu.edu FU MER; Mars Technology Program (MTP) FX The research described in this paper was performed at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under a contract with the National Aeronautics and Space Administration (contract NAS7-03001) and at Carnegie Mellon University (CMU) under a contract with the JPL (contract 1263676). This research was funded by the MER project and the Mars Technology Program (MTP) under task order NM0710764. CMU configured Field D* for MER and provided it to JPL under a research license with the California Institute of Technology, and JPL integrated Field D* into the MER flight software. CMU's work was performed under the MTP Reliable and Efficient Long-Range Autonomous Rover Navigation task, and JPUs work was performed under the MTP D* Integration into MER task. The authors would like to thank Mark Maimone for his sage advice during the integration and testing process. Without his assistance this process would have been infinitely more difficult. NR 16 TC 18 Z9 18 U1 0 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1556-4959 EI 1556-4967 J9 J FIELD ROBOT JI J. Field Robot. PD APR PY 2009 VL 26 IS 4 SI SI BP 337 EP 357 DI 10.1002/rob.20287 PG 21 WC Robotics SC Robotics GA 421HH UT WOS:000264349500002 ER PT J AU Helmick, D Angelova, A Matthies, L AF Helmick, Daniel Angelova, Anelia Matthies, Larry TI Terrain Adaptive Navigation for Planetary Rovers SO JOURNAL OF FIELD ROBOTICS LA English DT Article ID OFF-ROAD NAVIGATION; EXPLORATION ROVERS; OBSTACLE DETECTION; CLASSIFIER FUSION; MOBILE ROBOT; PERFORMANCE; SLIP AB This paper describes the design, implementation, and experimental results of a navigation system for planetary rovers called Terrain Adaptive Navigation (TANav). This system was designed to enable greater access to and more robust operations within terrains of widely varying slippage. The system achieves this goal by using onboard stereo cameras to remotely classify surrounding terrain, predict the slippage of that terrain, and use this information in the planning of a path to the goal. This navigation system consists of several integrated techniques: goodness map generation, terrain triage, terrain classification, remote slip prediction, path planning, High-Fidelity Traversability Analysis, and slip-compensated path following. Results from experiments with an end-to-end onboard implementation of the TANav system in a Mars analog environment are shown and compared to results from experiments with a more traditional navigation system that does not account for terrain properties. (C) 2009 Wiley Periodicals, Inc. C1 [Helmick, Daniel] CALTECH, Jet Prop Lab, Mobil & Manipulat Grp, Pasadena, CA 91109 USA. [Angelova, Anelia] CALTECH, Dept Comp Sci, Pasadena, CA 91125 USA. [Matthies, Larry] CALTECH, Jet Prop Lab, Comp Vis Grp, Pasadena, CA 91109 USA. RP Helmick, D (reprint author), CALTECH, Jet Prop Lab, Mobil & Manipulat Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM dmh@jpl.nasa.gov; anelia@vision.caltech.edu; lhm@jpl.nasa.gov FU NASA FX The research described in this publication was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract from the National Aeronautics and Space Administration (NASA), with funding from the Mars Technology Program, NASA Science Mission Directorate. NR 42 TC 31 Z9 32 U1 2 U2 9 PU JOHN WILEY & SONS INC PI HOBOKEN PA 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 1556-4959 J9 J FIELD ROBOT JI J. Field Robot. PD APR PY 2009 VL 26 IS 4 BP 391 EP 410 DI 10.1002/rob.20292 PG 20 WC Robotics SC Robotics GA 421HH UT WOS:000264349500004 ER PT J AU DeBonis, JR AF DeBonis, James R. TI RANS Analyses of Turbofan Nozzles With Internal Wedge Deflectors for Noise Reduction SO JOURNAL OF FLUIDS ENGINEERING-TRANSACTIONS OF THE ASME LA English DT Article; Proceedings Paper CT AIAA 46th Aerospace Sciences Meeting and Exhibit CY JAN 07-10, 2008 CL Reno, NV SP Amer Inst Aeronaut & Astronaut DE computational fluid dynamics; jets; Navier-Stokes equations; noise; nozzles; turbulence ID EXHAUST AB Computational fluid dynamics (CFD) was used to evaluate the flow field and thrust performance of a promising concept for reducing the noise at take-off of dual-stream turbofan nozzles. The concept, offset stream technology, reduces the jet noise observed on the ground by diverting (offsetting) a portion of the fan flow below the core flow, thickening and lengthening this layer between the high-velocity core flow and the ground observers. In this study a wedge placed in the internal fan stream is used as the diverter. Wind, a Reynolds averaged Navier-Stokes (RANS) code, was used to analyze the flow field of the exhaust plume and to calculate nozzle performance. Results showed that the wedge diverts all of the fan flow to the lower side of the nozzle, and the turbulent kinetic energy on the observer side of the nozzle is reduced. This reduction in turbulent kinetic energy should correspond to a reduction in noise. However, because all of the fan flow is diverted, the upper portion of the core flow is exposed to the freestream, and the turbulent kinetic energy on the upper side of the nozzle is increased, creating an unintended noise source. The blockage due to the wedge reduces the fan mass flow proportional to its blockage, and the overall thrust is consequently reduced. The CFD predictions are in very good agreement with experimental flow field data, demonstrating that RANS CFD can accurately predict the velocity and turbulent kinetic energy fields. While this initial design of a large scale wedge nozzle did not meet noise reduction or thrust goals, this study identified areas for improvement and demonstrated that RANS CFD can be used to improve the concept. C1 NASA, Inlet & Nozzle Branch, Glenn Res Ctr, Cleveland, OH 44135 USA. RP DeBonis, JR (reprint author), NASA, Inlet & Nozzle Branch, Glenn Res Ctr, Cleveland, OH 44135 USA. EM james.r.debonis@nasa.gov NR 18 TC 3 Z9 3 U1 2 U2 3 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA SN 0098-2202 J9 J FLUID ENG-T ASME JI J. Fluids Eng.-Trans. ASME PD APR PY 2009 VL 131 IS 4 AR 041104 DI 10.1115/1.3089536 PG 17 WC Engineering, Mechanical SC Engineering GA 418EY UT WOS:000264132100004 ER PT J AU Vila, DA de Goncalves, LGG Toll, DL Rozante, JR AF Vila, Daniel A. de Goncalves, Luis Gustavo G. Toll, David L. Rozante, Jose Roberto TI Statistical Evaluation of Combined Daily Gauge Observations and Rainfall Satellite Estimates over Continental South America SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID PRECIPITATION CLIMATOLOGY PROJECT; GLOBAL PRECIPITATION; PASSIVE MICROWAVE; RESOLUTION; DATASET AB This paper describes a comprehensive assessment of a new high-resolution, gauge-satellite-based analysis of daily precipitation over continental South America during 2004. This methodology is based on a combination of additive and multiplicative bias correction schemes to get the lowest bias when compared with the observed values ( rain gauges). Intercomparisons and cross-validation tests have been carried out between independent rain gauges and different merging techniques. This validation process was done for the control algorithm [Tropical Rainfall Measuring Mission(TRMM) Multisatellite Precipitation Analysis real-time algorithm] and five different merging schemes: additive bias correction; ratio bias correction; TRMM Multisatellite Precipitation Analysis, research version; and the combined scheme proposed in this paper. These methodologies were tested for different months belonging to different seasons and for different network densities. All compared, merging schemes produce better results than the control algorithm; however, when finer temporal ( daily) and spatial scale ( regional networks) gauge datasets are included in the analysis, the improvement is remarkable. The combined scheme consistently presents the best performance among the five techniques tested in this paper. This is also true when a degraded daily gauge network is used instead of a full dataset. This technique appears to be a suitable tool to produce real-time, high-resolution, gauge-and satellite-based analyses of daily precipitation over land in regional domains. C1 [Vila, Daniel A.] Univ Maryland, CICS, ESSIC, College Pk, MD 20742 USA. [de Goncalves, Luis Gustavo G.; Toll, David L.] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. [Rozante, Jose Roberto] Cachoeira Paulista, CPTEC, INPE, Sao Paulo, Brazil. RP Vila, DA (reprint author), Univ Maryland, CICS, ESSIC, 2207 Comp & Space Bldg, College Pk, MD 20742 USA. EM dvila@essic.umd.edu RI Vila, Daniel/G-8379-2012; de Goncalves, Luis Gustavo/G-2522-2012; OI Vila, Daniel/0000-0002-1015-5650; de Goncalves, Luis Gustavo/0000-0002-1571-0916 FU NASA [NNX06AG91G]; Oak Ridge Associated Universities (ORAU) FX This study was supported by NASA's LBA Ecology (Group CD36) Project under Grant NNX06AG91G and the NASA Postdoctoral Program under the Oak Ridge Associated Universities (ORAU). NR 24 TC 58 Z9 61 U1 5 U2 17 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD APR PY 2009 VL 10 IS 2 BP 533 EP 543 DI 10.1175/2008JHM1048.1 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 439PQ UT WOS:000265639900012 ER PT J AU Das, S Kyriakides, I Chattopadhyay, A Papandreou-Suppappola, A AF Das, S. Kyriakides, I. Chattopadhyay, A. Papandreou-Suppappola, A. TI Monte Carlo Matching Pursuit Decomposition Method for Damage Quantification in Composite Structures SO JOURNAL OF INTELLIGENT MATERIAL SYSTEMS AND STRUCTURES LA English DT Article DE wave propagation; structural health monitoring; fiber-reinforced composite; matching pursuit decomposition; particle filtering; monte carlo ID ROLLING-ELEMENT BEARINGS; FREQUENCY RESONANCE TECHNIQUE; PARTICLE FILTERS; TRACKING AB In wave-based approach, the presence of damage is visualized in terms of the changes in the signature of the resultant wave that propagates through the structure. In structural health monitoring, the fundamental goal is to detect, localize, and quantify these damage signatures. The current approach uses matching pursuit decomposition (MPD) to compare signals from healthy and damaged structures. However, the major drawback of the MPD is that, in the decomposition process, it performs an exhaustive search over a large dictionary of elementary functions. Therefore, this method of decomposition is associated with a large computational expense. In this research, the Monte Carlo matching pursuit decomposition (MCMPD) is proposed, that adapts a smaller dictionary to the signal structure, thus avoiding the exhaustive search over the time-frequency plane. The proposed algorithm, sequentially estimates a dictionary that contains only those components that match the waveform structure, uses the matching pursuits for the decomposition of the signal and if necessary, adapts the dictionary to the structure of the residues for further decomposition. Finally, we demonstrate using real life data that the MCMPD retains the ability of the matching pursuit to decompose waveforms and quantify them accurately while reducing computational expense. C1 [Das, S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Kyriakides, I.] Arizona State Univ, Dept Elect Engn, Tempe, AZ 85287 USA. [Chattopadhyay, A.] Arizona State Univ, Dept Mech & Aerosp Engn, Tempe, AZ 85287 USA. [Chattopadhyay, A.; Papandreou-Suppappola, A.] Arizona State Univ, Adapt Intelligent Mat & Syst AIMS Ctr, Tempe, AZ 85287 USA. [Papandreou-Suppappola, A.] Arizona State Univ, Dept Elect Engn, Tempe, AZ 85287 USA. RP Das, S (reprint author), NASA, Ames Res Ctr, MS 269-1, Moffett Field, CA 94035 USA. EM Santanu.Das@asu.edu FU Air Force Office of Scientific Research [F496200310174] FX This research was supported by the Air Force Office of Scientific Research, grant number: F496200310174, technical monitor Dr Clark Allred. The financial support is gratefully acknowledged. The authors would also like to thank the MURI Program, Air Force Office of Scientific Research, grant number: FA9550-06-1-0309; Technical Monitor, Dr Victor Giurgiutiu. NR 35 TC 14 Z9 14 U1 0 U2 1 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1045-389X J9 J INTEL MAT SYST STR JI J. Intell. Mater. Syst. Struct. PD APR PY 2009 VL 20 IS 6 BP 647 EP 658 DI 10.1177/1045389X08097386 PG 12 WC Materials Science, Multidisciplinary SC Materials Science GA 423TH UT WOS:000264518100001 ER PT J AU Xiang, Z Thomas, GW Thornburg, KM Cabrol, N Grin, E Anderson, RC AF Xiang, Zhen Thomas, Geb W. Thornburg, Kristopher M. Cabrol, Nathalie Grin, Edmond Anderson, Robert C. TI Slope Perception from Monoscopic Field Images: Applications to Mobile Robot Navigation SO JOURNAL OF INTELLIGENT & ROBOTIC SYSTEMS LA English DT Article DE Slope perception; Slope estimation; Robotic teleoperation; Slope perception model; Image perception ID SLANT UNDERESTIMATION; GEOGRAPHICAL-SLANT; URBAN SEARCH; MODEL AB When remotely navigating a mobile robot, operators must estimate the slope of local terrain in order to avoid areas that are too steep to climb or that slope so steeply downward that the operator would lose control of the rover. Although many rovers are equipped with sensor systems to aid the operator in this task, it is sometimes necessary to estimate slopes from two-dimensional images, either when planning operations or when the operator wishes to monitor the results of a sensor system. This experiment compares the operator's estimates of the slope in Martian terrain with the actual slope determined from three-dimensional data. The ten participants overestimated the slope of the indicated regions by an average of 19A degrees (SD 16A degrees). An analytic model of the error, based on psychophysical analysis, accurately predicts the average magnitude of the errors. Implementation of this model eliminates an average amount of participant error. However, the large estimate variance within and between participants and images still poses a challenge for accurate slope estimation. C1 [Xiang, Zhen; Thomas, Geb W.; Thornburg, Kristopher M.] Univ Iowa, Iowa City, IA 52242 USA. [Cabrol, Nathalie; Grin, Edmond] NASA Ames SETI, Moffett Field, CA USA. [Anderson, Robert C.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Thornburg, KM (reprint author), Univ Iowa, Iowa City, IA 52242 USA. EM kthornbu@engineering.uiowa.edu NR 19 TC 0 Z9 0 U1 1 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0921-0296 J9 J INTELL ROBOT SYST JI J. Intell. Robot. Syst. PD APR PY 2009 VL 54 IS 4 BP 595 EP 612 DI 10.1007/s10846-008-9281-y PG 18 WC Computer Science, Artificial Intelligence; Robotics SC Computer Science; Robotics GA 423GM UT WOS:000264484800003 ER PT J AU Foster, L Waagen, A Aijaz, N Hurley, M Luis, A Rinsky, J Satyavolu, C Way, MJ Gazis, P Srivastava, A AF Foster, Leslie Waagen, Alex Aijaz, Nabeela Hurley, Michael Luis, Apolonio Rinsky, Joel Satyavolu, Chandrika Way, Michael J. Gazis, Paul Srivastava, Ashok TI Stable and Efficient Gaussian Process Calculations SO JOURNAL OF MACHINE LEARNING RESEARCH LA English DT Article DE Gaussian processes; low rank approximations; numerical stability; photometric redshift; subset of regressors method ID PROCESS REGRESSION; FACTORIZATION AB The use of Gaussian processes can be an effective approach to prediction in a supervised learning environment. For large data sets, the standard Gaussian process approach requires solving very large systems of linear equations and approximations are required for the calculations to be practical. We will focus on the subset of regressors approximation technique. We will demonstrate that there can be numerical instabilities in a well known implementation of the technique. We discuss alternate implementations that have better numerical stability properties and can lead to better predictions. Our results will be illustrated by looking at an application involving prediction of galaxy redshift from broadband spectrum data. C1 [Foster, Leslie; Waagen, Alex; Aijaz, Nabeela; Hurley, Michael; Luis, Apolonio; Rinsky, Joel; Satyavolu, Chandrika] San Jose State Univ, Dept Math, San Jose, CA 95192 USA. [Way, Michael J.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Gazis, Paul; Srivastava, Ashok] NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA. RP Foster, L (reprint author), San Jose State Univ, Dept Math, San Jose, CA 95192 USA. EM FOSTER@MATH.SJSU.EDU; AWAAGEN@MAILBOLT.COM; NABBO_A@YAHOO.COM; MHURLEY@GMAIL.COM; JPOLOROLU@GMAIL.COM; JOEL_RINSKY@YAHOO.COM; CHANDRIKA_S84@YAHOO.COM; MICHAEL.J.WAY@NASA.GOV; PGAZIS@MAIL.ARC.NASA.GOV; ASHOK@EMAIL.ARC.NASA.GOV RI Way, Michael/D-5254-2012; OI Way, Michael/0000-0003-3728-0475 NR 30 TC 17 Z9 17 U1 0 U2 1 PU MICROTOME PUBL PI BROOKLINE PA 31 GIBBS ST, BROOKLINE, MA 02446 USA SN 1532-4435 J9 J MACH LEARN RES JI J. Mach. Learn. Res. PD APR PY 2009 VL 10 BP 857 EP 882 PG 26 WC Automation & Control Systems; Computer Science, Artificial Intelligence SC Automation & Control Systems; Computer Science GA 507BJ UT WOS:000270824600002 ER PT J AU Shi, C Zhang, Y Gu, C Chen, B Seballos, L Olson, T Zhang, JZ AF Shi, Chao Zhang, Yi Gu, Claire Chen, Bin Seballos, Leo Olson, Tammy Zhang, Jin Z. TI Molecular Fiber Sensors Based on Surface Enhanced Raman Scattering (SERS) SO JOURNAL OF NANOSCIENCE AND NANOTECHNOLOGY LA English DT Review DE Surface Enhanced Raman Scattering (SERS); Optical Fiber; Molecular Detection; Silver Nanoparticles (SNPs) ID RHODAMINE 6G MOLECULES; CHEMICAL SENSORS; SILVER ELECTRODE; OPTICAL-FIBERS; METAL-FILMS; SPECTROSCOPY; NANOPARTICLES; RESONANCE; DYE; BIOSENSORS AB Molecular sensors based on surface enhanced Raman scattering (SERS) and optical fibers have been widely used in biological, environmental and chemical detection procedures due to their unique advantages, such as molecular specificity, high sensitivity and flexibility In this paper, we review the development and highlight some of the important milestones of SERS fiber sensor development with emphasis on recent work to improve the sensitivity of the fiber sensors. In particular in the area to increase the sensitivity, we've reviewed various methods of sample preparation as well as different fiber SERS sensors. One way is to strengthen the field enhancement around the surface of the probe tip and the other is to increase the number of the interacting particles during the SERS process. These techniques are known as the double substrate "sandwich" structure (DSSS) and the liquid core photonic crystal fiber (LCPCF), and in both cases the sensitivities are significantly improved. These fiber sensors were tested with Rhodamine 6G, human insulin and tryptophan and showed excellent performance. C1 [Shi, Chao; Zhang, Yi; Gu, Claire] Univ Calif Santa Cruz, Dept Elect Engn, Santa Cruz, CA 95064 USA. [Chen, Bin] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Seballos, Leo; Olson, Tammy; Zhang, Jin Z.] Univ Calif Santa Cruz, Dept Chem & Biochem, Santa Cruz, CA 95064 USA. RP Gu, C (reprint author), Univ Calif Santa Cruz, Dept Elect Engn, Santa Cruz, CA 95064 USA. FU National Science Foundation [ECS-0401206]; NASA PIDDP; ASTEP; Department of Defense; UCSC special research grant; University Affiliated Research Center's Aligned Research Program FX We acknowledge the financial support from the National Science Foundation (ECS-0401206), NASA PIDDP and ASTEP partial supports, Department of Defense, the UCSC special research grant, and the University Affiliated Research Center's Aligned Research Program. NR 68 TC 19 Z9 19 U1 5 U2 36 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 APR PY 2009 VL 9 IS 4 BP 2234 EP 2246 DI 10.1166/jnn.2009.SE41 PG 13 WC Chemistry, Multidisciplinary; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA 423IK UT WOS:000264489800006 PM 19437961 ER PT J AU Sun, LQ Cui, RH Jalbout, AF Li, MJ Pan, XM Wang, RS Xie, HM AF Sun, L. Q. Cui, R. H. Jalbout, A. F. Li, M. J. Pan, X. M. Wang, R. S. Xie, H. M. TI LiFePO4 as an optimum power cell material SO JOURNAL OF POWER SOURCES LA English DT Article; Proceedings Paper CT 14th International Meeting on Lithium Batteries CY JUN 22-28, 2008 CL Tianjin, PEOPLES R CHINA SP Tianjin Inst Power Sources, China Ind Assoc Power Sources, Tianjin Local Govt DE LiFePO4; Polyacence; Lithium ion batteries; Power cells ID CARBON-COATED LIFEPO4; CATHODE MATERIALS; ELECTROCHEMICAL PROPERTIES; LITHIUM BATTERIES; ROUTE; COATINGS; LIXFEPO4; FEPO4; IRON AB Nano-crystallized LiFePO4 has been synthesized with a simple three-step-synthesis technology in the presence of nano-ferric oxide as iron source and polyacence (PAS) as a reductive agent and high conductive carbon source. The use of PAS increases the conductivity and prevents the particles growth. The most feasible calcined temperature and time was investigated and the best cell performance was delivered by the sample calcined at 700 degrees C for 4 h. This material shows excellent specific capacity and cycle efficiency at high current rates, almost no capacity loss can be observed Lip to 100 cycles which make it more superior as an optimum power cell cathode material. (c) 2008 Elsevier B.V. All rights reserved. C1 [Sun, L. Q.; Cui, R. H.; Li, M. J.; Pan, X. M.; Wang, R. S.; Xie, H. M.] NE Normal Univ, Fac Chem, Inst Funct Mat, Changchun 130024, Jilin, Peoples R China. [Jalbout, A. F.] NASA, Astrobiol Inst, Tucson, AZ 85721 USA. [Jalbout, A. F.] Univ Arizona, Dept Chem, Tucson, AZ 85721 USA. RP Wang, RS (reprint author), NE Normal Univ, Fac Chem, Inst Funct Mat, Changchun 130024, Jilin, Peoples R China. EM wangrs@nenu.edu.cn; xiehm136@nenu.edu.cn NR 23 TC 22 Z9 28 U1 2 U2 6 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-7753 J9 J POWER SOURCES JI J. Power Sources PD APR 1 PY 2009 VL 189 IS 1 SI SI BP 522 EP 526 DI 10.1016/j.jpowsour.2008.10.120 PG 5 WC Chemistry, Physical; Electrochemistry; Energy & Fuels; Materials Science, Multidisciplinary SC Chemistry; Electrochemistry; Energy & Fuels; Materials Science GA 435BG UT WOS:000265317600086 ER PT J AU Wesley, WR Simpson, JR Parker, PA Pignatiello, JJ AF Wesley, Wayne R. Simpson, James R. Parker, Peter A. Pignatiello, Joseph J., Jr. TI Exact Calculation of Integrated Prediction Variance for Response Surface Designs on Cuboidal and Spherical Regions SO JOURNAL OF QUALITY TECHNOLOGY LA English DT Article DE Design Optimality; IV-Criterion; Region Moments; Restricted Randomization ID SECOND-ORDER DESIGNS; SPLIT-PLOT DESIGNS; EQUIVALENT ESTIMATION; CONSTRUCTION; COMPOSITE; CRITERIA; MODELS AB Over the years, design optimality evaluation of response surface designs focused mainly on D-optimality and G-optimality criteria. The apparent limited use of the IV-optimality criterion appears to be influenced by the computational challenges associated with the criterion. The lack of available computer code appears to be the main reason for limited use of the IV-optimality criterion. In addition, the IV-optimality criterion appears more difficult to code than the D-optimality criterion because of the integration required over the specified design region. In this paper, an efficient and exact method is presented for computing the IV-optimality criterion for selected response surface designs. The pseudo-code for the computer program is also presented. The investigation examines both spherical and cuboidal regions of interest. In addition, an analytical approach is outlined for computing the IV-optimality criterion for second-order split-plot designs. A particular feature of the analytical expressions is that they are derived using the design parameters. In addition, several comparisons of second-order response surface designs are illustrated for completely randomized designs and split-plot designs. C1 [Wesley, Wayne R.] Univ Technol, Fac Engn & Comp, Kingston 6, Jamaica. [Simpson, James R.] 53d Test Management Grp, Eglin AFB, FL USA. [Parker, Peter A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Pignatiello, Joseph J., Jr.] Florida State Univ, Dept Ind & Mfg Engn, Tallahassee, FL 32310 USA. RP Wesley, WR (reprint author), Univ Technol, Fac Engn & Comp, Kingston 6, Jamaica. EM wwesley3@hotmail.com; James.Simpson@eglin.af.mil; peter.a.parker@nasa.gov; pigna@eng.fsu.edu NR 29 TC 1 Z9 1 U1 2 U2 4 PU AMER SOC QUALITY CONTROL-ASQC PI MILWAUKEE PA 600 N PLANKINTON AVE, MILWAUKEE, WI 53203 USA SN 0022-4065 J9 J QUAL TECHNOL JI J. Qual. Technol. PD APR PY 2009 VL 41 IS 2 BP 165 EP 180 PG 16 WC Engineering, Industrial; Operations Research & Management Science; Statistics & Probability SC Engineering; Operations Research & Management Science; Mathematics GA 424VH UT WOS:000264595900008 ER PT J AU Mishchenko, MI Geogdzhayev, IV Liu, L Lacis, AA Cairns, B Travis, LD AF Mishchenko, Michael I. Geogdzhayev, Igor V. Liu, Li Lacis, Andrew A. Cairns, Brian Travis, Larry D. TI Toward unified satellite climatology of aerosol properties: What do fully compatible MODIS and MISR aerosol pixels tell us? SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Tropospheric aerosols; Remote sensing ID OPTICAL DEPTH; RETRIEVALS; AERONET; OCEAN; SPACE; PRODUCTS; FUTURE; RECORD AB Because of the global nature of aerosol effects on climate, satellite observations have been and will be an indispensable source of information about aerosol characteristics for use in various assessments of climate and climate change. There have been parallel claims of unprecedented accuracy of aerosol retrievals with the moderate-resolution imaging spectroradiometer (MODIS) and multiangle imaging spectroradiometer (MISR). These claims have been based on limited comparisons with ground-based observations which, however, are not necessarily indicative of the actual global performance of these satellite sensors. Fortunately, both instruments have been flown for many years on the same Terra platform, which provides a unique opportunity to compare fully collocated pixel-level MODIS and MISR aerosol retrievals directly and globally. Our present extensive analysis of similar to 8 years of the MODIS-Terra and MISR aerosol data documents unexpected significant disagreements at the pixel level as well as between long-term and spatially averaged aerosol properties. The only point on which both datasets seem to fully agree is that there may have been a weak increasing tendency in the globally averaged aerosol optical thickness (AOT) over the land and no long-term AOT tendency over the oceans. Overall our new results suggest that the current knowledge of the global distribution of the AOT and, especially, aerosol microphysical characteristics remains unsatisfactory. Published by Elsevier Ltd. C1 [Mishchenko, Michael I.; Geogdzhayev, Igor V.; Liu, Li; Lacis, Andrew A.; Cairns, Brian; Travis, Larry D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM mmishchenko@giss.nasa.gov RI Lacis, Andrew/D-4658-2012; Mishchenko, Michael/D-4426-2012; OI Cairns, Brian/0000-0002-1980-1022 FU NASA EOS; National Polar-orbiting Operational Environmental Satellite System's Advanced Technology; Program Executive Office for Environmental Satellites FX We thank John Martonchik for valuable advice regarding the MISR aerosol retrieval algorithm and datasets, Lorraine Remer for her assistance in the understanding of the MODIS aerosol product, and Ralph Kahn for valuable discussions. This research was funded by the NASA EOS program and by the National Polar-orbiting Operational Environmental Satellite System's Advanced Technology and Plans Program Element of the Program Executive Office for Environmental Satellites. NR 24 TC 33 Z9 33 U1 1 U2 6 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 APR-MAY PY 2009 VL 110 IS 6-7 BP 402 EP 408 DI 10.1016/j.jqsrt.2009.01.007 PG 7 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 433VH UT WOS:000265233400009 ER PT J AU Floros, MW Johnson, W AF Floros, Matthew W. Johnson, Wayne TI Performance Analysis of the Slowed-Rotor Compound Helicopter Configuration SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY LA English DT Article AB The calculated performance of a slowed-rotor compound aircraft, particularly at high flight speeds, is examined. Correlation of calculated and measured performance is presented for a NASA Langley high advance ratio test to establish the capability to model rotors in such flight conditions. The predicted performance of an isolated rotor and a wing and rotor combination are examined in detail. Three tip speeds and a range of collective pitch settings are investigated. A tip speed of 230 ft/s and zero collective pitch are found to be the best condition to minimize rotor drag over a wide speed range. Detailed rotor and wing performance is examined for both sea level and cruise altitude conditions. Rotor and wing power are found to be primarily from profile drag, except at low speed where the wing is near stall. Increased altitude offloads lift from the rotor to the wing, reducing total power required. C1 [Floros, Matthew W.] USA, Res Lab, Hampton, VA USA. [Johnson, Wayne] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Floros, MW (reprint author), NASA, Langley Res Ctr, MS 266, Hampton, VA 23681 USA. EM matt.floros@us.army.mil NR 14 TC 9 Z9 9 U1 1 U2 4 PU AMER HELICOPTER SOC INC PI ALEXANDRIA PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA SN 0002-8711 J9 J AM HELICOPTER SOC JI J. Am. Helicopter Soc. PD APR PY 2009 VL 54 IS 2 AR 022002 DI 10.4050/JAHS.54.022002 PG 12 WC Engineering, Aerospace SC Engineering GA V16MQ UT WOS:000207874100002 ER PT J AU Savas, O Green, RB Caradonna, FX AF Savas, Oemer Green, Richard B. Caradonna, Francis X. TI Coupled Thrust and Vorticity Dynamics during Vortex Ring State SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY LA English DT Article AB This paper focuses on the vortex ring state (VRS) that is observed in the flow around a rotor during rapid descent. In VRS, the vortex filaments trailed off the blades coalesce around the rotor disk. This vortex ring detaches into the wake periodically, causing extreme oscillations in thrust, with periods on the order of several tens of rotor revolutions. The phase relation between the thrust cycle and vorticity distribution at the rotor disk is discussed. Maxima of the VRS thrust oscillations correlate well with the maxima of circulation, enstrophy, and minima of enstrophy dispersion radius observed in the vicinity of the rotor disk. C1 [Savas, Oemer] Univ Calif Berkeley, Dept Mech Engn, Berkeley, CA 94720 USA. [Green, Richard B.] Univ Glasgow, Dept Aerosp Engn, Glasgow G12 8QQ, Lanark, Scotland. [Caradonna, Francis X.] NASA Ames Res Ctr, Aeroflightdynam Directorate, Army RDECOM, Moffett Field, CA USA. RP Savas, O (reprint author), Univ Calif Berkeley, Dept Mech Engn, Berkeley, CA 94720 USA. EM savas@me.berkeley.edu NR 26 TC 3 Z9 3 U1 0 U2 1 PU AMER HELICOPTER SOC INC PI ALEXANDRIA PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA SN 0002-8711 J9 J AM HELICOPTER SOC JI J. Am. Helicopter Soc. PD APR PY 2009 VL 54 IS 2 AR 022001 DI 10.4050/JAHS.54.022001 PG 10 WC Engineering, Aerospace SC Engineering GA V16MQ UT WOS:000207874100001 ER PT J AU Grinstead, JH Wright, MJ Bogdanoff, DW Allen, GA AF Grinstead, Jay H. Wright, Michael J. Bogdanoff, David W. Allen, Gary A. TI Shock Radiation Measurements for Mars Aerocapture Radiative Heating Analysis SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER LA English DT Article; Proceedings Paper CT AIAA 46th Aerospace Sciences Meeting and Exhibit CY JAN 07-10, 2008 CL Reno, NV SP Amer Inst Aeronaut & Astronaut ID NONEQUILIBRIUM AB NASA's In-Space Propulsion Technology program is supporting the development of shock radial. ion transport models for aerocapture missions to Mars and Venus. Phenomenological models of nonequilibrium shock radiation will be incorporated into high-fidelity flowlield computations used to predict the aerothermal environments for a Mars or Venus aerocapture entry vehicle. These models are validated with shock radiance measurements obtained at flight-relevant conditions. A comprehensive test series in the NASA Ames Electric Arc Shock Tube facility at a representative freestream condition was recently completed. The facility's optical instrumentation enabled spectral measurements of shocked gas radiation from the vacuum ultraviolet to the near infrared. The instrumentation captured the nonequilibrium postshock excitation and relaxation dynamics of dispersed spectral features. A description of the shock tube facility, optical instrumentation, and examples of the test data are presented. C1 [Grinstead, Jay H.; Wright, Michael J.] NASA, Ames Res Ctr, Reacting Flow Environm Branch, Moffett Field, CA 94035 USA. [Bogdanoff, David W.; Allen, Gary A.] ELORET Corp, Reacting Flow Environm Branch, Moffett Field, CA 94035 USA. RP Grinstead, JH (reprint author), NASA, Ames Res Ctr, Reacting Flow Environm Branch, MS 230-2, Moffett Field, CA 94035 USA. NR 21 TC 11 Z9 11 U1 0 U2 1 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0887-8722 J9 J THERMOPHYS HEAT TR JI J. Thermophys. Heat Transf. PD APR-JUN PY 2009 VL 23 IS 2 BP 249 EP 255 DI 10.2514/1.37281 PG 7 WC Thermodynamics; Engineering, Mechanical SC Thermodynamics; Engineering GA 434JT UT WOS:000265271700003 ER PT J AU Marschall, J Pejakovic, DA Fahrenholtz, WG Hilmas, GE Zhu, SM Ridge, J Fletcher, DG Asma, CO Thomel, J AF Marschall, Jochen Pejakovic, Dusan A. Fahrenholtz, William G. Hilmas, Greg E. Zhu, Sumin Ridge, Jerry Fletcher, Douglas G. Asma, Cem O. Thomel, Jan TI Oxidation of ZrB(2)-SiC Ultrahigh-Temperature Ceramic Composites in Dissociated Air SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER LA English DT Article ID ATOMIC OXYGEN RECOMBINATION; DIBORIDE-SILICON CARBIDE; ZIRCONIUM DIBORIDE; PASSIVE TRANSITION; REENTRY CONDITIONS; 1500-DEGREES-C; CATALYCITY; PRESSURE; BEHAVIOR; HAFNIUM AB The oxidation behavior and surface properties of hot-pressed ZrB(2)-SiC ultrahigh-temperature ceramic composites are investigated under aerothermal heating conditions in the high-temperature, low-pressure partially dissociated airstream of the 1.2 MW Plasmatron facility at the von Karman Institute for Fluid Dynamics. Samples aer oxidized at different flow enthalpies for exposure times of up to 20 min at surface temperatures ranging from 1250 to 1575 degrees C. The microstructure and composition of the resulting oxide layers are characterized using electron and optical microscopies, x-ray diffraction, and energy-dispersive x-ray analysis. Comparisons are made with samples oxidized under similar temperature and pressure conditions in a furnace test environment in which atomic oxygen concentrations are negligible. Changes in surface optical properties are documented using spectral reflectance measurements, and effective catalytic efficiencies are estimated using computational fluid dynamics calculations together with measured surface temperatures and heat fluxes. C1 [Marschall, Jochen; Pejakovic, Dusan A.] SRI Int, Mol Phys Lab, Menlo Pk, CA 94025 USA. [Fahrenholtz, William G.; Hilmas, Greg E.; Zhu, Sumin] Missouri Univ Sci & Technol, Dept Mat Sci & Engn, Rolla, MO 65409 USA. [Ridge, Jerry] NASA, Ames Res Ctr, Thermal Protect Mat & Syst Branch, Moffett Field, CA 94035 USA. [Ridge, Jerry] ELORET Corp, Sunnyvale, CA 94086 USA. [Fletcher, Douglas G.; Asma, Cem O.; Thomel, Jan] Von Karman Inst Fluid Dynam, Aeronaut & Aerosp Dept, B-1640 Rhode St Genese, Belgium. RP Marschall, J (reprint author), SRI Int, Mol Phys Lab, 333 Ravenswood Ave, Menlo Pk, CA 94025 USA. EM jochen.marschall@sri.com; billf@mst.edu; ghilmas@mst.edu; Sumin.Zhu@usvesuvius.com; jerome.w.ridge@nasa.gov; douglas.fletcher@uvm.edu; asma@vki.ac.be; jan.thoemel@vki.ac.be RI Zhu, Sumin/D-3686-2009; OI Fahrenholtz, William/0000-0002-8497-0092; Pejakovic, Dusan/0000-0001-6067-6529 FU U.S. Air Force Office of Scientific Research [F49550-05-C-0020, FA9550-06-0125]; National Science Foundation [DMR-0435856, DMR-0346800]; European Office of Aerospace Research and Development [FA865506-1-3078] FX This research was supported by the Ceramics and Nonmetallic Materials Program of the U.S. Air Force Office of Scientific Research through contracts F49550-05-C-0020 (Marschall and Pejakovic) and FA9550-06-0125 (Fahrenholtz and Hilmas), the National Science Foundation through grants DMR-0435856 (Marschall) and DMR-0346800 (Fahrenholtz and Zhu), and the European Office of Aerospace Research and Development through, contract FA865506-1-3078 (Fletcher, Asma, and Thomel). The authors would like to thank Olivier Chazot at VKI for advice and support during Plasmatron testing, Eric Bohannan at the Missouri University of Science and Technology for XRD analysis, and Jeffry Wight at the Missouri University of Science and Technology for XPS analysis. NR 53 TC 22 Z9 22 U1 0 U2 9 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0887-8722 J9 J THERMOPHYS HEAT TR JI J. Thermophys. Heat Transf. PD APR-JUN PY 2009 VL 23 IS 2 BP 267 EP 278 DI 10.2514/1.39970 PG 12 WC Thermodynamics; Engineering, Mechanical SC Thermodynamics; Engineering GA 434JT UT WOS:000265271700005 ER PT J AU Wu, W Du, JH Lin, YR Chow, LC Notardonato, W AF Wu, W. Du, J. H. Lin, Y. R. Chow, L. C. Notardonato, W. TI Design and Experiment of Compact and Effective Carbon Foam Recuperative Heat Exchangers SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER LA English DT Article ID POROUS-MEDIA; FLUID; ENHANCEMENT; PLATE; MODEL; FLOW AB A. conceptual design for a compact, lightweight, recuperative heat exchanger with an effectiveness of 98%. is presented. This heat exchanger consists of discrete pair of carbon foam blocks packed between thin sheets of stainless steel. The flowpaths were piled alternately in a modular manner so that the hot and cold streams counterflow in the recuperative heat exchanger. Measures were taken to minimize the axial conduction in the heat exchanger. The anisotropic property of carbon foam was exploited to achieve higher effectiveness. The paper shows how the overall effectiveness of the heat exchanger can reach beyond 98% by placing many pair of carbon foam blocks in series. Experiments with four pair of carbon foam blocks were conducted to validate the design concept. Results show that carbon foam can effectively increase heat transfer between the hot and cold streams. With four pair of carbon foam blocks, an effectiveness greater than 80% was achieved. An effectiveness epsilon(total) of 98% can be reached by using 50 pair of carbon foam blocks. This new development has advantages in size and weight and can be easily scaled up for larger heat transfer requirements. C1 [Chow, L. C.] Univ Cent Florida, Dept Mech Mat & Aerosp Engn, Orlando, FL 32816 USA. [Notardonato, W.] NASA, Kennedy Space Ctr, Kennedy Space Ctr, FL 32899 USA. RP Chow, LC (reprint author), Univ Cent Florida, Dept Mech Mat & Aerosp Engn, Orlando, FL 32816 USA. EM lchow@mail.ucf.edu FU Florida Space Grant Consortium; NASA Kennedy Space Center FX This research was sponsored by Florida Space Grant Consortium and NASA Kennedy Space Center. NR 24 TC 4 Z9 5 U1 0 U2 3 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0887-8722 J9 J THERMOPHYS HEAT TR JI J. Thermophys. Heat Transf. PD APR-JUN PY 2009 VL 23 IS 2 BP 339 EP 345 DI 10.2514/1.40857 PG 7 WC Thermodynamics; Engineering, Mechanical SC Thermodynamics; Engineering GA 434JT UT WOS:000265271700012 ER PT J AU Moraru, L Keith, TG AF Moraru, Laurentiu Keith, Theo G., Jr. TI Application of the Amplitude Reduction Technique Within Probabilistic Rough EHL Models SO JOURNAL OF TRIBOLOGY-TRANSACTIONS OF THE ASME LA English DT Article; Proceedings Paper CT STLE/ASME 2006 International Joint Tribology Conference CY OCT 22-25, 2006 CL San Antonio, TX SP Soc Tribologists & Lubricat Engineers, Amer Soc Mech Engineers DE deformation; elasticity; elastodynamics; fast Fourier transforms; hydrodynamics; lubrication; plasticity ID LUBRICATED LINE CONTACTS; SURFACE MICRO-GEOMETRY; MIXED LUBRICATION; ELASTOHYDRODYNAMIC LUBRICATION; POINT CONTACTS; FILM THICKNESS; FRICTION; REGIME; STRESSES; SPEED AB Over the years, the deterministic elastohydrodynamic lubrication (EHL) approach has been widely used. This technique is very powerful in capturing details of asperity deformation and interaction. The probabilistic EHL methodology is still used when the main interest of the engineer is directed toward computations of bulk properties. During recent years, the results of many deterministic analyses have been published. The reduction of the waviness amplitude in EHL contacts under rolling-sliding was systematically studied and it was shown that the amplitude reduction is completely described by a single parameter that includes relative wavelength and the operating conditions. This approach, usually referred to as the amplitude reduction technique, has opened the way for developing improved probabilistic EHL models by incorporating the effects of fluid-induced roughness deformation, which is calculated using the fast fourier transform. In this paper we provide a review of the latest developments in the amplitude reduction technique and we present a probabilistic EHL algorithm for the computation of the load supported by the fluid, the elastically deformed asperities and the plastically deformed asperities, in a mixed EHL contact with either isotropic on nonisotropic roughness. The fluid-induced roughness deformation is incorporated into the probabilistic model via the use of the amplitude reduction technique. C1 [Keith, Theo G., Jr.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Moraru, Laurentiu] Univ Toledo, Dept Mech Engn, Toledo, OH 43606 USA. RP Moraru, L (reprint author), Univ Politehn Bucuresti, Elie Carafoli Aerosp Sci Dept, Spl Independentei 313, Bucharest 060042, Romania. EM laurentiu.moraru@gmail.com NR 55 TC 0 Z9 0 U1 0 U2 6 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA SN 0742-4787 J9 J TRIBOL-T ASME JI J. Tribol.-Trans. ASME PD APR PY 2009 VL 131 IS 2 AR 021703 DI 10.1115/1.2961919 PG 8 WC Engineering, Mechanical SC Engineering GA 416SP UT WOS:000264026100021 ER PT J AU Dhungel, A Lu, YP Phillips, W Ekkad, SV Heidmann, J AF Dhungel, Alok Lu, Yiping Phillips, Wynn Ekkad, Srinath V. Heidmann, James TI Film Cooling From a Row of Holes Supplemented With Antivortex Holes SO JOURNAL OF TURBOMACHINERY-TRANSACTIONS OF THE ASME LA English DT Article DE blades; cooling; gas turbines; heat transfer; turbulence; vortices ID COMPOUND ANGLE ORIENTATIONS; RESULTS DOWNSTREAM AB The primary focus of this paper is to study the film cooling performance for a row of cylindrical holes each supplemented with two symmetrical antivortex holes, which branch out from the main holes. The antivortex design was originally developed at NASA-Glenn Research Center by James Heidmann, coauthor of this paper. 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. The geometry and orientation of the antivortex holes greatly affect the cooling performance downstream, which is thoroughly investigated. By performing experiments at a single mainstream Reynolds number of 9683 based on the freestream velocity and film hole diameter at four different coolant-to-mainstream blowing ratios of 0.5, 1, 1.5, and 2 and using the transient IR thermography technique, detailed film cooling effectiveness and heat transfer coefficients are obtained simultaneously from a single test. When the antivortex holes are nearer the primary film cooling holes and are developing from the base of the primary holes, better film cooling is accomplished as compared to other antivortex hole orientations. When the antivortex holes are laid back in the upstream region, film cooling diminishes considerably. Although an enhancement in heat transfer coefficient is seen in cases with high film cooling effectiveness, the overall heat flux ratio as compared to standard cylindrical holes is much lower. Thus cases with antivortex holes placed near the main holes certainly show promising results. C1 [Ekkad, Srinath V.] Virginia Tech, Blacksburg, VA 24060 USA. [Heidmann, James] NASA, Glenn Res Ctr, Turbomachinery & Heat Transfer Branch, Cleveland, OH 44135 USA. [Dhungel, Alok; Lu, Yiping; Phillips, Wynn] Louisiana State Univ, Dept Mech Engn, Baton Rouge, LA 70803 USA. RP Ekkad, SV (reprint author), Virginia Tech, Blacksburg, VA 24060 USA. EM sekkad@vt.edu RI Ekkad, Srinath/E-9112-2014 NR 17 TC 12 Z9 14 U1 2 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 APR PY 2009 VL 131 IS 2 AR 021007 DI 10.1115/1.2950059 PG 10 WC Engineering, Mechanical SC Engineering GA 403WM UT WOS:000263112700007 ER PT J AU Walsh, BM AF Walsh, B. M. TI Review of Tm and Ho materials; spectroscopy and lasers SO LASER PHYSICS LA English DT Review ID PUMPED 1.9-MU-M THULIUM; SILICA-FIBER LASER; ENERGY-TRANSFER; UP-CONVERSION; YAG; TM,HO-YAG; YLF; LUMINESCENCE; SIMULATION; OPERATION AB A review of Tm and Ho materials is presented, covering some fundamental aspects on the spectroscopy and laser dynamics in both single and co-doped systems. Following an introduction to 2-mu m lasers, applications and historical development, the physics of quasi-four level lasers, energy transfer and modeling are discussed in some detail. Recent developments in using Tm lasers to pump Ho lasers are discussed, and seen to offer some advantages over conventional Tm:Ho lasers. This article is not intended as a complete review, but as a primer for introducing concepts and a resource for further study. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Walsh, BM (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM brian.m.walsh@nasa.gov NR 45 TC 118 Z9 126 U1 11 U2 97 PU MAIK NAUKA/INTERPERIODICA/SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013-1578 USA SN 1054-660X J9 LASER PHYS JI Laser Phys. PD APR PY 2009 VL 19 IS 4 BP 855 EP 866 DI 10.1134/S1054660X09040446 PG 12 WC Optics; Physics, Applied SC Optics; Physics GA 431EG UT WOS:000265043500044 ER PT J AU Graille, B Magin, TE Massot, M AF Graille, Benjamin Magin, Thierry E. Massot, Marc TI KINETIC THEORY OF PLASMAS: TRANSLATIONAL ENERGY SO MATHEMATICAL MODELS & METHODS IN APPLIED SCIENCES LA English DT Article DE Kinetic theory; plasmas in thermal nonequilibrium; conservation equations; multicomponent transport properties ID NAVIER-STOKES EQUATIONS; HYDRODYNAMIC LIMIT; IONIZED-GAS; TRANSPORT-PROPERTIES; PARTICLES REGIME; SIMULATION; DIFFUSION; DISCHARGE; MIXTURES; MODELS AB In the present study, we derive from kinetic theory a unified fluid model for multicomponent plasmas by accounting for the electromagnetic field influence. We deal with a possible thermal nonequilibrium of the translational energy of the particles, neglecting their internal energy and reactive collisions. Given the strong disparity of mass between the electrons and heavy particles, such as molecules, atoms, and ions, we conduct a dimensional analysis of the Boltzmann equation and introduce a scaling based on a multiscale perturbation parameter equal to the square root of the ratio of the electron mass to a characteristic heavy-particle mass. We then generalize the Chapman-Enskog method, emphasizing the role of the perturbation parameter on the collisional operator, the streaming operator, and the collisional invariants of the Boltzmann equation. The system is examined at successive orders of approximation, each corresponding to a physical timescale. At the highest approximation order investigated, the multicomponent Navier-Stokes regime is reached for the heavy particles and is coupled to first-order drift-diffusion equations for the electrons. The transport coefficients are then calculated in terms of bracket operators whose mathematical structure allows for positivity properties to be determined and Onsager's reciprocal relations to hold. The transport coefficients exhibit an anisotropic behavior when the magnetic field is strong enough. We also give a complete description of the Kolesnikov effect, i.e. the crossed contributions to the mass and energy transport fluxes coupling the electrons and heavy particles. Finally, the first and second laws of thermodynamics are proved to be satisfied by deriving a total energy equation and an entropy equation. Moreover, the purely convective system of equations is shown to be hyperbolic. C1 [Magin, Thierry E.] Stanford Univ, Ctr Turbulence Res, Stanford, CA 94305 USA. [Magin, Thierry E.] NASA, Ames Res Ctr, Reacting Flow Environm Branch, Moffett Field, CA 94035 USA. [Graille, Benjamin] Univ Paris 11, Lab Math Orsay, CNRS, UMR 8628, F-91405 Orsay, France. [Massot, Marc] Ecole Cent Paris, CNRS, Lab EM2C, UPR 288, F-92295 Chatenay Malabry, France. RP Magin, TE (reprint author), Stanford Univ, Ctr Turbulence Res, 488 Escondido Mall, Stanford, CA 94305 USA. EM benjamin.graille@math.u-psud.fr; magin@stanford.edu; marc.massot@em2c.ecp.fr RI Magin, Thierry/A-7533-2016 OI Magin, Thierry/0000-0002-4376-1518 NR 57 TC 13 Z9 13 U1 1 U2 4 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE SN 0218-2025 J9 MATH MOD METH APPL S JI Math. Models Meth. Appl. Sci. PD APR PY 2009 VL 19 IS 4 BP 527 EP 599 PG 73 WC Mathematics, Applied SC Mathematics GA 435YH UT WOS:000265378900002 ER PT J AU Herring, GC Meyers, JF Hart, RC AF Herring, G. C. Meyers, James F. Hart, Roger C. TI Shock-strength determination with seeded and seedless laser methods SO MEASUREMENT SCIENCE AND TECHNOLOGY LA English DT Article DE oblique shock strength; Prandtl-Meyer expansion; Doppler global velocimetry (DGV); laser-induced thermal acoustics (LITA) ID DOPPLER GLOBAL VELOCIMETRY; INDUCED THERMAL ACOUSTICS; FLOW AB Two noninvasive laser diagnostics were independently used to measure time-averaged and spatially resolved pressure change across a two-dimensional (2D) shock wave. The first method is Doppler global velocimetry (DGV) which uses water seeding and generates 2D maps of three-orthogonal components of velocity. A DGV-measured change in flow direction behind an oblique shock provides an indirect determination of pressure change across the shock, when used with the known incoming Mach number and ideal shock relations (or Prandtl-Meyer equations for an expansion fan). This approach was demonstrated at Mach 2 on 2D shock and expansion waves generated from a flat plate. This technique also works for temperature change (as well as pressure) and for normal shocks (as well as oblique). The second method, laser-induced thermal acoustics (LITA), is a seedless approach that was used to generate 1D spatial profiles of streamwise Mach number, sound speed, pressure and temperature over the same oblique waves. Excellent agreement was obtained between DGV and LITA, suggesting that either technique is viable for shock-strength measurement. C1 [Herring, G. C.] NASA, Langley Res Ctr, Adv Sensors & Optic Measurement Branch, Hampton, VA 23681 USA. RP Herring, GC (reprint author), NASA, Langley Res Ctr, Adv Sensors & Optic Measurement Branch, Hampton, VA 23681 USA. NR 19 TC 2 Z9 2 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0957-0233 EI 1361-6501 J9 MEAS SCI TECHNOL JI Meas. Sci. Technol. PD APR PY 2009 VL 20 IS 4 AR 045304 DI 10.1088/0957-0233/20/4/045304 PG 9 WC Engineering, Multidisciplinary; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 421VQ UT WOS:000264386800023 ER PT J AU Bajt, S Sandford, SA Flynn, GJ Matrajt, G Snead, CJ Westphal, AJ Bradley, JP AF Bajt, S. Sandford, S. A. Flynn, G. J. Matrajt, G. Snead, C. J. Westphal, A. J. Bradley, J. P. TI Infrared spectroscopy of Wild 2 particle hypervelocity tracks in Stardust aerogel: Evidence for the presence of volatile organics in cometary dust SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID DIFFUSE INTERSTELLAR-MEDIUM; INTERPLANETARY DUST; GALACTIC-CENTER; MU-M; 81P/WILD-2; MATTER; SAMPLES; HYDROCARBONS; MICROSCOPE; COLLECTION AB Infrared spectroscopy maps of some tracks made by cometary dust from 81P/Wild 2 impacting Stardust aerogel reveal an interesting distribution of organic material. Out of six examined tracks, three show presence of volatile organic components possibly injected into the aerogel during particle impacts. When particle tracks contained volatile organic material, they were found to be -CH2-rich, while the aerogel is dominated by the -CH3-rich contaminant. It is clear that the Population of cometary particles impacting the Stardust aerogel collectors also includes grains that contained little or none of this organic component. This observation is consistent with the highly heterogeneous nature of collected grains, as seen by a multitude of other analytical techniques. C1 [Bradley, J. P.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. [Sandford, S. A.] NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. [Flynn, G. J.] SUNY Coll Plattsburgh, Dept Phys, Plattsburgh, NY 12901 USA. [Matrajt, G.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Snead, C. J.; Westphal, A. J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Bajt, S (reprint author), DESY, Notkestr 85, D-22607 Hamburg, Germany. EM sasa.bajt@desy.de RI Bajt, Sasa/G-2228-2010 FU NASA Stardust Discovery Mission; NASA Stardust Participating Scientist Program; U.S. Department of Energy [W-7405-ENG-48, DE-AC03-76F00098, DE-AC02-98H10886] FX We are grateful for support and samples provided by the NASA Stardust Discovery Mission and the NASA Stardust Participating Scientist Program. We thank H. N. Chapman (LLNL) for technical discussions and M. C. Martin (ALS, LBNL), Z. Hao (ALS, LBNL) and G. L. Carr, L. Miller and R. Smith (NSLS, BNL) for assistance with the experiments. Part of this work was performed under the auspices of the U.S. Department of Energy by the Lawrence Livermore National Laboratory under contract no. W-7405-ENG-48, the Advanced Light Source, Lawrence Berkeley National Laboratory, which is supported by the Director, Office of Science, Office of Basic Energy Sciences, Materials Sciences Division, of the U.S. Department of Energy under contract no. DE-AC03-76F00098, and the National Synchrotron Light Source, Brookhaven National Laboratory, which is Supported by U. S. Department of Energy, Division of Materials Sciences and Division of Chemical Sciences, under contract no. DE-AC02-98H10886. This paper benefited from the thoughtful comments of three anonymous reviewers. NR 38 TC 20 Z9 20 U1 0 U2 2 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 APR PY 2009 VL 44 IS 4 BP 471 EP 484 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 458SZ UT WOS:000267045100001 ER PT J AU Chabot, NL Saslow, SA McDonough, WF Jones, JH AF Chabot, Nancy L. Saslow, Sarah A. McDonough, William F. Jones, John H. TI An investigation of the behavior of Cu and Cr during iron meteorite crystallization SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID FE-NI-S; TRACE-ELEMENT FRACTIONATION; SIDEROPHILE ELEMENTS; LIQUID-METAL; PARTITION-COEFFICIENTS; CORE FORMATION; GROUP IIIAB; SYSTEM; SOLIDIFICATION; CONSTRAINTS AB The measured Cu and Cr contents in magmatic iron meteorites appear to contradict the behavior predicted by experimental fractional crystallization Studies Currently available. To investigate the origin of Cu and Cr concentrations observed in these meteorites, a thorough set of solid metal/liquid metal experiments were conducted in the Fe-Ni-S system. In addition to Cu and Cr, partitioning values were also determined for As, Au, Bi, Co, Mo, Ni, Pb, Rh, Ru, Sb, Sri, V, and Zn from the experiments. Experimental results for Cu and Cr showed similar chalcophile partitioning behavior, whereas these elements have differently sloped trends within magmatic iron meteorite groups. Thus, fractional crystallization alone cannot control both the Cu and Cr concentrations in these iron meteorite groups. A simple fractional crystallization model based oil our experimental Cu partitioning results was able to match the Cu versus Au trend observed in the S-poor IVB iron meteorite group but not the decreasing Cu versus Au trends in the IIAB and IIIAB groups or the unique S-shaped Cu versus Au trend in the IVA group. However, the crystallization model calculations were found to be very sensitive to the specific choice for the mathematical expression of D(Cu), suggesting that any future refinement of the parameterization of D(Cu) Should Include a reassessment of the Cu fractional crystallization trends. The Cr versus Au trends in magmatic iron meteorite groups are steeper than those Of Cu and not explained by fractional crystallization. Other influences, such as the removal of chromite from the crystallizing system or sampling biases during iron meteorite compositional analyses, are likely responsible for the Cr trends in magmatic iron meteorite groups. C1 [Chabot, Nancy L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [McDonough, William F.] Univ Maryland, Dept Geol, College Pk, MD 20742 USA. [Jones, John H.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Chabot, NL (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM Nancy.Chabot@jhuapl.edu RI McDonough, William/C-4791-2009; Chabot, Nancy/F-5384-2015; McDonough, William/I-7720-2012 OI McDonough, William/0000-0001-9154-3673; Chabot, Nancy/0000-0001-8628-3176; McDonough, William/0000-0001-9154-3673 FU Geophysical Laboratory at the Carnegie Institution of Washington; NASA [NNG06GI13G, NNX08AH76G] FX We thank reviewers A. Kracher and H. Haack and associate editor E. R. D. Scott for constructive and thoughtful comments that resulted in Substantial improvements to this paper. We also thank Y. Fei of the Geophysical Laboratory at the Carnegie Institution of Washington for Supporting this study by providing access to the JEOL 8900L electron microprobe. This work was supported by NASA grant NNG06GI13G to NLC and NNX08AH76G to WFM and a NASA RTOP to JHJ. NR 33 TC 21 Z9 21 U1 1 U2 8 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 APR PY 2009 VL 44 IS 4 BP 505 EP 519 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 458SZ UT WOS:000267045100003 ER PT J AU Kebukawa, Y Nakashima, S Otsuka, T Nakamura-Messenger, K Zolensky, ME AF Kebukawa, Yoko Nakashima, Satoru Otsuka, Takahiro Nakamura-Messenger, Keiko Zolensky, Michael E. TI Rapid contamination during storage of carbonaceous chondrites prepared for micro FTIR measurements SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID INTERPLANETARY DUST PARTICLES; TAGISH LAKE METEORITE; POLYCYCLIC AROMATIC-HYDROCARBONS; DIFFUSE INTERSTELLAR-MEDIUM; ORGANIC-MATTER; COMET 81P/WILD-2; MU-M; ALIPHATIC-HYDROCARBONS; ELECTRON-MICROSCOPE; SOLAR-SYSTEM AB Organic contamination (similar to 2965 and similar to 1260 cm(-1) peaks) was found on Tagish Lake (C2) and Murchison (CM2) carbonaceous chondrites containing abundant hydrous minerals by Fourier transform infrared (FTIR) microspectroscopy oil the samples pressed on Al plates. On the other hand, anhydrous chondrite (Moss, CO3) was not contaminated. This contamination occurred within one day of storage, when the samples pressed on Al were stored within containers including silicone rubber mats. Volatile molecules having similar peaks to the contaminants were detected by long-path gas cell FTIR measurements for the silicone rubber mat. Rapid adsorption of the volatile contaminants also Occurred when silica gel and hydrous minerals such as serpentine were stored in containers including silicone rubber, silicone grease, or adhesive tape. However, they did not show any contamination when stored in glass and polystyrene containers without these compounds. Therefore, precious astronomical samples such as meteorites, interplanetary dust particles (IDPs), and mission-returned samples from cornets, asteroids, and Mars, should be measured by micro FTIR within one day of storage in glass containers without silicone rubber, silicone grease, or adhesive tape. C1 [Kebukawa, Yoko; Nakashima, Satoru; Otsuka, Takahiro] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan. [Nakamura-Messenger, Keiko; Zolensky, Michael E.] NASA, Lyndon B Johnson Space Ctr, KT, Houston, TX 77058 USA. RP Kebukawa, Y (reprint author), Osaka Univ, Dept Earth & Space Sci, 1-1 Machikaneyama, Osaka 5600043, Japan. EM yoko.soleil@ess.sci.osaka-u.ac.jp RI Kebukawa, Yoko/A-7315-2010 OI Kebukawa, Yoko/0000-0001-8430-3612 FU Japan Society for the Promotion of Science for Young Scientists FX This research was supported by Research Fellowships of the Japan Society for the Promotion of Science for Young Scientists to Y. K. NR 60 TC 13 Z9 13 U1 0 U2 8 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 APR PY 2009 VL 44 IS 4 BP 545 EP 557 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 458SZ UT WOS:000267045100006 ER PT J AU Korycansky, DG Plesko, CS Jutzi, M Asphaug, E Colaprete, A AF Korycansky, D. G. Plesko, Catherine S. Jutzi, Martin Asphaug, Erik Colaprete, Anthony TI Predictions for the LCROSS mission SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID HIGH-RESOLUTION SIMULATIONS; IMPACT PROCESSES; 3D MODELS; ASTEROIDS; FRACTURE; LAWS AB We describe the results of a variety of model calculations for predictions of observable results of the LCROSS mission to be launched in 2009. Several models covering different aspects of the event are described along with their results. Our aim is to bracket the range of expected results and produce a useful guide for mission planning. In this paper, we focus oil several different questions, which are modeled by different methods. The questions include the size of impact crater, the mass, velocity, and visibility of impact ejecta, and the mass and temperature of the initial vapor plume. The mass and velocity profiles of the ejecta are of primary interest, as the ejecta will be the main target of the S-S/C observations. In particular, we focus on Such quantities as the amount of mass that reaches various heights. A height of 2 km above the target is of special interest, as we expect that the EDUS impact will take place on the floor of a moderate-sized crater similar to 30 km in diameter, with a rim height of 1-2 km. The impact ejecta must rise above the crater rim at the target site in order to scatter sunlight and become visible to the detectors aboard the S-S/C. We start with a brief discussion of crater scaling relationships as applied to the impact of the EDUS second stage and resulting estimated crater diameter and ejecta mass. Next we describe results from the RAGE hydrocode as applied to modeling the short time scale (t <= 0.1 s) thermal plume that is expected to occur immediately after the impact. We present results from several large-scale smooth-particle hydrodynamics (SPH) calculations, along with results from a ZEUS-MP hydrocode model of the crater formation and ejecta mass-velocity distribution. We finish with two semi-analytic models, the first being a Monte Carlo model of the distribution of expected ejecta, based on scaling models using a plausible range of crater and ejecta parameters, and the second being a simple model of observational predictions for the shepherding spacecraft (S-S/C) that will follow the impact for several minutes until its own impact into the lunar surface. For the initial thermal plume, we predict an initial expansion velocity of similar to 7 km s(-1) and a maximum temperature of similar to 1200 K. Scaling relations for crater formation and the SPH calculation predict a crater with a diameter of similar to 15 m, a total ejecta mass of similar to 10(6) kg, with similar to 10(4) kg reaching all altitude of 2 km above the target. Both the SPH and ZEUS-MP calculations predict a maximum ejecta velocity of similar to 1 km s(-1). The semi-analytic Monte Carlo calculations produce more conservative estimates (by a factor of similar to 5) for ejecta at 2 km, but with a large dispersion in possible results. C1 [Korycansky, D. G.; Plesko, Catherine S.; Asphaug, Erik] Univ Calif Santa Cruz, Dept Earth Sci, CODEP, Santa Cruz, CA 95064 USA. [Plesko, Catherine S.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Jutzi, Martin] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. [Colaprete, Anthony] 245 3 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Korycansky, DG (reprint author), Univ Calif Santa Cruz, Dept Earth Sci, CODEP, Santa Cruz, CA 95064 USA. EM kory@pmc.ucsc.edu NR 31 TC 17 Z9 17 U1 1 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD APR PY 2009 VL 44 IS 4 BP 603 EP 620 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 458SZ UT WOS:000267045100011 ER PT J AU Croll, A Volz, MP AF Croell, Arne Volz, Martin P. TI Detached Bridgman Growth-A Standard Crystal Growth Method with a New Twist SO MRS BULLETIN LA English DT Article ID GERMANIUM-CRYSTALS; SURFACE-TENSION; SINGLE-CRYSTALS; ZERO GRAVITY; SOLIDIFICATION; MICROGRAVITY; CONTACT; MELTS; SEGREGATION; CRUCIBLES AB Bridgman or vertical gradient freeze (VGF) crystal growth processes have several advantages compared to other melt growth methods, especially the possibility to achieve a low level of thermal stress and low dislocation densities in the grown crystals. However, crystals grown in contact with a crucible usually suffer from mechanical stress during cooling, reducing the structural quality. The "detached" or "dewetted" Bridgman growth avoids this problem and has recently been investigated in more detail as a promising tool to improve crystal quality. Detached growth, where the crystal is separated from the crucible wall by a gap of 10-100 mu m, was found originally in some microgravity experiments going back to 1975. Considerable improvements of crystal quality were reported for those cases; however, the reasons for the detachment were not fully understood. In the last 10-15 years, theoretical investigations as well as new experiments have shown beyond a doubt that detached growth can, in principle, be achieved in Earth's gravity with the same advantages that were demonstrated in the crystals grown under microgravity. It could be shown that the ability to achieve detachment depends on a complex interplay of the wetting of the melt with the crucible and the crystal as well as the pressure balance in the system, including the hydrostatic pressure, the gas pressure above the melt, and the pressure below the melt. It turns out that for stable detachment, only, specific combinations of meniscus shape, gap size, wetting angle, growth angle, and pressures work. The conditions that lead to detachment are thus highly specific for a given system. C1 [Croell, Arne] Univ Freiburg, Inst Crystallog, D-79104 Freiburg, Germany. [Volz, Martin P.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Croll, A (reprint author), Univ Freiburg, Inst Crystallog, Hermann Herder Str 5, D-79104 Freiburg, Germany. EM arne.croell@krist.uni-freiburg.de; martin.volz@nasa.gov RI Croell, Arne/A-2480-2013 OI Croell, Arne/0000-0002-8673-9994 FU NASA; ESA; DLR FX The authors would like to thank their colleagues S.D. Cobb, R Dold, M. Fiederle, S. Motakef, O. Patzold, W. Palosz, N. Salk, M. Schweizer, F.R. Szofran, and J.S. Walker for all of their joint work and many discussions on detachment during the last 12 years. The financial assistance of NASA, ESA, and DLR during years of detached Bridgman research is greatly appreciated. NR 23 TC 10 Z9 10 U1 0 U2 2 PU MATERIALS RESEARCH SOC PI WARRENDALE PA 506 KEYSTONE DR, WARRENDALE, PA 15086 USA SN 0883-7694 J9 MRS BULL JI MRS Bull. PD APR PY 2009 VL 34 IS 4 BP 245 EP 250 DI 10.1557/mrs2009.74 PG 6 WC Materials Science, Multidisciplinary; Physics, Applied SC Materials Science; Physics GA 436HG UT WOS:000265402700013 ER PT J AU Milliken, RE Rivkin, AS AF Milliken, Ralph E. Rivkin, Andrew S. TI Brucite and carbonate assemblages from altered olivine-rich materials on Ceres SO NATURE GEOSCIENCE LA English DT Article ID ASTEROID 1 CERES; AQUEOUS ALTERATION; THERMAL EVOLUTION; WATER; CHONDRITES; MINERALS; SPECTROSCOPY; MATRIX; BODIES; VESTA AB The dwarf planet Ceres is the largest object in the asteroid belt, and is generally thought to be a differentiated body composed primarily of silicate materials and water ice(1,2). Some remotely observed features, however, indicate that Ceres may instead have a composition more similar to that of the most common types of carbonaceous meteorite(3-7). In particular, Ceres has been shown to have a distinct infrared absorption feature centred at a wavelength of similar to 3.06 mu m that is superimposed on a broader absorption from similar to 2.8 to 3.7 mu m (refs 5, 8), which suggests the presence of OH-or H(2)O-bearing phases. The specific mineral composition of Ceres and its relationship to known meteorite mineral assemblages, however, remains uncertain. Here we show that the spectral features of Ceres can be attributed to the presence of the hydroxide brucite, magnesium carbonates and serpentines, a mineralogy consistent with the aqueous alteration of olivine-rich materials. We therefore suggest that the thermal and aqueous alteration history of Ceres is different from that recorded by carbonaceous meteorites, and that samples from Ceres are not represented in existing meteorite collections. C1 [Milliken, Ralph E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rivkin, Andrew S.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Milliken, RE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Ralph.Milliken@jpl.nasa.gov RI Rivkin, Andrew/B-7744-2016 OI Rivkin, Andrew/0000-0002-9939-9976 FU NASA [NCC 5-538]; RELAB at Brown University FX This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. We also acknowledge support from RELAB at Brown University, the NASA Planetary Astronomy Program and the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement no. NCC 5-538 with the NASA Planetary Astronomy Program. NR 30 TC 60 Z9 60 U1 1 U2 16 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 J9 NAT GEOSCI JI Nat. Geosci. PD APR PY 2009 VL 2 IS 4 BP 258 EP 261 DI 10.1038/NGEO478 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 433XW UT WOS:000265240100014 ER PT J AU Shindell, D Faluvegi, G AF Shindell, Drew Faluvegi, Greg TI Climate response to regional radiative forcing during the twentieth century SO NATURE GEOSCIENCE LA English DT Article ID GISS MODELE; SENSITIVITY; SIMULATIONS; TEMPERATURE; OZONE; POLLUTANTS; REANALYSIS; SATELLITE; TRANSPORT; AEROSOLS AB Regional climate change can arise from three different effects: regional changes to the amount of radiative heating that reaches the Earth's surface, an inhomogeneous response to globally uniform changes in radiative heating and variability without a specific forcing. The relative importance of these effects is not clear, particularly because neither the response to regional forcings nor the regional forcings themselves are well known for the twentieth century. Here we investigate the sensitivity of regional climate to changes in carbon dioxide, black carbon aerosols, sulphate aerosols and ozone in the tropics, mid-latitudes and polar regions, using a coupled ocean-atmosphere model. We find that mid-and high-latitude climate is quite sensitive to the location of the forcing. Using these relationships between forcing and response along with observations of twentieth century climate change, we reconstruct radiative forcing from aerosols in space and time. Our reconstructions broadly agree with historical emissions estimates, and can explain the differences between observed changes in Arctic temperatures and expectations from non-aerosol forcings plus unforced variability. We conclude that decreasing concentrations of sulphate aerosols and increasing concentrations of black carbon have substantially contributed to rapid Arctic warming during the past three decades. C1 [Shindell, Drew] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Columbia Univ, New York, NY 10025 USA. RP Shindell, D (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM Drew.T.Shindell@nasa.gov RI Shindell, Drew/D-4636-2012 FU NASA's Atmospheric Chemistry Modeling and Analysis Program; Office of Science, US Department of Energy FX We thank NASA's Atmospheric Chemistry Modeling and Analysis Program for support and R. Reudy and H. Teich for technical assistance. We acknowledge the modelling groups,the Program for Climate Model Diagnosis and Intercomparison and the Working Group on Coupled Modelling for making available the CMIP3 data set,which is supported by the Office of Science, US Department of Energy. NR 39 TC 258 Z9 269 U1 3 U2 79 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 EI 1752-0908 J9 NAT GEOSCI JI Nat. Geosci. PD APR PY 2009 VL 2 IS 4 BP 294 EP 300 DI 10.1038/NGEO473 PG 7 WC Geosciences, Multidisciplinary SC Geology GA 433XW UT WOS:000265240100022 ER PT J AU Hoashi, M Bevacqua, DC Otake, T Watanabe, Y Hickman, AH Utsunomiya, S Ohmoto, H AF Hoashi, Masamichi Bevacqua, David C. Otake, Tsubasa Watanabe, Yumiko Hickman, Arthur H. Utsunomiya, Satoshi Ohmoto, Hiroshi TI Primary haematite formation in an oxygenated sea 3.46 billion years ago SO NATURE GEOSCIENCE LA English DT Article ID NONREDOX TRANSFORMATIONS; FOSSILS; AUSTRALIA; OXIDATION; MAGNETITE; SEDIMENTS; ORIGIN; CHERT AB The timing of the origin of photosynthesis on the early Earth is greatly debated. It is generally agreed, on the basis of the presence of biological molecules found in shales from the Hamersley Basin, Australia, that oxygenic photosynthesis had evolved 2.7 billion years (Gyr) ago. However, whether photosynthesis occurred before this time remains controversial. Here we report primary haematite crystals and associated minerals within the marine sedimentary rocks preserved in a jasper formation of the Pilbara Craton, Australia, which we interpret as evidence for the formation of these rocks in an oxygenated water body 3.46 Gyr ago. We suggest that these haematite crystals formed at temperatures greater than 60 degrees C from locally discharged hydrothermal fluids rich in ferrous iron. The crystals precipitated when the fluids rapidly mixed with overlying oxygenated sea water, at depths greater than 200m. As our findings imply the existence of noticeable quantities of molecular oxygen, we propose that organisms capable of oxygenic photosynthesis evolved more than 700 million years earlier than previously recognized, resulting in the oxygenation of at least some intermediate and deep ocean regions. C1 [Bevacqua, David C.; Otake, Tsubasa; Watanabe, Yumiko; Ohmoto, Hiroshi] Penn State Univ, NASA, Astrobiol Inst, University Pk, PA 16802 USA. [Bevacqua, David C.; Otake, Tsubasa; Watanabe, Yumiko; Ohmoto, Hiroshi] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Hoashi, Masamichi] Kagoshima Univ, Frontier Sci Res Ctr, Kagoshima 8900065, Japan. [Hickman, Arthur H.] Geol Survey Western Australia, Dept Ind & Resources, Perth, WA 6004, Australia. [Utsunomiya, Satoshi] Kyushu Univ, Dept Chem, Fukuoka 8108560, Japan. RP Ohmoto, H (reprint author), Penn State Univ, NASA, Astrobiol Inst, Univ Pk, University Pk, PA 16802 USA. EM ohmoto@geosc.psu.edu RI Otake, Tsubasa/D-6137-2012 FU The Archaean Biosphere Drilling Project; NASA; Japanese Ministry of Science, Education, Sports and Culture FX This study was carried out under The Archaean Biosphere Drilling Project (ABDP; see Supplementary Information), which was funded largely by the NASA Astrobiology Institute to H.O., the Geological Survey of Western Australia to A.H.H., the University of Western Australia to M. Barley and the Japanese Ministry of Science, Education, Sports and Culture to M. Nedachi. A.H.H. publishes with permission of the Executive Director of the Geological Survey of Western Australia. We are grateful to B. Runnegar, R. Grymes and A. Marshall for their support of the ABDP; Y. Suganuma and D. Walizer for laboratory assistance ; M. Nedachi, M. Barley, E. Altinok, K. E. Yamaguchi, Y. Kato and K. Nakamura for discussions;and P. Heaney,C. deRonde, A.W. Rose and H.L. Barnes for valuable comments on an earlier manuscript. NR 28 TC 41 Z9 47 U1 6 U2 29 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 J9 NAT GEOSCI JI Nat. Geosci. PD APR PY 2009 VL 2 IS 4 BP 301 EP 306 DI 10.1038/NGEO465 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 433XW UT WOS:000265240100023 ER PT J AU Muezzinoglu, MK Huerta, R Abarbanel, HDI Ryan, MA Rabinovich, MI AF Muezzinoglu, Mehmet K. Huerta, Ramon Abarbanel, Henry D. I. Ryan, Margaret A. Rabinovich, Mikhail I. TI Chemosensor-Driven Artificial Antennal Lobe Transient Dynamics Enable Fast Recognition and Working Memory SO NEURAL COMPUTATION LA English DT Article ID OLFACTORY NETWORK DYNAMICS; SHORT-TERM-MEMORY; ODOR REPRESENTATIONS; NEURAL ASSEMBLIES; CHEMICAL SENSORS; ELECTRONIC NOSE; MUSHROOM BODY; DROSOPHILA; SYSTEM; MODEL AB The speed and accuracy of odor recognition in insects can hardly be resolved by the raw descriptors provided by olfactory receptors alone due to their slow time constant and high variability. The animal overcomes these barriers by means of the antennal lobe (AL) dynamics, which consolidates the classificatory information in receptor signal with a spatiotemporal code that is enriched in odor sensitivity, particularly in its transient. Inspired by this fact, we propose an easily implementable AL-like network and show that it significantly expedites and enhances the identification of odors from slow and noisy artificial polymer sensor responses. The device owes its efficiency to two intrinsic mechanisms: inhibition ( which triggers a competition) and integration ( due to the dynamical nature of the network). The former functions as a sharpening filter extracting the features of receptor signal that favor odor separation, whereas the latter implements a working memory by accumulating the extracted features in trajectories. This cooperation boosts the odor specificity during the receptor transient, which is essential for fast odor recognition. C1 [Muezzinoglu, Mehmet K.; Abarbanel, Henry D. I.] Univ Calif San Diego, Inst Nonlinear Sci, Dept Phys, La Jolla, CA 92093 USA. [Ryan, Margaret A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Abarbanel, Henry D. I.] Univ Calif San Diego, Marine Phys Lab, Scripps Inst Oceanog, La Jolla, CA 92093 USA. RP Muezzinoglu, MK (reprint author), Univ Calif San Diego, Inst Nonlinear Sci, Dept Phys, La Jolla, CA 92093 USA. EM mmuezzin@ucsd.edu; rhuerta@ucsd.edu; hdia@ucsd.edu; Margaret.A.Ryan@jpl.nasa.gov; mrabinovich@ucsd.edu RI Huerta, Ramon/C-9296-2013; Huerta, Ramon/J-4316-2012 OI Huerta, Ramon/0000-0003-3925-5169; Huerta, Ramon/0000-0003-3925-5169 FU MURI [ONR N00014-07-1-0741] FX We thank Thomas Nowotny and Charles Elkan for useful comments. This work was supported by MURI grant ONR N00014-07-1-0741. The research related to the JPL Electronic Nose was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 52 TC 11 Z9 11 U1 0 U2 4 PU M I T PRESS PI CAMBRIDGE PA 238 MAIN STREET, STE 500, CAMBRIDGE, MA 02142-1046 USA SN 0899-7667 J9 NEURAL COMPUT JI Neural Comput. PD APR PY 2009 VL 21 IS 4 BP 1018 EP 1037 DI 10.1162/neco.2008.05-08-780 PG 20 WC Computer Science, Artificial Intelligence SC Computer Science GA 429BQ UT WOS:000264896200005 PM 19018701 ER PT J AU Cieciel, K Pyper, BJ Eckert, GL AF Cieciel, Kristin Pyper, Brian J. Eckert, Ginny L. TI Tag Retention and Effects of Tagging on Movement of the Giant Red Sea Cucumber Parastichopus californicus SO NORTH AMERICAN JOURNAL OF FISHERIES MANAGEMENT LA English DT Article ID CUCUMARIA-FRONDOSA; HOLOTHURIA-SCABRA; ECHINODERMATA; GROWTH; RECRUITMENT; PATTERNS AB We examined tag retention and the effects of tagging on short-term movements of the giant red sea cucumber Parastichopus californicus. Retention rates were monitored for six different tag types (Floy banner FTSL-73. cinch FT-4C, fingerling FTF-69. garment. single T-bar FD-94, and the coded wire tag), which were applied to 30 individuals under laboratory conditions. The single T-bar and coded wire tag had the highest retention rates: 70% and 60% after 16 weeks, and 40% and 37% after 32 weeks. To assess the effects of tagging and handling on movement, a field study was conducted in Amalga Harbor. Alaska, in which giant red sea cucumbers were tagged with T-bar tags and monitored for 24 h. Tagged and handled animals moved significantly farther than control animals. The median (linear) distance moved by control animals over 24 h was 1.8 m (range, 0.2-4.2 m), whereas the median distance for tagged animals was 4.2 m (range, 0.4-22.7 m). Short-term behavior was affected by both tagging and handling; therefore. we recommend that researchers minimize handling and wait at least 24 h after tagging before monitoring giant red sea cucumber movements. C1 [Cieciel, Kristin] Natl Marine Fisheries Serv, Natl Ocean & Atmospher Adm, Auke Bay Lab, Juneau, AK 99801 USA. [Eckert, Ginny L.] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Juneau Ctr, Juneau, AK 99801 USA. RP Cieciel, K (reprint author), Natl Marine Fisheries Serv, Natl Ocean & Atmospher Adm, Auke Bay Lab, 11305 Glacier Highway, Juneau, AK 99801 USA. EM kristin.cieciel@noaa.gov FU National Science Foundation REU fellowship [NSF OCE 96-102]; Alaska Department of Fish and Game (ADFG) [NA06FN0385] FX We thank K. Shotwell for Arcview aid and diving, S. McMurray for diving, and M. Cieciel and D. Greenwell for topside assistance. Funding for this project was provided by a National Science Foundation REU fellowship (NSF OCE 96-102) and a Nearshore Marine Research II award from the Alaska Department of Fish and Game (ADFG; National Oceanic and Atmospheric Administration Cooperative Agreement NA06FN0385). We extend our gratitude to the University of Alaska-Southeast and the ADFG in Juneau, Ketchikan, and Sitka for providing funding and logistical support for this project. Reference to trade names does not imply endorsement by the U.S. Government. NR 28 TC 6 Z9 7 U1 1 U2 12 PU AMER FISHERIES SOC PI BETHESDA PA 5410 GROSVENOR LANE SUITE 110, BETHESDA, MD 20814-2199 USA SN 0275-5947 J9 N AM J FISH MANAGE JI North Am. J. Fish Manage. PD APR PY 2009 VL 29 IS 2 BP 288 EP 294 DI 10.1577/M07-194.1 PG 7 WC Fisheries SC Fisheries GA 477FW UT WOS:000268505100003 ER PT J AU Grudinin, IS Yu, N Maleki, L AF Grudinin, Ivan S. Yu, Nan Maleki, Lute TI Generation of optical frequency combs with a CaF2 resonator SO OPTICS LETTERS LA English DT Article AB We demonstrate optical frequency combs using the fluorite whispering gallery mode resonator as a nonlinear Kerr medium. Two regimes of generation are observed, giving the record low repetition rate of 13 GHz, equal to the cavity's free spectral range (FSR) or high repetition rates of multiples of cavity FSR. An intermediate regime was also observed. Raman lasing spectrum similar to modulation instability in fibers was observed for the first time to the best of our knowledge. (C) 2009 Optical Society of America C1 [Grudinin, Ivan S.; Yu, Nan; Maleki, Lute] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Grudinin, IS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM grudinin@caltech.edu FU Defense Advanced Research Projects Agency (DARPA) FX We are grateful to D. Strekalov for help with measurements and to A. Matsko for helpful discussions and suggestions. This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA and with support from the Defense Advanced Research Projects Agency (DARPA). NR 18 TC 123 Z9 125 U1 4 U2 41 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0146-9592 J9 OPT LETT JI Opt. Lett. PD APR 1 PY 2009 VL 34 IS 7 BP 878 EP 880 PG 3 WC Optics SC Optics GA 436QI UT WOS:000265429100006 PM 19340157 ER PT J AU Aubrey, AD Cleaves, HJ Bada, JL AF Aubrey, A. D. Cleaves, H. J. Bada, Jeffrey L. TI The Role of Submarine Hydrothermal Systems in the Synthesis of Amino Acids SO ORIGINS OF LIFE AND EVOLUTION OF BIOSPHERES LA English DT Article DE Submarine hydrothermal systems; Amino acids; Prebiotic chemistry; Origin of life; Abiotic synthesis ID MID-ATLANTIC RIDGE; HIGH-TEMPERATURE; PREBIOTIC SYNTHESIS; ORGANIC-SYNTHESIS; HYDROGEN-CYANIDE; PRIMITIVE OCEAN; ASPARTIC-ACID; VENT FLUIDS; LIFE; FORMALDEHYDE AB There is little consensus regarding the plausibility of organic synthesis in submarine hydrothermal systems (SHSs) and its possible relevance to the origin of life. The primary reason for the persistence of this debate is that most experimental high temperature and high-pressure organic synthesis studies have neglected important geochemical constraints with respect to source material composition. We report here the results of experiments exploring the potential for amino acid synthesis at high temperature from synthetic seawater solutions of varying composition. The synthesis of amino acids was examined as a function of temperature, heating time, starting material composition and concentration. Using very favorable reactant conditions (high concentrations of reactive, reduced species), small amounts of a limited set of amino acids are generated at moderate temperature conditions (similar to 125-175A degrees C) over short heating times of a few days, but even these products are significantly decomposed after exposure times of approximately 1 week. The high concentration dependence observed for these synthetic reactions are demonstrated by the fact that a 10-fold drop in concentration results in orders of magnitude lower yields of amino acids. There may be other synthetic mechanisms not studied herein that merit investigation, but the results are likely to be similar. We conclude that although amino acids can be generated from simple likely environmentally available precursors under SHS conditions, the equilibrium at high temperatures characteristic of SHSs favors net amino acid degradation rather than synthesis, and that synthesis at lower temperatures may be more favorable. C1 [Bada, Jeffrey L.] Scripps Inst Oceanog, Geosci Res Div, La Jolla, CA 92093 USA. [Cleaves, H. J.] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. [Aubrey, A. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bada, JL (reprint author), Scripps Inst Oceanog, Geosci Res Div, 9500 Gilman Dr, La Jolla, CA 92093 USA. EM Andrew.D.Aubrey@jpl.nasa.gov; hjcleaves@ciw.edu; jbada@ucsd.edu OI Cleaves, Henderson/0000-0003-4101-0654 FU NASA Specialized Center of Research and Training (NSCORT) in Exobiology; UCSD Academic Senate Committee on Research; Oak Ridge Associated Universities through a contract with NASA FX This work was supported by the NASA Specialized Center of Research and Training (NSCORT) in Exobiology, a grant from the UCSD Academic Senate Committee on Research, and in part by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Oak Ridge Associated Universities through a contract with NASA. The authors would like to thank Dr. John H. Chalmers for laboratory assistance, and Dr. Evan A. Solomon and Prof. Joris M. Gieskes for helpful discussions. Special thanks are offered to Prof. Robert White and anonymous reviewers whose comments helped greatly improve this manuscript. NR 74 TC 31 Z9 32 U1 2 U2 36 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0169-6149 J9 ORIGINS LIFE EVOL B JI Orig. Life Evol. Biosph. PD APR PY 2009 VL 39 IS 2 BP 91 EP 108 DI 10.1007/s11084-008-9153-2 PG 18 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 425FQ UT WOS:000264622800001 PM 19034685 ER PT J AU Cleaves, HJ Aubrey, AD Bada, JL AF Cleaves, H. J. Aubrey, A. D. Bada, J. L. TI An Evaluation of the Critical Parameters for Abiotic Peptide Synthesis in Submarine Hydrothermal Systems SO ORIGINS OF LIFE AND EVOLUTION OF BIOSPHERES LA English DT Article DE Submarine hydrothermal vents; Peptides; Amino acids; Prebiotic chemistry; Origin of life; Chemical evolution ID ALPHA-AMINO-ACIDS; METAL IONS; PREBIOTIC OLIGOMERIZATION; THERMAL CONDENSATION; MINERAL SURFACES; AQUEOUS-SOLUTION; HIGH-TEMPERATURE; BOND HYDROLYSIS; FLOW REACTOR; LIFE AB It has been proposed that oligopeptides may be formed in submarine hydrothermal systems (SHSs). Oligopeptides have been synthesized previously under simulated SHS conditions which are likely geochemically implausible. We have herein investigated the oligomerization of glycine under SHS-like conditions with respect to the limitations imposed by starting amino acid concentration, heating time, and temperature. When 10(-1) M glycine solutions were heated at 250A degrees C for < 20 min glycine oligomers up to tetramers and diketopiperazine (DKP) were detectable. At 200A degrees C, less oligomerization was noted. Peptides beyond glycylglycine (gly(2)) and DKP were not detected below 150A degrees C. At 10(-2) M initial glycine concentration and below, only gly(2), DKP, and gly(3) were detected, and then only above 200A degrees C at < 20 min reaction time. Gly(3) was undetectable at longer reaction times. The major parameters limiting peptide synthesis in SHSs appear to be concentration, time, and temperature. Given the expected low concentrations of amino acids, the long residence times and range of temperatures in SHSs, it is unlikely that SHS environments were robust sources of even simple peptides. Possible unexplored solutions to the problems presented here are also discussed. C1 [Bada, J. L.] Scripps Inst Oceanog, Geosci Res Div, La Jolla, CA 92093 USA. [Aubrey, A. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cleaves, H. J.] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. RP Bada, JL (reprint author), Scripps Inst Oceanog, Geosci Res Div, 9500 Gilman Dr, La Jolla, CA 92093 USA. EM jbada@ucsd.edu OI Cleaves, Henderson/0000-0003-4101-0654 FU NASA Specialized Center of Research and Training (NSCORT) in Exobiology; UCSD Academic Senate committee on Research; Oak Ridge Associated Universities through a contract with NASA FX The authors would like to thank Dr. John H. Chalmers for assistance in the laboratory and Professor Joris Gieskes and Dr. Evan Solomon for discussions about the dynamics of hydrothermal vent systems. This work was supported by the NASA Specialized Center of Research and Training (NSCORT) in Exobiology and a grant from the UCSD Academic Senate committee on Research, and in part by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Oak Ridge Associated Universities through a contract with NASA. NR 94 TC 30 Z9 32 U1 1 U2 29 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0169-6149 J9 ORIGINS LIFE EVOL B JI Orig. Life Evol. Biosph. PD APR PY 2009 VL 39 IS 2 BP 109 EP 126 DI 10.1007/s11084-008-9154-1 PG 18 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 425FQ UT WOS:000264622800002 PM 19037745 ER PT J AU Summers, DP Noveron, J Basa, RCB AF Summers, David P. Noveron, Juan Basa, Ranor C. B. TI Energy Transduction Inside of Amphiphilic Vesicles: Encapsulation of Photochemically Active Semiconducting Particles SO ORIGINS OF LIFE AND EVOLUTION OF BIOSPHERES LA English DT Article DE Vesicles; Energy transduction; Photosynthesis; Semiconductors; Colloids; Protocells; Origin of life; Origin of photosynthesis ID BIOREDUCTIVE ALKYLATING QUINONES; PRIMITIVE EARTH CONDITIONS; F0F1 ATP SYNTHASE; ELECTRON-TRANSFER; PREBIOTIC CONDITIONS; ELECTROCHEMISTRY; MEMBRANE; LIFE; LIPOSOMES; TITANIUM AB Amphiphilic bilayer membrane structures (vesicles) have been postulated to have been abiotically formed and spontaneously assemble on the prebiotic Earth, providing compartmentalization for the origin of life. These vesicles are similar to modern cellular membranes and can serve to contain water-soluble species, concentrate species, and have the potential to catalyze reactions. The origin of the use of photochemical energy in metabolism (i.e. energy transduction) is one of the central issues in the origin of life. This includes such questions as how energy transduction may have occurred before complex enzymatic systems, such as required by contemporary photosynthesis, had developed and how simple a photochemical system is possible. It has been postulated that vesicle structures developed the ability to capture and transduce light, providing energy for reactions. It has also been shown that pH gradients across the membrane surface can be photochemically created, but coupling these to drive chemical reactions has been difficult. Colloidal semiconducting mineral particles are known to photochemically drive redox chemistry. We propose that encapsulation of these particles has the potential to provide a source of energy transduction inside vesicles, and thereby drive protocellular chemistry, and represents a model system for early photosynthesis. In our experiments we show that TiO(2) particles, in the similar to 20 nm size range, can be incorporated into vesicles and retain their photoactivity through the dehydration/rehydration cycles that have been shown to concentrate species inside a vesicle. C1 [Noveron, Juan] Univ Texas El Paso, El Paso, TX 79968 USA. [Summers, David P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Basa, Ranor C. B.] Foothill Coll, Los Altos Hills, CA USA. RP Summers, DP (reprint author), NASA, Ames Res Ctr, Mail Stop 239-4, Moffett Field, CA 94035 USA. EM David.P.Summers@nasa.gov FU NASA's Astrobiology: Exobiology and Evolutionary Biology Program FX The authors would like to gratefully acknowledge Dr. David Deamer for his advice and assistance and NASA's Astrobiology: Exobiology and Evolutionary Biology Program for financial support. NR 66 TC 11 Z9 12 U1 2 U2 12 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0169-6149 J9 ORIGINS LIFE EVOL B JI Orig. Life Evol. Biosph. PD APR PY 2009 VL 39 IS 2 BP 127 EP 140 DI 10.1007/s11084-009-9160-y PG 14 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 425FQ UT WOS:000264622800003 PM 19259781 ER PT J AU Russell, DF Balazs, GH AF Russell, Dennis F. Balazs, George H. TI Dietary Shifts by Green Turtles (Chelonia mydas) in the Kane'ohe Bay Region of the Hawaiian Islands: A 28-Year Study SO PACIFIC SCIENCE LA English DT Article ID NUTRITIONAL COMPOSITION; SEA-TURTLES; ARCHIPELAGO AB The green turtle, Chelonia mydas, has modified its feeding behavior to include the increasing abundance of normative algae growing in the greater Kane'ohe Bay area of O'ahu in the Hawaiian Islands. Changes in diet of the green turtle are correlated with an increase in abundance of seven species of nonnative algae between 1977 and 2005. Turtles were found to be eating 130 species of marine vegetation, and the three most common were the nonnative species Acanthophora spicifera, Hypnea musciformis, and Gracilaria salicornia. These three abundant and nutritious food sources are now an important part of the turtle diet in addition to native species found in and near Kane'ohe Bay. Chelonia mydas behavior has shifted to include these new seaweeds within 10 years of their introduction to the region. The turtles have also gradually included an additional four less-prolific slow-growing nonnative algal species (Eucheuma denticulatum, Gracilaria tikvahiae, Kappaphycus striatum, and Kappaphycus alvarezii), but the time it has taken turtles to include these species has been longer, 20-30 years, after the seaweeds were introduced. During this same 28-year time period numbers of C. mydas have increased throughout the Hawaiian Islands. C1 [Russell, Dennis F.] Amer Univ Sharjah, Dept Biol Chem & Environm Sci, Sharjah, U Arab Emirates. [Balazs, George H.] NOAA, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA. RP Russell, DF (reprint author), Amer Univ Sharjah, Dept Biol Chem & Environm Sci, POB 26666, Sharjah, U Arab Emirates. EM drussell@aus.edu NR 28 TC 18 Z9 21 U1 0 U2 27 PU UNIV HAWAII PRESS PI HONOLULU PA 2840 KOLOWALU ST, HONOLULU, HI 96822 USA SN 0030-8870 EI 1534-6188 J9 PAC SCI JI Pac. Sci. PD APR PY 2009 VL 63 IS 2 BP 181 EP 192 DI 10.2984/049.063.0202 PG 12 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 433ZX UT WOS:000265246100002 ER PT J AU Soenen, SA Peddle, DR Coburn, CA Hall, RJ Hall, FG AF Soenen, S. A. Peddle, D. R. Coburn, C. A. Hall, R. J. Hall, F. G. TI Canopy Reflectance Model Inversion in Multiple Forward Mode: Forest Structural Information Retrieval from Solution Set Distributions SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING LA English DT Article ID SPECTRAL MIXTURE ANALYSIS; LEAF-AREA INDEX; HEMISPHERICAL REFLECTANCES; TOPOGRAPHIC CORRECTION; BIOPHYSICAL VARIABLES; VEGETATION INDEXES; KYOTO PROTOCOL; FORWARD-MODE; CLASSIFICATION; RADIANCE AB Remote estimation of canopy structure is important in forestry and a variety of environmental applications. Multiple Forward Mode (MFM) look-tip table (LUT) inversion Of canopy reflectance models is one approach for obtaining forest canopy biophysical-structural information (BSI). MFM provides inversion results from models that are not invertible directly, and has advantages in terms of software requirements, model complexity, computational demands, and provision of physically-based BSI output. Proper handling of MFM-LUT parameterization and inherent uncertainty in the inversion procedure at the critical final BSI retrieval stage is essential, and is the theme of this paper. Three approaches are presented for deriving BSI from MFM-LUT multiple solution sets: reflectance equality (REQ), nearest spectral distance (NSD), and spectral range domain (SRD). These approaches were validated at a Rocky Mountain test site, for which SRD corresponded best with field data, with RMSE 0.4 m and 0.8 m obtained for horizontal and vertical crown radius, respectively. Recommendations for selecting MFM inversion approaches are provided for future applications. C1 [Soenen, S. A.; Peddle, D. R.; Coburn, C. A.; Hall, R. J.] Univ Lethbridge, Dept Geog, Lethbridge, AB T1K 3M4, Canada. [Hall, F. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hall, R. J.] Canadian Forest Serv, No Forest Ctr, Edmonton, AB T6H 3S5, Canada. RP Soenen, SA (reprint author), Univ Lethbridge, Dept Geog, 4401 Univ Dr W, Lethbridge, AB T1K 3M4, Canada. EM derek.peddle@uleth.ca FU Natural Sciences and Engineering Research Council of Canada (NSERC); Alberta Ingenuity Centre for Water Research (AICWR); Prairie Adaptation Research Collaborative (PARC); Water Institute for Semiarid Ecosystems (WISE); Natural Resources Canada; NASA Goddard Space Flight Centre/University of Maryland; Alberta Research Excellence Program; Miistakis Institute of the Rockies; Center for Remote Sensing, Boston University; University of Lethbridge FX This research was supported in part by grants to Dr. Peddle and collaboration from the Natural Sciences and Engineering Research Council of Canada (NSERC), Alberta Ingenuity Centre for Water Research (AICWR), Prairie Adaptation Research Collaborative (PARC), Water Institute for Semiarid Ecosystems (WISE), Natural Resources Canada, NASA Goddard Space Flight Centre/University of Maryland, Alberta Research Excellence Program, Miistakis Institute of the Rockies (DEM), Center for Remote Sensing, Boston University (GOMS model), and the University of Lethbridge. Computing resources were provided through the Western Canada Research Grid (West-Grid NETERA c3.ca). SPOT imagery was acquired from Iunctus Geomatics Corporation and the Alberta Terrestrial Imaging Centre (ATIC), both of Lethbridge Alberta. We are grateful to Sam Lieff, Adam Minke, and Kristin Yaehne for field assistance and the staff at the Kananaskis Field Stations for logistical support in the field. NR 45 TC 10 Z9 10 U1 0 U2 2 PU AMER SOC PHOTOGRAMMETRY PI BETHESDA PA 5410 GROSVENOR LANE SUITE 210, BETHESDA, MD 20814-2160 USA SN 0099-1112 J9 PHOTOGRAMM ENG REM S JI Photogramm. Eng. Remote Sens. PD APR PY 2009 VL 75 IS 4 BP 361 EP 374 PG 14 WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Geology; Remote Sensing; Imaging Science & Photographic Technology GA 430MB UT WOS:000264992100004 ER PT J AU Strekalov, DV Yu, N AF Strekalov, Dmitry V. Yu, Nan TI Generation of optical combs in a whispering gallery mode resonator from a bichromatic pump SO PHYSICAL REVIEW A LA English DT Article DE multiwave mixing; optical Kerr effect; optical pumping; optical resonators; whispering gallery modes ID LASER FREQUENCY COMB; CAVITY AB An optical comb is shown to arise from a whispering gallery mode resonator pumped by two optical frequencies. Two externally excited modes couple due to Kerr nonlinearity to initially empty modes and give rise to new frequency components. This thresholdless process is much more efficient than the previously reported single-pump four-wave mixing. As a result, a few milliwatt pump is sufficient to generate strong secondary fields that efficiently generate higher-order frequency components and so on in a cascade process leading to an optical comb. C1 [Strekalov, Dmitry V.; Yu, Nan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Strekalov, DV (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU internal Research and Technology Development program FX This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration and funded through the internal Research and Technology Development program. D. S. thanks Dr. Andrey Matsko and Dr. Anatoliy Savchenkov of OEwaves and Ivan Grudinin of Caltech for helpful discussions. NR 15 TC 29 Z9 29 U1 0 U2 16 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD APR PY 2009 VL 79 IS 4 AR 041805 DI 10.1103/PhysRevA.79.041805 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 443YO UT WOS:000265946900022 ER PT J AU Shaw, MD Bueno, J Day, P Bradford, CM Echternach, PM AF Shaw, M. D. Bueno, J. Day, P. Bradford, C. M. Echternach, P. M. TI Quantum capacitance detector: A pair-breaking radiation detector based on the single Cooper-pair box SO PHYSICAL REVIEW B LA English DT Article DE Cooper pairs; electromagnetic oscillations; infrared detectors; microwave oscillators; quasiparticles; resonators; submillimetre wave detectors; superconducting photodetectors ID SUPERCONDUCTING TRANSITION; PHOTON COUNTER; TRANSISTOR; JUNCTION AB We present a proposed design for a pair-breaking photodetector for far-infrared and submillimeter radiation. Antenna-coupled radiation generates quasiparticles in a superconducting absorber, the density of which are measured using a single Cooper-pair box. Readout is performed using an electromagnetic oscillator or a microwave resonator, which is well suited for frequency multiplexing in large arrays. Theoretical limits to detector sensitivity are discussed and modeled, with predicted sensitivities on the order of 10(-21) W/root Hz. We anticipate that this detector can be used to address key scientific goals in far-infrared and submillimeter astronomy. C1 [Shaw, M. D.] Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA. [Bueno, J.; Day, P.; Bradford, C. M.; Echternach, P. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Shaw, MD (reprint author), Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA. NR 34 TC 12 Z9 13 U1 2 U2 5 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 EI 1550-235X J9 PHYS REV B JI Phys. Rev. B PD APR PY 2009 VL 79 IS 14 AR 144511 DI 10.1103/PhysRevB.79.144511 PG 10 WC Physics, Condensed Matter SC Physics GA 443XD UT WOS:000265943200108 ER PT J AU Hannam, M Husa, S Baker, JG Boyle, M Brugmann, B Chu, T Dorband, N Herrmann, F Hinder, I Kelly, BJ Kidder, LE Laguna, P Matthews, KD van Meter, JR Pfeiffer, HP Pollney, D Reisswig, C Scheel, MA Shoemaker, D AF Hannam, Mark Husa, Sascha Baker, John G. Boyle, Michael Bruegmann, Bernd Chu, Tony Dorband, Nils Herrmann, Frank Hinder, Ian Kelly, Bernard J. Kidder, Lawrence E. Laguna, Pablo Matthews, Keith D. van Meter, James R. Pfeiffer, Harald P. Pollney, Denis Reisswig, Christian Scheel, Mark A. Shoemaker, Deirdre TI Samurai project: Verifying the consistency of black-hole-binary waveforms for gravitational-wave detection SO PHYSICAL REVIEW D LA English DT Review ID BOUNDARY VALUE-PROBLEM; NUMERICAL RELATIVITY; INITIAL DATA; GENERAL-RELATIVITY; EINSTEIN EQUATIONS; COMPACT BINARIES; MODELING KICKS; SPIN; EVOLUTION; RADIATION AB We quantify the consistency of numerical-relativity black-hole-binary waveforms for use in gravitational-wave (GW) searches with current and planned ground-based detectors. We compare previously published results for the (center dot=2,vertical bar m vertical bar=2) mode of the gravitational waves from an equal-mass nonspinning binary, calculated by five numerical codes. We focus on the 1000M (about six orbits, or 12 GW cycles) before the peak of the GW amplitude and the subsequent ringdown. We find that the phase and amplitude agree within each code's uncertainty estimates. The mismatch between the (center dot=2,vertical bar m vertical bar=2) modes is better than 10(-3) for binary masses above 60M with respect to the Enhanced LIGO detector noise curve, and for masses above 180M with respect to Advanced LIGO, Virgo, and Advanced Virgo. Between the waveforms with the best agreement, the mismatch is below 2x10(-4). We find that the waveforms would be indistinguishable in all ground-based detectors (and for the masses we consider) if detected with a signal-to-noise ratio of less than approximate to 14, or less than approximate to 25 in the best cases. C1 [Hannam, Mark] Univ Coll Cork, Dept Phys, Cork, Ireland. [Husa, Sascha] Univ Illes Balears, Dept Fis, E-07122 Palma de Mallorca, Spain. [Baker, John G.; Kelly, Bernard J.; van Meter, James R.] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA. [Boyle, Michael; Chu, Tony; Matthews, Keith D.; Pfeiffer, Harald P.; Scheel, Mark A.] CALTECH, Pasadena, CA 91125 USA. [Boyle, Michael; Kidder, Lawrence E.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [Bruegmann, Bernd] Univ Jena, Inst Theoret Phys, D-07743 Jena, Germany. [Dorband, Nils; Hinder, Ian; Pollney, Denis; Reisswig, Christian] Max Planck Inst Gravitat Phys, D-14475 Potsdam, Germany. [Herrmann, Frank] Univ Maryland, Ctr Sci Computat & Math Modeling, College Pk, MD 20742 USA. [Herrmann, Frank; Hinder, Ian; Laguna, Pablo; Shoemaker, Deirdre] Penn State Univ, Ctr Gravitat Wave Phys, University Pk, PA 16802 USA. [Laguna, Pablo; Shoemaker, Deirdre] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [van Meter, James R.] Univ Maryland Baltimore Cty, Dept Phys, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. RP Hannam, M (reprint author), Univ Coll Cork, Dept Phys, Cork, Ireland. RI van meter, james/E-7893-2011; Kelly, Bernard/G-7371-2011; OI Husa, Sascha/0000-0002-0445-1971; Reisswig, Christian/0000-0001-6855-9351 FU SFI [07/RFP/PHYF148]; VESF; European Gravitational Observatory ( EGO) [D/07/13385] FX The authors thank Badri Krishnan for the Enhanced LIGO noise curve, as provided by Rana Adhikari on behalf of the LIGO Scientific Collaboration, and Giovanni Losurdo for providing the Advanced Virgo noise curve on behalf of the Virgo Collaboration; Ben Owen and Alberto Vecchio for helpful comments on the manuscript; and Doreen Mu " ller for alerting us to a mislabeling of Fig. 4. M. Hannam was supported by SFI Grant No. 07/RFP/PHYF148, and thanks the Albert Einstein Institute in Potsdam for hospitality while some of this work was carried out. S. Husa has been supported in part by VESF and the European Gravitational Observatory ( EGO), by DAAD Grant No. D/07/13385, and by Grant No. FPA2007-60220 from the Spanish Ministerio de Educacion y Ciencia. B. Kelly was supported by the NASA Postdoctoral Program at the Oak Ridge Associated Universities. F. Herrmann, I. Hinder, P. Laguna, and D. Shoemaker acknowledge the support of the Center for Gravitational Wave Physics at Penn State funded by the National Science Foundation under Cooperative Agreement No. PHY-0114375. P. Laguna and D. Shoemaker were also supported by NSF Grant No. PHY- 0653443, No. PHY- 065303, and No. PHY- 0555436. F. Herrmann was also supported by NSF Grant No. PHY-0801213. J. NR 166 TC 56 Z9 56 U1 0 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD APR PY 2009 VL 79 IS 8 AR 084025 DI 10.1103/PhysRevD.79.084025 PG 17 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 450NQ UT WOS:000266408500087 ER PT J AU Horiuchi, S Beacom, JF Dwek, E AF Horiuchi, Shunsaku Beacom, John F. Dwek, Eli TI Diffuse supernova neutrino background is detectable in Super-Kamiokande SO PHYSICAL REVIEW D LA English DT Review ID STAR-FORMATION HISTORY; CORE-COLLAPSE SUPERNOVAE; SPITZER-SPACE-TELESCOPE; GALAXY REDSHIFT SURVEY; INITIAL MASS FUNCTION; MICRON SOURCE COUNTS; BLACK-HOLE FORMATION; GAMMA-RAYS; LUMINOSITY FUNCTION; COSMOLOGICAL IMPLICATIONS AB The diffuse supernova neutrino background (DSNB) provides an immediate opportunity to study the emission of MeV thermal neutrinos from core-collapse supernovae. The DSNB is a powerful probe of stellar and neutrino physics, provided that the core-collapse rate is large enough and that its uncertainty is small enough. To assess the important physics enabled by the DSNB, we start with the cosmic star formation history of Hopkins and Beacom (2006) and confirm its normalization and evolution by cross-checks with the supernova rate, extragalactic background light, and stellar mass density. We find a sufficient core-collapse rate with small uncertainties that translate into a variation of +/- 40% in the DSNB event spectrum. Considering thermal neutrino spectra with effective temperatures between 4-6 MeV, the predicted DSNB is within a factor 4-2 below the upper limit obtained by Super-Kamiokande in 2003. Furthermore, detection prospects would be dramatically improved with a gadolinium-enhanced Super-Kamiokande: the backgrounds would be significantly reduced, the fluxes and uncertainties converge at the lower threshold energy, and the predicted event rate is 1.2-5.6 events yr(-1) in the energy range 10-26 MeV. These results demonstrate the imminent detection of the DSNB by Super-Kamiokande and its exciting prospects for studying stellar and neutrino physics. C1 [Horiuchi, Shunsaku] Univ Tokyo, Sch Sci, Dept Phys, Tokyo 1130033, Japan. [Horiuchi, Shunsaku; Beacom, John F.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Horiuchi, Shunsaku; Beacom, John F.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Beacom, John F.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Dwek, Eli] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Horiuchi, S (reprint author), Univ Tokyo, Sch Sci, Dept Phys, Tokyo 1130033, Japan. RI Dwek, Eli/C-3995-2012 FU NSF [PHY-0547102]; NASA [LTSA 03-0000-065] FX We thank Shinichiro Ando, Maria Terese Botticella, Thomas Dahlen, Andrew Hopkins, Cecilia Lunardini, Katsuhiko Sato, Stephen Smartt, Todd Thompson, StephenWilkins, and Mark Vagins for helpful discussions; Matt Kistler and Hasan Yuksel for helpful discussions and technical assistance. S. H. thanks the hospitality of CCAPP, Ohio State University, where this work took place. S. H. was supported by CCAPP, J. F. B. was supported by NSF CAREER Grant No. PHY-0547102, and E. D. was partially supported by NASA Grant No. LTSA 03-0000-065. NR 156 TC 77 Z9 77 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD APR PY 2009 VL 79 IS 8 AR 083013 DI 10.1103/PhysRevD.79.083013 PG 14 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 450NQ UT WOS:000266408500021 ER PT J AU Rame, E Weislogel, MM AF Rame, Enrique Weislogel, Mark M. TI Gravity effects on capillary flows in sharp corners SO PHYSICS OF FLUIDS LA English DT Article DE capillarity; channel flow; flow instability ID WETTING LIQUID AB We analyze the effect of gravity on capillary flows in sharp corners. We consider gravity perpendicular and parallel to the channel axis. We analyze both steady and unsteady flows. In the steady analysis the main result is a closed form expression for the flow rate as a function of the two gravity components. Good agreement with steady experiments is offered as support of the model. The unsteady analysis is restricted to "small" values of the two gravity parameters and is accomplished using a similarity formulation. The similarity coefficients of the gravity corrections are fully determined by the coefficients of the gravityless problem. The main result of the unsteady analysis is the gravity corrections to the flow rate (or rate of advance) of the liquid in the channel. In addition, we obtain corrections for the liquid height as a function of position and time. We address in detail unsteady problems with select boundary conditions that are representative of typical flow types. In Appendix A we present a new exact solution to one of the gravityless similarity cases, which is analogous to a nonlinear heat conduction equation. In Appendix B we offer dimensional formulas for all the unsteady flow results, which are valuable for systems design and analysis. C1 [Rame, Enrique] NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res Fluids & Combust, Cleveland, OH 44135 USA. [Weislogel, Mark M.] Portland State Univ, Dept Mech & Mat Engn, Portland, OR 97201 USA. RP Rame, E (reprint author), NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res Fluids & Combust, MS 110-3, Cleveland, OH 44135 USA. NR 16 TC 5 Z9 5 U1 1 U2 10 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-6631 J9 PHYS FLUIDS JI Phys. Fluids PD APR PY 2009 VL 21 IS 4 AR 042106 DI 10.1063/1.3109685 PG 12 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA 456XF UT WOS:000266885400011 ER PT J AU Mancini, RC Bailey, JE Hawley, JF Kallman, T Witthoeft, M Rose, SJ Takabe, H AF Mancini, R. C. Bailey, J. E. Hawley, J. F. Kallman, T. Witthoeft, M. Rose, S. J. Takabe, H. TI Accretion disk dynamics, photoionized plasmas, and stellar opacities SO PHYSICS OF PLASMAS LA English DT Article; Proceedings Paper CT Meeting of the American-Physical-Society CY APR, 2008 CL St Louis, MO SP Amer Phys Soc ID DETAILED LINE TREATMENT; X-RAY SOURCES; BLACK-HOLE; SOLAR ABUNDANCES; OPTICALLY THIN; EXTREME-ULTRAVIOLET; MAGNETIC-FIELD; DRIVEN; HELIOSEISMOLOGY; ENERGY AB We present a brief review on the atomic kinetics, modeling and interpretation of astrophysical observations, and laboratory astrophysics experiments. The emphasis is on benchmarking of opacity calculations relevant for solar structure models, photoionized plasmas research, the magnetohydrodynamic numerical simulation of accretion disk dynamics, and a connection between radiation transport effects and plasma source geometry details. Specific cases of application are discussed with relevance to recent and proposed laboratory astrophysics experiments as well as Chandra and X-ray Multi-Mirror Mission Newton observations. (C) 2009 American Institute of Physics. [DOI: 10.1063/1.3101819] C1 [Mancini, R. C.] Univ Nevada, Dept Phys, Reno, NV 89557 USA. [Bailey, J. E.] Sandia Natl Labs, Albuquerque, NM 87545 USA. [Hawley, J. F.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Kallman, T.; Witthoeft, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rose, S. J.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2BZ, England. [Takabe, H.] Osaka Univ, Inst Laser Engn, Suita, Osaka 5650871, Japan. RP Mancini, RC (reprint author), Univ Nevada, Dept Phys, Reno, NV 89557 USA. OI Rose, Steven/0000-0001-6808-6355 NR 63 TC 27 Z9 27 U1 0 U2 6 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-664X J9 PHYS PLASMAS JI Phys. Plasmas PD APR PY 2009 VL 16 IS 4 AR 041001 DI 10.1063/1.3101819 PG 11 WC Physics, Fluids & Plasmas SC Physics GA 456XI UT WOS:000266885800004 ER PT J AU Landis, GA AF Landis, Geoffrey A. TI Engines for the 21st century SO PHYSICS TODAY LA English DT Letter C1 NASA, John Glenn Res Ctr, Cleveland, OH USA. RP Landis, GA (reprint author), NASA, John Glenn Res Ctr, Cleveland, OH USA. EM geoffrey.a.landis@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0031-9228 J9 PHYS TODAY JI Phys. Today PD APR PY 2009 VL 62 IS 4 BP 10 EP 10 PG 1 WC Physics, Multidisciplinary SC Physics GA 430LY UT WOS:000264991800006 ER PT J AU Lin, CL Zhang, ZW Chen, WP King, SK Lin, HC Wang, JH Mondal, S Alcock, C Axelrod, T Bianco, FB Byun, YI Coehlo, NK Cook, KH Dave, R de Pater, I Descamps, P Lehner, MJ Kim, DW Lee, T Lissauer, JJ Marshall, SL Porrata, R Protopapas, P Rice, JA Schwamb, ME Wang, SY Wen, CY AF Lin, Chi-Long Zhang, Zhi-Wei Chen, W. P. King, Sun-Kun Lin, Hung-Chin Wang, J. -H. Mondal, S. Alcock, C. Axelrod, T. Bianco, F. B. Byun, Y. -I. Coehlo, N. K. Cook, K. H. Dave, R. de Pater, I. Descamps, P. Lehner, M. J. Kim, D. -W. Lee, T. Lissauer, J. J. Marshall, S. L. Porrata, R. Protopapas, P. Rice, J. A. Schwamb, M. E. Wang, S. -Y. Wen, C. -Y. TI A Close Binary Star Resolved from Occultation by 87 Sylvia SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID ASTEROIDS; DUPLICITY AB The star BD +29 1748 was resolved to be a close binary from its occultation by the asteroid 87 Sylvia on 2006 December 18 UT. Four telescopes were used to observe this event at two sites separated by some 80 km. Two flux drops were observed at one site, whereas only one flux drop was detected at the other. From the long-term variation of Sylvia, we inferred the probable shape of the shadow during the occultation, and this in turn constrains the binary parameters: the two components of BD +29 1748 have a projected separation of 0 ''.097-0 ''.140 on the sky with a position angle 104 degrees-11 degrees 0. The asteroid was clearly resolved, with a size scale ranging from 130 to 290 km as projected onto the occultation direction, consistent with the size dimensions 385 x 265 x 230 km, measured by direct adaptive optics imaging. No occultation was detected for either of the two known moonlets of 87 Sylvia. C1 [Lin, Chi-Long] Natl Museum Nat Sci, Exhibit Div, Taichung 404, Taiwan. [Zhang, Zhi-Wei; Chen, W. P.; Lin, Hung-Chin; Wang, J. -H.; Mondal, S.] Natl Cent Univ, Inst Astron, Jhongli 32054, Taiwan. [King, Sun-Kun; Wang, J. -H.; Lehner, M. J.; Lee, T.; Wang, S. -Y.; Wen, C. -Y.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Mondal, S.] Aryabhatta Res Inst Observat Sci, Naini Tal 263129, India. [Alcock, C.; Bianco, F. B.; Lehner, M. J.; Protopapas, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Axelrod, T.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Bianco, F. B.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Byun, Y. -I.; Kim, D. -W.] Yonsei Univ, Dept Astron, Seoul 120749, South Korea. [Coehlo, N. K.; Rice, J. A.] Univ Calif Berkeley, Dept Stat, Berkeley, CA 94720 USA. [Cook, K. H.; Marshall, S. L.; Porrata, R.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. [Dave, R.; Protopapas, P.] Harvard Univ, Initiat Innovat Comp, Cambridge, MA 02138 USA. [de Pater, I.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Descamps, P.] Observ Paris, IMCCE, UMR 8028, F-75014 Paris, France. [Lissauer, J. J.] NASA, Space Sci & Astrobiol Div 245 3, Ames Res Ctr, Moffett Field, CA 94035 USA. [Marshall, S. L.] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Schwamb, M. E.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Lin, CL (reprint author), Natl Museum Nat Sci, Exhibit Div, 1 Kuan Chien Rd, Taichung 404, Taiwan. RI Lee, Typhoon/N-8347-2013 FU U. S. Department of Energy [DE-AC52-07NA27344] FX We thank David W. Dunham, Sato Isao, Dave Herald, and Mitsuru Soma for helpful discussions. KHC's work has been performed under the auspices of the U. S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. We acknowledge the anonymous referee, whose suggestions improved the quality of the paper. NR 22 TC 1 Z9 1 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD APR PY 2009 VL 121 IS 878 BP 359 EP 364 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 448BO UT WOS:000266236700005 ER PT J AU Pence, WD Seaman, R White, RL AF Pence, W. D. Seaman, R. White, R. L. TI Lossless Astronomical Image Compression and the Effects of Noise SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article AB We compare a variety of lossless image compression methods on a large sample of astronomical images and show how the compression ratios and speeds of the algorithms are affected by the amount of noise (that is, entropy) in the images. In the ideal case where the image pixel values have a random Gaussian distribution, the equivalent number of uncompressible noise bits per pixel is given by N(bits) = log(2)(sigma root 12) and the lossless compression ratio is given by R = BITPIX/(N(bits) + K) where BITPIX is the bit length of the pixel values (typically 16 or 32), and K is a measure of the efficiency of the compression algorithm. We show that real astronomical CCD images also closely follow these same relations, by using a robust algorithm for measuring the equivalent number of noise bits from the dispersion of the pixel values in background regions of the image. We perform image compression tests on a large sample of 16-bit integer astronomical CCD images using the GZIP compression program and using a newer FITS tiled-image compression method that currently supports four compression algorithms: Rice, Hcompress, PLIO, and the same Lempel-Ziv algorithm that is used by GZIP. Overall, the Rice compression algorithm strikes the best balance of compression and computational efficiency; it is 2-3 times faster and produces about 1.4 times greater compression than GZIP (the uncompression speeds are about the same). The Rice algorithm has a measured K value of 1.2 bits pixel(-1), and thus produces 75%-90% (depending on the amount of noise in the image) as much compression as an ideal algorithm with K = 0. Hcompress produces slightly better compression but at the expense of three times more CPU time than Rice. Compression tests on a sample of 32-bit integer images show similar results, but the relative speed and compression ratio advantage of Rice over GZIP is even greater. We also briefly discuss a technique for compressing floating point images that converts the pixel values to scaled integers. The image compression and uncompression utility programs used in this study (called fpack and funpack) are publicly available from the HEASARC web site. A simple command-line interface may be used to compress or uncompress any FITS image file. C1 [Pence, W. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Seaman, R.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [White, R. L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Pence, WD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM William.Pence@nasa.gov RI White, Richard/A-8143-2012 NR 23 TC 29 Z9 30 U1 0 U2 2 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 APR PY 2009 VL 121 IS 878 BP 414 EP 427 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 448BO UT WOS:000266236700011 ER PT J AU Johnson, RT Parker, PA Montgomery, DC Cutler, AD Danehy, PM Rhew, RD AF Johnson, Rachel T. Parker, Peter A. Montgomery, Douglas C. Cutler, Andrew D. Danehy, Paul M. Rhew, Ray D. TI Design Strategies for Response Surface Models for the Study of Supersonic Combustion SO QUALITY AND RELIABILITY ENGINEERING INTERNATIONAL LA English DT Article DE response surface methodology; design of experiments; robust parameter design; sub-sampling; replication AB An application of a classical design approach to an experiment involving the study of supersonic combustion is described in this paper. The case study described is that of an experiment whose objective is to create response surfaces of the mean and variance of several flow parameters as a function of location within a supersonic jet flow field. The approach demonstrated in this paper involves the use of a classic response surface methodology design in a unique manner. Additionally a unique application involving the sub-sampling and replication strategies is developed in a similar manner to those of robust parameter design. The sub-sampling and replication techniques allow for the ability to systematically account for the precision in mean and variance models of the output response variables. The final design prescribed met the experimental objectives of the project by creating the ability to fit response surfaces and allowing for the experimenters to understand the relative precision of their estimates based on the final sub-sampling and replication techniques. Results from one section of the region of interest are used to illustrate two different modeling approaches. The performance of both modeling approaches in prediction of new data is illustrated. The conclusions also include a discussion of the future work that will follow. Copyright (C) 2008 John Wiley & Sons, Ltd. C1 [Johnson, Rachel T.; Montgomery, Douglas C.] Arizona State Univ, Dept Ind Engn, Tempe, AZ 85287 USA. [Parker, Peter A.; Danehy, Paul M.; Rhew, Ray D.] NASA, Hampton, VA 23681 USA. [Cutler, Andrew D.] George Washington Univ, Newport News, VA 23602 USA. RP Johnson, RT (reprint author), Arizona State Univ, Dept Ind Engn, Tempe, AZ 85287 USA. EM rachel.t.johnson@asu.edu FU NASA Langley Research Center FX The authors gratefully acknowledge the support of Phil Drummond, Sara Tedder, and Daniel Bivolaru from NASA Langley Research Center and Gaetano Magnotti from the George Washington University for their interest, support, and application of statistical methods in the air breathing propulsion research efforts. NR 14 TC 5 Z9 5 U1 1 U2 7 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND SN 0748-8017 J9 QUAL RELIAB ENG INT JI Qual. Reliab. Eng. Int. PD APR PY 2009 VL 25 IS 3 BP 365 EP 377 DI 10.1002/qre.983 PG 13 WC Engineering, Multidisciplinary; Engineering, Industrial; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA 425NO UT WOS:000264644600009 ER PT J AU Goldblatt, C Lenton, TM Watson, AJ AF Goldblatt, C. Lenton, T. M. Watson, A. J. TI An evaluation of the long-wave radiative transfer code used in the Met Office Unified Model SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY LA English DT Article DE climate model; radiative forcing; GCM; carbon dioxide; methane; nitrous oxide; WMGHG; greenhouse gas ID CLIMATE-CHANGE; ATMOSPHERIC FLUXES; COOLING RATES; EARLY EARTH; DATABASE; CO2 AB A detailed evaluation of the radiative transfer code used in the Met Office Unified Climate-Forecast Model is performed, comparing it with a line-by-line model and testing the climatic effects of errors in a radiative-convective model. The radiative forcing at the tropopause due to CO2 changes within SIZES Scenarios and across Quaternary glacial cycles is represented with reasonable accuracy, suggesting that surface temperature will be correctly predicted. However, this is achieved by partial cancellation of opposing errors in upward and downward fluxes. The changes in the vertical profiles of radiative fluxes and the changes to surface and top-of-atmosphere fluxes all show significant errors, even at twice pre-industrial CO2. This causes a sign error in the change in the convective flux in the radiative-convective model. Performance of the code deteriorates rapidly above four times pre-industrial CO2. For less-abundant greenhouse gases, CH4 and N2O, the errors are larger as a proportion of their radiative forcings. Errors for Surface and top-of-atmosphere fluxes for CO2, are similar to those from the mean of the general circulation model (GCM) codes submitted to the intercomparison of radiation codes for IPCC AR4, implying that errors as found here may not be uncommon in climate models. A renewed emphasis on accuracy in radiative transfer calculations and openness in intercomparison Studies is necessary to improve the modelling of climate change. Copyright (C) 2009 Royal Meteorological Society C1 [Goldblatt, C.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Goldblatt, C.; Lenton, T. M.; Watson, A. J.] Univ E Anglia, Sch Environm Sci, Norwich NR4 7TJ, Norfolk, England. RP Goldblatt, C (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, MS 245-3, Moffett Field, CA 94035 USA. EM colin.goldblatt@nasa.gov NR 28 TC 11 Z9 11 U1 0 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-9009 EI 1477-870X J9 Q J ROY METEOR SOC JI Q. J. R. Meteorol. Soc. PD APR PY 2009 VL 135 IS 640 BP 619 EP 633 DI 10.1002/qj.403 PN A PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 452PB UT WOS:000266552400005 ER PT J AU Johnson, BT Christopher, S Haywood, JM Osborne, SR McFarlane, S Hsu, C Salustro, C Kahn, R AF Johnson, B. T. Christopher, S. Haywood, J. M. Osborne, S. R. McFarlane, S. Hsu, C. Salustro, C. Kahn, R. TI Measurements of aerosol properties from aircraft, satellite and ground-based remote sensing: A case-study from the Dust and Biomass-burning Experiment (DABEX) SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY LA English DT Article DE aircraft measurement; AERONET; MODIS; MISR; optical properties ID SINGLE-SCATTERING ALBEDO; RADIATIVE PROPERTIES; OPTICAL-PROPERTIES; C-130 AIRCRAFT; SOURCE REGIONS; SAFARI 2000; RETRIEVALS; ALGORITHM; THICKNESS; AFRICA AB This paper presents aircraft measurements of aerosol optical properties and radiative effects from the Dust and Biomass-burning Experiment (DABEX) over West Africa. On 19 January 2006 cloud-free skies and high aerosol loading provided ideal conditions for an intercomparison of aircraft, satellite and ground-based remote sensing instruments. Aerosol size distributions, optical properties, aerosol optical depth (AOD) and downwelling solar radiation were measured by the UK FAAM aircraft in the region of Niamey, Niger. The aircraft in situ measurements showed a mixture of dust and biomass-burning aerosols and indicated an AOD of 0.79 (at 550 nm) that compared well against AODs from the Banizoumbou Aerosol Robotic Network (AERONET) site (0.74) and a Microtops sunphotometer (0.72). AERONET size distributions showed a good degree of similarity with the aircraft in situ measurements. AERONET single-scattering albedos were also in fairly close agreement with the aircraft, having values of 0.85 and 0.87, respectively (at 550 nm). Measurements of downwelling solar radiation from the aircraft compared well with measurements from the Atmospheric Radiation Measurement (ARM) Mobile Facility (AMF) at Niamey. Radiative transfer modelling suggested a 130-160 W m(-2) instantaneous reduction of downwelling solar radiation by the aerosol column (15-18% of the total flux). Measurements of downwelling solar radiation compared reasonably well against radiative transfer modelling based on the aircraft in situ data. Satellite retrievals of AOD from MISR and MODIS Deep Blue were within 0.05 of the ground-based sunphotometers measurements although there were discrepancies in optical properties retrieved by MISR, as compared to AERONET and the aircraft. Copyright (C) Royal Meteorological Society, Crown Copyright 2009 C1 [Johnson, B. T.; Haywood, J. M.; Osborne, S. R.] Met Off, Exeter EX1 3PB, Devon, England. [McFarlane, S.] Pacific NW Natl Lab, Richland, WA 99352 USA. [Christopher, S.] Univ Alabama, Huntsville, AL 35899 USA. [Hsu, C.; Salustro, C.; Kahn, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Salustro, C.] Sci Syst & Applicat Inc, Lanham, MD USA. RP Johnson, BT (reprint author), Met Off, FitzRoy Rd, Exeter EX1 3PB, Devon, England. EM ben.johnson@metoffice.gov.uk RI McFarlane, Sally/C-3944-2008; Christopher, Sundar/E-6781-2011; Johnson, Ben/A-6563-2013; Hsu, N. Christina/H-3420-2013; Kahn, Ralph/D-5371-2012 OI Kahn, Ralph/0000-0002-5234-6359 FU Met Office; Natural Environment Research Council FX The FAAM aircraft is jointly funded by the Met Office and the Natural Environment Research Council. We thank Didier Tanre for his efforts in establishing and maintaining the Banizoumbou AERONET site, and Clare McConnell for processing the Microtops data. We thank Connor Flynn for his help with the MFRSR data, and Chuck Long and Yan Shi for processing the AMF radiometer data. NR 40 TC 32 Z9 32 U1 0 U2 13 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-9009 EI 1477-870X J9 Q J ROY METEOR SOC JI Q. J. R. Meteorol. Soc. PD APR PY 2009 VL 135 IS 641 BP 922 EP 934 DI 10.1002/qj.420 PN B PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 473QL UT WOS:000268222800008 ER PT J AU Klein, SA McCoy, RB Morrison, H Ackerman, AS Avramov, A de Boer, G Chen, MX Cole, JNS Del Genio, AD Falk, M Foster, MJ Fridlind, A Golaz, JC Hashino, T Harrington, JY Hoose, C Khairoutdinov, MF Larson, VE Liu, XH Luo, YL McFarquhar, GM Menon, S Neggers, RAJ Park, S Poellot, MR Schmidt, JM Sednev, I Shipway, BJ Shupe, MD Spangenbery, DA Sud, YC Turner, DD Veron, DE von Salzen, K Walker, GK Wang, ZE Wolf, AB Xie, SC Xu, KM Yang, FL Zhang, G AF Klein, Stephen A. McCoy, Renata B. Morrison, Hugh Ackerman, Andrew S. Avramov, Alexander de Boer, Gijs Chen, Mingxuan Cole, Jason N. S. Del Genio, Anthony D. Falk, Michael Foster, Michael J. Fridlind, Ann Golaz, Jean-Christophe Hashino, Tempei Harrington, Jerry Y. Hoose, Corinna Khairoutdinov, Marat F. Larson, Vincent E. Liu, Xiaohong Luo, Yali McFarquhar, Greg M. Menon, Surabi Neggers, Roel A. J. Park, Sungsu Poellot, Michael R. Schmidt, Jerome M. Sednev, Igor Shipway, Ben J. Shupe, Matthew D. Spangenbery, Douglas A. Sud, Yogesh C. Turner, David D. Veron, Dana E. von Salzen, Knut Walker, Gregory K. Wang, Zhien Wolf, Audrey B. Xie, Shaocheng Xu, Kuan-Man Yang, Fanglin Zhang, Gong TI Intercomparison of model simulations of mixed-phase clouds observed during the ARM Mixed-Phase Arctic Cloud Experiment. I: Single-layer cloud SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY LA English DT Review DE mixed-phase cloud; Arctic clouds; single-column models; cloud-resolving models ID COMMUNITY ATMOSPHERE MODEL; MOMENT MICROPHYSICS PARAMETERIZATION; LARGE-SCALE MODELS; LIQUID WATER PATH; STRATIFORM CLOUDS; BOUNDARY-LAYER; VERSION-3 CAM3; CLIMATE MODELS; BEAUFORT SEA; PART II AB Results are presented from an intercomparison of single-column and cloud-resolving model simulations of a cold-air outbreak mixed-phase stratocumulus cloud observed during the Atmospheric Radiation Measurement (ARM) programme's Mixed-Phase Arctic Cloud Experiment. The observed cloud occurred in a well-mixed boundary layer with a cloud-top temperature of -15 degrees C. The average liquid water path of around 160 g m(-2) was about two-thirds of the adiabatic value and far greater than the average mass of ice which when integrated from the surface to cloud top was around 15 g m(-2). Simulations of 17 single-column models (SCMs) and 9 cloud-resolving models (CRMs) are compared. While the simulated ice water path is generally consistent with observed values, the median SCM and CRM liquid water path is a factor-of-three smaller than observed. Results from a sensitivity study in which models removed ice microphysics suggest that in many models the interaction between liquid and ice-phase microphysics is responsible for the large model underestimate of liquid water path. Despite this underestimate, the simulated liquid and ice water paths of several models are consistent with observed values. Furthermore, models with more sophisticated microphysics simulate liquid and ice water paths that are in better agreement with the observed values, although considerable scatter exists. Although no single factor guarantees a good simulation, these results emphasize the need for improvement in the model representation of mixed-phase microphysics. Copyright (C) 2009 Royal Meteorological Society C1 [Klein, Stephen A.; McCoy, Renata B.; Xie, Shaocheng] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. [Morrison, Hugh] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Ackerman, Andrew S.; Del Genio, Anthony D.; Fridlind, Ann; Wolf, Audrey B.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Avramov, Alexander; Harrington, Jerry Y.] Penn State Univ, University Pk, PA 16802 USA. [de Boer, Gijs; Hashino, Tempei; Turner, David D.] Univ Wisconsin, Madison, WI USA. [Chen, Mingxuan] Colorado State Univ, Ft Collins, CO 80523 USA. [Cole, Jason N. S.] Univ British Columbia, Vancouver, BC V5Z 1M9, Canada. [Falk, Michael; Larson, Vincent E.] Univ Wisconsin, Milwaukee, WI 53201 USA. [Foster, Michael J.] Rutgers State Univ, New Brunswick, NJ 08903 USA. [Golaz, Jean-Christophe] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA. [Hoose, Corinna] ETH, Inst Atmospher & Climate Sci, Zurich, Switzerland. [Khairoutdinov, Marat F.] SUNY Stony Brook, Stony Brook, NY 11794 USA. [Liu, Xiaohong] Pacific NW Natl Lab, Richland, WA 99352 USA. [Luo, Yali] Chinese Acad Meteorol Sci, State Key Lab Severe Weather, Beijing, Peoples R China. [McFarquhar, Greg M.; Zhang, Gong] Univ Illinois, Urbana, IL 61801 USA. [Menon, Surabi; Sednev, Igor] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. [Neggers, Roel A. J.] KNMI, Utrecht, Netherlands. [Park, Sungsu] Univ Washington, Seattle, WA 98195 USA. [Poellot, Michael R.] Univ N Dakota, Grand Forks, ND 58201 USA. [Schmidt, Jerome M.] USN, Res Lab, Monterey, CA USA. [Shipway, Ben J.] Met Off, Exeter, Devon, England. [Shupe, Matthew D.] Univ Colorado, NOAA, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Spangenbery, Douglas A.] Sci Syst & Applicat Inc, Hampton, VA USA. [Sud, Yogesh C.; Walker, Gregory K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Veron, Dana E.] Univ Delaware, Newark, DE USA. [von Salzen, Knut] Canadian Ctr Climate, Vancouver, BC, Canada. [Wang, Zhien] Univ Wyoming, Laramie, WY 82071 USA. [Xu, Kuan-Man] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Yang, Fanglin] Natl Ctr Environm Predict, Camp Springs, MD USA. RP Klein, SA (reprint author), Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. EM klein21@llnl.gov RI Klein, Stephen/H-4337-2016; Hoose, Corinna/A-4295-2009; Shipway, Ben/E-1375-2011; de Boer, Gijs/F-3949-2011; Wang, Zhien/F-4857-2011; Ackerman, Andrew/D-4433-2012; Del Genio, Anthony/D-4663-2012; Fridlind, Ann/E-1495-2012; Yang, Fanglin/A-1948-2013; Xu, Kuan-Man/B-7557-2013; Xie, Shaocheng/D-2207-2013; Golaz, Jean-Christophe/D-5007-2014; Liu, Xiaohong/E-9304-2011; Shupe, Matthew/F-8754-2011 OI Klein, Stephen/0000-0002-5476-858X; Cole, Jason/0000-0003-0450-2748; McFarquhar, Greg/0000-0003-0950-0135; Hoose, Corinna/0000-0003-2827-5789; Shipway, Ben/0000-0002-7419-0789; de Boer, Gijs/0000-0003-4652-7150; Ackerman, Andrew/0000-0003-0254-6253; Del Genio, Anthony/0000-0001-7450-1359; Xu, Kuan-Man/0000-0001-7851-2629; Xie, Shaocheng/0000-0001-8931-5145; Golaz, Jean-Christophe/0000-0003-1616-5435; Liu, Xiaohong/0000-0002-3994-5955; Shupe, Matthew/0000-0002-0973-9982 FU Office of Science of the United States (US) Department of Energy [DE-AI02-94ER61768, DE-FG02-02ER63370, DE-FG02-02ER63337, DE-FG02-03ER63539, DE-FG02-05ER63955, DE-FG02-05ER63959, DE-FG02-05ER64058, DE-FG02-05ER64069, DE-AI02-06ER64173, DE-FG02-06ER64167, DE-FG02-06ER64168, DE-AI02-06ER64183, DE-FG02-06ER64187, DE-FG02-07ER64378]; US National Aeronautics and Space Administration's (NASA) [NNG06GBB1G]; National Science Foundation (NSF) [ATM-0415184, ATM-0442605, G-7424-1]; Canadian Foundation for Climate and Atmospheric Sciences; Department of Defense Center for Geosciences/Atmospheric Research at Colorado State University via Cooperative [DAAD19-02-2-0005]; Swiss National Centre of Competence in Research; Chinese Academy of Meteorological Sciences; Colorado State University under cooperative [ATM-0425247]; Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; Pacific Northwest National Laboratory is operated for the Department of Energy by Battelle Memorial Institute [DE-AC06-76RLO-1830] FX This work is supported by the Office of Science of the United States (US) Department of Energy under grants DE-AI02-94ER61768 (Del Genio), DE-FG02-02ER63370 (Chen), DE-FG02-02ER63337 (McFarquhar), DE-FG02-03ER63539 (Morrison), DE-FG02-05ER63955 (Cole), DE-FG02-05ER63959 (Park), DE-FG02-05ER64058 (Harrington), DE-FG02-05ER64069 (Wang), DE-AI02-06ER64173 (Ackerman and Fridlind), DE-FG02-06ER64167 (Turner), DE-FG02-06ER64168 (Poellot), DE-AI02-06ER64183 (Xu), DE-FG02-06ER64187 (de Boer), and DE-FG02-07ER64378 (McFarquhar). A. Ackerman and A. Fridlind are supported by the US National Aeronautics and Space Administration's (NASA) Radiation Sciences Program and the NASA Advanced Supercomputing Division. M. Chen is supported by National Science Foundation (NSF) grant ATM-0415184. J. Cole is supported by the Canadian Foundation for Climate and Atmospheric Sciences. M. Falk and V. Larson are supported by NSF grant ATM-0442605 and subaward G-7424-1 from the Department of Defense Center for Geosciences/Atmospheric Research at Colorado State University via Cooperative Agreement DAAD19-02-2-0005 with the Army Research Laboratory. C. Hoose is supported by the climate programme of the Swiss National Centre of Competence in Research. Y. Luo is supported by the Chinese Academy of Meteorological Sciences and NASA's Cloud Modeling and Analysis Initiative. H. Morrison is supported by NASA grant NNG06GBB1G and by the NSF Science and Technology Center for Multi-Scale Modeling of Atmospheric Processes, managed by Colorado State University under cooperative agreement ATM-0425247. The contribution of S. Klein, R. McCoy, and S. Xie to this work is performed under the auspices of the US Department of Energy by Lawrence Livermore National Laboratory under contract DE-AC52-07NA27344. The Pacific Northwest National Laboratory is operated for the Department of Energy by Battelle Memorial Institute under contract DE-AC06-76RLO-1830. The National Center for Atmospheric Research is sponsored by the National Science Foundation. Gratitude is expressed to A. Beljaars for providing ECMWF analysis data. Comments of R. Pincus and three anonymous reviewers are appreciated. NR 102 TC 97 Z9 97 U1 3 U2 38 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-9009 J9 Q J ROY METEOR SOC JI Q. J. R. Meteorol. Soc. PD APR PY 2009 VL 135 IS 641 BP 979 EP 1002 DI 10.1002/qj.416 PN B PG 24 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 473QL UT WOS:000268222800013 ER PT J AU Morrison, H McCoy, RB Klein, SA Xie, SC Luo, YL Avramov, A Chen, MX Cole, JNS Falk, M Foster, MJ Del Genio, AD Harrington, JY Hoose, C Khairoutdinov, MF Larson, VE Liu, XH McFarquhar, GM Poellot, MR von Salzen, K Shipway, BJ Shupe, MD Sud, YC Turner, DD Veron, DE Walker, GK Wang, ZE Wolf, AB Xu, KM Yang, FL Zhang, G AF Morrison, Hugh McCoy, Renata B. Klein, Stephen A. Xie, Shaocheng Luo, Yali Avramov, Alexander Chen, Mingxuan Cole, Jason N. S. Falk, Michael Foster, Michael J. Del Genio, Anthony D. Harrington, Jerry Y. Hoose, Corinna Khairoutdinov, Marat F. Larson, Vincent E. Liu, Xiaohong McFarquhar, Greg M. Poellot, Michael R. von Salzen, Knut Shipway, Ben J. Shupe, Matthew D. Sud, Yogesh C. Turner, David D. Veron, Dana E. Walker, Gregory K. Wang, Zhien Wolf, Audrey B. Xu, Kuan-Man Yang, Fanglin Zhang, Gong TI Intercomparison of model simulations of mixed-phase clouds observed during the ARM Mixed-Phase Arctic Cloud Experiment. II: Multilayer cloud SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY LA English DT Article DE mixed-phase cloud; Arctic clouds; single-column models; cloud-resolving models ID SINGLE-COLUMN MODEL; LIQUID WATER PATH; STRATUS CLOUDS; REMOTE SENSORS; BOUNDARY-LAYER; MICROPHYSICS; RADIATION; BULK; SHEBA; STRATOCUMULUS AB Results are presented from an intercomparison of single-column and cloud-resolving model simulations of a deep, multilayered, mixed-phase cloud system observed during the Atmospheric Radiation Measurement (ARM) Mixed-Phase Arctic Cloud Experiment. This cloud system was associated with strong surface turbulent sensible and latent heat fluxes as cold air flowed over the open Arctic Ocean, combined with a low pressure system that supplied moisture at mid-levels. The simulations, performed by 13 single-column and 4 cloud-resolving models, generally overestimate liquid water path and strongly underestimate ice water path, although there is a large spread among models. This finding is in contrast with results for the single-layer, low-level mixed-phase stratocumulus case in Part I, as well as previous studies of shallow mixed-phase Arctic clouds, that showed an underprediction of liquid water path. These results suggest important differences in the ability of models to simulate deeper Arctic mixed-phase clouds versus the shallow, single-layered mixed-phase clouds in Part I. The observed liquid-ice mass ratios were much smaller than in Part I, despite the similarity of cloud temperatures. Thus, models employing microphysics schemes with temperature-based partitioning of cloud liquid and ice masses are not able to produce results consistent with observations for both cases. Models with more sophisticated, two-moment treatment of cloud microphysics produce a somewhat smaller liquid water path closer to observations. Cloud-resolving models tend to produce a larger cloud fraction than single-column models. The liquid water path and cloud fraction have a large impact on the cloud radiative forcing at the surface, which is dominated by long-wave flux. Copyright (C) 2009 Royal Meteorological Society C1 [Morrison, Hugh] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [McCoy, Renata B.; Klein, Stephen A.; Xie, Shaocheng] Lawrence Livermore Natl Lab, Livermore, CA USA. [Avramov, Alexander; Harrington, Jerry Y.] Penn State Univ, University Pk, PA 16802 USA. [Chen, Mingxuan] Colorado State Univ, Ft Collins, CO 80523 USA. [Khairoutdinov, Marat F.] SUNY Stony Brook, Stony Brook, NY 11794 USA. [Liu, Xiaohong] Pacific NW Natl Lab, Richland, WA 99352 USA. [Luo, Yali] Chinese Acad Meterol Sci, State Key Lab Severe Weather, Beijing, Peoples R China. [Xu, Kuan-Man] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Hoose, Corinna] ETH, Inst Atmospher & Climate Sci, Zurich, Switzerland. [Cole, Jason N. S.] Univ British Columbia, Vancouver, BC V5Z 1M9, Canada. [Yang, Fanglin] Natl Ctr Environm Predict, Camp Springs, MD USA. [Sud, Yogesh C.; Walker, Gregory K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Del Genio, Anthony D.; Wolf, Audrey B.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Veron, Dana E.] Univ Delaware, Newark, DE USA. [Shipway, Ben J.] Met Off, Exeter, Devon, England. [Foster, Michael J.] Rutgers State Univ, New Brunswick, NJ 08903 USA. [Falk, Michael; Larson, Vincent E.] Univ Wisconsin, Milwaukee, WI 53201 USA. [McFarquhar, Greg M.; Zhang, Gong] Univ Illinois, Urbana, IL 61801 USA. [Shupe, Matthew D.] Univ Colorado, NOAA, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Turner, David D.] Univ Wisconsin, Madison, WI USA. [Wang, Zhien] Univ Wyoming, Laramie, WY 82071 USA. [Poellot, Michael R.] Univ N Dakota, Grand Forks, ND 58201 USA. [von Salzen, Knut] Canadian Ctr Climate, Vancouver, BC, Canada. RP Morrison, H (reprint author), Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. EM morrison@ucar.edu RI Shipway, Ben/E-1375-2011; Wang, Zhien/F-4857-2011; Del Genio, Anthony/D-4663-2012; Yang, Fanglin/A-1948-2013; Xu, Kuan-Man/B-7557-2013; Xie, Shaocheng/D-2207-2013; Liu, Xiaohong/E-9304-2011; Shupe, Matthew/F-8754-2011; Klein, Stephen/H-4337-2016; Hoose, Corinna/A-4295-2009 OI McFarquhar, Greg/0000-0003-0950-0135; Shipway, Ben/0000-0002-7419-0789; Del Genio, Anthony/0000-0001-7450-1359; Xu, Kuan-Man/0000-0001-7851-2629; Xie, Shaocheng/0000-0001-8931-5145; Liu, Xiaohong/0000-0002-3994-5955; Shupe, Matthew/0000-0002-0973-9982; Klein, Stephen/0000-0002-5476-858X; Cole, Jason/0000-0003-0450-2748; Hoose, Corinna/0000-0003-2827-5789 FU Office of Science of the United States Department of Energy [DE-A102-94ER61768, DE-FG02-02ER63337, DE-FG02-03ER63539, DE-FG02-05ER64058, DE-FG02-05ER64069, DE-FG02-06ER64167, DE-FG02-02ER63370, DE-FG02-06ER64168, DE-AI02-06ER64183, DE-FG02-07ER64378]; National Science Foundation [ATM-0415184, ATM-0442605, G7424-1]; Canadian Foundation for Climate and Atmospheric Sciences; Department of Defense Center for Geosciences/Atmospheric Research at Colorado State University via Cooperative Agreement [DAAD19-02-2-0005]; Swiss National Centre of Competence in Research; Chinese Academy of Meteorological Sciences; United States National Aeronautics and Space Administration's Cloud Modeling and Analysis Initiative; NASA [NNG06GBBIG]; Colorado State University under cooperative agreement [ATM-0425247]; US Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; Battelle Memorial Institute [DE-AC06-76RLO-1830] FX This work is supported by the Office of Science of the United States Department of Energy under grants DE-A102-94ER61768 (Del Genio), DE-FG02-02ER63337 (McFarquhar), DE-FG02-03ER63539 (Morrison), DE-FG02-05ER64058 (Harrington), DE-FG02-05ER64069 (Wang), DE-FG02-06ER64167 (Turner), DE-FG02-02ER63370 (Chen), DE-FG02-06ER64168 (Poellot), DE-AI02-06ER64183 (Xu and Luo), and DE-FG02-07ER64378 (McFarquhar). M. Chen also is also supported by National Science Foundation grant ATM-0415184. J. Cole is supported by the Canadian Foundation for Climate and Atmospheric Sciences. M. Falk and V. Larson are supported by National Science Foundation grant ATM-0442605 and sub-award G7424-1 from the Department of Defense Center for Geosciences/Atmospheric Research at Colorado State University via Cooperative Agreement DAAD19-02-2-0005 with the Army Research Laboratory. C. Hoose is supported by the climate programme of the Swiss National Centre of Competence in Research. Y. Luo is supported by the Chinese Academy of Meteorological Sciences and the United States National Aeronautics and Space Administration's Cloud Modeling and Analysis Initiative. H. Morrison is supported by NASA grant NNG06GBBIG and by the NSF Science and Technology Center for MultiScale Modeling of Atmospheric Processes, managed by Colorado State University under cooperative agreement ATM-0425247. The contribution of S. Klein, R. McCoy, and S. Xie to this work is performed under the auspices of the US Department of Energy by Lawrence Livermore National Laboratory under contract DE-AC52-07NA27344. X. Liu acknowledges that the Pacific Northwest National Laboratory is operated for the Department of Energy by Battelle Memorial Institute under contract DE-AC06-76RLO-1830. National Center for Atmospheric Research is sponsored by the National Science Foundation. Comments on the manuscript by R. Pincus and two anonymous reviewers are appreciated. NR 37 TC 36 Z9 36 U1 1 U2 19 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND SN 0035-9009 J9 Q J ROY METEOR SOC JI Q. J. R. Meteorol. Soc. PD APR PY 2009 VL 135 IS 641 BP 1003 EP 1019 DI 10.1002/qj.415 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 473QL UT WOS:000268222800014 ER PT J AU Garcia, J Sanchez, N Velasquez, R AF Garcia, J. Sanchez, N. Velasquez, R. TI QUANTITATIVE STELLAR SPECTRAL CLASSIFICATION. IV. APPLICATION TO THE OPEN CLUSTER IC 2391 SO REVISTA MEXICANA DE ASTRONOMIA Y ASTROFISICA LA English DT Article DE methods: data analysis; open clusters and associations: individual (IC 2391); stars: fundamental parameters, classification ID SOUTHERN GALACTIC CLUSTERS; IC-2391; STARS AB In this work we perform the first test of a stellar spectral classification method (Stock & Stock 1999) by applying it to early type stars. The sample of stars are the members of the open cluster IC 2391 that have high-resolution spectra available in the UVES Project of Paranal Observatory. We show that, in general; absolute magnitudes M-V and intrinsic colors (B - V)% can be recovered within the uncertainties stated in the original calibration (similar to 0.4 for the magnitudes and similar to 0.03 for the colors). This accuracy allows us to estimate distances and to infer membership of individual stars to obtain in average distance to the cluster of 156 +/- 24 pc, which is in good agreement with previously reported determinations. Finally, we identify and discuss the real strengths and limitations of this method and we suggest brow it; can be improved for future studies. C1 [Garcia, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sanchez, N.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Velasquez, R.] Univ Zulia, Ctr Modelado Cient, Maracaibo 4004, Venezuela. [Garcia, J.] Catholic Univ Amer, Dept Phys, IACS, Washington, DC 20064 USA. RP Garcia, J (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. EM javier@milkyway.gsfc.nasa.gov; nestor@iaa.es; raulv@cida.ve RI Sanchez, Nestor/K-9848-2014; OI Sanchez, Nestor/0000-0002-0042-3180 FU MEC of Spain [AYA2007-64052]; Consejeria de Educacion y Ciencia (Junta de Andalucia) [TIC-101] FX NS acknowledges financial support from MEC of Spain through grant AYA2007-64052 and from Consejeria de Educacion y Ciencia (Junta de Andalucia) through TIC-101. NR 25 TC 0 Z9 0 U1 0 U2 0 PU UNIV NACIONAL AUTONOMA MEXICO, INST DE ASTRONOMIA PI MEXICO CITY PA APDO POSTAL 70-264, MEXICO CITY 04510, MEXICO SN 0185-1101 J9 REV MEX ASTRON ASTR JI Rev. Mex. Astron. Astrofis. PD APR PY 2009 VL 45 IS 1 BP 13 EP 24 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 428ZF UT WOS:000264889900002 ER PT J AU Gizon, L Schunker, H Baldner, CS Basu, S Birch, AC Bogart, RS Braun, DC Cameron, R Duvall, TL Hanasoge, SM Jackiewicz, J Roth, M Stahn, T Thompson, MJ Zharkov, S AF Gizon, L. Schunker, H. Baldner, C. S. Basu, S. Birch, A. C. Bogart, R. S. Braun, D. C. Cameron, R. Duvall, T. L., Jr. Hanasoge, S. M. Jackiewicz, J. Roth, M. Stahn, T. Thompson, M. J. Zharkov, S. TI Helioseismology of Sunspots: A Case Study of NOAA Region 9787 SO SPACE SCIENCE REVIEWS LA English DT Review DE Sun; Sunspots; Helioseismology ID TIME-DISTANCE HELIOSEISMOLOGY; RING-DIAGRAM ANALYSIS; SOLAR ACTIVE REGIONS; MODE TRAVEL-TIMES; LOCAL HELIOSEISMOLOGY; WAVE-PROPAGATION; SOUND SPEED; P-MODES; FLOWS; INVERSION AB Various methods of helioseismology are used to study the subsurface properties of the sunspot in NOAA Active Region 9787. This sunspot was chosen because it is axisymmetric, shows little evolution during 20-28 January 2002, and was observed continuously by the MDI/SOHO instrument. AR 9787 is visible on helioseismic maps of the farside of the Sun from 15 January, i.e. days before it crossed the East limb. Oscillations have reduced amplitudes in the sunspot at all frequencies, whereas a region of enhanced acoustic power above 5.5 mHz (above the quiet-Sun acoustic cutoff) is seen outside the sunspot and the plage region. This enhanced acoustic power has been suggested to be caused by the conversion of acoustic waves into magneto-acoustic waves that are refracted back into the interior and re-emerge as acoustic waves in the quiet Sun. Observations show that the sunspot absorbs a significant fraction of the incoming p and f modes around 3 mHz. A numerical simulation of MHD wave propagation through a simple model of AR 9787 confirmed that wave absorption is likely to be due to the partial conversion of incoming waves into magneto-acoustic waves that propagate down the sunspot. Wave travel times and mode frequencies are affected by the sunspot. In most cases, wave packets that propagate through the sunspot have reduced travel times. At short travel distances, however, the sign of the travel-time shifts appears to depend sensitively on how the data are processed and, in particular, on filtering in frequency-wavenumber space. We carry out two linear inversions for wave speed: one using travel-times and phase-speed filters and the other one using mode frequencies from ring analysis. These two inversions give subsurface wave-speed profiles with opposite signs and different amplitudes. The travel-time measurements also imply different subsurface flow patterns in the surface layer depending on the filtering procedure that is used. Current sensitivity kernels are unable to reconcile these measurements, perhaps because they rely on imperfect models of the power spectrum of solar oscillations. We present a linear inversion for flows of ridge-filtered travel times. This inversion shows a horizontal outflow in the upper 4 Mm that is consistent with the moat flow deduced from the surface motion of moving magnetic features. From this study of AR 9787, we conclude that we are currently unable to provide a unified description of the subsurface structure and dynamics of the sunspot. C1 [Gizon, L.; Schunker, H.; Cameron, R.; Jackiewicz, J.; Roth, M.; Stahn, T.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Baldner, C. S.; Basu, S.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Birch, A. C.; Braun, D. C.] Colorado Res Associates, Boulder, CO 80301 USA. [Bogart, R. S.; Hanasoge, S. M.] Stanford Univ, Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Duvall, T. L., Jr.] NASA, Goddard Space Flight Ctr, Lab Solar Phys, Greenbelt, MD 20771 USA. [Thompson, M. J.; Zharkov, S.] Univ Sheffield, Sch Math & Stat, Sheffield S3 7RH, S Yorkshire, England. RP Gizon, L (reprint author), Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. EM gizon@mps.mpg.de RI Gizon, Laurent/B-9457-2008; Duvall, Thomas/C-9998-2012; Basu, Sarbani/B-8015-2014 OI Basu, Sarbani/0000-0002-6163-3472 NR 65 TC 68 Z9 68 U1 0 U2 6 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 APR PY 2009 VL 144 IS 1-4 BP 249 EP 273 DI 10.1007/s11214-008-9466-5 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 428LQ UT WOS:000264850100015 ER PT J AU Hathaway, DH AF Hathaway, David H. TI Solar Cycle Forecasting SO SPACE SCIENCE REVIEWS LA English DT Review DE Solar activity; Sunspot cycle; Solar cycle forecasting ID FLUX; AMPLITUDE; DYNAMO; MINIMUM; MODELS; FIELD; SIZE AB Predicting the behavior of a solar cycle after it is well underway (2-3 years after minimum) can be done with a fair degree of skill using auto-regression and curve fitting techniques that don't require any knowledge of the physics involved. Predicting the amplitude of a solar cycle near, or before, the time of solar cycle minimum can be done using precursors such as geomagnetic activity and polar fields that do have some connection to the physics but the connections are uncertain and the precursors provide less reliable forecasts. Predictions for the amplitude of cycle 24 using these precursor techniques give drastically different values. Recently, dynamo models have been used directly with assimilated data to predict the amplitude of sunspot cycle 24 but have also given significantly different predictions. While others have questioned both the predictability of the solar cycle and the ability of current dynamo models to provide predictions, it is clear that cycle 24 will help to discriminate between some opposing dynamo models. C1 NASA, MSFC, Huntsville, AL 35812 USA. RP Hathaway, DH (reprint author), NASA, MSFC, Huntsville, AL 35812 USA. EM David.Hathaway@nasa.gov NR 35 TC 41 Z9 42 U1 1 U2 2 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 APR PY 2009 VL 144 IS 1-4 BP 401 EP 412 DI 10.1007/s11214-008-9430-4 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 428LQ UT WOS:000264850100020 ER PT J AU Gotsis, PK Chamis, CC David, K Abdi, F AF Gotsis, P. K. Chamis, C. C. David, K. Abdi, F. TI Progressive fracture of laminated composite stiffened plate SO THEORETICAL AND APPLIED FRACTURE MECHANICS LA English DT Article DE Laminates; Composites; Stiffened panel; Simulation; Fracture; Degradation AB Laminated fiber-reinforced composite stiffened plate with [0/90/+/- 45](S) plies made of S-Glass/epoxy are evaluated via computational simulation to study damage and fracture progression. The loads are pressure and temperature which varies from 21 to 65.5 degrees C (case I) and from 143.3 to 21 degrees C (case II). An integrated computer code is used for the simulation of the damage progression. Results show that damage initiation begins at low load level, with matrix cracking at the 0 degrees (bottom and top) plies, fiber fracture at the bottom (0 degrees) ply and interply delamination at the top (0 degrees) ply. increasing the applied pressure, the damage growth is expended resulting in fracture through the thickness of the structure. At this stage, 90% of the plies damage at applied pressure 15.306 MPa for the case I and 15.036 MPa for the case II. After this stage, the cracks propagate rapidly and the structure collapses. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Gotsis, P. K.; David, K.] Inst Educ Technol, Terma Magnisias 62120, Serres, Greece. [Chamis, C. C.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Abdi, F.] Alpha STAR Corp, Long Beach, CA 90804 USA. RP Gotsis, PK (reprint author), Inst Educ Technol, Terma Magnisias 62120, Serres, Greece. EM pkgotsis@teiser.gr; Christos.C.Chamis@grc.nasa.gov; david@teiser.gr; fabdi@alphastarcorp.com FU Technological Educational Institute of Serres, Greece, FX The first author would like to thank the Research Committee of Technological Educational Institute of Serres, Greece, for funding this research project. NR 10 TC 3 Z9 3 U1 1 U2 8 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0167-8442 J9 THEOR APPL FRACT MEC JI Theor. Appl. Fract. Mech. PD APR PY 2009 VL 51 IS 2 BP 144 EP 147 DI 10.1016/j.tafmec.2009.04.008 PG 4 WC Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA 464LN UT WOS:000267506500008 ER PT J AU Borovsky, JE Lavraud, B Kuznetsova, MM AF Borovsky, Joseph E. Lavraud, Benoit Kuznetsova, Maria M. TI Polar cap potential saturation, dayside reconnection, and changes to the magnetosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID INTERPLANETARY MAGNETIC-FIELD; SOLAR-WIND; ELECTRIC-FIELD; EARTHS MAGNETOSPHERE; VISCOUS INTERACTION; IONOSPHERIC CONDUCTANCE; MHD SIMULATIONS; ALIGNED CURRENT; HILL MODEL; MAGNETOPAUSE AB Global MHD simulations of the Earth's magnetosphere using the Block-Adaptive-Tree Solarwind Roe Upwind Scheme code at the Community Coordinated Modeling Center are run with a high-resolution dayside magnetopause and variable-resolution near-Earth regions to study the phenomena of polar cap saturation. In the simulations a resistive spot is maintained on the moving magnetopause to ensure that the correct dayside reconnection rate is obtained. The solar wind parameters are held fixed, and the ionospheric Pedersen conductivity is varied. Strong reduction of the cross-polar cap potential is observed, with modest increases in the cross-polar cap current, and no changes in the local and global reconnection rates. Changes in the magnetosphere associated with the saturation of the polar cap are explored: these include a weakening of the dayside magnetic field strength, an equatorward shift of the cusps, a flattening in Z of the closed field line region of the dayside magnetosphere, and a taillike stretching of the dipole field lines at the terminator. Measurements of the currents and voltages of the polar cap indicate that the solar wind acts like a current-limited voltage generator. A simple circuit model is analyzed using measurements from the MHD simulations, and physically reasonable values for the circuit elements are obtained. Nine models for polar cap saturation are assessed against the findings of the present study. C1 [Borovsky, Joseph E.; Lavraud, Benoit] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Kuznetsova, Maria M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Borovsky, JE (reprint author), Los Alamos Natl Lab, Mail Stop D466, Los Alamos, NM 87545 USA. EM jborovsky@lanl.gov RI Kuznetsova, Maria/F-6840-2012 FU NSF National Space Weather Program ( at Los Alamos); Los Alamos LDRD Program FX The authors wish to thank Joachim Birn, Aaron Ridley, and Howard Singer for helpful conversations. All simulations were performed using the Community Coordinated Modeling Center ( CCMC) at Goddard Space Flight Center using the BATSRUS Model. The CCMC is a multiagency partnership between NASA, NSF, AFMC, AFOSR, AFRL, AFWA, NOAA, and ONR. The BATSRUS Model was developed by the Center for Space Environment Modeling at the University of Michigan. Joe Borovsky would also like to acknowledge the CCMC at NASA/Goddard Space Flight Center for their hospitality. This work was supported by the NSF National Space Weather Program ( at Los Alamos) and by the Los Alamos LDRD Program. NR 75 TC 32 Z9 32 U1 1 U2 4 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 MAR 31 PY 2009 VL 114 AR A03224 DI 10.1029/2009JA014058 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 428QZ UT WOS:000264865400006 ER PT J AU VanHandel, M Alizadeh, D Zhang, LY Kateb, B Bronikowski, M Manohara, H Badie, B AF VanHandel, Michelle Alizadeh, Darya Zhang, Leying Kateb, Babak Bronikowski, Michael Manohara, Harish Badie, Behnam TI Selective uptake of multi-walled carbon nanotubes by tumor macrophages in a murine glioma model SO JOURNAL OF NEUROIMMUNOLOGY LA English DT Article DE Carbon nanotubes; Nanotechnology; Glioma; Immunotherapy; Nanoparticles; Macrophage; Microglia; Brain tumor ID BRAIN-TUMORS; BUNDLE ARRAYS; MICROGLIA; DELIVERY; GROWTH; IMMUNOTHERAPY; SURVEILLANCE; INFLAMMATION; RESPONSES; EDEMA AB Carbon nantotubes (CNTs) are emerging as a new family of nanovectors for drug and gene delivery into biological systems. To evaluate potential application of this technology for brain tumor therapy, we, studied uptake and toxicity of multi-walled CNTs (MWCNTs) in the GL261 murine intracranial glioma model. Within 24 h of a single intratumoral injection of labeled MWCNTs (5 mu g), nearly 10-20% of total cells demonstrated CNT internalization. Most CNT uptake, however, occurred by tumor-associated macrophages (MP), which accounted for most (75%) MWCNT-positive cells. Within 24 h of injection, nearly 30% of tumor MP became MWCNT-positive. Despite a transient increase in inflammatory cell infiltration into both normal and tumor-bearing brains following MWCNT injection, no significant toxicity was noted in mice, and minor changes in tumor cytokine expression were observed. This study suggests that MWCNTs could potentially be used as a novel and non-toxic vehicle for targeting MP in brain tumors. (C) 2008 Elsevier B.V. All rights reserved. C1 [VanHandel, Michelle; Alizadeh, Darya; Zhang, Leying; Kateb, Babak; Badie, Behnam] City Hope Natl Med Ctr, Div Neurosurg, Duarte, CA 91010 USA. [VanHandel, Michelle; Alizadeh, Darya; Zhang, Leying; Kateb, Babak; Badie, Behnam] Beckman Res Inst, Duarte, CA 91010 USA. [Bronikowski, Michael; Manohara, Harish] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bronikowski, Michael; Manohara, Harish] CALTECH, Pasadena, CA 91125 USA. [Kateb, Babak] Brain Mapping Fdn, Hollywood, CA 90046 USA. RP Badie, B (reprint author), City Hope Natl Med Ctr, Div Neurosurg, 1500 E Duarte Rd, Duarte, CA 91010 USA. EM Bbadie@coh.org FU American Cancer Society Research Scholar [RSG-03-142-01-CNE]; ONR [N0001402-1 0958]; DOD [1435-04-03G17-73134]; NSF [DBI-9970143] FX This work was supported by the American Cancer Society Research Scholar Grant (RSG-03-142-01-CNE). The City of Hope Flow Cytometry Core was equipped in part through funding provided by ONR N0001402-1 0958, DOD 1435-04-03G17-73134, and NSF DBI-9970143. The nanotube synthesis work 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 (NASA). NR 41 TC 40 Z9 41 U1 1 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0165-5728 J9 J NEUROIMMUNOL JI J. Neuroimmunol. PD MAR 31 PY 2009 VL 208 IS 1-2 BP 3 EP 9 DI 10.1016/j.jneuroim.2008.12.006 PG 7 WC Immunology; Neurosciences SC Immunology; Neurosciences & Neurology GA 435QJ UT WOS:000265358100001 PM 19181390 ER PT J AU Cook, BI Miller, RL Seager, R AF Cook, Benjamin I. Miller, Ron L. Seager, Richard TI Amplification of the North American "Dust Bowl" drought through human-induced land degradation SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE dust aerosols; land surface feedbacks ID UNITED-STATES; GREAT-PLAINS; CLIMATE; VARIABILITY; 1930S; PRECIPITATION; SIMULATIONS; AEROSOLS; ANALOGS; SAHEL AB The "Dust Bowl" drought of the 1930s was highly unusual for North America, deviating from the typical pattern forced by "La Nina" with the maximum drying in the central and northern Plains, warm temperature anomalies across almost the entire continent, and widespread dust storms. General circulation models (GCMs), forced by sea surface temperatures (SSTs) from the 1930s, produce a drought, but one that is centered in southwestern North America and without the warming centered in the middle of the continent. Here, we show that the inclusion of forcing from human land degradation during the period, in addition to the anomalous SSTs, is necessary to reproduce the anomalous features of the Dust Bowl drought. The degradation over the Great Plains is represented in the GCM as a reduction in vegetation cover and the addition of a soil dust aerosol source, both consequences of crop failure. As a result of land surface feedbacks, the simulation of the drought is much improved when the new dust aerosol and vegetation boundary conditions are included. Vegetation reductions explain the high temperature anomaly over the northern U.S., and the dust aerosols intensify the drought and move it northward of the purely ocean-forced drought pattern. When both factors are included in the model simulations, the precipitation and temperature anomalies are of similar magnitude and in a similar location compared with the observations. Human-induced land degradation is likely to have not only contributed to the dust storms of the 1930s but also amplified the drought, and these together turned a modest SST-forced drought into one of the worst environmental disasters the U.S. has experienced. C1 [Cook, Benjamin I.; Seager, Richard] Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Cook, Benjamin I.; Miller, Ron L.] NASA, Goddard Inst Space Studies, New York, NY 10024 USA. RP Cook, BI (reprint author), Lamont Doherty Earth Observ, 61 Route 9W, Palisades, NY 10964 USA. EM bc9z@ldeo.columbia.edu RI Miller, Ron/E-1902-2012; Cook, Benjamin/H-2265-2012 FU National Oceanic and Atmospheric Administration (NOAA) Climate; Global Change Postdoctoral Fellowship Program; University Corporation for Atmospheric Research; Climate Dynamics Program of the National Science Foundation (NSF) [ATM-06-20066]; NOAA [NA03OAR4320179, NA06OAR4310151]; NSF [ATM-05-01878]; National Aeronautics and Space Administration Atmospheric Composition Program; Lamont [7242] FX We thank two anonymous reviewers for their comments. This work was supported by the National Oceanic and Atmospheric Administration (NOAA) Climate and Global Change Postdoctoral Fellowship Program, administered by the University Corporation for Atmospheric Research (B.I.C.), along with the Climate Dynamics Program of the National Science Foundation (NSF) through Grant ATM-06-20066. R.S. was supported by NOAA Grants NA03OAR4320179 and NA06OAR4310151 and NSF Grant ATM-05-01878. R.L.M. was additionally supported by the National Aeronautics and Space Administration Atmospheric Composition Program. This is Lamont contribution #7242. NR 30 TC 91 Z9 95 U1 18 U2 65 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAR 31 PY 2009 VL 106 IS 13 BP 4997 EP 5001 DI 10.1073/pnas.0810200106 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 427PG UT WOS:000264790600010 PM 19289836 ER PT J AU Molotch, NP AF Molotch, Noah P. TI Reconstructing snow water equivalent in the Rio Grande headwaters using remotely sensed snow cover data and a spatially distributed snowmelt model SO HYDROLOGICAL PROCESSES LA English DT Article DE snow and ice; snowmelt; modelling; remote sensing; water supply ID WESTERN UNITED-STATES; ENERGY-BALANCE; RUNOFF MODEL; MOUNTAIN BASINS; FOREST CANOPIES; BOREAL FOREST; RIVER-BASIN; RADIATION; SURFACE; SCALE AB Snow covered area (SCA) observations from the Landsat Enhanced Thematic Mapper (ETM+) were used in combination with a distributed snowmelt model to estimate snow water equivalent (SWE) in the headwaters of the Rio Grande basin (3,419 km(2)) - a spatial scale that is an order of magnitude greater than previous reconstruction model applications. In this reconstruction approach, modeled snowmelt over each pixel is integrated over the time of ETM+ observed snow cover to estimate SWE. Considerable differences in the magnitude of SWE were simulated during the study. Basin-wide mean SWE was 2.6 times greater in April 2001 versus 2002. Despite these climatological differences, the model adequately recovered SWE at intensive study areas (ISAs); mean absolute SWE error was 23% relative to observed SWE. Reconstruction model SWE errors were within one standard deviation of the mean observed SWE over 37 and 55% of the four 16-km(2) intensive field campaign study sites in 2001 and 20(12, respectively; a result comparable to previous works at much smaller scales. A key strength of the technique is that spatially distributed SWE estimates are not dependent upon ground-based observations of SWE. Moreover, the model was relatively insensitive to the location of forcing observations relative to commonly used statistical SWE interpolation models. Hence, the reconstruction technique is a viable approach for obtaining high-resolution SWE estimates at larger scales (e.g. > 1000 km(2)) and in locations where detailed hydrometeorological observations are scarce. Copyright (C) 2009 John Wiley & Sons, Ltd. C1 [Molotch, Noah P.] CALTECH, Jet Prop Lab, Water & Carbon Cycles Grp, NASA, Pasadena, CA 91109 USA. [Molotch, Noah P.] Univ Calif Los Angeles, Dept Civil & Environm Engn, Los Angeles, CA 90095 USA. RP Molotch, NP (reprint author), CALTECH, Jet Prop Lab, Water & Carbon Cycles Grp, NASA, M-S300-233,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM noah.p.molotch@jpl.nasa.gov RI Molotch, Noah/C-8576-2009 NR 59 TC 51 Z9 52 U1 1 U2 16 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND SN 0885-6087 J9 HYDROL PROCESS JI Hydrol. Process. PD MAR 30 PY 2009 VL 23 IS 7 BP 1076 EP 1089 DI 10.1002/hyp.7206 PG 14 WC Water Resources SC Water Resources GA 422XI UT WOS:000264460600012 ER PT J AU Martin, JW Moffitt, RB Mclaughlin, PA AF Martin, Joel W. Moffitt, Robert B. Mclaughlin, Patsy A. TI Additions to the decapod crustacean fauna of the Hawaiian Islands, II. First record of the unusual hermit crab genera Porcellanopagurus Filhol, 1885, and Solitariopagurus Turkay, 1986 (Decapoda, Anomura, Paguridae) SO ZOOTAXA LA English DT Article DE Hawaii; hermit crabs; Porcellanopagurus; Solitariopagurus ID CARCINIZATION; MORPHOLOGY; FICTION; FACT AB The rare and unusual deep water hermit crab genera Porcellanopagurus Filhol and Solitariopagurus Turkay are reported for the first time from Hawaiian waters. Each genus is represented by a single specimen collected from Penguin Banks, off the southwest coast of Moloka'i, Hawaii. The specimen of Porcellanopagurus is identified as P. platei, a species that has not been reported since its original description in 1902 based on specimens from the Juan Fernandez Islands off southern Chile. Therefore, the record is a major range extension for the species. The specimen of P. platei from Hawaii is an ovigerous female found inhabiting a fissurellid limpet shell; the species is redescribed based on type material. The specimen of Solitariopagurus, S. tuerkayi, was found carrying (inhabiting) one half of a bivalve mollusk shell (the lucinid Ctena bella), the first confirmation of this habitat for the species. A second specimen, photographed but now missing, was associated with a different species of bivalve (a mytilid). In addition to being new records of these genera for the Hawaiian Islands, the report also marks the first record of the genus Porcellanopagurus from the central Pacific and only the second record of the genus Solitariopagurus in the northern hemisphere. C1 [Martin, Joel W.] Nat Hist Museum Los Angeles County, Res & Collect Branch, Los Angeles, CA 90007 USA. [Moffitt, Robert B.] NOAA, Natl Marine Fisheries Serv, Honolulu, HI 96822 USA. [Mclaughlin, Patsy A.] Washington Univ, Shannon Point Marine Ctr, Anacortes, WA 98221 USA. RP Martin, JW (reprint author), Nat Hist Museum Los Angeles County, Res & Collect Branch, 900 Exposit Blvd, Los Angeles, CA 90007 USA. EM jmartin@nhm.org; Robert.Moffitt@noaa.gov; hermit@fidalgo.net NR 16 TC 4 Z9 4 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAR 30 PY 2009 IS 2057 BP 53 EP 62 PG 10 WC Zoology SC Zoology GA 425ZZ UT WOS:000264678400003 ER PT J AU Gautam, R Liu, ZY Singh, RP Hsu, NC AF Gautam, Ritesh Liu, Zhaoyan Singh, Ramesh P. Hsu, N. Christina TI Two contrasting dust-dominant periods over India observed from MODIS and CALIPSO data SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID AEROSOL AB Each year, prior to the onset of the Indian Summer Monsoon, the Gangetic Plains (GP), bounded by the high-altitude Himalayan mountains, are strongly influenced by the transport of dust outbreaks originating in the northwestern desert in India (known as the Thar Desert). Dust particles constitute the bulk of the regional aerosol loading which peaks annually during the pre-monsoon season. This paper integrates observations from space-borne sensors, namely MODIS and CALIPSO, together with ground sunphotometer measurements, to infer dust loading in the pre-monsoon aerosol build-up over source and sink regions in northern India. Detailed aerosol characterization from the synergetic observational assessment suggests that the two pre-monsoon seasons of 2007 and 2008 were strikingly contrasting in terms of the dust loading over both the Thar Desert and the GP. Further analysis of aerosol loading and optical properties, from the entire record of MODIS and sunphotometer observations, reveals that the 2007 pre-monsoon season was an unusually weak dust-laden period. Our findings suggest the plausible role of the immediately preceding excess winter monsoon rainfall in the suppressed dust activity during the 2007 pre-monsoon season. Citation:Gautam, R., Z. Liu, R. P. Singh, and N. C. Hsu (2009), Two contrasting dust-dominant periods over India observed from MODIS and CALIPSO data, Geophys. Res. Lett., 36, L06813, doi:10.1029/2008GL036967. C1 [Gautam, Ritesh] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. [Liu, Zhaoyan] Natl Inst Aerosp, Hampton, VA 23666 USA. [Singh, Ramesh P.] Chapman Univ, Dept Phys Computat Sci & Engn, Schmid Coll Sci, Orange, CA 92866 USA. [Gautam, Ritesh; Hsu, N. Christina] NASA, Goddard Space Flight Ctr, Climate & Radiat Branch, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Gautam, R (reprint author), Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. EM rgautam@umbc.edu RI Liu, Zhaoyan/A-9604-2009; Liu, Zhaoyan/B-1783-2010; Gautam, Ritesh/E-9776-2010; Singh, Ramesh/G-7240-2012; Hsu, N. Christina/H-3420-2013 OI Liu, Zhaoyan/0000-0003-4996-5738; Gautam, Ritesh/0000-0002-2177-9346; NR 18 TC 87 Z9 88 U1 2 U2 13 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 MAR 28 PY 2009 VL 36 AR L06813 DI 10.1029/2008GL036967 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 426AJ UT WOS:000264679500002 ER PT J AU Savtchenko, A AF Savtchenko, Andrey TI Deep convection and upper-tropospheric humidity: A look from the A-Train SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID PRECIPITATION; AIRS/AMSU/HSB; SATELLITE; MISSION; SYSTEMS; CLOUDS AB This work investigates the links between deep convective clouds and upper-tropospheric humidity. We collocate data from AIRS, CloudSat, and the GDAS model output, and globally average and grid our results to seasonal scales for one year, 2007. The CloudSat cloud scenario retrieval is used as a reliable identifier of deep convective events, during which we extract the nearest 300-mb humidity from AIRS and GDAS data. The zonal averages of thus screened data clearly show significant increase in the humidity, and suppression of the all-sky outgoing long-wave radiation. Citation: Savtchenko, A. (2009), Deep convection and upper-tropospheric humidity: A look from the A-Train, Geophys. Res. Lett., 36, L06814, doi:10.1029/2009GL037508. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Savtchenko, A (reprint author), NASA, Goddard Space Flight Ctr, Code 610 2,GES DISC Wyle IS, Greenbelt, MD 20771 USA. EM andrey.savtchenko@nasa.gov FU NASA [NNH05ZDA001N] FX This work is sponsored under NASA grant NRA NNH05ZDA001N-ACCESS. I would also like to extend my gratitude to Steven Platnick, Joel Susskind, and anonymous reviewers, for their constructive critique and suggestions. NR 11 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 MAR 28 PY 2009 VL 36 AR L06814 DI 10.1029/2009GL037508 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 426AJ UT WOS:000264679500006 ER PT J AU Haddad, ZS Park, KW AF Haddad, Ziad S. Park, Kyung-Won TI Vertical profiling of precipitation using passive microwave observations: The main impediment and a proposed solution SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID COMBINED RADAR; RAIN-RATE; RETRIEVAL; ALGORITHM AB Several methods have been proposed to train microwave radiometers to retrieve precipitation rates estimated by a radar that observed the same location at the same time. These radar-trained passive microwave algorithms differ in the quantities that are estimated; some estimate the vertically integrated liquid water, whereas others estimate the near-surface precipitation. Since it is no more or less credible to estimate the rain rate at the surface than it is to estimate the rain rate at any discrete altitude, it is particularly interesting to quantify to what extent it is indeed feasible to estimate vertical profiles of precipitation from a passive microwave radiometer, what the obstacles are, and what vertical resolution would be achievable. To that end, we selected five study regions and started by quantifying the vertical variability of rainfall as derived from the Tropical Rainfall Measuring Mission (TRMM) radar. Two cases emerged: a monsoon-like case where the first principal component of the vertical precipitation accounts for about 90% of the variability and a Mediterranean-like case where the first principal component accounts for about 80% of the variability. A Bayesian approach was applied to the TRMM Microwave Imager measurements colocated with the radar profiles. For the monsoon-like regions, it produced estimates of rain rates at 250-meter vertical increments, which compared well with the TRMM radar estimates. For the Mediterranean-like regions, the retrieval errors were very large. We therefore proceeded to identify the main reason for the failure of the straightforward training method. It turns out to be the unknown signature of the sea surface in the portion of the beam that does not contain precipitation. In the problematic Mediterranean case, our original straightforward approach can still be applied to measurements that do not suffer from this identifiable partial beam filling. For measurements that do, we derive a filtering approach to neutralize the variability of the partial surface signature and thus overcome the problem. C1 [Haddad, Ziad S.; Park, Kyung-Won] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Haddad, ZS (reprint author), CALTECH, Jet Prop Lab, Mail Code 300-227,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ziad.haddad@jpl.nasa.gov FU National Aeronautics and Space Administration FX We wish to thank C. Kummerow for pointing out similarities with other groups' results. This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 10 TC 5 Z9 5 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAR 28 PY 2009 VL 114 AR D06118 DI 10.1029/2008JD010744 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 426CA UT WOS:000264683900002 ER PT J AU Krishnamurti, TN Chakraborty, A Martin, A Lau, WK Kim, KM Sud, Y Walker, G AF Krishnamurti, T. N. Chakraborty, Arindam Martin, Andrew Lau, William K. Kim, Kyu-Myong Sud, Yogesh Walker, Gregory TI Impact of Arabian Sea pollution on the Bay of Bengal winter monsoon rains SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID RELAXED ARAKAWA-SCHUBERT; ATMOSPHERIC BROWN CLOUDS; INDIAN-OCEAN EXPERIMENT; PART I; STOCHASTIC CONDENSATION; GENERAL-CIRCULATION; HYDROLOGICAL CYCLE; MOIST-CONVECTION; SOUTHEAST-ASIA; SCHEME MCRAS AB Accumulation of pollution over the southern Arabian Sea has been documented in numerous studies that followed the INDOEX field project of 1992. In this paper, we show several examples of this feature from the MODIS/CALIPSO data sets. We identify this feature as the Bombay Plume that makes its way into the Arabian Sea from the west coast of India. A second part of this work is on modeling the impacts of pollution. We use a NASA Goddard Earth Observing System (GEOS) model to carry out many comparative forecast simulation experiments that include the pollution based on MODIS and control runs that utilize climatological estimates of pollutions. The model invokes both the direct and indirect effects of aerosols. Our observations are as follows: ( 1) The Arabian Sea experienced above normal rain during these periods for the MODIS experiments as compared to the control. ( 2) The most interesting feature is the divergent outflow center, in the upper troposphere, over polluted regions of the atmosphere over the Arabian Sea as a consequence of tropospheric aerosol heating. ( 3) An important related feature is a compensating downward lobe with a divergent inflow in the upper troposphere center over the Bay of Bengal. ( 4) The presence of this downward lobe over the Bay of Bengal relates to a reduction of winter monsoon rains over the southeast coast of India. ( 5) We also show evidence of similarly reduced winter monsoon rains in raingauge data over the southeast coast of India during high-pollution events ascertained from MODIS data. C1 [Krishnamurti, T. N.; Chakraborty, Arindam; Martin, Andrew] Florida State Univ, Dept Meteorol, Tallahassee, FL 32306 USA. [Kim, Kyu-Myong; Sud, Yogesh; Walker, Gregory] NASA, Goddard Space Flight Ctr, Climate & Radiat Branch Code 613 2, Greenbelt, MD 20771 USA. [Lau, William K.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 613, Greenbelt, MD 20771 USA. [Kim, Kyu-Myong] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Walker, Gregory] Sci Applicat Int Corp, Beltsville, MD USA. RP Krishnamurti, TN (reprint author), Florida State Univ, Dept Meteorol, Room 404 Love Bldg,1017 Acad Way, Tallahassee, FL 32306 USA. EM tnk@io.met.fsu.edu RI Kim, Kyu-Myong/G-5398-2014; Chakraborty, Arindam/M-9044-2014; Lau, William /E-1510-2012 OI Chakraborty, Arindam/0000-0002-4288-0216; Lau, William /0000-0002-3587-3691 FU NSF [ATM-0533966] FX This work was supported by NSF grant ATM-0533966. NR 38 TC 24 Z9 24 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 MAR 28 PY 2009 VL 114 AR D06213 DI 10.1029/2008JD010679 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 426CA UT WOS:000264683900001 ER PT J AU Gamayunov, KV Khazanov, GV Liemohn, MW Fok, MC Ridley, AJ AF Gamayunov, K. V. Khazanov, G. V. Liemohn, M. W. Fok, M. -C. Ridley, A. J. TI Self-consistent model of magnetospheric electric field, ring current, plasmasphere, and electromagnetic ion cyclotron waves: Initial results SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Review ID GLOBAL MAGNETOHYDRODYNAMIC SIMULATIONS; ITERATIVE MAPPING PROCEDURE; 1-2 MAGNETIC PULSATIONS; PITCH-ANGLE SCATTERING; LAW BOUNDARY-CONDITION; EQUATORIAL MAGNETOSPHERE; GEOMAGNETIC STORMS; OUTER MAGNETOSPHERE; EMIC WAVES; IONOSPHERE AB Further development of our self-consistent model of interacting ring current (RC) ions and electromagnetic ion cyclotron (EMIC) waves is presented. This model incorporates large-scale magnetosphere-ionosphere coupling and treats self-consistently not only EMIC waves and RC ions, but also the magnetospheric electric field, RC, and plasmasphere. Initial simulations indicate that the region beyond geostationary orbit should be included in the simulation of the magnetosphere-ionosphere coupling. Additionally, a self-consistent description, based on first principles, of the ionospheric conductance is required. These initial simulations further show that in order to model the EMIC wave distribution and wave spectral properties accurately, the plasmasphere should also be simulated self-consistently, since its fine structure requires as much care as that of the RC. Finally, an effect of the finite time needed to reestablish a new potential pattern throughout the ionosphere and to communicate between the ionosphere and the equatorial magnetosphere cannot be ignored. C1 [Gamayunov, K. V.] NASA, George C Marshall Space Flight Ctr, USRA, Huntsville, AL 35805 USA. [Khazanov, G. V.; Fok, M. -C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Liemohn, M. W.; Ridley, A. J.] Univ Michigan, Atmospher Ocean & Space Sci Dept, Ann Arbor, MI 49109 USA. RP Gamayunov, KV (reprint author), NASA, George C Marshall Space Flight Ctr, USRA, 320 Sparkman Dr, Huntsville, AL 35805 USA. EM konstantin.gamayunov-1@nasa.gov; george.v.khazanov@nasa.gov; liemohn@umich.edu; mei-ching.h.fok@nasa.gov; ridley@umich.edu RI Gamayunov, Konstantin/A-8505-2009; Ridley, Aaron/F-3943-2011; Fok, Mei-Ching/D-1626-2012; Liemohn, Michael/H-8703-2012; feggans, john/F-5370-2012 OI Gamayunov, Konstantin/0000-0002-8768-8527; Ridley, Aaron/0000-0001-6933-8534; Liemohn, Michael/0000-0002-7039-2631; FU NASA [UPN 370-16-10]; NASA HQ POLAR Project; NASA LWS Program FX We would like to thank M. Thomsen for providing LANL data. The solar wind magnetic field and plasma data are obtained from the CDAWeb maintained by the MFI team (R. Lepping, PI) and the SWE team (K. Ogilvie, PI) of the Wind satellite. We thank D. Ober for providing the code of the dynamic global core plasma model. Funding in support of this study was provided by NASA grant UPN 370-16-10, NASA HQ POLAR Project, and the NASA LWS Program.; [51] Zuyin Pu thanks the reviewers for their assistance in evaluating this paper. NR 119 TC 18 Z9 18 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAR 28 PY 2009 VL 114 AR A03221 DI 10.1029/2008JA013597 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 426DE UT WOS:000264687200001 ER PT J AU Reale, O Lau, WK Susskind, J Brin, E Liu, E Riishojgaard, LP Fuentes, M Rosenberg, R AF Reale, O. Lau, W. K. Susskind, J. Brin, E. Liu, E. Riishojgaard, L. P. Fuentes, M. Rosenberg, R. TI AIRS impact on the analysis and forecast track of tropical cyclone Nargis in a global data assimilation and forecasting system SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB Tropical cyclones in the northern Indian Ocean pose serious challenges to operational weather forecasting systems, partly due to their shorter lifespan and more erratic track, compared to those in the Atlantic and the Pacific. Moreover, the automated analyses of cyclones over the northern Indian Ocean, produced by operational global data assimilation systems (DASs), are generally of inferior quality than in other basins, partly because of asymmetric data distribution and the absence of targeted observations inside cyclones. In this work it is shown that the assimilation of Atmospheric Infrared Sounder (AIRS) temperature retrievals under partial cloudy conditions can significantly impact the representation of the cyclone Nargis (which caused devastating loss of life in Myanmar in May 2008) in a global DAS. Forecasts produced from these improved analyses by a global model produce substantially smaller track errors. The impact of the assimilation of clear-sky radiances on the same DAS and forecasting system is positive, but smaller than the one obtained by ingestion of AIRS retrievals, probably due to poorer coverage. Citation: Reale, O., W. K. Lau, J. Susskind, E. Brin, E. Liu, L. P. Riishojgaard, M. Fuentes, and R. Rosenberg (2009), AIRS impact on the analysis and forecast track of tropical cyclone Nargis in a global data assimilation and forecasting system, Geophys. Res. Lett., 36, L06812, doi: 10.1029/2008GL037122. C1 [Reale, O.; Lau, W. K.; Susskind, J.; Fuentes, M.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Brin, E.; Rosenberg, R.] NASA, Goddard Space Flight Ctr, Software Integrat & Visualizat Off, Greenbelt, MD 20771 USA. [Reale, O.; Riishojgaard, L. P.] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. [Brin, E.; Liu, E.; Rosenberg, R.] Sci Applicat Int Corp, Beltsville, MD USA. [Liu, E.; Riishojgaard, L. P.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Riishojgaard, L. P.] Joint Ctr Satellite Data Assimilat, Camp Springs, MD USA. [Fuentes, M.] Howard Univ, Program Atmospher Sci, Washington, DC 20059 USA. RP Reale, O (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 613, Greenbelt, MD 20771 USA. EM oreste.reale-1@nasa.gov RI Lau, William /E-1510-2012 OI Lau, William /0000-0002-3587-3691 FU NASA [MAP/04-0180-0070] FX The authors thank Don Anderson for support through grant MAP/04-0180-0070 and acknowledge use of NASA High-End Computing systems. Thanks are due to Bo-Wen Shen for helpful comments. NR 15 TC 36 Z9 36 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 MAR 27 PY 2009 VL 36 AR L06812 DI 10.1029/2008GL037122 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 426AG UT WOS:000264679200003 ER PT J AU Lahiri, M Wolf, E Fischer, DG Shirai, T AF Lahiri, Mayukh Wolf, Emil Fischer, David G. Shirai, Tomohiro TI Determination of Correlation Functions of Scattering Potentials of Stochastic Media from Scattering Experiments SO PHYSICAL REVIEW LETTERS LA English DT Article ID X-RAYS AB The classic "Ewald-sphere construction" for determining the structure of crystalline objects from x-ray and neutron diffraction experiments is generalized to determine the correlation functions of scattering potentials of stationary random media from scattering experiments. C1 [Lahiri, Mayukh; Wolf, Emil] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Wolf, Emil] Univ Rochester, Inst Opt, Rochester, NY 14627 USA. [Fischer, David G.] NASA, Glenn Res Ctr, Res & Technol Directorate, Cleveland, OH 44135 USA. [Shirai, Tomohiro] AIST, Photon Res Inst, Tsukuba, Ibaraki 3058564, Japan. RP Lahiri, M (reprint author), Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. EM ewlupus@pas.rochester.edu RI Shirai, Tomohiro/A-2589-2013 OI Shirai, Tomohiro/0000-0002-6210-0619 FU US Air Force Office of Scientific Research [FA9550-08-1-0417]; Air Force Research Laboratory (ARFC) [FA9451-04-C-0296] FX We would like to express our gratitude to Prof. Miguel Alonso for helpful comments and to Mrs. Sandra Cherin for help with checking the references. This research was supported by the US Air Force Office of Scientific Research under Grant No. FA9550-08-1-0417 and by the Air Force Research Laboratory (ARFC) under Contract No. FA9451-04-C-0296. NR 14 TC 49 Z9 53 U1 2 U2 4 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 MAR 27 PY 2009 VL 102 IS 12 AR 123901 DI 10.1103/PhysRevLett.102.123901 PG 4 WC Physics, Multidisciplinary SC Physics GA 425JF UT WOS:000264632100022 PM 19392277 ER PT J AU Abdo, AA Ackermann, M Arimoto, M Asano, K Atwood, WB Axelsson, M Baldini, L Ballet, J Band, DL Barbiellini, G Baring, MG Bastieri, D Battelino, M Baughman, BM Bechtol, K Bellardi, F Bellazzini, R Berenji, B Bhat, PN Bissaldi, E Blandford, RD Bloom, ED Bogaert, G Bogart, JR Bonamente, E Bonnell, J Borgland, AW Bouvier, A Bregeon, J Brez, A Briggs, MS Brigida, M Bruel, P Burnett, TH Burrows, D Busetto, G Caliandro, GA Cameron, RA Caraveo, PA Casandjian, JM Ceccanti, M Cecchi, C Celotti, A Charles, E Chekhtman, A Cheung, CC Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Cominsky, LR Connaughton, V Conrad, J Costamante, L Cutini, S DeKlotz, M Dermer, CD de Angelis, A de Palma, F Digel, SW Dingus, BL Silva, EDE Drell, PS Dubois, R Dumora, D Edmonds, Y Evans, PA Fabiani, D Farnier, C Favuzzi, C Finke, J Fishman, G Focke, WB Frailis, M Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giebels, B Giglietto, N Giommi, P Giordano, F Glanzman, T Godfrey, G Goldstein, A Granot, J Greiner, J Grenier, IA Grondin, MH Grove, JE Guillemot, L Guiriec, S Haller, G Hanabata, Y Harding, AK Hayashida, M Hays, E Morata, JAH Hoover, A Hughes, RE Johannesson, G Johnson, AS Johnson, RP Johnson, TJ Johnson, WN Kamae, T Katagiri, H Kataoka, J Kavelaars, A Kawai, N Kelly, H Kennea, J Kerr, M Kippen, RM Knodlseder, J Kocevski, D Kocian, ML Komin, N Kouveliotou, C Kuehn, F Kuss, M Lande, J Landriu, D Larsson, S Latronico, L Lavalley, C Lee, B Lee, SH Lemoine-Goumard, M Lichti, GG Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Madejski, GM Makeev, A Marangelli, B Mazziotta, MN McBreen, S McEnery, JE McGlynn, S Meegan, C Meszaros, P Meurer, C Michelson, PF Minuti, M Mirizzi, N Mitthumsiri, W Mizuno, T Moiseev, AA Monte, C Monzani, ME Moretti, E Morselli, A Moskalenko, IV Murgia, S Nakamori, T Nelson, D Nolan, PL Norris, JP Nuss, E Ohno, M Ohsugi, T Okumura, A Omodei, N Orlando, E Ormes, JF Ozaki, M Paciesas, WS Paneque, D Panetta, JH Parent, D Pelassa, V Pepe, M Perri, M Pesce-Rollins, M Petrosian, V Pinchera, M Piron, F Porter, TA Preece, R Raino, S Ramirez-Ruiz, E Rando, R Rapposelli, E Razzano, M Razzaque, S Rea, N Reimer, A Reimer, O Reposeur, T Reyes, LC Ritz, S Rochester, LS Rodriguez, AY Roth, M Ryde, F Sadrozinski, HFW Sanchez, D Sander, A Parkinson, PMS Scargle, JD Schalk, TL Segal, KN Sgro, C Shimokawabe, T Siskind, EJ Smith, DA Smith, PD Spandre, G Spinelli, P Stamatikos, M Starck, JL Stecker, FW Steinle, H Stephens, TE Strickman, MS Suson, DJ Tagliaferri, G Tajima, H Takahashi, H Takahashi, T Tanaka, T Tenze, A Thayer, JB Thayer, JG Thompson, DJ Tibaldo, L Torres, DF Tosti, G Tramacere, A Turri, M Tuvi, S Usher, TL van der Horst, AJ Vigiani, L Vilchez, N Vitale, V von Kienlin, A Waite, AP Williams, DA Wilson-Hodge, C Winer, BL Wood, KS Wu, XF Yamazaki, R Ylinen, T Ziegler, M AF Abdo, A. A. Ackermann, M. Arimoto, M. Asano, K. Atwood, W. B. Axelsson, M. Baldini, L. Ballet, J. Band, D. L. Barbiellini, G. Baring, M. G. Bastieri, D. Battelino, M. Baughman, B. M. Bechtol, K. Bellardi, F. Bellazzini, R. Berenji, B. Bhat, P. N. Bissaldi, E. Blandford, R. D. Bloom, E. D. Bogaert, G. Bogart, J. R. Bonamente, E. Bonnell, J. Borgland, A. W. Bouvier, A. Bregeon, J. Brez, A. Briggs, M. S. Brigida, M. Bruel, P. Burnett, T. H. Burrows, D. Busetto, G. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Casandjian, J. M. Ceccanti, M. Cecchi, C. Celotti, A. Charles, E. Chekhtman, A. Cheung, C. C. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Cominsky, L. R. Connaughton, V. Conrad, J. Costamante, L. Cutini, S. DeKlotz, M. Dermer, C. D. de Angelis, A. de Palma, F. Digel, S. W. Dingus, B. L. do Couto e Silva, E. Drell, P. S. Dubois, R. Dumora, D. Edmonds, Y. Evans, P. A. Fabiani, D. Farnier, C. Favuzzi, C. Finke, J. Fishman, G. Focke, W. B. Frailis, M. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giebels, B. Giglietto, N. Giommi, P. Giordano, F. Glanzman, T. Godfrey, G. Goldstein, A. Granot, J. Greiner, J. Grenier, I. A. Grondin, M. -H. Grove, J. E. Guillemot, L. Guiriec, S. Haller, G. Hanabata, Y. Harding, A. K. Hayashida, M. Hays, E. Morata, J. A. Hernando Hoover, A. Hughes, R. E. Johannesson, G. Johnson, A. S. Johnson, R. P. Johnson, T. J. Johnson, W. N. Kamae, T. Katagiri, H. Kataoka, J. Kavelaars, A. Kawai, N. Kelly, H. Kennea, J. Kerr, M. Kippen, R. M. Knoedlseder, J. Kocevski, D. Kocian, M. L. Komin, N. Kouveliotou, C. Kuehn, F. Kuss, M. Lande, J. Landriu, D. Larsson, S. Latronico, L. Lavalley, C. Lee, B. Lee, S. -H. Lemoine-Goumard, M. Lichti, G. G. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Madejski, G. M. Makeev, A. Marangelli, B. Mazziotta, M. N. McBreen, S. McEnery, J. E. McGlynn, S. Meegan, C. Meszaros, P. Meurer, C. Michelson, P. F. Minuti, M. Mirizzi, N. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Moretti, E. Morselli, A. Moskalenko, I. V. Murgia, S. Nakamori, T. Nelson, D. Nolan, P. L. Norris, J. P. Nuss, E. Ohno, M. Ohsugi, T. Okumura, A. Omodei, N. Orlando, E. Ormes, J. F. Ozaki, M. Paciesas, W. S. Paneque, D. Panetta, J. H. Parent, D. Pelassa, V. Pepe, M. Perri, M. Pesce-Rollins, M. Petrosian, V. Pinchera, M. Piron, F. Porter, T. A. Preece, R. Raino, S. Ramirez-Ruiz, E. Rando, R. Rapposelli, E. Razzano, M. Razzaque, S. Rea, N. Reimer, A. Reimer, O. Reposeur, T. Reyes, L. C. Ritz, S. Rochester, L. S. Rodriguez, A. Y. Roth, M. Ryde, F. Sadrozinski, H. F. -W. Sanchez, D. Sander, A. Parkinson, P. M. Saz Scargle, J. D. Schalk, T. L. Segal, K. N. Sgro, C. Shimokawabe, T. Siskind, E. J. Smith, D. A. Smith, P. D. Spandre, G. Spinelli, P. Stamatikos, M. Starck, J. -L. Stecker, F. W. Steinle, H. Stephens, T. E. Strickman, M. S. Suson, D. J. Tagliaferri, G. Tajima, H. Takahashi, H. Takahashi, T. Tanaka, T. Tenze, A. Thayer, J. B. Thayer, J. G. Thompson, D. J. Tibaldo, L. Torres, D. F. Tosti, G. Tramacere, A. Turri, M. Tuvi, S. Usher, T. L. van der Horst, A. J. Vigiani, L. Vilchez, N. Vitale, V. von Kienlin, A. Waite, A. P. Williams, D. A. Wilson-Hodge, C. Winer, B. L. Wood, K. S. Wu, X. F. Yamazaki, R. Ylinen, T. Ziegler, M. CA Fermi LAT Collaboration Fermi GBM Collaboration TI Fermi Observations of High-Energy Gamma-Ray Emission from GRB 080916C SO SCIENCE LA English DT Article ID BURST SPECTRA; BATSE OBSERVATIONS; SHOCK MODEL; NEUTRINOS; COMPONENT; PHOTONS AB Gamma-ray bursts (GRBs) are highly energetic explosions signaling the death of massive stars in distant galaxies. The Gamma-ray Burst Monitor and Large Area Telescope onboard the Fermi Observatory together record GRBs over a broad energy range spanning about 7 decades of gamma-ray energy. In September 2008, Fermi observed the exceptionally luminous GRB 080916C, with the largest apparent energy release yet measured. The high-energy gamma rays are observed to start later and persist longer than the lower energy photons. A simple spectral form fits the entire GRB spectrum, providing strong constraints on emission models. The known distance of the burst enables placing lower limits on the bulk Lorentz factor of the outflow and on the quantum gravity mass. C1 [Baughman, B. M.; Bhat, P. N.; Briggs, M. S.; Connaughton, V.; Goldstein, A.; Paciesas, W. S.] Univ Alabama, Huntsville, AL 35899 USA. [Abdo, A. A.; Chekhtman, A.; Dermer, C. D.; Finke, J.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Makeev, A.; Razzaque, S.; Strickman, M. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Ackermann, M.; Blandford, R. D.; Bloom, E. D.; Bogart, J. R.; Borgland, A. W.; Bouvier, A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Costamante, L.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Edmonds, Y.; Focke, W. 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[de Angelis, A.; Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.; Frailis, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Coll Udine, I-33100 Udine, Italy. [Dingus, B. L.; Hoover, A.; Kippen, R. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Dumora, D.; Grondin, M. -H.; Guillemot, L.; Lemoine-Goumard, M.; Lott, B.; Parent, D.; Reposeur, T.; Smith, D. A.] CEN Bordeaux Gradignan, CNRS, IN2P3, UMR 5797, F-33175 Gradignan, France. [Dumora, D.; Grondin, M. -H.; Guillemot, L.; Lemoine-Goumard, M.; Lott, B.; Parent, D.; Reposeur, T.; Smith, D. A.] Univ Bordeaux, CEN Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France. [Evans, P. A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Fishman, G.; Kouveliotou, C.; Meegan, C.; Preece, R.; van der Horst, A. J.; Wilson-Hodge, C.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. [Katagiri, H.; Mizuno, T.; Ohsugi, T.; Takahashi, H.; Yamazaki, R.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima 7398526, Japan. [Katagiri, H.; Mizuno, T.; Ohsugi, T.; Takahashi, H.; Yamazaki, R.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima 7398526, Japan. [Gehrels, N.; Johnson, T. J.; Ritz, S.] Univ Maryland, College Pk, MD 20742 USA. Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Morata, J. A. Hernando] European Org Nucl Res CERN, CH-1211 Geneva, Switzerland. [Kawai, N.] Inst Phys & Chem Res RIKEN, Cosm Radiat Lab, Wako, Saitama 3510198, Japan. [Knoedlseder, J.; Vilchez, N.] UPS, CNRS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. [Lee, B.] Orbital Network Engn, Cupertino, CA 95014 USA. [McBreen, S.] Univ Coll Dublin, Dublin 4, Ireland. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Norris, J. P.; Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. 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F.] J CPNPC, Nanjing 210093, Peoples R China. [Wu, X. F.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. [Ylinen, T.] Univ Kalmar, Sch Pure & Appl Nat Sci, SE-39182 Kalmar, Sweden. RP Briggs, MS (reprint author), Univ Alabama, Huntsville, AL 35899 USA. EM michael.briggs@nasa.gov; charles.dermer@nrl.navy.mil; htajima@slac.stanford.edu RI Nolan, Patrick/A-5582-2009; De Angelis, Alessandro/B-5372-2009; Starck, Jean-Luc/D-9467-2011; Thompson, David/D-2939-2012; Stecker, Floyd/D-3169-2012; Harding, Alice/D-3160-2012; Gehrels, Neil/D-2971-2012; McEnery, Julie/D-6612-2012; Baldini, Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Morselli, Aldo/G-6769-2011; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Tosti, Gino/E-9976-2013; Komin, Nukri/J-6781-2015; Bissaldi, Elisabetta/K-7911-2016; Wu, Xuefeng/G-5316-2015; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; Saz Parkinson, Pablo Miguel/I-7980-2013; Ozaki, Masanobu/K-1165-2013; Rando, Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Johnson, Neil/G-3309-2014; Reimer, Olaf/A-3117-2013; Funk, Stefan/B-7629-2015; Rea, Nanda/I-2853-2015; Gargano, Fabio/O-8934-2015; Loparco, Francesco/O-8847-2015; Johannesson, Gudlaugur/O-8741-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016 OI Starck, Jean-Luc/0000-0003-2177-7794; Thompson, David/0000-0001-5217-9135; lubrano, pasquale/0000-0003-0221-4806; Morselli, Aldo/0000-0002-7704-9553; giglietto, nicola/0000-0002-9021-2888; Cutini, Sara/0000-0002-1271-2924; Gasparrini, Dario/0000-0002-5064-9495; Tramacere, Andrea/0000-0002-8186-3793; Baldini, Luca/0000-0002-9785-7726; Tagliaferri, Gianpiero/0000-0003-0121-0723; Komin, Nukri/0000-0003-3280-0582; Preece, Robert/0000-0003-1626-7335; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Pesce-Rollins, Melissa/0000-0003-1790-8018; Perri, Matteo/0000-0003-3613-4409; Moretti, Elena/0000-0001-5477-9097; Bissaldi, Elisabetta/0000-0001-9935-8106; Wu, Xuefeng/0000-0002-6299-1263; Torres, Diego/0000-0002-1522-9065; Sgro', Carmelo/0000-0001-5676-6214; Giordano, Francesco/0000-0002-8651-2394; Dingus, Brenda/0000-0001-8451-7450; Stephens, Thomas/0000-0003-3065-6871; SPINELLI, Paolo/0000-0001-6688-8864; giommi, paolo/0000-0002-2265-5003; De Angelis, Alessandro/0000-0002-3288-2517; Frailis, Marco/0000-0002-7400-2135; Caraveo, Patrizia/0000-0003-2478-8018; Reimer, Olaf/0000-0001-6953-1385; Funk, Stefan/0000-0002-2012-0080; Rea, Nanda/0000-0003-2177-6388; Gargano, Fabio/0000-0002-5055-6395; Loparco, Francesco/0000-0002-1173-5673; Johannesson, Gudlaugur/0000-0003-1458-7036; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; FU NASA; Department of Energy in the United States; Commissariat a lEnergie Atomique; Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; Agenzia Spaziale Italiana; Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture, Sports, Science and Technology (MEXT); High Energy Accelerator Research Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan; K. A. Wallenberg Foundation; Swedish Research Council; Swedish National Space Board in Sweden; Deutsches Zentrum fur Luftund Raumfahrt in Germany FX A. A. Abdo, J. Finke, and S. Razzaque are National Research Council Research Associates. A. J. van der Horst is a NASA Postdoctoral Program Fellow. The Fermi LAT Collaboration acknowledges the support of a number of agencies and institutes. These include NASA and the Department of Energy in the United States; the Commissariat a lEnergie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy; the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK), and Japan Aerospace Exploration Agency (JAXA) in Japan; and the K. A. Wallenberg Foundation, the Swedish Research Council, and the Swedish National Space Board in Sweden. J.C. is a Royal Swedish Academy of Sciences Research fellow supported by a grant from the K. A. Wallenberg foundation. The Fermi GBM Collaboration acknowledges the support of NASA in the United States and Deutsches Zentrum fur Luftund Raumfahrt in Germany and thanks L. Gibby, A. English, and F. Kroeger. NR 39 TC 395 Z9 399 U1 4 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 MAR 27 PY 2009 VL 323 IS 5922 BP 1688 EP 1693 DI 10.1126/science.1169101 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 424IG UT WOS:000264559800029 ER PT J AU Varnai, T Marshak, A AF Varnai, Tamas Marshak, Alexander TI MODIS observations of enhanced clear sky reflectance near clouds SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID AEROSOL; PRODUCTS; TERRA; OCEAN; SMOKE; CERES AB Several recent studies have found that the brightness of clear sky systematically increases near clouds. Understanding this increase is important both for a correct interpretation of observations and for improving our knowledge of aerosol-cloud interactions. However, while the studies suggested several processes to explain the increase, the significance of each process is yet to be determined. This study examines one of the suggested processes-three-dimensional (3-D) radiative interactions between clouds and their surroundings-by analyzing a large dataset of MODIS (Moderate Resolution Imaging Spectroradiometer) observations over the Northeast Atlantic Ocean. The results indicate that 3-D effects are responsible for a large portion of the observed increase, which extends to about 15 km away from clouds and is stronger (i) at shorter wavelengths (ii) near optically thicker clouds and (iii) near illuminated cloud sides. This implies that it is important to account for 3-D radiative effects in the interpretation of solar reflectance measurements over clear regions in the vicinity of clouds. Citation: Varnai, T., and A. Marshak (2009), MODIS observations of enhanced clear sky reflectance near clouds, Geophys. Res. Lett., 36, L06807, doi:10.1029/2008GL037089. C1 [Varnai, Tamas] Univ Maryland Baltimore Cty, Goddard Space Flight Ctr, Joint Ctr Earth Syst Technol, NASA, Greenbelt, MD 20771 USA. [Marshak, Alexander] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Varnai, T (reprint author), Univ Maryland Baltimore Cty, Goddard Space Flight Ctr, Joint Ctr Earth Syst Technol, NASA, Code 613-2, Greenbelt, MD 20771 USA. EM tamas.varnai@nasa.gov RI Marshak, Alexander/D-5671-2012 FU NASA Radiation Sciences Program FX We gratefully acknowledge support for this research by the NASA Radiation Sciences Program managed by Hal Maring. We thank R. F. Cahalan, C. Chiu, J. A. Coakley, A. B. Davis, K. F. Evans, I. Koren, N. G. Loeb, L. A. Remer, G. Wen and X. Xiong for stimulating discussions. NR 21 TC 49 Z9 50 U1 1 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 26 PY 2009 VL 36 AR L06807 DI 10.1029/2008GL037089 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 426AF UT WOS:000264679100006 ER PT J AU Redemann, J Zhang, Q Russell, PB Livingston, JM Remer, LA AF Redemann, Jens Zhang, Qin Russell, Philip B. Livingston, John M. Remer, Lorraine A. TI Case studies of aerosol remote sensing in the vicinity of clouds SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID CLEAR-SKY REFLECTANCE; TROPOSPHERIC AEROSOL; SUN PHOTOMETER; CUMULUS CLOUDS; WATER-VAPOR; IN-SITU; OCEAN; SUNPHOTOMETER; RESOLUTION; PRODUCTS AB Studying the spatial variability of aerosol properties in the vicinity of clouds is essential to our ability to determine aerosol direct and indirect effects on climate. In this paper, we describe aerosol observations collected near cloud edges by an airborne Sun photometer over dark ocean waters. Focusing on case studies of aerosol measurements near eight cloud edges within a dissipating stratiform cloud deck, we compare the airborne Sun photometer observations to retrievals of aerosol properties using the standard Moderate Resolution Imaging Spectroradiometer (MODIS) aerosol algorithm applied to 500-m-resolution MODIS spectral reflectances. We find a persistent, spectrally neutral increase in the Sun photometer-derived aerosol optical depth (AOD) of up to 10% (0.015) in the 2-km distances closest to the edges of several distinct clouds. At midvisible wavelengths, the MODIS AOD retrievals show similar increases toward cloud edges, although a larger increase in AOD is found in the MODIS along-scan direction. At short-wave infrared (SWIR) wavelengths (1240-2130 nm), the MODIS-derived AOD increases near cloud edges are of the order of 0.03 and as such three times as large as the Sun photometer-derived values. Hence, in contrast to recently discussed "bluing'' of aerosols near cloud edges, i.e., a preferential apparent increase in the visible reflectances of clearsky pixels due to 3-D radiative transfer effects in the vicinity of clouds, we find a "reddening'' of aerosols in the MODIS 500-m-resolution aerosol retrievals near clouds. This "reddening'' in our study can be traced to larger absolute increases in SWIR reflectances when compared to visible reflectances near clouds, which in turn seem to stem from larger electronic cross talk in the MODIS SWIR bands (5-7). We note that the lack of "bluing'' in our MODIS observations is likely due to the small geometric and optical thicknesses of the clouds considered. C1 [Redemann, Jens; Zhang, Qin] BAER Inst, Sonoma, CA 95476 USA. [Russell, Philip B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Livingston, John M.] SRI Int, Menlo Pk, CA 94035 USA. [Remer, Lorraine A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Redemann, J (reprint author), BAER Inst, 560 3rd St W, Sonoma, CA 95476 USA. EM jredemann@mail.arc.nasa.gov FU NASA [EOS/03-05840647] FX The authors would like to thank Shana Mattoo (SSAI) for help with the adaptation and implementation of the MODIS standard aerosol retrieval algorithm. We are grateful to Larry Di Girolamo (University of Illinois) and two anonymous reviewers for useful comments on our manuscript. Funding through NASA grant EOS/03-05840647 is gratefully acknowledged. NR 30 TC 41 Z9 42 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAR 26 PY 2009 VL 114 AR D06209 DI 10.1029/2008JD010774 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 426BV UT WOS:000264683400002 ER PT J AU Gopalswamy, N Makela, P Xie, H Akiyama, S Yashiro, S AF Gopalswamy, N. Maekelae, P. Xie, H. Akiyama, S. Yashiro, S. TI CME interactions with coronal holes and their interplanetary consequences SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ENERGETIC PARTICLE EVENTS; II RADIO-BURSTS; MASS EJECTIONS; SOLAR-WIND; MAGNETIC CLOUDS; ACTIVE-REGION; 1 AU; EARTH; SHOCK; PROMINENCE AB A significant number of interplanetary shocks (similar to 17%) during cycle 23 were not followed by drivers. The number of such "driverless'' shocks steadily increased with the solar cycle with 15%, 33%, and 52% occurring in the rise, maximum, and declining phase of the solar cycle. The solar sources of 15% of the driverless shocks were very close the central meridian of the Sun ( within similar to 15 degrees), which is quite unexpected. More interestingly, all the driverless shocks with their solar sources near the solar disk center occurred during the declining phase of solar cycle 23. When we investigated the coronal environment of the source regions of driverless shocks, we found that in each case there was at least one coronal hole nearby, suggesting that the coronal holes might have deflected the associated coronal mass ejections (CMEs) away from the Sun-Earth line. The presence of abundant low-latitude coronal holes during the declining phase further explains why CMEs originating close to the disk center mimic the limb CMEs, which normally lead to driverless shocks due to purely geometrical reasons. We also examined the solar source regions of shocks with drivers. For these, the coronal holes were located such that they either had no influence on the CME trajectories, or they deflected the CMEs toward the Sun-Earth line. We also obtained the open magnetic field distribution on the Sun by performing a potential field source surface extrapolation to the corona. It was found that the CMEs generally move away from the open magnetic field regions. The CME-coronal hole interaction must be widespread in the declining phase and may have a significant impact on the geoeffectiveness of CMEs. C1 [Gopalswamy, N.; Maekelae, P.; Xie, H.; Akiyama, S.; Yashiro, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Maekelae, P.; Xie, H.; Akiyama, S.; Yashiro, S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM gopals@ssedmail.gsfc.nasa.gov RI Gopalswamy, Nat/D-3659-2012 FU NASA LWS; SRT programs FX We thank the SOHO, Wind, and ACE science teams for making the shock data available online. This research was supported by NASA LWS and SR&T programs. SOHO is a project of international cooperation between ESA and NASA. The authors thank the anonymous referees for critical comments, which helped improve the presentation of the paper. NR 49 TC 70 Z9 73 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAR 26 PY 2009 VL 114 AR A00A22 DI 10.1029/2008JA013686 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 426DD UT WOS:000264687100004 ER PT J AU Jenniskens, P Shaddad, MH Numan, D Elsir, S Kudoda, AM Zolensky, ME Le, L Robinson, GA Friedrich, JM Rumble, D Steele, A Chesley, SR Fitzsimmons, A Duddy, S Hsieh, HH Ramsay, G Brown, PG Edwards, WN Tagliaferri, E Boslough, MB Spalding, RE Dantowitz, R Kozubal, M Pravec, P Borovicka, J Charvat, Z Vaubaillon, J Kuiper, J Albers, J Bishop, JL Mancinelli, RL Sandford, SA Milam, SN Nuevo, M Worden, SP AF Jenniskens, P. Shaddad, M. H. Numan, D. Elsir, S. Kudoda, A. M. Zolensky, M. E. Le, L. Robinson, G. A. Friedrich, J. M. Rumble, D. Steele, A. Chesley, S. R. Fitzsimmons, A. Duddy, S. Hsieh, H. H. Ramsay, G. Brown, P. G. Edwards, W. N. Tagliaferri, E. Boslough, M. B. Spalding, R. E. Dantowitz, R. Kozubal, M. Pravec, P. Borovicka, J. Charvat, Z. Vaubaillon, J. Kuiper, J. Albers, J. Bishop, J. L. Mancinelli, R. L. Sandford, S. A. Milam, S. N. Nuevo, M. Worden, S. P. TI The impact and recovery of asteroid 2008 TC3 SO NATURE LA English DT Article ID UREILITES; METEORITE; EARTH AB In the absence of a firm link between individual meteorites and their asteroidal parent bodies, asteroids are typically characterized only by their light reflection properties, and grouped accordingly into classes(1-3). On 6 October 2008, a small asteroid was discovered with a flat reflectance spectrum in the 554-995nm wavelength range, and designated 2008 TC3 (refs 4-6). It subsequently hit the Earth. Because it exploded at 37km altitude, no macroscopic fragments were expected to survive. Here we report that a dedicated search along the approach trajectory recovered 47 meteorites, fragments of a single body named Almahata Sitta, with a total mass of 3.95 kg. Analysis of one of these meteorites shows it to be an achondrite, a polymict ureilite, anomalous in its class: ultra-fine-grained and porous, with large carbonaceous grains. The combined asteroid and meteorite reflectance spectra identify the asteroid as F class(3), now firmly linked to dark carbon-rich anomalous ureilites, a material so fragile it was not previously represented in meteorite collections. C1 [Jenniskens, P.; Albers, J.; Bishop, J. L.; Mancinelli, R. L.] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA. [Shaddad, M. H.; Numan, D.; Kudoda, A. M.] Univ Khartoum, Dept Phys, Khartoum 11115, Sudan. [Elsir, S.] Juba Univ, Dept Phys, Juba, Sudan. [Zolensky, M. E.; Le, L.; Robinson, G. A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Le, L.; Robinson, G. A.] Jacobs Technol Engn Sci Contact Grp, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Friedrich, J. M.] Fordham Univ, Dept Chem, Bronx, NY 10458 USA. [Friedrich, J. M.] Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA. [Rumble, D.; Steele, A.] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. [Chesley, S. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Fitzsimmons, A.; Duddy, S.; Hsieh, H. H.] Queens Univ Belfast, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland. [Ramsay, G.] Armagh Observ, Armagh BT61 9DG, North Ireland. [Brown, P. G.; Edwards, W. N.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Tagliaferri, E.] ET Space Syst, Camarillo, CA 93012 USA. [Boslough, M. B.; Spalding, R. E.] Sandia Natl Labs, Albuquerque, NM 87185 USA. [Dantowitz, R.; Kozubal, M.] Dexter Sch, Clay Ctr Observ, Brookline, MA 02445 USA. [Dantowitz, R.; Kozubal, M.] Southfield Sch, Clay Ctr Observ, Brookline, MA 02445 USA. [Pravec, P.; Borovicka, J.] Acad Sci Czech Republic, Astron Inst, Ondrejov 25165, Czech Republic. [Charvat, Z.] Czech Hydrometeorol Inst, Prague 14306 4, Czech Republic. [Vaubaillon, J.] Inst Mecan Celeste & Calcul Ephemerides, F-75014 Paris, France. [Kuiper, J.] Dutch Meteor Soc, NL-3732 XD De Bilt, Netherlands. [Sandford, S. A.; Milam, S. N.; Nuevo, M.; Worden, S. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Jenniskens, P (reprint author), Carl Sagan Ctr, SETI Inst, 515 N Whisman Rd, Mountain View, CA 94043 USA. EM Petrus.M.Jenniskens@nasa.gov RI Milam, Stefanie/D-1092-2012; Borovicka, Jiri/F-4257-2014; Pravec, Petr/G-9037-2014; Mancinelli, Rocco/L-8971-2016 OI Milam, Stefanie/0000-0001-7694-4129; FU NASA Planetary Astronomy program; NASA's Cosmochemistry program [NNX07AI48G] FX We thank the University of Khartoum for support of the field campaigns, and students and staff of the Physics Department of the Faculty of Sciences for their efforts to recover the meteorites. P. J. is supported by the NASA Planetary Astronomy program. D. R. acknowledges the support of NASA's Cosmochemistry program (grant NNX07AI48G). A. Alunni, J. Travis-Garcia and L. Hofland of NASA Ames Research Center, and J. Herrin of NASA Johnson Space Flight Center, provided laboratory assistance. The work conducted at JPL/Caltech was under contract with NASA. The William Hershel Telescope is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. NR 27 TC 171 Z9 171 U1 1 U2 19 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD MAR 26 PY 2009 VL 458 IS 7237 BP 485 EP 488 DI 10.1038/nature07920 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 423YJ UT WOS:000264532400039 PM 19325630 ER PT J AU Zent, AP Hecht, MH Cobos, DR Campbell, GS Campbell, CS Cardell, G Foote, MC Wood, SE Mehta, M AF Zent, Aaron P. Hecht, Michael H. Cobos, Doug R. Campbell, Gaylon S. Campbell, Colin S. Cardell, Greg Foote, Marc C. Wood, Stephen E. Mehta, Manish TI Thermal and Electrical Conductivity Probe (TECP) for Phoenix SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID GENERAL-CIRCULATION MODEL; GROUND ICE; TEMPERATURE-DEPENDENCE; FREEZING-POINT; HIGH OBLIQUITY; WATER-CONTENT; NEAR-SURFACE; MARS; PERMITTIVITY; PERMAFROST AB The Thermal and Electrical Conductivity Probe (TECP) is a component of the Microscopy, Electrochemistry and Conductivity Analyzer (MECA) payload on the Phoenix Lander. TECP will measure the temperature, thermal conductivity, and volumetric heat capacity of the regolith. It will also detect and quantify the population of mobile H2O molecules in the regolith, if any, throughout the polar summer, by measuring the electrical conductivity of the regolith as well as the dielectric permittivity. In the vapor phase, TECP is capable of measuring the atmospheric H2O vapor abundance as well as augmenting the wind velocity measurements from the meteorology instrumentation. TECP is mounted near the end of the 2.3 m Robotic Arm and can be placed either in the regolith material or held aloft in the atmosphere. This paper describes the development and calibration of the TECP. In addition, substantial characterization of the instrument has been conducted to identify behavioral characteristics that might affect landed surface operations. The greatest potential issue identified in characterization tests is the extraordinary sensitivity of the TECP to placement. Small gaps alter the contact between the TECP and regolith, complicating data interpretation. Testing with the Phoenix Robotic Arm identified mitigation techniques that will be implemented during flight. A flight model of the instrument was also field tested in the Antarctic Dry Valleys during the 2007-2008 International Polar Year. C1 [Zent, Aaron P.] NASA, Ames Res Ctr, Planetary Syst Branch, Moffett Field, CA 94035 USA. [Hecht, Michael H.; Cardell, Greg; Foote, Marc C.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Cobos, Doug R.; Campbell, Gaylon S.; Campbell, Colin S.] Decagon Devices, Pullman, WA USA. [Wood, Stephen E.] Univ Washington, Seattle, WA USA. [Mehta, Manish] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI USA. RP Zent, AP (reprint author), NASA, Ames Res Ctr, Planetary Syst Branch, MS 245-3, Moffett Field, CA 94035 USA. EM Aaron.P.Zent@nasa.govc RI Wood, Stephen/R-5592-2016 OI Wood, Stephen/0000-0002-9330-434X NR 51 TC 32 Z9 32 U1 0 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAR 25 PY 2009 VL 114 AR E00A27 DI 10.1029/2007JE003052 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 426CR UT WOS:000264685800001 ER PT J AU Panchenko, M Khodachenko, ML Kislyakov, AG Rucker, HO Hanasz, J Kaiser, ML Bale, SD Lamy, L Cecconi, B Zarka, P Goetz, K AF Panchenko, M. Khodachenko, M. L. Kislyakov, A. G. Rucker, H. O. Hanasz, J. Kaiser, M. L. Bale, S. D. Lamy, L. Cecconi, B. Zarka, P. Goetz, K. TI Daily variations of auroral kilometric radiation observed by STEREO SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID DENSITY; INTENSITY; REGION AB Daily variations of terrestrial auroral kilometric radiation (AKR) are considered; an effect that is detected in STEREO/WAVES data. It has been found that the intensities of the AKR emitted from Northern and Southern sources are modulated with a period of similar to 24 hours. The occurrence frequency of the AKR has been shown to be strongly dependent on the orientation of the rotating oblique magnetic dipole of the Earth relative to the Sun. AKR is found to occur more often and emit in a broader frequency range when the axis of the terrestrial magnetic dipole in the given hemisphere is oriented toward the nightside. We suggest that the observed similar to 24 h variations of AKR are connected with diurnal changes of the ambient plasma density in the auroral region. Citation: Panchenko, M., et al. (2009), Daily variations of auroral kilometric radiation observed by STEREO, Geophys. Res. Lett., 36, L06102, doi: 10.1029/2008GL037042. C1 [Panchenko, M.; Khodachenko, M. L.; Rucker, H. O.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria. [Kislyakov, A. G.] Lobachevsky State Univ, Dept Radiophys, Nizhnii Novgorod 603950, Russia. [Kaiser, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hanasz, J.] PAS, Space Res Ctr, PL-87100 Torun, Poland. [Bale, S. D.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Zarka, P.] Univ Paris Diderot, UPMC, CNRS, Observ Paris,LESIA, F-92190 Meudon, France. [Goetz, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. RP Panchenko, M (reprint author), Austrian Acad Sci, Space Res Inst, Schmiedlstr 6, A-8042 Graz, Austria. EM mykhaylo.panchenko@oeaw.ac.at RI Bale, Stuart/E-7533-2011 OI Bale, Stuart/0000-0002-1989-3596 FU Austrian Fonds zur Forderung der wissenschaftlichen Forschung [P20680-N16]; WTZ-OeAD Program "Austria-Russia'' [18/2006]; Ministry of Science and Higher Education in Poland [4T12E 006 30] FX The authors are grateful to the referees for their comments which significantly improved the manuscript. Thanks are due to the Plasma Physics Data Center team for providing the S/WAVES data. This work was financed by the "Austrian Fonds zur Forderung der wissenschaftlichen Forschung'' (project P20680-N16), WTZ-OeAD Program "Austria-Russia'' (project 18/2006) and the Ministry of Science and Higher Education in Poland (grant 4T12E 006 30). NR 17 TC 3 Z9 3 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 24 PY 2009 VL 36 AR L06102 DI 10.1029/2008GL037042 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 426AA UT WOS:000264678500004 ER PT J AU Tigelaar, DM Palker, AE Jackson, CM Anderson, KM Wainright, J Savinell, RF AF Tigelaar, Dean M. Palker, Allyson E. Jackson, Christine M. Anderson, Kellina M. Wainright, Jesse Savinell, Robert F. TI Synthesis and Properties of Novel Proton-Conducting Aromatic Poly(ether sulfone)s That Contain Triazine Groups SO MACROMOLECULES LA English DT Article ID FUEL-CELL APPLICATIONS; SULFONATED POLY(ARYLENE ETHER); POLYMER ELECTROLYTE MEMBRANES; PYRIDINE UNITS; POLYBENZIMIDAZOLES; SUBSTITUTION; POLYETHERS; COPOLYMERS; CHEMISTRY; ANALOGS AB A series of novel fully aromatic poly(arylene ether sulfone)s that contain 1,3,5-s-triazine groups were synthesized by the reaction of triazine-containing bisphenols with bis(4-fluorophenylsulfone) to study the effects of branching groups on solubility as well as thermal and mechanical properties. Polymers had inherent viscosities from 0.43 to 1.10 dL/g, thermal stabilities >500 degrees C in air, glass transition temperatures from 136 to 289 degrees C, and good film forming abilities. The polymer with pendant diphenylamine groups on the triazine ring were further investigated for use in proton exchange membranes based on solubility, thermo-oxidative stability, and case of monomer synthesis. A series of copolymers made from 4,6-bis(4-hydroxyphenyl)-N,N-diphenyl-1,3,5-triazin-2-amine and 4,4'-biphenol were sulfonated with chlorosulfonic acid to achieve ion exchange capacities up to 2.62 mmol/g. The homopolymer was sulfonated exclusively on the diphenylamine branch and had the highest proton conductivity (0.11 S/cm at 95 degrees C and 100% relative humidity), even though it had the lowest water uptake and ion exchange capacity. Unsulfonated polymers and sulfonated copolymers showed little uptake of phosphoric acid. However, the sulfonated homopolymer with pendant diphenylamine groups had a 200-250 wt % uptake when soaked in 85% H(3)PO(4) at 90 degrees C, but the proton conductivity of this polymer was lower than the hydrated polymer without H(3)PO(4) added. C1 [Tigelaar, Dean M.; Palker, Allyson E.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Jackson, Christine M.; Anderson, Kellina M.; Wainright, Jesse; Savinell, Robert F.] Case Western Reserve Univ, Dept Chem Engn, Cleveland, OH 44106 USA. OI Jackson, Christine/0000-0002-8119-4593 FU NASA NRA [NNC07BA13B] FX The authors thank Daniel Scheiman for TGA and DMA analysis. The authors also thank Derek Quade and Andrea IIg for help with tensile testing. DMT was funded by NASA NRA Contract NNC07BA13B. NR 41 TC 34 Z9 36 U1 4 U2 28 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0024-9297 J9 MACROMOLECULES JI Macromolecules PD MAR 24 PY 2009 VL 42 IS 6 BP 1888 EP 1896 DI 10.1021/ma802553w PG 9 WC Polymer Science SC Polymer Science GA 420MY UT WOS:000264295100017 ER PT J AU Okumura, M Sander, SP AF Okumura, Mitchio Sander, Stanley P. TI Chemistry and spectroscopy of peroxy radicals SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Okumura, Mitchio] CALTECH, Arthur Amos Noyes Lab Chem Phys, Div Chem & Chem Engn, Pasadena, CA 91125 USA. [Sander, Stanley P.] CALTECH, Jet Prop Lab, Earth & Space Sci Div, Pasadena, CA 91109 USA. EM mo@its.caltech.edu; ssander@jpl.nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 3 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 22 PY 2009 VL 237 MA 12-ANYL BP 283 EP 283 PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V16GJ UT WOS:000207857800258 ER PT J AU Sander, S Bayes, K Hume, K AF Sander, Stanley Bayes, Kyle Hume, Kelly TI Laboratory studies of rate-limiting steps in the catalytic destruction of polar stratospheric ozone SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Sander, Stanley; Bayes, Kyle; Hume, Kelly] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM Stanley.P.Sander@jpl.nasa.gov; kdbayes@jpl.nasa.gov; kelly.l.hume@jpl.nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 22 PY 2009 VL 237 MA 133-ANYL BP 362 EP 362 PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V16GJ UT WOS:000207857800337 ER PT J AU Salawitch, R Canty, T Stimpfle, R Wilmouth, D Anderson, JG von Hobe, M Stroh, F Rex, M Schofield, R Santee, M Kinnison, DE Kurylo, MJ Sinnhuber, BM AF Salawitch, Ross Canty, Tim Stimpfle, Richard Wilmouth, David Anderson, James G. von Hobe, Marc Stroh, Fred Rex, Markus Schofield, Robyn Santee, Michelle Kinnison, Douglas Edward Kurylo, Michael J. Sinnhuber, Bjoern-Martin TI Impact of recent laboratory measurements of the ClOOCl cross section on our understanding of polar ozone chemistry SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Salawitch, Ross; Canty, Tim; Kurylo, Michael J.] Univ Maryland, Dept Chem & Biochem, College Pk, MD 20742 USA. [Stimpfle, Richard; Wilmouth, David; Anderson, James G.] Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA. [von Hobe, Marc; Stroh, Fred] Forschungszentrum Juelich, Inst Chem & Dynam Geosphere ICG Stratosphere 1, D-52425 Julich, Germany. [Rex, Markus; Schofield, Robyn] Alfred Wegener Inst, Potsdam, Germany. [Santee, Michelle] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kinnison, Douglas Edward] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80503 USA. [Sinnhuber, Bjoern-Martin] Univ Bremen, Inst Environm Phys, D-28334 Bremen, Germany. EM rjs@atmos.umd.edu; tcanty@atmos.umd.edu; rick@huarp.harvard.edu; wilmouth@fas.harvard.edu; anderson@huarp.harvard.edu; m.von.hobe@fz-juelich.de; Markus.Rex@awi.de; robyn.schofield@awi.de; dkin@ucar.edu; michael.j.kurylo@nasa.gov; bms@iup.physik.uni-bremen.de RI Sinnhuber, Bjorn-Martin/A-7007-2013; Stroh, Fred/A-6505-2009; von Hobe, Marc/A-7969-2013; Schofield, Robyn/A-4062-2010 OI Sinnhuber, Bjorn-Martin/0000-0001-9608-7320; Stroh, Fred/0000-0002-4492-2977; Schofield, Robyn/0000-0002-4230-717X NR 0 TC 1 Z9 1 U1 0 U2 4 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 22 PY 2009 VL 237 MA 131-ANYL BP 363 EP 363 PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V16GJ UT WOS:000207857800338 ER PT J AU Becker, JA Beck, BR Beiersdorfer, P Brown, GV Moody, KJ Wilhelmy, JB Porter, FS Kilbourne, CA Kelley, RL AF Becker, John A. Beck, B. R. Beiersdorfer, P. Brown, G. V. Moody, Kenton J. Wilhelmy, Jerry B. Porter, F. S. Kilbourne, C. A. Kelley, R. L. TI Energy splitting of the ground-state doublet in the nucleus 229Th SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Becker, John A.; Beck, B. R.; Beiersdorfer, P.; Brown, G. V.] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. [Moody, Kenton J.] Lawrence Livermore Natl Lab, AX Div, Livermore, CA 94550 USA. [Wilhelmy, Jerry B.] Los Alamos Natl Lab, C INC, Los Alamos, NM 87545 USA. [Porter, F. S.; Kilbourne, C. A.; Kelley, R. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM jabecker@llnl.gov; j_wilhelmy@lanl.gov RI Porter, Frederick/D-3501-2012; Kelley, Richard/K-4474-2012 OI Porter, Frederick/0000-0002-6374-1119; NR 0 TC 0 Z9 0 U1 0 U2 2 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 22 PY 2009 VL 237 MA 25-NUCL PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V16GJ UT WOS:000207857805850 ER PT J AU Brandon, EJ AF Brandon, Erik J. TI PHYS 486-New materials for space power SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Brandon, Erik J.] CALTECH, Jet Prop Lab, Mat & Device Technol Grp, Power & Sensor Syst Sect, Pasadena, CA 91109 USA. EM erik.j.brandon@jpl.nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 22 PY 2009 VL 237 MA 486-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V16GJ UT WOS:000207857808453 ER PT J AU Guo, HQ Scheiman, DA Nguyen, BN Meador, MAB AF Guo, Haiquan Scheiman, Daniel A. Nguyen, Baochau N. Meador, Mary Ann B. TI Flexible aerogel synthesized by bis[3-triethoxysilyl)propyl]disulfide and diglycidyl ether terminated poly(dimethylsiloxane) SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Nguyen, Baochau N.] Ohio Aerosp Inst, Mat & Struct Div, Cleveland, OH 44135 USA. [Scheiman, Daniel A.] ASRC Aerosp, Mat & Struct Div, Cleveland, OH 44135 USA. [Meador, Mary Ann B.] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA. EM HaiquanGuo@oai.org; daniel.a.scheiman@nasa.gov; Baochau.N.Nguyen@grc.nasa.gov; maryann.meador@nasa.gov NR 0 TC 0 Z9 0 U1 1 U2 5 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 22 PY 2009 VL 237 MA 161-COLL PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V16GJ UT WOS:000207857803334 ER PT J AU Harrison, JS Lowther, SE Kang, JH Park, C AF Harrison, Joycelyn S. Lowther, Sharon E. Kang, Jin Ho Park, Cheol TI Electroactive nanotube polymer nanocomposites for sensors and actuators SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Harrison, Joycelyn S.; Lowther, Sharon E.] NASA Langley, Adv Mat & Proc Branch, Hampton, VA 23681 USA. [Kang, Jin Ho; Park, Cheol] Natl Inst Aerosp, Hampton, VA 23666 USA. EM joycelyn.s.harrison@nasa.gov; sharon.e.lowther@nasa.gov; jin.h.kang@nasa.gov; cheol.park-1@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 22 PY 2009 VL 237 MA 64-PMSE PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V16GJ UT WOS:000207857807332 ER PT J AU Ibrahim, E Chipara, MD Wilkins, R Chipara, AC Lozano, K Chipara, M AF Ibrahim, Elamin Chipara, Magdalena D. Wilkins, Richard Chipara, Alin Cristian Lozano, Karen Chipara, Mircea TI Spectroscopic investigations on polyethylene-functionalized single wall carbon nanotube composites SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Ibrahim, Elamin; Chipara, Alin Cristian] Univ Texas Pan Amer, Dept Chem, Edinburg, TX 78541 USA. [Chipara, Magdalena D.; Chipara, Mircea] Univ Texas Pan Amer, Dept Phys & Geol, Edinburg, TX 78541 USA. [Wilkins, Richard] Prairie View A&M Univ, NASA, Ctr Appl Radiat Res, Prairie View, TX 77446 USA. [Lozano, Karen] Univ Texas Pan Amer, Dept Mech Engn, Edinburg, TX 78541 USA. EM amin@utpa.edu; magdachipara@yahoo.com; lozanok@utpa.edu; mchipara@utpa.edu RI Chipara, Mircea/B-2849-2009; Chipara, Mircea/F-1552-2011 OI Chipara, Mircea/0000-0003-3584-4863 NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 22 PY 2009 VL 237 MA 166-PMSE PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V16GJ UT WOS:000207857807327 ER PT J AU Lin, Y Williams, TV Connell, JW AF Lin, Yi Williams, Tiffany V. Connell, John W. TI Soluble exfoliated hexagonal boron nitride nanosheets SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Lin, Yi; Connell, John W.] NASA Postdoctoral Fellow, NASA Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA. EM yi.lin-1@nasa.gov; john.w.connell@nasa.gov NR 0 TC 0 Z9 0 U1 2 U2 9 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 22 PY 2009 VL 237 MA 653-INOR PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V16GJ UT WOS:000207857805435 ER PT J AU Lovell, C Fitz-Gerald, JM Park, C Harrison, JS AF Lovell, Conrad Fitz-Gerald, James M. Park, Cheol Harrison, Joycelyn S. TI Shear piezoelectricity in biopolymers and their carbon nanotube composites SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Lovell, Conrad; Fitz-Gerald, James M.] Univ Virginia, Dept Mat Sci & Engn, Charlottesville, VA 22904 USA. [Park, Cheol] Natl Inst Aerosp, Hampton, VA 23666 USA. [Harrison, Joycelyn S.] NASA Langley, Adv Mat & Proc Branch, Hampton, VA 23681 USA. EM lovell@nianet.org; jfitz@virginia.edu; cheol.park-1@nasa.gov; joycelyn.s.harrison@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 22 PY 2009 VL 237 MA 69-PMSE PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V16GJ UT WOS:000207857807338 ER PT J AU Nguyen, BN Meador, MA Medoro, A Shonkwiler, B McCorkle, L AF Nguyen, Baochau N. Meador, Mary Ann Medoro, Alexandra Shonkwiler, Brian McCorkle, Linda TI Tailoring elastic properties of silica aerogels crosslinked with an isocyanate SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Nguyen, Baochau N.] NASA, Ohio Aerosp Inst, Glenn Res Ctr, Cleveland, OH 44135 USA. [McCorkle, Linda] NASA, Mat & Struct Div, Glenn Res Ctr, Cleveland, OH 44135 USA. [Shonkwiler, Brian] Clark Atlanta Univ, Atlanta, GA 30314 USA. EM Baochau.N.Nguyen@nasa.gov; maryann.meador@nasa.gov; bshonk@mindspring.com NR 0 TC 0 Z9 0 U1 1 U2 2 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 22 PY 2009 VL 237 MA 272-POLY PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V16GJ UT WOS:000207857807452 ER PT J AU Troupe, L Perkins, J AF Troupe, Latoya Perkins, James TI Chemical and lubricating properties of a series of solutions for use as "ionic lubricants" SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Troupe, Latoya] Oakwood Univ, Dept Chem, Huntsville, AL 35896 USA. [Perkins, James] NASA, Mat Proc Lab, MSFC, Huntsville, AL 35896 USA. EM latoyatroupe2005@yahoo.com; james.h.perkins@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 22 PY 2009 VL 237 MA 560-CHED PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V16GJ UT WOS:000207857802589 ER PT J AU Vivod, SL Meador, MAB Nguyen, BN Perry, R AF Vivod, Stephanie L. Meador, Mary Ann B. Nguyen, Baochau N. Perry, Renee TI Di-isocyanate crosslinked silica aerogels with hexyl links incorporated into the underlying silica backbone SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Vivod, Stephanie L.; Meador, Mary Ann B.] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA. [Nguyen, Baochau N.] Ohio Aerosp Inst, Cleveland, OH 44135 USA. [Perry, Renee] Bucknell Univ, Lewisburg, PA 17837 USA. EM Stephanie.L.Vivod@nasa.gov; maryann.meador@nasa.gov; baochau.n.nguyen@nasa.gov; rnp003@bucknell.edu NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 22 PY 2009 VL 237 MA 80-POLY PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V16GJ UT WOS:000207857807704 ER PT J AU Weber, AS Johnson, PV Hodyss, R AF Weber, Amanda S. Johnson, Paul V. Hodyss, Robert TI PHYS 340-Hydrogen-deuterium atom exchange in photolyzed methane-water ice mixtures SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Weber, Amanda S.] Univ S Dakota, Dept Chem, Vermillion, SD 57069 USA. [Johnson, Paul V.; Hodyss, Robert] NASA Jet Prop Lab, Planetary Ices Grp, Pasadena, CA 91109 USA. EM Amanda.Weber@usd.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 22 PY 2009 VL 237 MA 340-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V16GJ UT WOS:000207857808082 ER PT J AU Zhang, ZY Jaffe, RL Philpott, MR Lawson, J AF Zhang, Zhiyong Jaffe, Richard L. Philpott, Michael R. Lawson, John TI CO2 reduction and formation of organic molecules on pyrite surface and pyrite surface supported cubane clusters SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Zhang, Zhiyong] Stanford Univ, Stanford Nanofabricat Facil, Stanford, CA 94305 USA. [Jaffe, Richard L.; Lawson, John] NASA, Ames Res Ctr, Nanotechnol Branch, Moffett Field, CA 94035 USA. [Philpott, Michael R.] Tohoku Univ, Inst Mat Res, Ctr Computat Mat Sci, Aoba Ku, Sendai, Miyagi 9808577, Japan. EM zyzhang@stanford.edu; rjaffe@mail.arc.nasa.gov; philpott@imr.edu; john.w.lawson@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 4 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 22 PY 2009 VL 237 MA 162-FUEL PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V16GJ UT WOS:000207857803802 ER PT J AU Offermann, D Gusev, O Donner, M Forbes, JM Hagan, M Mlynczak, MG Oberheide, J Preusse, P Schmidt, H Russell, JM AF Offermann, D. Gusev, O. Donner, M. Forbes, J. M. Hagan, M. Mlynczak, M. G. Oberheide, J. Preusse, P. Schmidt, H. Russell, J. M., III TI Relative intensities of middle atmosphere waves SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID STRATOSPHERIC MOUNTAIN WAVES; LATENT-HEAT RELEASE; GRAVITY-WAVES; LOWER THERMOSPHERE; PLANETARY-WAVES; ROTATIONAL TEMPERATURES; MODEL; MESOSPHERE; TIDES; VACILLATIONS AB Climatologies of gravity waves, quasi-stationary planetary waves, and tides are compared in the upper stratosphere, mesosphere, and lower thermosphere. Temperature standard deviations from zonal means are used as proxies for wave activity. The sum of the waves is compared to directly measured total temperature fluctuations. The resulting difference is used as a proxy for traveling planetary waves. A preliminary climatology for these waves is proposed. A ranking of the four wave types in terms of their impact on the total wave state of the atmosphere is achieved, which is dependent on altitude and latitude. At extratropical latitudes, gravity waves mostly play a major role. Traveling planetary waves are found to play a secondary role. Quasi-stationary planetary waves and tides yield a lesser contribution there. Vertical profiles of total temperature fluctuations show a sharp vertical gradient change("kink" or "bend") in the mesosphere. This is interpreted in terms of a change of wave damping, and the concept of a "wave turbopause" is suggested. The altitude of this wave turbopause is found to be mostly determined by the relative intensities of gravity waves and planetary waves. The turbopause is further analyzed, including earlier mass spectrometer data. It is found that the wave turbopause and the mass spectrometer turbopause occur rather close together. The turbopause forms a layer about 8 km thick, and the data suggest an additional 3 km mixing layer on top. C1 [Offermann, D.; Gusev, O.; Oberheide, J.] Univ Wuppertal, Dept Phys, D-42097 Wuppertal, Germany. [Gusev, O.] Deutsch Zentrum Luft & Raumfahrt, Oberpfaffenhofen, Germany. [Donner, M.] Donner Tontech, D-42857 Remscheid, Germany. [Forbes, J. M.] Univ Colorado, Boulder, CO 80309 USA. [Hagan, M.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Mlynczak, M. G.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Preusse, P.] Forschungszentrum Julich, Inst Chem & Dynam Geosphare Stratosphare 1, D-52425 Julich, Germany. [Schmidt, H.] Max Planck Inst Meteorol, D-20146 Hamburg, Germany. [Russell, J. M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. RP Offermann, D (reprint author), Univ Wuppertal, Dept Phys, Gaussstr 20, D-42097 Wuppertal, Germany. EM offerm@uni-wuppertal.de RI Oberheide, Jens/C-6156-2011; Mlynczak, Martin/K-3396-2012; Preusse, Peter/A-1193-2013; Schmidt, Hauke/J-4469-2013; Hagan, Maura/C-7200-2008; OI Oberheide, Jens/0000-0001-6721-2540; Preusse, Peter/0000-0002-8997-4965; Schmidt, Hauke/0000-0001-8271-6456; Hagan, Maura/0000-0002-8866-7429; FORBES, JEFFREY/0000-0001-6937-0796 FU Deutsche Forschungsgemeinschaft (DFG, Bonn); German Climate Computing Centre (DKRZ, Hamburg); NASA TIMED Program [NNX07AB74G] FX This work was supported by Deutsche Forschungsgemeinschaft (DFG, Bonn) as part of the CAWSES priority program. We acknowledge the support of the German Climate Computing Centre (DKRZ, Hamburg) where the HAMMONIA simulations were performed. J.M.F. acknowledges support under grant NNX07AB74G from the NASA TIMED Program. D.O. thanks Ralf Koppmann for continuous discussions and support. NR 60 TC 31 Z9 32 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 MAR 21 PY 2009 VL 114 AR D06110 DI 10.1029/2008JD010662 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 422PH UT WOS:000264439700002 ER PT J AU Smirnov, A Holben, BN Slutsker, I Giles, DM McClain, CR Eck, TF Sakerin, SM Macke, A Croot, P Zibordi, G Quinn, PK Sciare, J Kinne, S Harvey, M Smyth, TJ Piketh, S Zielinski, T Proshutinsky, A Goes, JI Nelson, NB Larouche, P Radionov, VF Goloub, P Moorthy, KK Matarrese, R Robertson, EJ Jourdin, F AF Smirnov, A. Holben, B. N. Slutsker, I. Giles, D. M. McClain, C. R. Eck, T. F. Sakerin, S. M. Macke, A. Croot, P. Zibordi, G. Quinn, P. K. Sciare, J. Kinne, S. Harvey, M. Smyth, T. J. Piketh, S. Zielinski, T. Proshutinsky, A. Goes, J. I. Nelson, N. B. Larouche, P. Radionov, V. F. Goloub, P. Moorthy, K. Krishna Matarrese, R. Robertson, E. J. Jourdin, F. TI Maritime Aerosol Network as a component of Aerosol Robotic Network SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SUN PHOTOMETER MEASUREMENTS; OPTICAL-THICKNESS; SEA-SALT; SATELLITE; OCEAN; DEPTH; CLIMATOLOGY; PERFORMANCE; RETRIEVALS; VALIDATION AB The paper presents the current status of the Maritime Aerosol Network (MAN), which has been developed as a component of the Aerosol Robotic Network (AERONET). MAN deploys Microtops handheld Sun photometers and utilizes the calibration procedure and data processing (Version 2) traceable to AERONET. A web site dedicated to the MAN activity is described. A brief historical perspective is given to aerosol optical depth (AOD) measurements over the oceans. A short summary of the existing data, collected on board ships of opportunity during the NASA Sensor Intercomparison and Merger for Biological and Interdisciplinary Oceanic Studies (SIMBIOS) Project is presented. Globally averaged oceanic aerosol optical depth (derived from island-based AERONET measurements) at 500 nm is similar to 0.11 and Angstrom parameter (computed within spectral range 440-870 nm) is calculated to be similar to 0.6. First results from the cruises contributing to the Maritime Aerosol Network are shown. MAN ship-based aerosol optical depth compares well to simultaneous island and near-coastal AERONET site AOD. C1 [Smirnov, A.; Holben, B. N.; Slutsker, I.; Giles, D. M.; Eck, T. F.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. [Smirnov, A.; Slutsker, I.; Giles, D. M.] Sci Syst & Applicat Inc, Lanham, MD USA. [McClain, C. R.] NASA, Goddard Space Flight Ctr, Ocean Sci Branch, Greenbelt, MD 20771 USA. [Eck, T. F.] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. [Sakerin, S. M.] Russian Acad Sci, Inst Atmospher Opt, Siberian Branch, Tomsk 634055, Russia. [Macke, A.; Croot, P.] Univ Kiel, Leibniz Inst Marine Sci, D-24105 Kiel, Germany. [Zibordi, G.] Joint Res Ctr, Inst Environm & Sustainabil, I-21027 Ispra, Italy. [Quinn, P. K.] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA. [Sciare, J.] Lab Sci Climat & Environm, F-91191 Gif Sur Yvette, France. [Kinne, S.] Univ Hamburg, Inst Meteorol, D-20146 Hamburg, Germany. [Harvey, M.] Natl Inst Water & Atmospher Res, Wellington 6021, New Zealand. [Smyth, T. J.] Plymouth Marine Lab, Plymouth PL1 3DH, Devon, England. [Piketh, S.] Univ Witwatersrand, Climatol Res Grp, ZA-2050 Johannesburg, South Africa. [Zielinski, T.] Polish Acad Sci, Inst Oceanol, PL-81712 Sopot, Poland. [Proshutinsky, A.] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA. [Goes, J. I.] Bigelow Lab Ocean Sci, W Boothbay Harbor, ME 04575 USA. [Nelson, N. B.] Univ Calif Santa Barbara, Inst Computat Earth Syst Sci, Santa Barbara, CA 93106 USA. [Larouche, P.] Inst Maurice Lamontagne, Mont Joli, PQ G5H 3Z4, Canada. [Radionov, V. F.] Arctic & Antarctic Res Inst, St Petersburg 199397, Russia. [Goloub, P.] Univ Sci & Tech Lille, Opt Atmospher Lab, F-59650 Villeneuve Dascq, France. [Moorthy, K. Krishna] Vikram Sarabhai Space Ctr, Space Phys Lab, Trivandrum 695022, Kerala, India. [Matarrese, R.] Univ Bari, Dept Phys, I-70122 Bari, Italy. [Robertson, E. J.] Univ Cape Town, Dept Oceanog, ZA-7701 Cape Town, South Africa. [Jourdin, F.] Serv Hydrog & Oceanog Marine, F-29228 Brest, France. RP Smirnov, A (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Code 614-4,Bldg 33,Room G406, Greenbelt, MD 20771 USA. EM Alexander.Smirnov-1@nasa.gov RI Smirnov, Alexander/C-2121-2009; Smyth, Tim/D-2008-2012; ECK, THOMAS/D-7407-2012; Nelson, Norman/B-7343-2014; Croot, Peter/C-8460-2009; Harvey, Mike/A-5354-2010; Matarrese, Raffaella/D-5174-2016; Quinn, Patricia/R-1493-2016 OI Moorthy, K. Krishna/0000-0002-7234-3868; Smirnov, Alexander/0000-0002-8208-1304; Nelson, Norman/0000-0003-1767-7598; Croot, Peter/0000-0003-1396-0601; Harvey, Mike/0000-0002-0979-0227; Matarrese, Raffaella/0000-0002-3923-9639; Quinn, Patricia/0000-0003-0337-4895 FU Polish national grant AERONET59 FX The authors thank Hal Maring (NASA Headquarters) for his support of AERONET. The authors would like to acknowledge managerial and operational support from W. W. Newcomb, M. Sorokin, A. Scully, A. Tran, D. A. Siegel, K. Knobelspiesse, D. Hamilton, L. Rainville, A. Jayakumar, S. Schick, and D. Menzies (USA); N. T. O'Neill, C. Bourgeault- Brunelle, and M. Palmer (Canada); M. Panchenko, O. Kopelevich, S. Gulev, D. Kabanov, S. Terpugova, V. Polkin, A. Tikhomirov, A. Sinitsyn, Y. Turchinovich, and N. Vlasov (Russia); L. Blarel, J. Nicolas, S. Devidal, L. Martinon, M. Faillot, and C. Petus (France); A. Baker and C. Powell (UK); A. Herber, Y. Zoll, A. Wassmann, and M. Heller (Germany); H. Power, T. Bromley, and R. Martin (New Zealand); J. Piskozub, J. Kowalczyk, and A. Ponczkowska (Poland); D. Williams and B. Kuyper (South Africa); J. Stamnes and S. Iversen (Norway); and K. Niranjan, S. Babu, and S. K. Satheesh (India). We thank the AERONET site managers and the SIMBIOS principal investigators for maintaining the instruments and making collection of these data possible. Jean Sciare would like to thank Institut Polaire Francais (IPEV) and the IPEV-AEROTRACE observatory program for providing technical support and infrastructure. The work of Tymon Zielinski was supported by Polish national grant AERONET59. NR 41 TC 90 Z9 97 U1 1 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAR 21 PY 2009 VL 114 AR D06204 DI 10.1029/2008JD011257 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 422PH UT WOS:000264439700007 ER PT J AU Usoskin, IG Field, CV Schmidt, GA Leppanen, AP Aldahan, A Kovaltsov, GA Possnert, G Ungar, RK AF Usoskin, Ilya G. Field, Christy V. Schmidt, Gavin A. Leppaenen, Ari-Pekka Aldahan, Ala Kovaltsov, Gennady A. Possnert, Goeran Ungar, R. Kurt TI Short-term production and synoptic influences on atmospheric Be-7 concentrations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID COSMOGENIC NUCLIDE PRODUCTION; GENERAL-CIRCULATION MODEL; CHEMICAL TRACER MODEL; TEST-BAN TREATY; EARTHS ATMOSPHERE; PRODUCTION-RATES; ENERGY-SPECTRA; SURFACE AIR; TRANSPORT; SOLAR AB Variations of the cosmogenic radionuclide Be-7 in the global atmosphere are driven by cooperation of processes of its production, air transports, and removal. We use a combination of the Goddard Institute for Space Studies ModelE and the OuluCRAC: Be-7 production model to simulate the variations in the Be-7 concentration in the atmosphere for the period from 1 January to 28 February 2005. This period features significant synoptic variability at multiple monitoring stations around the globe and spans an extreme solar energetic particle (SEP) event that occurred on 20 January. Using nudging from observed horizontal winds, the model correctly reproduces the overall level of the measured Be-7 concentration near ground and a great deal of the synoptic variability at timescales of 4 days and longer. This verifies the combined model of production and transport of the Be-7 radionuclide in the atmosphere. The impact of an extreme SEP event of January 2005 is seen dramatically in polar stratospheric Be-7 concentration but is small near the surface (about 2%) and indistinguishable given the amount of intrinsic variability and the uncertainties of the surface observations. C1 [Usoskin, Ilya G.] Univ Oulu, Oulu Unit, Sodankyla Geophys Observ, FIN-90014 Oulu, Finland. [Field, Christy V.; Schmidt, Gavin A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Leppaenen, Ari-Pekka] STUK Radiat & Nucl Safety Author, Reg Lab No Finland, FIN-96500 Rovaniemi, Finland. [Aldahan, Ala] Uppsala Univ, Dept Earth Sci, SE-75236 Uppsala, Sweden. [Aldahan, Ala] United Arab Emirates Univ, Dept Geol, Al Ain, U Arab Emirates. [Kovaltsov, Gennady A.] AF Ioffe Phys Tech Inst, RU-194021 St Petersburg, Russia. [Possnert, Goeran] Uppsala Univ, Tandem Lab, SE-75236 Uppsala, Sweden. [Ungar, R. Kurt] Radiat Protect Bur Hlth Canada, Ottawa, ON K1A 1C1, Canada. RP Usoskin, IG (reprint author), Univ Oulu, Oulu Unit, Sodankyla Geophys Observ, POB 3000, FIN-90014 Oulu, Finland. EM ilya.usoskin@oulu.fi RI Schmidt, Gavin/D-4427-2012; Usoskin, Ilya/E-5089-2014; Kovaltsov, Gennady/F-5191-2014 OI Schmidt, Gavin/0000-0002-2258-0486; Usoskin, Ilya/0000-0001-8227-9081; FU NASA Modeling, Analysis and Prediction program; US National Science Foundation; Academy of Finland and Suomalainen Tiedeakatemia (Vaisala Foundation); Program of Presidium RAS [N16-3-5.4] FX We gratefully acknowledge CTBTO for funding, building, and maintaining the monitoring station network. We thank the Finnish National Data Centre for providing access to the 7Be data in the FiNDC database. We also acknowledge national authorities in United States, Canada, Sweden, Germany, Australia, and New Zealand for providing the necessary permissions for use of monitoring data in scientific studies. Climate modeling at GISS is supported by NASA Modeling, Analysis and Prediction program. C. F. also acknowledges support from the US National Science Foundation through a Fellowship in the IGERT Joint Program in Applied Mathematics and Earth and Environmental Sciences at Columbia University. Supports from the Academy of Finland and Suomalainen Tiedeakatemia (Vaisala Foundation) are acknowledged. G. A. K. was partly supported by the Program of Presidium RAS N16-3-5.4. NR 51 TC 26 Z9 27 U1 0 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 MAR 21 PY 2009 VL 114 AR D06108 DI 10.1029/2008JD011333 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 422PH UT WOS:000264439700008 ER PT J AU Haider, SA Abdu, MA Batista, IS Sobral, JH Luan, XL Kallio, E Maguire, WC Verigin, MI Singh, V AF Haider, S. A. Abdu, M. A. Batista, I. S. Sobral, J. H. Luan, Xiaoli Kallio, Esa Maguire, W. C. Verigin, M. I. Singh, V. TI D, E, and F layers in the daytime at high-latitude terminator ionosphere of Mars: Comparison with Earth's ionosphere using COSMIC data SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID RADIO OCCULTATION MEASUREMENTS; ELECTRON-ENERGY DEGRADATION; YIELD SPECTRUM APPROACH; SOLAR-WIND INTERACTION; MARTIAN ATMOSPHERE; MODEL; PRECIPITATION; SPECTROMETER; CHEMISTRY; MISSION AB We report the first model result for ion production rates and densities of positive ions, negative ions, and electrons in the dayside Martian ionosphere from 0 to 220 km. These calculations are made at solar zenith angle 77 degrees for low solar activity periods. The calculated electron density is compared with the radio occultation measurements made by Mars Global Surveyor (MGS) and Mars 4/5 on Mars and by Constellation Observing System for Meteorology, Ionosphere and Climate ( COSMIC) on Earth. Our calculation suggests that the daytime ionosphere of Mars can be divided into D, E, and F layers at altitude ranges similar to 25-35 km, similar to 100-112 km, and similar to 125-145 km with the concentrations 7 x 10(1) cm(-3), 2.4 x 10(4) cm(-3), and 8.4 x 10(4) cm(-3) owing to the impact of galactic cosmic rays, X rays (10-90 angstrom), and solar EUV (90-1026 angstrom) radiations, respectively. The water cluster ions H(3)O(+)(H(2)O)(n), NO(2)(-)(H(2)O)(n), and CO(3)(-)( H(2)O)(n) are dominated in the D region, while NO(+), CO(2)(+), and O(2)(+) are major ions in the E and F regions. The calculated E and F peak heights are in good agreement with MGS observation. The value of D peak density is lowered by 1 and 2 orders of magnitude from the measurements on Mars and Earth, respectively. The height of F layer peak is lower by factor of 1.8 in the Martian ionosphere as compared to that observed in the ionosphere of Earth. E regions are created at nearly the same heights in the ionospheres of both planets, but the layer thickness is considerably less on Mars than on Earth. This implies that solar EUV energy is deposited within smaller-altitude range in the upper ionosphere of Mars as compared to the corresponding altitude range in the upper ionosphere of Earth. C1 [Haider, S. A.] Phys Res Lab, Ahmadabad 380009, Gujarat, India. [Abdu, M. A.; Batista, I. S.; Sobral, J. H.] Inst Nacl Pesquisas Espaciais, Dept Aeron, BR-12227010 Sao Paulo, Brazil. [Kallio, Esa] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland. [Luan, Xiaoli] Natl Ctr Atmospher Res, Boulder, CO 80301 USA. [Maguire, W. C.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Singh, V.] Univ Brescia, Fac Engn, Dept Elect Automat, I-25123 Brescia, Italy. [Verigin, M. I.] Russian Acad Sci, Space Res Inst, Moscow, Russia. RP Haider, SA (reprint author), Phys Res Lab, Ahmadabad 380009, Gujarat, India. EM haider@prl.res.in RI Batista, Inez/F-2899-2012; Kallio, Esa/F-9410-2014 OI Kallio, Esa/0000-0002-9791-804X FU National Science Foundation; National Oceanic and Atmospheric Administration; FAPESP [2007/06736-8] FX Authors are thankful to Dave Hinson and G.L. Tyler, Stanford University Stanford, California, USA, for providing us MGS radio science data of electron density profiles through the Web site http://nova.stanford.edu/projects/mgs/dmwr.html. Development of the COSMIC Data Analysis Archival Center is primarily supported by National Science Foundation and the National Oceanic and Atmospheric Administration. COSMIC data are provided by Taiwan's National Space Organization and University Corporation for Atmospheric Research. S.A. Haider also thanks FAPESP for the support through a visiting scientist fellowship by the process 2007/06736-8 to work at INPE, Brazil. NR 60 TC 17 Z9 18 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAR 21 PY 2009 VL 114 AR A03311 DI 10.1029/2008JA013709 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 422PX UT WOS:000264441300004 ER PT J AU Fabian, AC Vasudevan, RV Mushotzky, RF Winter, LM Reynolds, CS AF Fabian, A. C. Vasudevan, R. V. Mushotzky, R. F. Winter, L. M. Reynolds, C. S. TI Radiation pressure and absorption in AGN: results from a complete unbiased sample from Swift SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiative transfer; galaxies: ISM; galaxies: nuclei; quasars: general ID ACTIVE GALACTIC NUCLEI; MASSIVE BLACK-HOLES; GALAXIES; QUASARS; OBJECTS; GROWTH; SLOPE; DUST AB Outward radiation pressure can exceed the inward gravitational pull on gas clouds in the neighbourhood of a luminous active galactic nucleus (AGN). This creates a forbidden region for long-lived dusty clouds in the observed columnn density-Eddington fraction plane. (The Eddington fraction lambda(Edd) is the ratio of the bolometric luminosity of an AGN to the Eddington limit for its black hole mass.) The Swift/Burst Alert Telescope catalogue is the most complete hard X-ray selected sample of AGN and has 97 low-redshift AGN with measured column densities N-H and inferred black hole masses. Eddington fractions for the sources have been obtained using recent bolometric corrections and the sources have been plotted on the N-H-lambda(Edd) plane. Only one source lies in the forbidden region and it has a large value of N-H due to an ionized warm absorber, for which radiation pressure is reduced. The effective Eddington limit for the source population indicates that the high column density clouds in the more luminous objects lie within the inner few pc, where the central black hole provides at least half the mass. Our result shows that radiation pressure does affect the presence of gas clouds in the inner galaxy bulge. We discuss briefly how the N-H-lambda(Edd) plane may evolve to higher redshift, when feedback due to radiation pressure may have been strong. C1 [Fabian, A. C.; Vasudevan, R. V.] Inst Astron, Cambridge CB3 0HA, England. [Mushotzky, R. F.] NASA, GSFC, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. [Winter, L. M.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Winter, L. M.; Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Fabian, AC (reprint author), Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM acf@ast.cam.ac.uk FU Royal Society; UK Science and Technology Funding Council (STFC) FX ACF thanks The Royal Society for support, RVV acknowledges support from the UK Science and Technology Funding Council (STFC). We thank the BAT Team for their work which has made our study possible. NR 29 TC 25 Z9 25 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 21 PY 2009 VL 394 IS 1 BP L89 EP L92 DI 10.1111/j.1745-3933.2009.00617.x PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 594ZT UT WOS:000277581200019 ER PT J AU Indebetouw, R de Messieres, GE Madden, S Engelbracht, C Smith, JD Meixner, M Brandl, B Smith, LJ Boulanger, F Galliano, F Gordon, K Hora, JL Sewilo, M Tielens, AGGM Werner, M Wolfire, MG AF Indebetouw, R. de Messieres, G. E. Madden, S. Engelbracht, C. Smith, J. D. Meixner, M. Brandl, B. Smith, L. J. Boulanger, F. Galliano, F. Gordon, K. Hora, J. L. Sewilo, M. Tielens, A. G. G. M. Werner, M. Wolfire, M. G. TI PHYSICAL CONDITIONS IN THE IONIZED GAS OF 30 DORADUS SO ASTROPHYSICAL JOURNAL LA English DT Article DE H II regions; infrared: ISM; ISM: individual (30 Doradus); Magellanic Clouds ID LARGE-MAGELLANIC-CLOUD; SPITZER-SPACE-TELESCOPE; SUPERNOVA REMNANT CANDIDATES; COMBINED STELLAR STRUCTURE; GALAXY EVOLUTION SAGE; COMPACT HII-REGIONS; WOLF-RAYET STARS; H-II REGIONS; INTERSTELLAR-MEDIUM; MASSIVE STARS AB We present a mid-infrared spectroscopic data cube of the central part of 30 Doradus, observed with Spitzer's Infrared Spectrograph and Multiband Imaging Photometer for Spitzer/spectral energy distribution mode. Aromatic dust emission features and emission lines from molecular and atomic hydrogen are detected but they are not particularly strong. The dominant spectral features are emission lines from moderately ionized species of argon, neon, and sulfur, which are used to determine the physical conditions in the ionized gas. The ionized gas excitation shows strong variations on parsec scales, some of which can plausibly be associated with individual hot stars. We fit the ionic line strengths with photoionization and shock models, and find that photoionization dominates in the region. The ionization parameter U traces the rim of the central bubble, as well as highlighting isolated sources of ionization, and at least one quiescent clump. The hardness of the ionizing radiation field T(rad) reveals several "hot spots" that are either the result of individual very hot stars or trace the propagation of the diffuse ionizing field through the surrounding neutral cloud. Consistent with other measurements of giant H II regions, log(U) ranges between -3 and -0.75, and T(rad) between 30,000 and 85,000 K. C1 [Indebetouw, R.; de Messieres, G. E.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Indebetouw, R.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Madden, S.] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Engelbracht, C.; Gordon, K.] Univ Arizona, Steward Observ, Tucson, AZ 85719 USA. [Smith, J. D.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Meixner, M.; Smith, L. J.; Sewilo, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Brandl, B.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Smith, L. J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Boulanger, F.] CNRS, IAP, UPR 341, F-75014 Paris, France. [Galliano, F.; Wolfire, M. G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Hora, J. L.] Harvard Univ, Ctr Astrophys, Cambridge, MA 02138 USA. [Tielens, A. G. G. M.] NASA, Ames Res Ctr, SOFIA Off, Moffett Field, CA 94035 USA. [Werner, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Indebetouw, R (reprint author), Univ Virginia, Dept Astron, POB 3818, Charlottesville, VA 22903 USA. EM remy@virginia.edu; ged3j@virginia.edu OI Hora, Joseph/0000-0002-5599-4650 NR 74 TC 26 Z9 26 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2009 VL 694 IS 1 BP 84 EP 106 DI 10.1088/0004-637X/694/1/84 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 420LQ UT WOS:000264291700009 ER PT J AU Watanabe, S Sato, R Takahashi, T Kataoka, J Madejski, G Sikora, M Tavecchio, F Sambruna, R Romani, R Edwards, PG Pursimo, T AF Watanabe, Shin Sato, Rie Takahashi, Tadayuki Kataoka, Jun Madejski, Greg Sikora, Marek Tavecchio, Fabrizio Sambruna, Rita Romani, Roger Edwards, Philip G. Pursimo, Tapio TI SUZAKU OBSERVATIONS OF THE EXTREME MeV BLAZAR SWIFT J0746.3+2548 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; quasars: individual (J0746.3+2548); X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; HOBBY-EBERLY TELESCOPE; BURST ALERT TELESCOPE; AMBIENT RADIATION; NONTHERMAL FLARES; RELATIVISTIC JET; LOUD QUASARS; BOARD SUZAKU; VARIABILITY AB We report the Suzaku observations of the high luminosity blazar SWIFT J0746.3+2548 (J0746) conducted in 2005 November. This object, which, with z = 2.979, is the highest redshift source observed in the Suzaku Guaranteed Time Observer period, is likely to show high gamma-ray flux peaking in the MeV range. As a result of the good photon statistics and high signal-to-noise ratio spectrum, the Suzaku observation clearly confirms that J0746 has an extremely hard spectrum in the energy range of 0.3-24 keV, which is well represented by a single power-law with a photon index of Gamma(ph) similar or equal to 1.17 and Galactic absorption. The multiwavelength spectral energy distribution of J0746 shows two continuum components, and is well modeled assuming that the high-energy spectral component results from Comptonization of the broad-line region photons. In this paper, we search for the bulk Compton spectral features predicted to be produced in the soft X-ray band by scattering external optical/UV photons by cold electrons in a relativistic jet. We discuss and provide constraints on the pair content resulting from the apparent absence of such features. C1 [Watanabe, Shin; Sato, Rie; Takahashi, Tadayuki; Edwards, Philip G.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Watanabe, Shin; Takahashi, Tadayuki] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. [Kataoka, Jun] Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528551, Japan. [Madejski, Greg; Romani, Roger] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Sikora, Marek] Nicholas Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Tavecchio, Fabrizio] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. [Sambruna, Rita] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Edwards, Philip G.] CSIRO, Australia Telescope Natl Facil, Narrabri, NSW 2390, Australia. [Pursimo, Tapio] Nord Opt Telescope, Santa Cruz De La Palma 38700, Spain. RP Watanabe, S (reprint author), JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. EM watanabe@astro.isas.jaxa.jp RI XRAY, SUZAKU/A-1808-2009 FU Department of Energy [DE-AC3-76SF00515]; NASA [NNX07AB05G] FX We thank the anonymous referee for her/his valuable comments that helped to improve this paper. The National Radio Astronomy Observatory (NRAO) is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NRAO is thanked for the provision of Target of Opportunity time for the observations, and Barry Clark is thanked for assistance is the preparation of observing files. The research described herewe supported in part by the Department of Energy contract to SLAC no. DE-AC3-76SF00515, and NASA grant to Stanford University no. NNX07AB05G. Based on observations made with the Nordic Optical Telescope, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. NR 41 TC 7 Z9 7 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2009 VL 694 IS 1 BP 294 EP 301 DI 10.1088/0004-637X/694/1/294 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 420LQ UT WOS:000264291700028 ER PT J AU Scott, JE Arav, N Gabel, JR Kriss, GA Quijano, JK Kaastra, JS Costantini, E Korista, K AF Scott, Jennifer E. Arav, Nahum Gabel, Jack R. Kriss, Gerard A. Quijano, Jessica Kim Kaastra, Jelle S. Costantini, Elisa Korista, Kirk TI VARIABLE INTRINSIC ABSORPTION IN Mrk 279 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (Mrk 279); galaxies: Seyfert; quasars: absorption lines; ultraviolet: galaxies; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; TELESCOPE IMAGING SPECTROGRAPH; SEYFERT-GALAXY NGC-4151; ULTRAVIOLET-SPECTROSCOPIC-EXPLORER; RAY/ULTRAVIOLET OBSERVING CAMPAIGN; X-RAY OBSERVATIONS; DRIVEN DISK WINDS; IONIZED-GAS; SPACE-TELESCOPE; PHYSICAL CONDITIONS AB We examine the variability in the intrinsic absorption in the Seyfert 1 galaxy Mrk 279 using three epochs of observations from the Far Ultraviolet Spectroscopic Explorer and two epochs of observations with the Space Telescope Imaging Spectrograph on the Hubble Space Telescope. Rather than finding simple photoionization responses of the absorbing gas to changes in the underlying continuum, the observed changes in the absorption profiles can be understood more clearly if the effective covering fraction of the gas in all emission components, continuum, and broad and intermediate velocity width emission lines, is accounted for. While we do not uniquely solve for all of these separate covering fractions and the ionic column densities using the spectral data, we examine the parameter space using previously well-constrained solutions for continuum and single emission component covering fractions. Assuming full coverage of the continuum, we find that of the two velocity components of the Mrk 279 absorption most likely associated with its outflow, one likely has zero coverage of the intermediate-line region (ILR) while the other does not. For each component, however, the broad-line region is more fully covered than the ILR. Changes in the O VI column densities are unconstrained due to saturation, but we show that small changes in the nonsaturated C IV and N V column densities are consistent with the outflow gas having zero or partial covering of the ILR and an ionization parameter changing from similar to 0.01 to similar to 0.1 from 2002 to 2003 as the UV continuum flux increased by a factor of similar to 8. The absence of a change in the C III absorbing column density is attributed to this species arising outside the Mrk 279 outflow. C1 [Scott, Jennifer E.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Arav, Nahum; Gabel, Jack R.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Kriss, Gerard A.; Quijano, Jessica Kim] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kriss, Gerard A.] Johns Hopkins Univ, Dept Phys & Astron, Ctr Astrophys Sci, Baltimore, MD 21218 USA. [Kaastra, Jelle S.; Costantini, Elisa] SRON, Natl Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Korista, Kirk] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. RP Scott, JE (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. EM jescott@towson.edu; arav@vt.edu; jackgabel@creighton.edu; gak@stsci.edu; jkimgak@stsci.edu; J.S.Kaastra@sron.nl; e.costantini@sron.nl; korista@wmich.edu FU National Research Council Associateship FX J. E. S. acknowledges the support of a National Research Council Associateship held at NASA Goddard Space Flight Center and the support of the Jess and Mildred Fisher Endowed Chair in the Biological and Physical Sciences, held at Towson University. We thank the anonymous referee for helpful comments. NR 47 TC 2 Z9 2 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2009 VL 694 IS 1 BP 438 EP 448 DI 10.1088/0004-637X/694/1/438 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 420LQ UT WOS:000264291700043 ER PT J AU Zasowski, G Kemper, F Watson, DM Furlan, E Bohac, CJ Hull, C Green, JD AF Zasowski, G. Kemper, F. Watson, Dan M. Furlan, E. Bohac, C. J. Hull, C. Green, J. D. TI SPITZER INFRARED SPECTROGRAPH OBSERVATIONS OF CLASS I/II OBJECTS IN TAURUS: COMPOSITION AND THERMAL HISTORY OF THE CIRCUMSTELLAR ICES SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; infrared: ISM; ISM: abundances; ISM: molecules; stars: pre-main sequence ID YOUNG STELLAR OBJECTS; DIFFUSE INTERSTELLAR-MEDIUM; STAR-FORMING REGIONS; SOLID CARBON-DIOXIDE; MAIN-SEQUENCE STARS; CLASS-I PROTOSTARS; MU-M; ABSORPTION FEATURES; SPACE-TELESCOPE; SPECTROSCOPIC SURVEY AB We present observations of Taurus-Auriga Class I/II protostars obtained with the Spitzer InfraRed Spectrograph. Detailed spectral fits to the 6 and 15.2 micron ice features are made, using publicly available laboratory data, to constrain the molecular composition, abundances, and levels of thermal processing along the lines of sight. We provide an inventory of the molecular environments observed, which have an average composition dominated by water-ice with similar to 12% CO(2) ( abundance relative to H(2)O), greater than or similar to 2%-9% CH(3)OH, similar to 14% NH(3), similar to 3% CH(4), similar to 2% H(2)CO, similar to 0.6% HCOOH, and similar to 0.5% SO(2). We find CO(2)/H(2)O ratios nearly equivalent to those observed in cold clouds and lines of sight toward the galactic center. The unidentified 6.8 micron profiles vary from source to source, and it is shown to be likely that even combinations of the most common candidates ( NH(4)(+) and CH(3)OH) are inadequate to explain the feature fully. We discuss correlations among SED spectral indices, abundance ratios, and thermally processed ice fractions and their implications for CO(2) formation and evolution. Comparison of our spectral fits with cold molecular cloud sight lines indicates abundant prestellar ice environments made even richer by the radiative effects of protostars. Our results add additional constraints and a finer level of detail to current full-scale models of protostellar and protoplanetary systems. C1 [Zasowski, G.; Kemper, F.; Hull, C.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Watson, Dan M.; Bohac, C. J.; Green, J. D.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Kemper, F.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Furlan, E.] Univ Calif Los Angeles, NASA, Astrobiol Inst, Los Angeles, CA 90095 USA. [Furlan, E.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. RP Zasowski, G (reprint author), Univ Virginia, Dept Astron, POB 400325, Charlottesville, VA 22904 USA. EM gailis@virginia.edu; Ciska.Kemper@manchester.ac.uk; dmw@pas.rochester.edu; furlan@astro.ucla.edu; urgradcb@gmail.com; chat.hull@gmail.com; joel@pas.rochester.edu RI Kemper, Francisca/D-8688-2011; OI Kemper, Francisca/0000-0003-2743-8240; Furlan, Elise/0000-0001-9800-6248 FU NASA [1257184] FX We thank the anonymous referee for a thorough and stimulating review. We are grateful to Edwin Bergin and Claudia Knez for providing us with the field star spectra, to Melissa McClure for assistance with data reduction issues, and to Adwin Boogert for stimulating discussion. Extensive usewasmade of Leiden University's Sackler Laboratory ice analog databases and of the NASA ADS Abstract Service. This work is based on observations made with the SST, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. Support for this work was provided by NASA through contract number 1257184 issued by JPL/Caltech. E. F. acknowledges support from a NASA Postdoctoral Program Fellowship. NR 91 TC 65 Z9 65 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2009 VL 694 IS 1 BP 459 EP 478 DI 10.1088/0004-637X/694/1/459 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 420LQ UT WOS:000264291700045 ER PT J AU Ofman, L AF Ofman, L. TI THREE-DIMENSIONAL MAGNETOHYDRODYNAMIC MODELS OF TWISTED MULTITHREADED CORONAL LOOP OSCILLATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE MHD; Sun: corona; Sun: flares; Sun: magnetic fields; waves ID ALFVEN WAVES; RESONANT ABSORPTION; MAGNETIC-FIELD; TRANSVERSE OSCILLATIONS; KINK OSCILLATIONS; SOLAR ATMOSPHERE; ACTIVE-REGION; SCALING LAWS; SEISMOLOGY; TRACE AB The multithreaded structure of active region coronal loops was deduced from past spectroscopic observations. Recent high-resolution observations by Transition Region and Coronal Explorer and Hinode satellites provided direct evidence that active region loops consist of multiple magnetic threads filled with plasma with higher density than neighboring loop material. High-resolution observations of loops near a flare site suggest that the threads are twisted or tangled, the magnetic field is not force free, and flows are present. To better understand these observations, we developed for the first time a three-dimensional magnetohydrodynamic model of twisted multithreaded loops that oscillate as a result of an impulsive event. The twist is induced by applying a rotating velocity field at the footpoint of the initially parallel set of threads, and parallel flow is included. The oscillations of the twisted loops are excited by a fast magnetosonic pulse. The evolution and the damping of the fast magnetosonic wave excited in the twisted multithreaded loop are compared to oscillations of a four-parallel-threaded loop. It was found that twisted loop oscillations result in filamented current and velocity structure that cannot be described by the fundamental kink mode. When parallel flow is present, the oscillation induces nonlinear compressive modulation of the flow and density in the threads. The twisted loop oscillates and damps faster than the parallel-threaded loop. The results of the study demonstrate the effects of the twist, internal loop structure, and flow on the evolution of the waves in coronal active region loops. C1 [Ofman, L.] Catholic Univ Amer, Dept Phys, Greenbelt, MD 20771 USA. [Ofman, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ofman, L (reprint author), Tel Aviv Univ, IL-69978 Tel Aviv, Israel. EM Leon.Ofman@gsfc.nasa.gov FU NASA [NNG06GI55G]; NRL [N00173-06-1-G033] FX This work was supported by NASA grant NNG06GI55G, NRL contract N00173-06-1-G033, and by NASA Sun-Earth Connection Theory Program. The computations in this work were carried out on NASAs Columbia system. NR 38 TC 31 Z9 31 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2009 VL 694 IS 1 BP 502 EP 511 DI 10.1088/0004-637X/694/1/502 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 420LQ UT WOS:000264291700048 ER PT J AU Boersma, C Mattioda, AL Bauschlicher, CW Peeters, E Tielens, AGGM Allamandola, LJ AF Boersma, C. Mattioda, A. L. Bauschlicher, C. W. Peeters, E. Tielens, A. G. G. M. Allamandola, L. J. TI THE 5.25 AND 5.7 mu m ASTRONOMICAL POLYCYCLIC AROMATIC HYDROCARBON EMISSION FEATURES (vol 690, pg 1208, 2009) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Boersma, C.; Tielens, A. G. G. M.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Mattioda, A. L.; Bauschlicher, C. W.; Tielens, A. G. G. M.; Allamandola, L. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Mattioda, A. L.; Peeters, E.] SETI Inst, Mountain View, CA 94043 USA. [Peeters, E.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. RP Boersma, C (reprint author), Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands. EM C.Boersma@astro.rug.nl RI Boersma, Christiaan/L-7696-2014 OI Boersma, Christiaan/0000-0002-4836-217X NR 1 TC 0 Z9 0 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2009 VL 694 IS 1 BP 704 EP 705 DI 10.1088/0004-637X/694/1/704 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 420LQ UT WOS:000264291700063 ER PT J AU Mastichiadis, A Kazanas, D AF Mastichiadis, A. Kazanas, D. TI THE SUPERCRITICAL PILE GAMMA-RAY BURST MODEL: THE PROMPT TO AFTERGLOW EVOLUTION SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gamma rays: bursts ID BLAST-WAVE MODEL; 28 FEBRUARY 1997; LIGHT CURVES; EMISSION; BATSE AB The "Supercritical Pile" is a very economical gamma-ray burst (GRB) model that provides for the efficient conversion of the energy stored in the protons of a relativistic blast wave (RBW) into radiation and at the same time produces-in the prompt GRB phase, even in the absence of any particle acceleration-a spectral peak at energy similar to 1MeV. We extend this model to include the evolution of the RBW Lorentz factor Gamma and thus follow its spectral and temporal features into the early GRB afterglow stage. One of the novel features of the present treatment is the inclusion of the feedback of the GRB produced radiation on the evolution of Gamma with radius. This feedback and the presence of kinematic and dynamic thresholds in the model are sources of potentially very rich time evolution which we have began to explore. In particular, one can this way obtain afterglow light curves with steep decays followed by the more conventional flatter afterglow slopes, while at the same time preserving the desirable features of the model, i.e., the well-defined relativistic electron source and radiative processes that produce the proper peak in the nu F-nu spectra. In this Letter, we present the results of a specific set of parameters of this model with emphasis on the multiwavelength prompt emission and transition to the early afterglow. C1 [Mastichiadis, A.] Univ Athens, Dept Phys, GR-15783 Zografos, Greece. [Kazanas, D.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Mastichiadis, A (reprint author), Univ Athens, Dept Phys, GR-15783 Zografos, Greece. FU Special Funds for Research (ELKE) of the University of Athens; INTEGRAL GO FX We would like to thank the referee for comments that helped improve this Letter. This research was funded in part by a grant from the Special Funds for Research (ELKE) of the University of Athens. D. K. acknowledges support by an INTEGRAL GO grant. NR 25 TC 10 Z9 10 U1 0 U2 1 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 MAR 20 PY 2009 VL 694 IS 1 BP L54 EP L58 DI 10.1088/0004-637X/694/1/L54 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 419CK UT WOS:000264196500012 ER PT J AU Xiong, XX Wu, AS Wenny, BN AF Xiong, Xiaoxiong Wu, Aisheng Wenny, Brian N. TI Using Dome C for moderate resolution imaging spectroradiometer calibration stability and consistency SO JOURNAL OF APPLIED REMOTE SENSING LA English DT Article DE MODIS; solar diffuser; blackbody; calibration; Dome C; inter-comparison; sensor ID THERMAL EMISSIVE BANDS; IN-FLIGHT VALIDATION; ON-ORBIT CALIBRATION; BIDIRECTIONAL REFLECTANCE; SURFACE TEMPERATURE; RADIOMETRIC CALIBRATION; INFRARED DATA; LAKE TAHOE; MODIS; TERRA AB Currently, there are two nearly identical moderate resolution imaging spectroradiometer (MODIS) instruments operated in space: one on the Terra spacecraft launched in December 1999 and another on the Aqua spacecraft launched in May 2002. MODIS has 36 spectral bands with wavelengths covering from visible (VIS) to long-wave infrared (LWIR). Since launch, MODIS observations and data products have significantly enabled studies of changes in the Earth system of land, oceans, and atmosphere. In order to maintain its on-orbit calibration and data product quality, MODIS was built with a comprehensive set of on-board calibrators. MODIS reflective solar bands (RSB) are calibrated on-orbit by a system that consists of a solar diffuser (SD) and a solar diffuser stability monitor (SDSM) on a regular basis. Its thermal emissive bands (TEB) calibration is executed on a scan-by-scan basis using an on-board blackbody (BB). The MODIS Characterization Support Team (MCST) at NASA/GSFC has been responsible for supporting sensor calibration and characterization tasks from pre-launch to post launch. In this paper, we describe current MCST efforts and progress made to examine sensor stability and intercalibration consistency using observations over Dome Concordia, Antarctica. Results show that this site can provide useful calibration reference for Earth-observing sensors. C1 [Xiong, Xiaoxiong] NASA, Sci & Explorat Directorate, GSFC, Greenbelt, MD 20771 USA. [Wu, Aisheng; Wenny, Brian N.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. RP Xiong, XX (reprint author), NASA, Sci & Explorat Directorate, GSFC, Greenbelt, MD 20771 USA. EM xiaoxiong.xiong-1@nasa.gov; aisheng_wu@ssaihq.com; brian.n.wenny@nasa.gov NR 32 TC 13 Z9 13 U1 0 U2 3 PU SPIE-SOC PHOTOPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 1931-3195 J9 J APPL REMOTE SENS JI J. Appl. Remote Sens. PD MAR 20 PY 2009 VL 3 AR 033520 DI 10.1117/1.3116663 PG 12 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 520SU UT WOS:000271869100002 ER PT J AU Loh, CY Jorgenson, PCE AF Loh, Ching Y. Jorgenson, Philip C. E. TI Multi-dimensional dissipation for cure of pathological behaviors of upwind scheme SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE Compressible flow; Upwind finite volume scheme; Pathological behaviors; Multi-dimensional dissipation C1 [Loh, Ching Y.; Jorgenson, Philip C. E.] NASA, Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA. RP Loh, CY (reprint author), NASA, Glenn Res Ctr Lewis Field, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM Ching.Y.Loh@grc.nasa.gov NR 6 TC 8 Z9 9 U1 0 U2 1 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0021-9991 J9 J COMPUT PHYS JI J. Comput. Phys. PD MAR 20 PY 2009 VL 228 IS 5 BP 1343 EP 1346 DI 10.1016/j.jcp.2008.10.044 PG 4 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA 407NC UT WOS:000263370600001 ER PT J AU Chato, DJ AF Chato, David J. TI Phase field modeling of liquid jets in low gravity SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE Incompressible flow; Surface tension; Low gravity; Liquid jets AB An axisymmetric phase field model is developed and used to model surface tension forces on liquid jets in microgravity. The previous work in this area is reviewed and a baseline drop tower experiment selected for model comparison. The model is solved numerically with a compact fourth order stencil on an equally spaced axisymmetric grid. After grid convergence studies, a grid is selected and all drop tower tests modeled. Agreement was assessed by comparing predicted and measured free surface rise. Trend wise agreement is good but agreement in magnitude is only fair. Suspected sources of disagreement are the simple turbulence model and the existence of slosh baffles in the experiment that were not included in the model. Parametric investigation was conducted to study the influence of key parameters on the geysers formed by jets in microgravity. Investigation of the contact angle showed the expected trend of increasing contact angle increasing geyser height. Investigation of the tank radius showed some interesting effects and demonstrated the zone of free surface deformation is quite large. Variation of the surface tension with a laminar jet showed clearly the evolution of free surface shape with Weber number. A breakthrough Weber number of 1 was predicted by the variation of the surface tension model which is close to the experimentally measured Weber number of 1.5 found in prior experimental work. Published by Elsevier Inc. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Chato, DJ (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,Mail Stop 301-3, Cleveland, OH 44135 USA. EM David.J.Chato@nasa.gov RI Chato, David/B-2698-2013 OI Chato, David/0000-0003-2990-0646 NR 40 TC 0 Z9 0 U1 0 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0021-9991 J9 J COMPUT PHYS JI J. Comput. Phys. PD MAR 20 PY 2009 VL 228 IS 5 BP 1521 EP 1540 DI 10.1016/j.jcp.2008.10.031 PG 20 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA 407NC UT WOS:000263370600013 ER PT J AU Abbott, BP Abbott, R Adhikari, R Ajith, P Allen, B Allen, G Amin, RS Anderson, SB Anderson, WG Arain, MA Araya, M Armandula, H Armor, P Aso, Y Aston, S Aufmuth, P Aulbert, C Babak, S Baker, P Ballmer, S Bantilan, H Barish, BC Barker, C Barker, D Barr, B Barriga, P Barsotti, L Barton, MA Bartos, I Bassiri, R Bastarrika, M Behnke, B Benacquista, M Betzwieser, J Beyersdorf, PT Bilenko, IA Billingsley, G Biswas, R Black, E Blackburn, JK Blackburn, L Blair, D Bland, B Bodiya, TP Bogue, L Bork, R Boschi, V Bose, S Brady, PR Braginsky, VB Brau, JE Brinkmann, M Brooks, AF Brown, DA Brunet, G Bullington, A Buonanno, A Burmeister, O Byer, RL Cadonati, L Cagnoli, G Camp, JB Cannizzo, J Cannon, KC Cao, J Cardenas, L Cardoso, V Caride, S Casebolt, T Castaldi, G Caudill, S Cavaglia, M Cepeda, C Chalkley, E Charlton, P Chatterji, S Chelkowski, S Chen, Y Christensen, N Clark, D Clark, J Clayton, JH Cokelaer, T Conte, R Cook, D Corbitt, TRC Cornish, N Coyne, DC Creighton, JDE Creighton, TD Cruise, AM Cumming, A Cunningham, L Cutler, RM Danzmann, K Daudert, B Davies, G DeBra, D Degallaix, J 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 Dwyer, J Echols, C Edgar, M Effler, A Ehrens, P Ely, G Espinoza, E Etzel, T Evans, M Evans, T Fairhurst, S Faltas, Y Fan, Y Fazi, D Fejer, MM Finn, LS Flasch, K Foley, S Forrest, C Fotopoulos, N Franzen, A Frei, Z Freise, A Frey, R Fricke, TT Fritschel, P Frolov, VV Fyffe, M Garofoli, JA Gholami, I Giaime, JA Giampanis, S Giardina, KD Goda, K Goetz, E Goggin, LM 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 Hanna, C Hanson, J Harms, J Harry, GM Harstad, ED Haughian, E Hayama, K Hayler, T Heefner, J Heng, IS Heptonstall, A Hewitson, M Hild, S Hirose, E Hoak, D Holt, K 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 Khalaidovski, A Khalili, FY Khan, R Khazanov, E King, P Kissel, JS Klimenko, S Kocsis, B Kokeyama, K Kondrashov, V Kopparapu, R Koranda, S Kozak, D Kozhevatov, I Krishnan, B Kwee, P Landry, M Lantz, B Lazzarini, A Lei, M Leonor, I Li, C Lin, H Lindquist, PE Littenberg, TB Lockerbie, NA Lodhia, D Lormand, M Lu, P Lubinski, M Lucianetti, A Luck, H Machenschalk, B MacInnis, M Mageswaran, M Mailand, K Mandel, I Mandic, V Marka, S Marka, Z Markosyan, A Markowitz, J Maros, E Martin, IW Martin, RM Marx, JN Mason, K Matichard, F Matone, L Matzner, R Mavalvala, N McCarthy, R McClelland, DE McGuire, SC McHugh, M McIntyre, G McKechan, D McKenzie, K Mehmet, M Melissinos, A Mendell, G Mercer, RA Meshkov, S Messenger, CJ Meyers, D Miller, A Miller, J Minelli, J Mitra, S Mitrofanov, VP Mitselmakher, G Mittleman, R Miyakawa, O Moe, B Mohanty, SD Moreno, G Mors, K Mossavi, K MowLowry, C Mueller, G Muhammad, D Mukherjee, S Mukhopadhyay, H Mullavey, A Muller-Ebhardt, H Munch, J Murray, PG Myers, E Myers, J Nash, T Nelson, J Newton, G Nishizawa, A Numata, K Ochsner, E 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 Perraca, A Petrie, T Pinto, IM Pitkin, M Pletsch, HJ Plissi, MV Postiglione, F Principe, M Prix, R Quetschke, V Raab, FJ Rabeling, DS Radkins, H Raffai, P Rainer, N Rakhmanov, M Ramsunder, M Reed, T Rehbein, H Reid, S Reitze, DH Riesen, R Riles, K Rivera, B Robertson, NA Robinson, C Robinson, EL Roddy, S Rogan, AM Rollins, J Romano, JD Romie, JH Rowan, S Rudiger, A Ruet, L Russell, P Ryan, K Sakata, S de la Jordana, LS Sandberg, V Sannibale, V Santamaria, L Saraf, S Sarin, P Sathyaprakash, BS Sato, S Saulson, PR Savage, R Savov, P Scanlan, M Schediwy, SW Schilling, R Schnabel, R Schofield, R Schutz, BF Schwinberg, P Scott, J Scott, SM Searle, AC Sears, B Seifert, F Sellers, D Sengupta, AS Sergeev, A Shapiro, B Shawhan, P Shoemaker, DH Sibley, A Siemens, X Sigg, D Sinha, S Sintes, AM Slagmolen, BJJ Slutsky, J Smith, JR Smith, MR Smith, ND Somiya, K Sorazu, B Stein, LC Strain, KA 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 Ugolini, D Urbanek, K Vahlbruch, H Van den Broeck, C van der Sluys, MV van Veggel, AA Vass, S Vaulin, R Vecchio, A Veitch, JD Veitch, P Villar, A Vorvick, C Vyachanin, SP Waldman, SJ Wallace, L Ward, H Ward, RL Weinert, M Weinstein, AJ Weiss, R Wen, L Wen, S Wette, K Whelan, JT Whitcomb, SE Whiting, BF Wilkinson, C Willems, PA Williams, HR Williams, L Willke, B Wilmut, I Winkler, W Wipf, CC Wiseman, AG Woan, G Wooley, R Worden, J Wu, W Yakushin, I Yamamoto, H Yan, Z Yoshida, S Zanolin, M Zhang, J Zhang, L Zhao, C Zotov, N Zucker, ME zur Muhlen, H Zweizig, J AF Abbott, B. P. Abbott, R. Adhikari, R. Ajith, P. Allen, B. Allen, G. Amin, R. S. Anderson, S. B. Anderson, W. G. Arain, M. A. Araya, M. Armandula, H. Armor, P. Aso, Y. Aston, S. Aufmuth, P. Aulbert, C. Babak, S. Baker, P. Ballmer, S. Bantilan, H. Barish, B. C. Barker, C. Barker, D. Barr, B. Barriga, P. Barsotti, L. Barton, M. A. Bartos, I. Bassiri, R. Bastarrika, M. Behnke, B. Benacquista, M. Betzwieser, J. Beyersdorf, P. T. Bilenko, I. A. Billingsley, G. Biswas, R. Black, E. Blackburn, J. K. Blackburn, L. Blair, D. Bland, B. Bodiya, T. P. Bogue, L. Bork, R. Boschi, V. Bose, S. Brady, P. R. Braginsky, V. B. Brau, J. E. Brinkmann, M. Brooks, A. F. Brown, D. A. Brunet, G. Bullington, A. Buonanno, A. Burmeister, O. Byer, R. L. Cadonati, L. Cagnoli, G. Camp, J. B. Cannizzo, J. Cannon, K. C. Cao, J. Cardenas, L. Cardoso, V. Caride, S. Casebolt, T. Castaldi, G. Caudill, S. Cavagli, M. Cepeda, C. Chalkley, E. Charlton, P. Chatterji, S. Chelkowski, S. Chen, Y. Christensen, N. Clark, D. Clark, J. Clayton, J. H. Cokelaer, T. Conte, R. Cook, D. Corbitt, T. R. C. Cornish, N. Coyne, D. C. Creighton, J. D. E. Creighton, T. D. Cruise, A. M. Cumming, A. Cunningham, L. Cutler, R. M. Danzmann, K. Daudert, B. Davies, G. DeBra, D. Degallaix, J. Dergachev, V. Desai, S. DeSalvo, R. Dhurandhar, S. Diaz, M. Dickson, J. Dietz, A. Donovan, F. Dooley, K. L. Doomes, E. E. Drever, R. W. P. Duke, I. Dumas, J. -C. Dwyer, J. Echols, C. Edgar, M. Effler, A. Ehrens, P. Ely, G. Espinoza, E. Etzel, T. Evans, M. Evans, T. Fairhurst, S. Faltas, Y. Fan, Y. Fazi, D. Fejer, M. M. Finn, L. S. Flasch, K. Foley, S. Forrest, C. Fotopoulos, N. Franzen, A. Frei, Z. Freise, A. Frey, R. Fricke, T. T. Fritschel, P. Frolov, V. V. Fyffe, M. Garofoli, J. A. Gholami, I. Giaime, J. A. Giampanis, S. Giardina, K. D. Goda, K. Goetz, E. Goggin, L. M. Gonzalez, G. Gossler, S. Gouaty, R. Grant, A. Gras, S. Gray, C. Gray, M. Greenhalgh, R. J. S. Gretarsson, A. M. Grimaldi, F. Grosso, R. Grote, H. Grunewald, S. Guenther, M. Gustafson, E. K. Gustafson, R. Hage, B. Hallam, J. M. Hanna, C. Hanson, J. Harms, J. Harry, G. M. Harstad, E. D. Haughian, E. Hayama, K. Hayler, T. Heefner, J. Heng, I. S. Heptonstall, A. Hewitson, M. Hild, S. Hirose, E. Hoak, D. Holt, K. Hosken, D. 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. Khalaidovski, A. Khalili, F. Ya. Khan, R. Khazanov, E. King, P. Kissel, J. S. Klimenko, S. Kocsis, B. Kokeyama, K. Kondrashov, V. Kopparapu, R. Koranda, S. Kozak, D. Kozhevatov, I. Krishnan, B. Kwee, P. Landry, M. Lantz, B. Lazzarini, A. Lei, M. Leonor, I. Li, C. Lin, H. Lindquist, P. E. Littenberg, T. B. Lockerbie, N. A. Lodhia, D. Lormand, M. Lu, P. Lubinski, M. Lucianetti, A. Lueck, H. Machenschalk, B. MacInnis, M. Mageswaran, M. Mailand, K. Mandel, I. Mandic, V. Marka, S. Marka, Z. Markosyan, A. Markowitz, J. Maros, E. Martin, I. W. Martin, R. M. Marx, J. N. Mason, K. Matichard, F. Matone, L. Matzner, R. Mavalvala, N. McCarthy, R. McClelland, D. E. McGuire, S. C. McHugh, M. McIntyre, G. McKechan, D. McKenzie, K. Mehmet, M. Melissinos, A. Mendell, G. Mercer, R. A. Meshkov, S. Messenger, C. J. Meyers, D. Miller, A. Miller, J. Minelli, J. Mitra, S. Mitrofanov, V. P. Mitselmakher, G. Mittleman, R. Miyakawa, O. Moe, B. Mohanty, S. D. Moreno, G. Mors, K. Mossavi, K. MowLowry, C. Mueller, G. Muhammad, D. Mukherjee, S. Mukhopadhyay, H. Mullavey, A. Mueller-Ebhardt, H. Munch, J. Murray, P. G. Myers, E. Myers, J. Nash, T. Nelson, J. Newton, G. Nishizawa, A. Numata, K. Ochsner, E. 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. Perraca, A. Petrie, T. Pinto, I. M. Pitkin, M. Pletsch, H. J. Plissi, M. V. Postiglione, F. Principe, M. Prix, R. Quetschke, V. Raab, F. J. Rabeling, D. S. Radkins, H. Raffai, P. Rainer, N. Rakhmanov, M. Ramsunder, M. Reed, T. Rehbein, H. Reid, S. Reitze, D. H. Riesen, R. Riles, K. Rivera, B. Robertson, N. A. Robinson, C. Robinson, E. L. Roddy, S. Rogan, A. M. Rollins, J. Romano, J. D. Romie, J. H. Rowan, S. Ruediger, A. Ruet, L. Russell, P. Ryan, K. Sakata, S. de la Jordana, L. Sancho Sandberg, V. Sannibale, V. Santamaria, L. Saraf, S. Sarin, P. Sathyaprakash, B. S. Sato, S. Saulson, P. R. Savage, R. Savov, P. Scanlan, M. Schediwy, S. W. Schilling, R. Schnabel, R. Schofield, R. Schutz, B. F. Schwinberg, P. Scott, J. Scott, S. M. Searle, A. C. Sears, B. Seifert, F. Sellers, D. Sengupta, A. S. Sergeev, A. Shapiro, B. Shawhan, P. Shoemaker, D. H. Sibley, A. Siemens, X. Sigg, D. Sinha, S. Sintes, A. M. Slagmolen, B. J. J. Slutsky, J. Smith, J. R. Smith, M. R. Smith, N. D. Somiya, K. Sorazu, B. Stein, L. C. Strain, K. A. 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. Ugolini, D. Urbanek, K. Vahlbruch, H. Van den Broeck, C. van der Sluys, M. V. van Veggel, A. A. Vass, S. Vaulin, R. Vecchio, A. Veitch, J. D. Veitch, P. Villar, A. Vorvick, C. Vyachanin, S. P. Waldman, S. J. Wallace, L. Ward, H. Ward, R. L. Weinert, M. Weinstein, A. J. Weiss, R. Wen, L. Wen, S. Wette, K. Whelan, J. T. Whitcomb, S. E. Whiting, B. F. Wilkinson, C. Willems, P. A. Williams, H. R. Williams, L. Willke, B. Wilmut, I. Winkler, W. Wipf, C. C. Wiseman, A. G. Woan, G. Wooley, R. Worden, J. Wu, W. Yakushin, I. Yamamoto, H. Yan, Z. Yoshida, S. Zanolin, M. Zhang, J. Zhang, L. Zhao, C. Zotov, N. Zucker, M. E. zur Muehlen, H. Zweizig, J. CA LIGO Sci Collaboration TI All-Sky LIGO Search for Periodic Gravitational Waves in the Early Fifth-Science-Run Data SO PHYSICAL REVIEW LETTERS LA English DT Article ID PULSARS AB We report on an all-sky search with the LIGO detectors for periodic gravitational waves in the frequency range 50-1100 Hz and with the frequency's time derivative in the range -5x10(-9)-0 Hz s(-1). Data from the first eight months of the fifth LIGO science run (S5) have been used in this search, which is based on a semicoherent method (PowerFlux) of summing strain power. Observing no evidence of periodic gravitational radiation, we report 95% confidence-level upper limits on radiation emitted by any unknown isolated rotating neutron stars within the search range. Strain limits below 10(-24) are obtained over a 200-Hz band, and the sensitivity improvement over previous searches increases the spatial volume sampled by an average factor of about 100 over the entire search band. 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[Buonanno, A.; Kanner, J.; Ochsner, E.; Pan, Y.; Shawhan, P.] Univ Maryland, College Pk, MD 20742 USA. [Cadonati, L.] Univ Massachusetts, Amherst, MA 01003 USA. [Dergachev, V.; Goetz, E.; Gustafson, R.; Riles, K.; Zhang, J.] Univ Michigan, Ann Arbor, MI 48109 USA. [Mandic, V.] Univ Minnesota, Minneapolis, MN 55455 USA. [Cardoso, V.; Cavagli, M.] Univ Mississippi, University, MS 38677 USA. [Brau, J. E.; Frey, R.; Harstad, E. D.; Ito, M.; Leonor, I.; Schofield, R.] Univ Oregon, Eugene, OR 97403 USA. [Forrest, C.; Fricke, T. T.; Giampanis, S.; Melissinos, A.] Univ Rochester, Rochester, NY 14627 USA. [Conte, R.; Postiglione, F.] Univ Salerno, I-84084 Salerno, Italy. [Castaldi, G.; Pinto, I. M.; Principe, M.] Univ Sannio Benevento, I-82100 Benevento, Italy. [Lockerbie, N. A.] Univ Strathclyde, Glasgow G1 1XQ, Lanark, Scotland. [Barriga, P.; Blair, D.; Dumas, J. -C.; Fan, Y.; Gras, S.; Ju, L.; Schediwy, S. W.; Yan, Z.; Zhao, C.] Univ Western Australia, Washington, DC 6009, Australia. [Allen, B.; Anderson, W. G.; Armor, P.; Biswas, R.; Brady, P. R.; Clayton, J. H.; Creighton, J. D. E.; Flasch, K.; Fotopoulos, N.; Koranda, S.; Miller, A.; Moe, B.; Papa, M. A.; Siemens, X.; Vaulin, R.; Wiseman, A. G.] Univ Wisconsin, Milwaukee, WI 53201 USA. [Bose, S.; Rogan, A. M.] Washington State Univ, Pullman, WA 99164 USA. [Dickson, J.; Gray, M.; McClelland, D. E.; McKenzie, K.; MowLowry, C.; Mullavey, A.; Rabeling, D. S.; Scott, S. M.; Slagmolen, B. J. J.; Wette, K.] Australian Natl Univ, Canberra, ACT 0200, Australia. [Greenhalgh, R. J. S.; Hayler, T.; O'Dell, J.; Wilmut, I.] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Doomes, E. E.; McGuire, S. C.] A&M Coll, Baton Rouge, LA 70813 USA. [Benacquista, M.; Creighton, T. D.; Diaz, M.; Grosso, R.; Hayama, K.; Mohanty, S. D.; Mukherjee, S.; Rakhmanov, M.; Romano, J. D.] Univ Texas Brownsville & Texas Southmost Coll, Brownsville, TX 78520 USA. [Aston, S.; Chelkowski, S.; Cruise, A. M.; Freise, A.; Hallam, J. M.; Hild, S.; Kasprzyk, D.; Lodhia, D.; Perraca, A.; Robinson, E. L.; Vecchio, A.; Veitch, J. D.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England. [Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England. RP Abbott, BP (reprint author), Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany. RI Cardoso, Vitor/K-1877-2015; Biswas, Rahul/H-7474-2016; Bartos, Imre/A-2592-2017; Frey, Raymond/E-2830-2016; Sergeev, Alexander/F-3027-2017; Ward, Robert/I-8032-2014; Khazanov, Efim/B-6643-2014; Lucianetti, Antonio/G-7383-2014; Khalili, Farit/D-8113-2012; Kocsis, Bence/C-3061-2013; Vecchio, Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Khan, Rubab/F-9455-2015; Ottaway, David/J-5908-2015; Postiglione, Fabio/O-4744-2015; Sigg, Daniel/I-4308-2015; Pinto, Innocenzo/L-3520-2016; Harms, Jan/J-4359-2012; Mitrofanov, Valery/D-8501-2012; Bilenko, Igor/D-5172-2012; Allen, Bruce/K-2327-2012; Chen, Yanbei/A-2604-2013; Barker, David/A-5671-2013; Zhao, Chunnong/C-2403-2013; Ju, Li/C-2623-2013; Pitkin, Matthew/I-3802-2013; Schutz, Bernard/B-1504-2010; Vyatchanin, Sergey/J-2238-2012; 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; Santamaria, Lucia/A-7269-2012; McClelland, David/E-6765-2010; Hild, Stefan/A-3864-2010; Rowan, Sheila/E-3032-2010; Strain, Kenneth/D-5236-2011; Raab, Frederick/E-2222-2011; Martin, Iain/A-2445-2010 OI Freise, Andreas/0000-0001-6586-9901; Mandel, Ilya/0000-0002-6134-8946; Whiting, Bernard F/0000-0002-8501-8669; Principe, Maria/0000-0002-6327-0628; Kanner, Jonah/0000-0001-8115-0577; Minelli, Jeff/0000-0002-5330-912X; Santamaria, Lucia/0000-0002-5986-0449; Hallam, Jonathan Mark/0000-0002-7087-0461; Cardoso, Vitor/0000-0003-0553-0433; Nishizawa, Atsushi/0000-0003-3562-0990; Biswas, Rahul/0000-0002-0774-8906; Sorazu, Borja/0000-0002-6178-3198; Zweizig, John/0000-0002-1521-3397; O'Shaughnessy, Richard/0000-0001-5832-8517; Frey, Raymond/0000-0003-0341-2636; Stein, Leo/0000-0001-7559-9597; Cokelaer, Thomas/0000-0001-6286-1138; Ward, Robert/0000-0001-5503-5241; Whelan, John/0000-0001-5710-6576; 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; Kocsis, Bence/0000-0002-4865-7517; Vecchio, Alberto/0000-0002-6254-1617; Khan, Rubab/0000-0001-5100-5168; Postiglione, Fabio/0000-0003-0628-3796; Sigg, Daniel/0000-0003-4606-6526; Allen, Bruce/0000-0003-4285-6256; Zhao, Chunnong/0000-0001-5825-2401; Pitkin, Matthew/0000-0003-4548-526X; Lueck, Harald/0000-0001-9350-4846; Finn, Lee Samuel/0000-0002-3937-0688; McClelland, David/0000-0001-6210-5842; Strain, Kenneth/0000-0002-2066-5355; FU U. S. National Science Foundation; Science and Technology Facilities Council of the U. K; Max Planck Society; State of Niedersachsen, Germany; Australian Research Council; Council of Scientific and Industrial Research of India; Istituto Nazionale di Fisica Nucleare of Italy; Spanish Ministerio de Educacion y Ciencia; Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears; Royal Society; Scottish Funding Council; Scottish Universities Physics Alliance; The National Aeronautics and Space Administration; Carnegie Trust; Leverhulme Trust; David and Lucile Packard Foundation; Research Corporation; Alfred P. Sloan Foundation FX We thank Deepto Chakrabarty and David Kaplan for useful discussions. The authors gratefully acknowledge the support of the U. S. National Science Foundation for the construction and operation of the LIGO Laboratory and the Science and Technology Facilities Council of the U. K., the Max Planck Society, and the State of Niedersachsen, Germany, for support of the construction and operation of the GEO600 detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Educacion y Ciencia, the Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, The National Aeronautics and Space Administration, the Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, and the Alfred P. Sloan Foundation. NR 19 TC 60 Z9 60 U1 2 U2 19 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD MAR 20 PY 2009 VL 102 IS 11 AR 111102 DI 10.1103/PhysRevLett.102.111102 PG 6 WC Physics, Multidisciplinary SC Physics GA 421TC UT WOS:000264380200013 PM 19392186 ER PT J AU Jess, DB Mathioudakis, M Erdelyi, R Crockett, PJ Keenan, FP Christian, DJ AF Jess, David B. Mathioudakis, Mihalis Erdelyi, Robert Crockett, Philip J. Keenan, Francis P. Christian, Damian J. TI Alfven Waves in the Lower Solar Atmosphere SO SCIENCE LA English DT Article ID CORONAL LOOPS; BRIGHT POINTS; H-ALPHA; CHROMOSPHERE; MODES; WIND; FLUX; KINK; SUN AB The flow of energy through the solar atmosphere and the heating of the Sun's outer regions are still not understood. Here, we report the detection of oscillatory phenomena associated with a large bright-point group that is 430,000 square kilometers in area and located near the solar disk center. Wavelet analysis reveals full-width half-maximum oscillations with periodicities ranging from 126 to 700 seconds originating above the bright point and significance levels exceeding 99%. These oscillations, 2.6 kilometers per second in amplitude, are coupled with chromospheric line-of-sight Doppler velocities with an average blue shift of 23 kilometers per second. A lack of cospatial intensity oscillations and transversal displacements rules out the presence of magneto-acoustic wave modes. The oscillations are a signature of Alfven waves produced by a torsional twist of +/- 22 degrees. A phase shift of 180 degrees across the diameter of the bright point suggests that these torsional Alfven oscillations are induced globally throughout the entire brightening. The energy flux associated with this wave mode is sufficient to heat the solar corona. C1 [Jess, David B.; Mathioudakis, Mihalis; Crockett, Philip J.; Keenan, Francis P.] Queens Univ Belfast, Astrophys Res Ctr, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland. [Jess, David B.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. [Erdelyi, Robert] Univ Sheffield, Solar Phys & Space Plasma Res Ctr, Sheffield S3 7RH, S Yorkshire, England. [Christian, Damian J.] Calif State Univ Northridge, Dept Phys & Astron, Northridge, CA 91330 USA. RP Jess, DB (reprint author), Queens Univ Belfast, Astrophys Res Ctr, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland. EM d.jess@qub.ac.uk OI Jess, David/0000-0002-9155-8039; Christian, Damian/0000-0003-1746-3020 FU Northern Ireland Department for Employment and Learning [Studentship]; NSF, Hungary [K67746]; Atomic Weapons Establishment Aldermaston [William Penney Fellowship]; Science and Technology Facilities Council FX D.B.J. is supported by a Northern Ireland Department for Employment and Learning studentship and thanks NASA Goddard Space Flight Center for a Co-operative Award in Science and Technology studentship. R.E. thanks M. Keray for encouragement and is grateful to NSF, Hungary (Orszagos Tudomanyos Kutatasi Alapprogram, ref. no. K67746), for financial support. F.P.K. is grateful to the Atomic Weapons Establishment Aldermaston for the award of a William Penney Fellowship. The SST is operated on the island of La Palma by the Institute for Solar Physics of the Royal Swedish Academy of Sciences in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. These observations have been funded by the Optical Infrared Coordination network, an international collaboration supported by the Research Infrastructures Programme of the European Commission's Sixth Framework Programme. This work is supported by the Science and Technology Facilities Council, and we thank L. H. M. Rouppe van der Voort for help with MOMFBD image processing. NR 27 TC 201 Z9 203 U1 2 U2 18 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 MAR 20 PY 2009 VL 323 IS 5921 BP 1582 EP 1585 DI 10.1126/science.1168680 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 421EN UT WOS:000264342300032 PM 19299614 ER PT J AU Lee, C Lawson, WG Richardson, MI Heavens, NG Kleinbohl, A Banfield, D McCleese, DJ Zurek, R Kass, D Schofield, JT Leovy, CB Taylor, FW Toigo, AD AF Lee, C. Lawson, W. G. Richardson, M. I. Heavens, N. G. Kleinboehl, A. Banfield, D. McCleese, D. J. Zurek, R. Kass, D. Schofield, J. T. Leovy, C. B. Taylor, F. W. Toigo, A. D. TI Thermal tides in the Martian middle atmosphere as seen by the Mars Climate Sounder SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID ASYNOPTIC SATELLITE-OBSERVATIONS; GENERAL-CIRCULATION MODEL; TES NADIR DATA; EMISSION SPECTROMETER; SAMPLING THEORY; OPTICAL DEPTH; DUST STORMS; WAVES; OSCILLATIONS; SIMULATION AB The first systematic observations of the middle atmosphere of Mars (35-80km) with the Mars Climate Sounder (MCS) show dramatic patterns of diurnal thermal variation, evident in retrievals of temperature and water ice opacity. At the time of writing, the data set of MCS limb retrievals is sufficient for spectral analysis within a limited range of latitudes and seasons. This analysis shows that these thermal variations are almost exclusively associated with a diurnal thermal tide. Using a Martian general circulation model to extend our analysis, we show that the diurnal thermal tide dominates these patterns for all latitudes and all seasons. C1 [Lee, C.; Lawson, W. G.; Richardson, M. I.; Heavens, N. G.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Kleinboehl, A.; McCleese, D. J.; Zurek, R.; Kass, D.; Schofield, J. T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Banfield, D.; Toigo, A. D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Leovy, C. B.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. [Taylor, F. W.] Univ Oxford, Dept Phys, Oxford OX1 3PU, England. RP Lee, C (reprint author), CALTECH, Div Geol & Planetary Sci, Mail Stop 150-21, Pasadena, CA 91125 USA. EM lee@gps.caltech.edu OI Banfield, Don/0000-0003-2664-0164; Heavens, Nicholas/0000-0001-7654-503X FU National Aeronautics; Space Administration through the Mars Reconnaissance Orbiter project FX The authors acknowledge J. Shirley, C. Backus, T. Pavlicek, and E. Sayfi for their contribution to the acquisition and analysis of MCS data and thank the anonymous reviewers for their useful comments and work in improving this manuscript. This work was funded by the National Aeronautics and Space Administration through the Mars Reconnaissance Orbiter project. NR 49 TC 39 Z9 39 U1 1 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAR 19 PY 2009 VL 114 AR E03005 DI 10.1029/2008JE003285 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 422PP UT WOS:000264440500001 ER PT J AU Taktakishvili, A Kuznetsova, M MacNeice, P Hesse, M Rastatter, L Pulkkinen, A Chulaki, A Odstrcil, D AF Taktakishvili, A. Kuznetsova, M. MacNeice, P. Hesse, M. Rastaetter, L. Pulkkinen, A. Chulaki, A. Odstrcil, D. TI Validation of the coronal mass ejection predictions at the Earth orbit estimated by ENLIL heliosphere cone model SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID SOLAR-WIND; MAGNETIC-FIELD; ARRIVAL TIMES; 1-AU ARRIVAL; SHOCKS AB Modeling is an important tool in understanding physical processes in the space weather. Model performance studies evaluate the quality of model operation by comparing its output to a measurable parameter of interest. In this paper we studied the performance of the combination of the halo coronal mass ejection (CME) analytical cone model and ENLIL three-dimensional MHD heliosphere model. We examined the CME arrival time and magnitude of impact at 1 AU for different geoeffective events, including the October 2003 Halloween Storm and the 14 December 2006 storm CMEs. The results of the simulation are compared with the ACE satellite observations. The comparison of the simulation results with the observations demonstrates that ENLIL cone model performs better compared to reference mean velocity and empirical models. C1 [Taktakishvili, A.; Kuznetsova, M.; MacNeice, P.; Hesse, M.; Rastaetter, L.; Pulkkinen, A.; Chulaki, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Odstrcil, D.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Taktakishvili, A.; Pulkkinen, A.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. RP Taktakishvili, A (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 130, Greenbelt, MD 20771 USA. EM aleksandre.taktakishvili-1@nasa.gov RI Hesse, Michael/D-2031-2012; Rastaetter, Lutz/D-4715-2012; MacNeice, Peter/F-5587-2012; Kuznetsova, Maria/F-6840-2012 OI Rastaetter, Lutz/0000-0002-7343-4147; FU NSF/CISM; NASA/LWS FX We wish to thank George Siscoe for most valuable comments and help. We wish also to thank Mei-Ching Fok for helping and important remarks. This work was partially performed while A. T. held ORAU Research Associateship and Award at Goddard Space Flight Center, and D. O. was partially supported by NSF/CISM and NASA/LWS grants. All simulations carried out for this work were done at the Community Coordinated Modeling Center at the NASA Goddard Flight Center. NR 20 TC 43 Z9 47 U1 0 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 MAR 19 PY 2009 VL 7 AR S03004 DI 10.1029/2008SW000448 PG 7 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 422QD UT WOS:000264441900001 ER PT J AU Tsurutani, BT Verkhoglyadova, OP Lakhina, GS Yagitani, S AF Tsurutani, Bruce T. Verkhoglyadova, Olga P. Lakhina, Gurbax S. Yagitani, Satoshi TI Properties of dayside outer zone chorus during HILDCAA events: Loss of energetic electrons SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Review ID RADIATION BELT ELECTRONS; SOLAR-WIND STREAMS; WHISTLER-MODE CHORUS; DAWN-DUSK ASYMMETRY; STORM-TIME CHORUS; MAGNETIC STORMS; AURORAL-ZONE; RELATIVISTIC ELECTRONS; LION ROARS; ALFVEN WAVES AB The dayside outer zone (DOZ) portion of the magnetosphere is a region where chorus intensities are statistically found to be the most intense. In this study, DOZ chorus have been examined using OGO-5 plasma wave and GEOTAIL plasma wave, magnetic field and energetic particle data. Dayside chorus is noted to be composed of similar to 0.1 to 0.5 s rising-tone emissions called "elements.'' The duration of the elements and their frequency-time characteristics are repeatable throughout the chorus event (lasting from tens of minutes to hours), but may differ from event to event. Chorus is a right-hand, circularly polarized electromagnetic plane wave. Waves are detected propagating from along the ambient magnetic field, B-o, to oblique angles near the Gendrin angle, theta(Gendrin). All waves, independent of wave direction of propagation relative to Bo, are found to be circularly polarized, to first order. Chorus rising-tone elements are composed of coherent "subelements'' or "packets'' with durations of similar to 5 to 10 ms. Consecutive subelements/packets step in frequency with time to form the elements. The peak amplitudes within a packet can be similar to 0.2 nT or greater. The subelement or packet amplitudes are at least an order of magnitude larger than previously estimated chorus amplitudes obtained by power spectral measurements. This discrepancy is due to the presence of interspacings between chorus elements, the interspacings between subelements/packets within an element, and the different frequencies of subelements/packets within a rising-tone. DOZ chorus studied here were found to be consistent with generation via the loss cone instability of substorm-injected temperature-anisotropic (T-perpendicular to/T parallel to > 1) E = 5 to 40 keV electrons drifting from the midnight sector to the DOZ region. Using a large amplitude subelement/packet wave magnetic field amplitude of similar to 0.2 nT, it is shown that the instantaneous Kennel-Petschek pitch angle diffusion rate D-alpha alpha is similar to 5 x 10 similar to 2 s(-1). This latter quantity is based on incoherent waves. If energetic electrons stay in cyclotron resonance throughout their interaction with a coherent subelement of duration 10 ms, they may be "pitch angle transported'' by similar to 5 degrees. Therefore electrons within 5 degrees of the loss cone can be lost in a single wave-particle interaction. Several such interactions as the electrons traverse the wave region can lead to much larger pitch angle transport angles. The similar time-scales of chorus elements and bremsstrahlung X-ray microbursts (similar to 0.5 s) can be explained by the "pitch angle transport'' mechanism described above. Increasing and decreasing pitch angle transport via this mechanism will lead to much higher pitch angle diffusion or "super diffusion'' rates. Isotropic unpolarized noise of similar to 20 pT peak amplitude has also been detected. The noise is well above instrument noise levels and is speculated to be remnants of chorus or hiss. C1 [Tsurutani, Bruce T.; Verkhoglyadova, Olga P.] CALTECH, Jet Prop Lab, Pasadena, CA 91190 USA. [Verkhoglyadova, Olga P.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Lakhina, Gurbax S.] India Inst Geomagnetism, Bombay, Maharashtra, India. [Yagitani, Satoshi] Kanazawa Univ, Grad Sch Nat Sci & Technol, Kanazawa, Ishikawa 9201192, Japan. RP Tsurutani, BT (reprint author), CALTECH, Jet Prop Lab, M-S 138-308,4800 Oak Grove Dr, Pasadena, CA 91190 USA. EM olga.verkhoglyadova@jpl.nasa.gov RI Lakhina, Gurbax /C-9295-2012; YAGITANI, Satoshi/E-7072-2015; OI Lakhina, Gurbax /0000-0002-8956-486X; Verkhoglyadova, Olga/0000-0002-9295-9539 FU Indian National Science Academy, New Delhi FX Portions of this research were done at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. BTT and OPV would like to acknowledge RISH, Kyoto University, for their hospitality while the chorus data was gathered and the effort was initiated. OPV thanks Y. Omura and a JSPS fellowship for financial support during her stay. BTT thanks M. Schulz for useful scientific discussions concerning minimum B pockets. GSL thanks the Indian National Science Academy, New Delhi, for support under the Senior Scientist Scheme. NR 108 TC 66 Z9 66 U1 0 U2 7 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 MAR 17 PY 2009 VL 114 AR A03207 DI 10.1029/2008JA013353 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 422PV UT WOS:000264441100002 ER PT J AU Foschini, L Maraschi, L Tavecchio, F Ghisellini, G Gliozzi, M Sambruna, RM AF Foschini, L. Maraschi, L. Tavecchio, F. Ghisellini, G. Gliozzi, M. Sambruna, R. M. TI Blazar nuclei in radio-loud narrow-line Seyfert 1? SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Radio-loud narrow-line Seyfert 1; Blazars; Relativistic jets ID X-RAY-EMISSION; ACTIVE GALACTIC NUCLEI; SKY SURVEY; GALAXIES; VARIABILITY; PKS-0558-504; SEQUENCE; QUASARS; SAMPLE; AGNS AB It has been suggested that some radio-loud narrow-line Seyfert 1 contain relativistic jets, on the basis of their flat-spectrum radio nuclei and studies on variability. We present preliminary results of ail ongoing investigation of the X-ray and multiwavelength properties of 5 radio-loud NLS1 based oil archival data front Swift and XMM-Newton. Some sources present interesting characteristics, very uncharacteristic For a radio-quiet narrow-line Seyfert 1, such as very hard X-ray spectra, and correlated optical and ultraviolet variability, However, none of the studied sources show conclusive evidence for relativistic jets. gamma-Ray observations with Fermi are strongly recommended to definitely decide oil the presence or not of relativistic jets. (C) 2009 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Foschini, L.] INAF IASF Bologna, I-40129 Bologna, Italy. [Maraschi, L.; Tavecchio, F.; Ghisellini, G.] INAF Osservatorio Astron Brera, I-20121 Milan, Italy. [Gliozzi, M.] George Mason Univ, Fairfax, VA 22030 USA. [Sambruna, R. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Foschini, L (reprint author), INAF IASF Bologna, Via Gobetti 101, I-40129 Bologna, Italy. EM foschini@isafbo.inaf.it RI Foschini, Luigi/H-3833-2012; OI Foschini, Luigi/0000-0001-8678-0324; Ghisellini, Gabriele/0000-0002-0037-1974 NR 32 TC 20 Z9 20 U1 0 U2 0 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 MAR 16 PY 2009 VL 43 IS 6 BP 889 EP 894 DI 10.1016/j.asr.2008.12.021 PG 6 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 425FH UT WOS:000264621900001 ER PT J AU Katsuda, S Tsunemi, H Mori, K AF Katsuda, Satoru Tsunemi, Hiroshi Mori, Koji TI Is Vela Jr. a young supernova remnant? SO ADVANCES IN SPACE RESEARCH LA English DT Article DE ISM: individual (RX J0852.0-4622: Vela Jr.); Shock waves; Supernova remnants; X-rays ISM ID GALACTIC SUPERNOVA; X-RAYS; EXPANSION; CHANDRA; G266.2-1.2; CASSIOPEIA; EMISSION; TI-44 AB The supernova remnant RX J0952.0-4622 (or Vela Jr.) has been considered to be very young (similar to 680 yr) based mainly oil the possible detection of a radioactive decay line of (44)Ti whose lifetime is only similar to 90 yr. Here, we report oil expansion measurements of the northwestern rim of this remnant, based on XMM-Newton observations separated by 6.5 yr. The expansion rate is derived to be 0.026 +/- 0.05 +/- 0.09% yr(-1) (the first and second-term errors are responsible for statistical and systematic uncertainties, respectively). We estimate the age of this remnant to be similar to 1000-3000 yr. Therefore, Vela Jr. turns out to be not so young as it was considered previously. The distance to this remnant is also derived to be at least similar to 740 pc, assuming a high shock speed of 3000 km s (1). (C) 2009 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Katsuda, Satoru; Tsunemi, Hiroshi] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Osaka 5600043, Japan. [Katsuda, Satoru] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mori, Koji] Miyazaki Univ, Fac Engn, Dept Appl Phys, Nishi Ku, Miyazaki 8892192, Japan. RP Katsuda, S (reprint author), Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, 1-1 Machikaneyama, Osaka 5600043, Japan. EM Satoru.Katsuda@nasa.gov; tsune-mi@ess.sci.osaka-u.ac.jp; mori@astro.miyazaki-u.ac.jp FU Ministry of Education, Culture, Sports, Science and Technology [16002004]; 21st Century COE Program; JSPS Research Fellowship; NASA [NNG06EO90A] FX This work is partly supported by a Grant-in-Aid for Scientific Research by the Ministry of Education, Culture, Sports, Science and Technology (16002004). This study is also carried out as part of the 21st Century COE Program, 'Towards a new basic science: depth and synthesis'. S.K. is supported by a JSPS Research Fellowship for Young Scientists. S.K. is also supported in part by the NASA grant under the Contract NNG06EO90A. NR 24 TC 4 Z9 4 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 MAR 16 PY 2009 VL 43 IS 6 BP 895 EP 899 DI 10.1016/j.asr.2009.01.004 PG 5 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 425FH UT WOS:000264621900002 ER PT J AU Ting, DZY Bandara, SV Gunapala, SD Mumolo, JM Keo, SA Hill, CJ Liu, JK Blazejewski, ER Rafol, SB Chang, YC AF Ting, David Z. -Y. Bandara, Sumith V. Gunapala, Sarath D. Mumolo, Jason M. Keo, Sam A. Hill, Cory J. Liu, John K. Blazejewski, Edward R. Rafol, Sir B. Chang, Yia-Chung TI Submonolayer quantum dot infrared photodetector SO APPLIED PHYSICS LETTERS LA English DT Article DE infrared detectors; monolayers; photodetectors; quantum dots ID FOCAL-PLANE ARRAY; DETECTIVITY; ISLANDS; WELL AB We describe the concept of the submonolayer quantum dot infrared photodetector (SML QDIP) and report experimental device results on long-wavelength infrared detection. An SML QDIP structure was fabricated into megapixel focal plane arrays, which produced clear infrared images up to 80 K. Detectors in the focal plane showed a responsivity peak at 7.8 mu m and noise equivalent temperature difference of 33 mK at 70 K. C1 [Ting, David Z. -Y.; Bandara, Sumith V.; Gunapala, Sarath D.; Mumolo, Jason M.; Keo, Sam A.; Hill, Cory J.; Liu, John K.; Blazejewski, Edward R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rafol, Sir B.] Infravis Syst, Altadena, CA 91001 USA. [Chang, Yia-Chung] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. RP Ting, DZY (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM david.z.ting@jpl.nasa.gov RI Chang, Yia-Chung/F-4239-2011 NR 24 TC 41 Z9 41 U1 0 U2 7 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 EI 1077-3118 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD MAR 16 PY 2009 VL 94 IS 11 AR 111107 DI 10.1063/1.3095812 PG 3 WC Physics, Applied SC Physics GA 421TD UT WOS:000264380300007 ER PT J AU Connor, LN Laxon, SW Ridout, AL Krabill, WB McAdoo, DC AF Connor, Laurence N. Laxon, Seymour W. Ridout, Andrew L. Krabill, William B. McAdoo, David C. TI Comparison of Envisat radar and airborne laser altimeter measurements over Arctic sea ice SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Satellite altimetry; Radar altimeter; Laser altimetry; Sea ice thickness; Snow depth ID PROCESSING SCHEME; THICKNESS; MOTION; OCEAN; COVER; SHEET; MAPS AB Sea ice thickness is a crucial, but very undersampled cryospheric parameter of fundamental importance for climate modeling. Advances in satellite altimetry have enabled the measurement of sea ice freeboard using satellite microwave altimeters. Unfortunately, validation of these new techniques has suffered from a lack of ground truth measurements. Therefore, an airborne campaign was carried out in March 2006 using laser altimetry and photo imagery to validate sea ice elevation measurements derived from the Envisat/RA-2 microwave altimeter. We present a comparative analysis of Envisat/RA-2 sea ice elevation processing with collocated airborne measurements collected north of the Canadian Archipelago. Consistent overall relationships between block-averaged airborne laser and Envisat elevations are found, over both leads and floes, along the full 1300 km aircraft track. The fine resolution of the airborne laser altimeter data is exploited to evaluate elevation variability within the RA-2 ground footprint. Our analysis shows good agreement between RA-2 derived sea ice elevations and those measured by airborne laser altimetry, particularly over refrozen leads where the overall mean difference is about I cm. Notwithstanding this small 1 cm mean difference. we identify a larger elevation uncertainty (of order 10 cm) associated with the uncertain location of dominant radar targets within the particular RA-2 footprint. Sources of measurement uncertainty or ambiguity are identified, and include snow accumulation, tracking noise, and the limited coverage of airborne measurements. Published by Elsevier Inc. C1 [Connor, Laurence N.; McAdoo, David C.] NOAA, Lab Satellite Altimetry, SSMC1, E RA31, Silver Spring, MD 20910 USA. [Laxon, Seymour W.; Ridout, Andrew L.] UCL, Ctr Polar Observ & Modelling, London WC1E 6BT, England. [Krabill, William B.] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Wallops Isl, VA 23337 USA. RP Connor, LN (reprint author), NOAA, Lab Satellite Altimetry, SSMC1, E RA31, 1335 East West Highway, Silver Spring, MD 20910 USA. EM Laurence.Connor@noaa.gov RI Laxon, Seymour/C-1644-2008; McAdoo, Dave/F-5612-2010; Connor, Laurence/E-7930-2011 OI McAdoo, Dave/0000-0002-7533-5564; Connor, Laurence/0000-0002-5276-6257 FU NASA P-3 Aircrew; NOAA; NASA FX The authors wish to thank the NASA P-3 Aircrew for their support during the AAA 2006 Campaign and Serdar Manizade and Chreston Martin for their expertise and assistance with the ATM data processing. The March 27, 2006 AAA flight was supported by NOAA and NASA. The views, opinions, and findings contained in this report are those of the authors and should not be construed as an official National Oceanic and Atmospheric Administration or US Government position, policy, or decision. NR 26 TC 42 Z9 44 U1 1 U2 23 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 MAR 16 PY 2009 VL 113 IS 3 BP 563 EP 570 DI 10.1016/j.rse.2008.10.015 PG 8 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 406PV UT WOS:000263308300009 ER PT J AU Kuchinke, CP Gordon, HR Franz, BA AF Kuchinke, Christopher P. Gordon, Howard R. Franz, Bryan A. TI Spectral optimization for constituent retrieval in Case 2 waters I: Implementation and performance SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Remote Sensing; Ocean color; Case 2 waters; Atmospheric correction; Aerosol absorption; Chlorophyll a; Colored Dissolved Material; Backscattering; Bio-optical coefficients ID OCEAN-COLOR IMAGERY; BOUND-CONSTRAINED OPTIMIZATION; ATMOSPHERIC CORRECTION; AEROSOL ABSORPTION; LEAVING RADIANCE; CHESAPEAKE BAY; ALGORITHM; SYSTEM; MODEL; VALIDATION AB We describe in detail the implementation of the spectral optimization algorithm (SCA) for Case 2 waters for processing of ocean color data. This algorithm uses aerosol models and a bio-optical reflectance model to provide the top-of atmosphere (TOA) reflectance. The parameters of both models are then determined by fitting the modeled TOA reflectance to that observed from space, using non-linear optimization. The algorithm will be incorporated into the SeaDAS software package as an optional processing switch of the Multi-Sensor Level-1 to Level-2 code. To provide potential users with an understanding of the accuracy and limitations of the algorithm, we generated a synthetic data set and tested the performance of the SCA with both correct and incorrect bio-optical model parameters. Application of the SOA to actual SeaWiFS data in the Lower Chesapeake Bay (for which surface measurements were available) showed that 20% errors in the bio-optical model parameters still enabled retrieval of chlorophyll a and the total absorption coefficient dissolved plus particulate detrital material at 443 nm with an error of less than 30% and 20%, respectively. In a companion paper we present a validation study of the application of the algorithm in the Chesapeake Bay. (c) 2008 Elsevier Inc. All rights reserved. C1 [Kuchinke, Christopher P.; Gordon, Howard R.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA. [Franz, Bryan A.] NASA, Goddard Space Flight Ctr, SAIC, Ocean Biol Proc Grp, Greenbelt, MD 20771 USA. RP Gordon, HR (reprint author), Univ Miami, Dept Phys, POB 248046, Coral Gables, FL 33124 USA. EM gordon@physics.miami.edu RI Franz, Bryan/D-6284-2012 OI Franz, Bryan/0000-0003-0293-2082 NR 31 TC 27 Z9 28 U1 0 U2 7 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD MAR 16 PY 2009 VL 113 IS 3 BP 571 EP 587 DI 10.1016/j.rse.2008.11.001 PG 17 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 406PV UT WOS:000263308300010 ER PT J AU Coops, NC Ferster, CJ Waring, RH Nightingale, J AF Coops, Nicholas C. Ferster, Colin J. Waring, Richard H. Nightingale, Joanne TI Comparison of three models for predicting gross primary production across and within forested ecoregions in the contiguous United States SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Gross primary production; Modeling; MODIS; SPOT; 3PG ID TERRESTRIAL PRIMARY PRODUCTION; NET PRIMARY PRODUCTION; CARBON MASS FLUXES; C-FIX MODEL; WATER-VAPOR; FRACTION; DIOXIDE; BOREAL; OREGON; DRIVEN AB Gross primary production (GPP), the photosynthetic uptake of carbon, is an important variable in the global carbon cycle. Although continuous measurements of GPP are being collected from a network of micro-meteorological towers, each site represents a small area with records available for only a limited period. As a result, GPP is commonly modeled over forested landscapes as a function of climatic and soil variables, often supplemented with satellite-derived estimates of the vegetation's light-absorbing properties. Since the late 1990s, a number of models have been developed to provide seasonal and annual estimates of GPP across much of the Earth. Each model, however, contains different underlying assumptions and requires different amounts of data. As a result, predictions vary, sometimes significantly. In this paper we compare modeled estimates of GPP for forested areas across the U.S.A. derived from: NASA's MODIS Product (MOD17): the C-Fix model using SPOT-VGT satellite-derived vegetation data; and the Physiological Principles Predicting Growth from Satellites (3-PGS) model, a process-based model that requires information on both climate and soil properties. The models predicted average ecoregion values of forest GPP between 9.8 and 14.1 MgC ha(-1) y(-1) across the United States. 3-PGS predicted the lowest values while the C-Fix model, which included a CO(2) fertilization factor, produced the highest estimates. In the western part of the country, estimates of GPP within a given ecoregion varied by as much as 50%, whereas in the northeast, where topography and climate are less extreme, variation in GPP was less than 10%. Within ecoregions, 3PGS predicted the most variation, reflecting its sensitivity to variation in soil properties. We conclude that where model predictions disagree, an opportunity is presented to evaluate underlying assumptions through sensitivity analyses, additional data collection and where more detailed study is warranted. (c) 2008 Elsevier Inc. All rights reserved. C1 [Coops, Nicholas C.; Ferster, Colin J.] Univ British Columbia, Dept Forest Resource Management, Vancouver, BC V6T 1Z4, Canada. [Waring, Richard H.] Oregon State Univ, Coll Forestry, Corvallis, OR 97331 USA. [Nightingale, Joanne] NASA, Goddard Space Flight Ctr, Terrestrial Informat Syst Branch, Greenbelt, MD 20771 USA. RP Coops, NC (reprint author), Univ British Columbia, Dept Forest Resource Management, 2424 Main Mall, Vancouver, BC V6T 1Z4, Canada. EM nicholas.coops@ubc.ca RI Coops, Nicholas/J-1543-2012 OI Coops, Nicholas/0000-0002-0151-9037 FU National Aeronautics and Space Administration [NNG04GK26G] FX This study was supported by the National Aeronautics and Space Administration (NASA Grant NNG04GK26G) as part of the Biodiversity and Ecological Forecasting program, and the University of British Columbia (UBC). Meteorological data were provided by the NTSG group at the University of Montana. We are particularly grateful to Maosheng Zhao for providing interpolation code to allow us to utilize these clatasets. In addition we thank the scientists in GMAO, especially Mahendra K. Karki, for providing consistent GECIS4 GMAO data. NR 35 TC 21 Z9 25 U1 2 U2 16 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 MAR 16 PY 2009 VL 113 IS 3 BP 680 EP 690 DI 10.1016/j.rse.2008.11.013 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 406PV UT WOS:000263308300019 ER PT J AU Nelson, R Ranson, KJ Sun, G Kimes, DS Kharuk, V Montesano, P AF Nelson, R. Ranson, K. J. Sun, G. Kimes, D. S. Kharuk, V. Montesano, P. TI Estimating Siberian timber volume using MODIS and ICESat/GLAS SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Boreal forest; GLAS; LiDAR; MODIS; Multispectral; Siberia; Timber volume ID FOREST STAND CHARACTERISTICS; AIRBORNE SCANNING LASER; LAND-COVER; ABOVEGROUND BIOMASS; VERTICAL STRUCTURE; BOREAL FOREST; LIDAR; RADAR; BACKSCATTER; INVENTORY AB Geosciences Laser Altimeter System (GLAS) space LiDAR data are used to attribute a MODerate resolution Imaging Spectrometer (MODIS) 500 m land cover classification of a 10 degrees latitude by 12 degrees longitude study area in south-central Siberia. Timber volume estimates are generated for 16 forest classes, i.e., four forest cover types x four canopy density classes, across this 811,414 km(2) area and compared with a ground-based regional volume estimate. Two regional GLAS/MODIS timber volume products, one considering only those pulses falling on slopes <= 10 degrees and one utilizing all GLAS pulses regardless of slope, are generated. Using a two-phase (GLAS-ground plot) sampling design, GLAS/MODIS volumes average 163.4 +/- 11.8 m(3)/ha across all 16 forest classes based on GLAS pulses on slopes <= 10 degrees and 171.9 +/- 12.4 m(3)/ha considering GLAS shots on all slopes. The increase in regional GLAS volume per-hectare estimates as a function of increasing slope most likely illustrate the effects of vertical waveform expansion due to the convolution of topography with the forest canopy response. A comparable, independent, ground-based estimate is 146 m(3)/ha [Shepashenko, D., Shvidenko, A., and Nilsson, S. (1998). Phytomass (live biomass) and carbon of Siberian forests. Biomass and Bioenergy, 14, 21-31], a difference of 11.9% and 17.7% for GLAS shots on slopes <= 10 degrees and all GLAS shots regardless of slope, respectively. A ground-based estimate of total volume for the entire study area, 7.46 x 109 m(3). is derived using Shepashenko et al.'s per-hectare volume estimate in conjunction with forest area derived from a 1990 forest map [Grasia, M.G. (ed.). (1990). Forest Map of USSR. Soyuzgiproleskhoz, Moscow, RU. Scale: 1:2,500,000]. The comparable GLAS/MODIS estimate is 7.38 x 10(9) m(3), a difference of less than 1.1 %. Results indicate that GLAS data can be used to attribute digital land cover maps to estimate forest resources over subcontinental areas encompassing hundreds of thousands of square kilometers. Published by Elsevier Inc. C1 [Nelson, R.; Ranson, K. J.; Kimes, D. S.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. [Sun, G.] Univ Maryland, Dept Geog, College Pk, MD 20742 USA. [Kharuk, V.] Sukachev Forest Inst, Academgorodok, Russia. [Montesano, P.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. RP Nelson, R (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Code 614-4, Greenbelt, MD 20771 USA. EM ross.f.nelson@nasa.gov RI Ranson, Kenneth/G-2446-2012; Nelson, Ross/H-8266-2014 OI Ranson, Kenneth/0000-0003-3806-7270; NR 53 TC 98 Z9 103 U1 4 U2 29 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 MAR 16 PY 2009 VL 113 IS 3 BP 691 EP 701 DI 10.1016/j.rse.2008.11.010 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 406PV UT WOS:000263308300020 ER PT J AU Lee, JH Feng, XH Posmentier, ES Faiia, AM Taylor, S AF Lee, Jeonghoon Feng, Xiahong Posmentier, Eric S. Faiia, Anthony M. Taylor, Susan TI Stable isotopic exchange rate constant between snow and liquid water SO CHEMICAL GEOLOGY LA English DT Article DE Isotopic exchange rate constants; Snowmelt isotope; Liquid to ice ratio ID ONE-DIMENSIONAL MODEL; HYDROGRAPH SEPARATION; MELTING SNOWPACK; OXYGEN-ISOTOPE; FRACTIONATION; EVOLUTION; CATCHMENT; MELTWATER; RUNOFF AB The isotopic exchange rate between liquid water and ice is crucial in determining the isotopic evolution of a snowpack and its melt. The rate constant for oxygen isotopic exchange has been reported by Tayloretal. [Taylor, S., Feng, X, Renshaw, C.E., Kirchner,J.W., 2002a. Isotopic evolution of snowmelt-2. Verification and parameterization of a one-dimensional model using laboratory experiments. Water Resources Research 38(10), 1218. doi:10.1029/2001WR000815] using three melting experiments with different column heights and melting rates. In this work, we obtained the hydrogen isotopic exchange rate constant using samples from two out of three experiments in Taylor et al. [Taylor, S., Feng, X., Renshaw, C.E., Kirchner,J.W., 2002a. Isotopic evolution of snowmelt-2. Verification and parameterization of a one-dimensional model using laboratory experiments. Water Resources Research 38 (10),1218. doi: 10.1029/2001WR000815]. The 1-D model developed by Feng et al. [Feng, X, Taylor, S., Renshaw, C.E., Kirchner, J.W., 2002. Isotopic evolution of snowmelt-1. A physically based one-dimensional model. Water Resources Research 38(10),1217. doi: 10.1029/2001WR000814] was fit to the isotopic results by adjusting the value of two parameters, the isotopic exchange rite constant (k(r)) and the fraction of ice participating in the exchange (f). We report that the best estimated k(r) values are from 0.070 to 0.19 h(-1) for oxygen isotopic exchange between liquid and ice, and 0.078 to 020 h(-1) for hydrogen exchange. The model results suggest that f, the fraction of ice involved in the isotopic exchange, increases with increasing wetness of snow, and is related to snow metamorphism. We discuss the physical significance of the observed variations in k(r) and f. The relationship between delta D and delta(18)O in the melt water is modeled, and the slope is close to 6. This slope is significantly different from the slope of the meteoric water line, while it is close to the ratio of ice-liquid fractionation of hydrogen to that of oxygen. (C) 2008 Elsevier B.V. All rights reserved. C1 [Lee, Jeonghoon; Feng, Xiahong; Posmentier, Eric S.; Faiia, Anthony M.] Dartmouth Coll, Dept Earth Sci, Hanover, NH 03755 USA. [Taylor, Susan] USA, Cold Reg Res & Engn Lab, Hanover, NH 03755 USA. RP Lee, JH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM jeonghoon.lee@jpl.nasa.gov RI Lee, Jeonghoon/C-7354-2008; Lee, Jeonghoon/E-8116-2010 OI Lee, Jeonghoon/0000-0002-1256-4431 FU National Science Foundation [EAR-9903281, EAR-0111403, EAR 0418809]; Dartmouth College FX This research was partially supported by the National Science Foundation (EAR-9903281, EAR-0111403, EAR 0418809) and by Dartmouth College. NR 25 TC 13 Z9 13 U1 5 U2 17 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2541 J9 CHEM GEOL JI Chem. Geol. PD MAR 15 PY 2009 VL 260 IS 1-2 BP 57 EP 62 DI 10.1016/j.chemgeo.2008.11.023 PG 6 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 424RA UT WOS:000264583100005 ER PT J AU Herndon, SC Wood, EC Northway, MJ Miake-Lye, R Thornhill, L Beyersdorf, A Anderson, BE Dowlin, R Dodds, W Knighton, WB AF Herndon, Scott C. Wood, Ezra C. Northway, Megan J. Miake-Lye, Richard Thornhill, Lee Beyersdorf, Andreas Anderson, Bruce E. Dowlin, Renee Dodds, Willard Knighton, W. Berk TI Aircraft Hydrocarbon Emissions at Oakland International Airport SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID REACTION MASS-SPECTROMETRY; USE COMMERCIAL AIRCRAFT; NITROGEN-OXIDES; AIR-QUALITY; ENGINE; QUANTIFICATION; SPECIATION; EXHAUST; IMPACT; AREA AB To help airports improve emission inventory data, speciated hydrocarbon emission indices have been measured from in-use commercial, airfreight, and general aviation aircraft at Oakland International Airport. The compounds reported here include formaldehyde, acetaldehyde, ethene, propene, and benzene. At idle, the magnitude of hydrocarbon emission indices was variable and reflected differences in engine technology, actual throttle setting, and ambient temperature. Scaling the measured emission indices to the simultaneously measured formaldehyde (HCHO) emission index eliminated most of the observed variability. This result supports a uniform hydrocarbon emissions profile across engine types when the engine is operating near idle, which can greatly simplify how speciated hydrocarbons are handled in emission inventories. The magnitude of the measured hydrocarbon emission index observed in these measurements (ambient temperature range 12-22 degrees C) is a factor of 1.5-2.2 times larger than the certification benchmarks. Using estimates of operational fuel flow rates at idle, this analysis suggests that current emission inventories at the temperatures encountered at this airport underestimate hydrocarbon emissions from the idle phase of operation by 16-45%. C1 [Herndon, Scott C.; Wood, Ezra C.; Northway, Megan J.; Miake-Lye, Richard] Aerodyne Res Inc, Billerica, MA USA. [Thornhill, Lee; Beyersdorf, Andreas; Anderson, Bruce E.] NASA, Langley Res Ctr, Div Atmospher Sci, Hampton, VA USA. [Dowlin, Renee] Port Portland, Portland, OR USA. [Dodds, Willard] Gen Elect Aviat, Cincinnati, OH USA. [Knighton, W. Berk] Montana State Univ, Bozeman, MT 59717 USA. RP Herndon, SC (reprint author), Aerodyne Res Inc, Billerica, MA USA. EM herndon@aerodyne.com RI Beyersdorf, Andreas/N-1247-2013 FU NASA; Missouri University of Science and Technology Center of Excellence FX This work was funded in part by NASA: Chowen Wey, FAA: Carl Ma through PARTNER, CARB: Steve Church through the Missouri University of Science and Technology Center of Excellence. We gratefully acknowledge FedEx Powerplant Engineering for assistance with specific engine model identification. We also thank David Senzig and Ted Thrasher with their help in identifying general aviation aircraft from the video record. We gratefully acknowledge the cooperation from Southwest Airlines and the Port of Oakland. NR 25 TC 22 Z9 22 U1 1 U2 13 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD MAR 15 PY 2009 VL 43 IS 6 BP 1730 EP 1736 DI 10.1021/es801307m PG 7 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 417WI UT WOS:000264108800015 PM 19368164 ER PT J AU Shazly, M Prakash, V Lerch, BA AF Shazly, Mostafa Prakash, Vikas Lerch, Bradley A. TI High strain-rate behavior of ice under uniaxial compression SO INTERNATIONAL JOURNAL OF SOLIDS AND STRUCTURES LA English DT Article DE Ice mechanics; Split Hopkinson pressure bar; High strain-rates; Uniaxial compression; Dynamic peak strength ID HOPKINSON PRESSURE BAR; LOW SLIDING VELOCITIES; SITU TENSILE-STRENGTH; FRESH-WATER ICE; DYNAMIC COMPRESSION; FRACTURE-TOUGHNESS; FRICTION; INITIATION; FAILURE; IMPACTS AB In the present study, a modified split Hopkinson pressure bar (SHPB) is employed to investigate the dynamic response of ice under uniaxial compression in the range of strain rates from 60 to 1400 s(-1) and at initial test temperatures of -10 and -30 degrees C. The compressive strength of ice shows positive strain-rate sensitivity over the range of strain rates employed; a slight influence of ice microstructure is observed, but it is much less than that reported previously for ice deformation under quasi-static loading conditions [Schulson, E.M., Iliescu, D., Frott, A., 2005. Characterization of ice for return-to-flight of the space shuttle. Part 1 - Hard ice. NASA CR-2005-213643-Part 1]. Specimen thickness, within the range studied, was found to have little or no effect on the peak (failure) strength of ice, while lowering the test temperature from -10 to -30 degrees C had a considerable effect, with ice behaving stronger at the lower test temperature. Moreover, unlike in the case of uniaxial quasi-static compression of ice, the effect of specimen end-constraint during the high rate compression was found to be negligible. One important result of these experiments, which may have important implications in modeling ice impacts, involves the post "peak-stress" behavior of the ice in that the ice samples do not catastrophically lose their load carrying capacity even after the attainment of peak stress during dynamic compression. This residual (tail) strength of the damaged/fragmented ice is sizable, and in some cases is larger than the quasi-static compression strength reported for ice. Moreover, this residual strength is observed to be dependent on sample thickness and the strain rate, being higher for thinner samples and at higher strain-rates during dynamic compression. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Shazly, Mostafa; Prakash, Vikas] Case Western Reserve Univ, Dept Mech & Aerosp Engn, Cleveland, OH 44106 USA. [Lerch, Bradley A.] NASA, GRC, Cleveland, OH 44135 USA. RP Prakash, V (reprint author), Case Western Reserve Univ, Dept Mech & Aerosp Engn, 10900 Euclid Ave,Glennan 616B, Cleveland, OH 44106 USA. EM vikas.prakash@case.edu FU NASA Glenn Research Center [NASA - NNC05VA03P]; NSF's Major Research Instrumentation program [CMS 0079458] FX The authors acknowledge financial support from NASA Glenn Research Center under contract # NASA - NNC05VA03P. The authors also thank Prof. E.M. Schulson and the Ice Research Laboratory at Dartmouth College, Hanover, NH, for providing ice samples, micro-structural analysis of the ice specimens, and many helpful discussions. Funding for the high-speed camera was provided by NSF's Major Research Instrumentation program through award No.CMS 0079458. NR 40 TC 18 Z9 22 U1 0 U2 13 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0020-7683 J9 INT J SOLIDS STRUCT JI Int. J. Solids Struct. PD MAR 15 PY 2009 VL 46 IS 6 BP 1499 EP 1515 DI 10.1016/j.ijsolstr.2008.11.020 PG 17 WC Mechanics SC Mechanics GA 417AU UT WOS:000264047700021 ER PT J AU Reysenbach, AL Hamamura, N Podar, M Griffiths, E Ferreira, S Hochstein, R Heidelberg, J Johnson, J Mead, D Pohorille, A Sarmiento, M Schweighofer, K Seshadri, R Voytek, MA AF Reysenbach, Anna-Louise Hamamura, N. Podar, M. Griffiths, E. Ferreira, S. Hochstein, R. Heidelberg, J. Johnson, J. Mead, D. Pohorille, A. Sarmiento, M. Schweighofer, K. Seshadri, R. Voytek, M. A. TI Complete and Draft Genome Sequences of Six Members of the Aquificales SO JOURNAL OF BACTERIOLOGY LA English DT Article ID BACTERIUM AQUIFEX-AEOLICUS; SP NOV.; SULFURIHYDROGENIBIUM-AZORENSE; MICROBIAL GENOMES AB The Aquificales are widespread in marine and terrestrial hydrothermal environments. Here, we report the complete and draft genome sequences of six new members of the Aquificales: two marine species, Persephonella marina strain EX-H1 and Hydrogenivirga strain 128-5-R1 (from the East Pacific Rise, 9 degrees 50.3'N, 104 degrees 17.5'W, and the Eastern Lau Spreading Center, 176 degrees 11.5'W, 20 degrees 45.8'S, respectively), and four terrestrial isolates, Sulfurihydrogenibium azorense strain Az-Fu1, Sulfurihydrogenibium yellowstonense strain SS-5, and Sulfurihydrogenibium strain Y03AOP1 (from Furnas, Azores, Portugal, and Calcite Springs and Obsidian Pool in Yellowstone National Park, United States, respectively), and the only thermoacidophilic isolate, Hydrogenobaculum strain Y04AAS1 (from a stream adjacent to Obsidian Pool). Significant differences among the different species exist that include nitrogen metabolism, hydrogen utilization, chemotaxis, and signal transduction, providing insights into their ecological niche adaptations. C1 [Reysenbach, Anna-Louise; Hamamura, N.] Portland State Univ, Dept Biol, Portland, OR 97201 USA. [Podar, M.] Oak Ridge Natl Lab, Biosci Div, Oak Ridge, TN 37831 USA. [Griffiths, E.] McMaster Univ, Dept Biochem & Biomed Sci, Hamilton, ON L8S 4L8, Canada. [Voytek, M. A.] US Geol Survey, Reston, VA 20192 USA. [Seshadri, R.] Synth Genom Inc, La Jolla, CA 92037 USA. [Schweighofer, K.] Affymetrix Corp, Santa Clara, CA 95051 USA. [Ferreira, S.; Johnson, J.; Sarmiento, M.] J Craig Venter Inst, Rockville, MD 20850 USA. [Hochstein, R.] Montana State Univ, Bozeman, MT 59715 USA. [Heidelberg, J.] Univ So Calif, Wrigley Inst Environm Studies, Dept Biol Sci, Avalon, CA 90704 USA. [Mead, D.] Lucigen Corp, Middleton, WI 53562 USA. [Pohorille, A.] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94025 USA. RP Reysenbach, AL (reprint author), Portland State Univ, Dept Biol, Portland, OR 97201 USA. EM reysenbacha@pdx.edu RI Hamamura, Natsuko/D-8837-2013; OI Heidelberg, John/0000-0003-0673-3224; Podar, Mircea/0000-0003-2776-0205 FU NSF [0236856]; The Gordon and Betty Moore Foundation; Joint Genome Institute; GBMF FX We thank Jennifer Meneghin, Karl Rustenholtz, Isabel Ferreira, and all those who assisted in many different ways to see these genome sequences be made available to the scientific community. Many thanks in particular to Nikos Kyrpides and many others at JGI who were instrumental in facilitating the deposition of the data into IMG and data analysis. Thanks to Loren Hauser at Oak Ridge National Laboratory and the JGI annotation team for their help. We thank Jason Miller and Granger Sutton and their team for the ongoing development and maintenance of the Celera Assembler and related tools. We thank Robert Friedman for his leadership of the GBMF-funded project. We acknowledge the J. Craig Venter Institute (JCVI) Joint Technology Center, under the leadership of Yu-Hui Rogers, for producing the genomic libraries and the sequence data. NR 10 TC 48 Z9 520 U1 0 U2 11 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0021-9193 J9 J BACTERIOL JI J. Bacteriol. PD MAR 15 PY 2009 VL 191 IS 6 BP 1992 EP 1993 DI 10.1128/JB.01645-08 PG 2 WC Microbiology SC Microbiology GA 413VB UT WOS:000263819500029 PM 19136599 ER PT J AU Strekalov, DV Savchenkov, AA Matsko, AB Yu, N AF Strekalov, D. V. Savchenkov, A. A. Matsko, A. B. Yu, N. TI Efficient upconversion of subterahertz radiation in a high-Q whispering gallery resonator SO OPTICS LETTERS LA English DT Article ID RECEIVER; UPCONVERSION AB We demonstrate efficient upconversion of subterahertz radiation into the optical domain in a high-Q whispering gallery mode resonator with quadratic optical nordinearity. The 5 X 10(-3) power conversion efficiency of a cw 100 GHz signal is achieved with only 16 mW of optical pump. (C) 2009 Optical Society of America C1 [Strekalov, D. V.; Savchenkov, A. A.; Matsko, A. B.; Yu, N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Strekalov, DV (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM dmitry.v.strekalov@jpl.nasa.gov FU NASA FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 16 TC 28 Z9 28 U1 2 U2 5 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0146-9592 J9 OPT LETT JI Opt. Lett. PD MAR 15 PY 2009 VL 34 IS 6 BP 713 EP 715 PG 3 WC Optics SC Optics GA 430GG UT WOS:000264976200003 PM 19282908 ER PT J AU Miller, RL Slingo, A Barnard, JC Kassianov, E AF Miller, R. L. Slingo, A. Barnard, J. C. Kassianov, E. TI Seasonal contrast in the surface energy balance of the Sahel SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID RADIATIVE FLUX DIVERGENCE; ECLATS FIELD EXPERIMENT; LEAF-AREA INDEX; RAINFALL VARIABILITY; SAHARAN AEROSOLS; WEST-AFRICA; CLIMATE; BUDGET; PRECIPITATION; EVAPORATION AB Over much of the world, heating of the surface by sunlight is balanced predominately by evaporative cooling. However, at the Atmospheric Radiation Measurement (ARM) Mobile Facility (AMF) in Niamey, Niger, evaporation makes a significant contribution to the surface energy balance only at the height of the rainy season, when precipitation has replenished the reservoir of soil moisture. The AMF was placed at Niamey from late 2005 to early 2007 to provide measurements of surface fluxes in coordination with geostationary satellite retrievals of radiative fluxes at the top of the atmosphere, as part of the RADAGAST experiment to calculate atmospheric radiative divergence. We use observations at the mobile facility to investigate how the surface adjusts to radiative forcing throughout the year. The surface response to solar heating varies with changes in atmospheric water vapor associated with the seasonal reversal of the West African monsoon, which modulates the greenhouse effect and the ability of the surface to radiate thermal energy directly to space. During the dry season, sunlight is balanced mainly by longwave radiation and the turbulent flux of sensible heat. The ability of longwave radiation to cool the surface drops after the onset of southwesterly surface winds at Niamey, when moist, oceanic air flows onshore, increasing local column moisture and atmospheric opacity. Following the onset of southwesterly flow, evaporation remains limited by the supply of moisture from precipitation. By the height of the rainy season, however, sufficient precipitation has accumulated that evaporation is controlled by incident sunlight, and radiative forcing of the surface is balanced comparably by the latent, sensible, and longwave fluxes. Evaporation increases with the leaf area index, suggesting that plants are a significant source of atmospheric moisture and may tap moisture stored beneath the surface that accumulated during a previous rainy season. Surface radiative forcing during a dust aerosol outbreak is balanced comparably by net surface longwave and the sensible heat flux during the dry season, with the sensible flux increasing in importance with the onset of the summer monsoon winds. Measurements of surface fluxes by the AMF indicate broader features of the West African monsoon circulation and should be used to evaluate model simulations of the Sahel climate. C1 [Miller, R. L.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Barnard, J. C.; Kassianov, E.] Pacific NW Natl Lab, Richland, WA 99352 USA. [Miller, R. L.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. [Slingo, A.] Univ Reading, Environm Syst Sci Ctr, Reading, Berks, England. RP Miller, RL (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM rmiller@giss.nasa.gov RI Miller, Ron/E-1902-2012 FU Atmospheric Radiation Measurement (ARM) Program; U.S. Department of Energy, Office of Science, Office of Biological and Environmental Research, Environmental Sciences Division; National Science Foundation [ATM-06-20066]; The Pacific Northwest National Laboratory; Battelle Memorial Institute, Pacific Northwest Division; U.S. Department of Energy (DOE); Atmospheric Radiation Measurement (ARM) [AC05-76RL01830] FX Data were obtained from the Atmospheric Radiation Measurement (ARM) Program sponsored by the U.S. Department of Energy, Office of Science, Office of Biological and Environmental Research, Environmental Sciences Division. The article was improved by the comments of three anonymous reviewers. We also thank Nazim Bharmal, Chris Bishop, Brian Cairns, Anthony Del Genio, Hamidou Hama, Kenneth Kehoe, Randall Koster, Peter Lamb, Issa Lele, Sally McFarlane, Mark Miller, Sharon Nicholson, Randy Peppler, Michael Puma, Chris Taylor, Dave Turner, Peng Xian, and Wenze Yang for their comments and advice. In addition, we thank Didier Tanre for aerosol retrievals from the AERONET site at Banizoumbou, Niger, and the Boston University Group for their MODIS vegetation products. This work was supported by the Climate Dynamics Program of the National Science Foundation through ATM-06-20066. A. S. was supported by the United Kingdom Natural Environment Research Council. The Pacific Northwest National Laboratory is operated by Battelle Memorial Institute, Pacific Northwest Division, for the U.S. Department of Energy (DOE). This research was supported in part by the DOE office of Biological and Environmental Research through the Atmospheric Radiation Measurement (ARM) program under contract DE-AC05-76RL01830 to the Pacific Northwest National Laboratory. This article is dedicated to the memory of Christopher Bishop and Anthony Slingo. NR 54 TC 8 Z9 8 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 MAR 14 PY 2009 VL 114 AR D00E05 DI 10.1029/2008JD010521 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 419PG UT WOS:000264231000002 ER PT J AU Wilcox, EM Harshvardhan Platnick, S AF Wilcox, Eric M. Harshvardhan Platnick, Steven TI Estimate of the impact of absorbing aerosol over cloud on the MODIS retrievals of cloud optical thickness and effective radius using two independent retrievals of liquid water path SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OCEAN ALGORITHM; SAFARI 2000; BIOMASS; PARTICLES; RADIATION AB Two independent satellite retrievals of cloud liquid water path (LWP) from the NASA Aqua satellite are used to diagnose the impact of absorbing biomass burning aerosol overlaying boundary-layer marine water clouds on the Moderate Resolution Imaging Spectrometer (MODIS) retrievals of cloud optical thickness (tau) and cloud droplet effective radius (re). In the MODIS retrieval over oceans, cloud reflectance in the 0.86-mu m and 2.13-mu m bands is used to simultaneously retrieve t and re. A low bias in the MODIS t retrieval may result from reductions in the 0.86-mm reflectance, which is only very weakly absorbed by clouds, owing to absorption by aerosols in cases where biomass burning aerosols occur above water clouds. MODIS LWP, derived from the product of the retrieved t and re, is compared with LWP ocean retrievals from the Advanced Microwave Scanning Radiometer-EOS (AMSR-E), determined from cloud microwave emission that is transparent to aerosols. For the coastal Atlantic southern African region investigated in this study, a systematic difference between AMSR-E and MODIS LWP retrievals is found for stratocumulus clouds over three biomass burning months in 2005 and 2006 that is consistent with above-cloud absorbing aerosols. Biomass burning aerosol is detected using the ultraviolet aerosol index from the Ozone Monitoring Instrument (OMI) on the Aura satellite. The LWP difference (AMSR-E minus MODIS) increases both with increasing t and increasing OMI aerosol index. During the biomass burning season the mean LWP difference is 14 g m(-2), which is within the 15-20 g m(-2) range of estimated uncertainties in instantaneous LWP retrievals. For samples with only low amounts of overlaying smoke (OMI AI <= 1) the difference is 9.4, suggesting that the impact of smoke aerosols on the mean MODIS LWP is 5.6 g m(-2). Only for scenes with OMI aerosol index greater than 2 does the average LWP difference and the estimated bias in MODIS cloud optical thickness attributable to the impact of overlaying biomass burning aerosol exceed the instantaneous uncertainty in the retrievals. C1 [Wilcox, Eric M.; Platnick, Steven] NASA, Goddard Space Flight Ctr, Climate & Radiat Branch, Atmospheres Lab, Greenbelt, MD 20771 USA. [Harshvardhan] Purdue Univ, Dept Earth & Atmospher Sci, W Lafayette, IN 47907 USA. RP Wilcox, EM (reprint author), NASA, Goddard Space Flight Ctr, Climate & Radiat Branch, Atmospheres Lab, Code 613-2, Greenbelt, MD 20771 USA. EM eric.m.wilcox@nasa.gov RI Platnick, Steven/J-9982-2014 OI Platnick, Steven/0000-0003-3964-3567 FU NASA Radiation Sciences Program; NASA Earth Science REASoN DISCOVER Project FX This research was supported by the NASA Radiation Sciences Program. AMSR-E data are produced by Remote Sensing Systems and sponsored by the NASA Earth Science REASoN DISCOVER Project and the AMSR-E Science Team. These data are available at www.remss.com. OMI data are distributed by the Goddard Earth Sciences Data and Information Services Center. NR 23 TC 33 Z9 33 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 MAR 14 PY 2009 VL 114 AR D05210 DI 10.1029/2008JD010589 PG 7 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 419PG UT WOS:000264231000003 ER PT J AU Satheesh, SK Torres, O Remer, LA Babu, SS Vinoj, V Eck, TF Kleidman, RG Holben, BN AF Satheesh, S. K. Torres, O. Remer, L. A. Babu, S. Suresh Vinoj, V. Eck, T. F. Kleidman, R. G. Holben, B. N. TI Improved assessment of aerosol absorption using OMI-MODIS joint retrieval SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID INDIAN-OCEAN EXPERIMENT; ANTHROPOGENIC AEROSOLS; SPECTRAL RADIANCES; LIGHT-ABSORPTION; OPTICAL DEPTH; SAHARAN DUST; INSTRUMENT; SATELLITE; RADIATION; CLOUDS AB The Ozone Monitoring Instrument (OMI) aboard EOS-Aura and the Moderate Resolution Imaging Spectroradiometer (MODIS) onboard EOS-Aqua fly in formation as part of the A-train. Though OMI retrieves aerosol optical depth (AOD) and aerosol absorption, it must assume aerosol layer height. The MODIS cannot retrieve aerosol absorption, but MODIS aerosol retrieval is not sensitive to aerosol layer height and with its smaller pixel size is less affected by subpixel clouds. Here we demonstrate an approach that uses MODIS-retrieved AOD to constrain the OMI retrieval, freeing OMI from making an a priori estimate of aerosol height and allowing a more direct retrieval of aerosol absorption. To predict near-UV optical depths using MODIS data we rely on the spectral curvature of the MODIS-retrieved visible and near-IR spectral AODs. Application of an OMI-MODIS joint retrieval over the north tropical Atlantic shows good agreement between OMI and MODIS-predicted AODs in the UV, which implies that the aerosol height assumed in the OMI-standard algorithm is probably correct. In contrast, over the Arabian Sea, MODIS-predicted AOD deviated from the OMI-standard retrieval, but combined OMI-MODIS retrievals substantially improved information on aerosol layer height (on the basis of validation against airborne lidar measurements). This implies an improvement in the aerosol absorption retrieval, but lack of UV absorption measurements prevents a true validation. Our study demonstrates the potential of multisatellite analysis of A-train data to improve the accuracy of retrieved aerosol products and suggests that a combined OMI-MODIS-CALIPSO retrieval has large potential to further improve assessments of aerosol absorption. C1 [Satheesh, S. K.; Vinoj, V.] Indian Inst Sci, Ctr Atmospher & Ocean Sci, Bangalore 560012, Karnataka, India. [Satheesh, S. K.; Remer, L. A.; Eck, T. F.; Kleidman, R. G.; Holben, B. N.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Torres, O.] Hampton Univ, Dept Atmospher & Planetary Sci, Hampton, VA 23668 USA. [Babu, S. Suresh] Vikram Sarabhai Space Ctr, Space Phys Lab, Thiruvananthapuram 695022, Kerala, India. RP Satheesh, SK (reprint author), Indian Inst Sci, Ctr Atmospher & Ocean Sci, Bangalore 560012, Karnataka, India. EM satheesh@caos.iisc.ernet.in RI Vinoj, V./C-3241-2008; ECK, THOMAS/D-7407-2012; Torres, Omar/G-4929-2013 OI Vinoj, V./0000-0001-8573-6073; FU NASA; NASA's Atmospheric Composition program led by Phil DeCola and Rangasayi Halthore FX This research was carried out when one of the authors (SKS) was supported by an appointment to the NASA postdoctoral program at the NASA Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. We also acknowledge funding through NASA's Atmospheric Composition program led by Phil DeCola and Rangasayi Halthore. We thank the principal investigators and their staff for establishing and maintaining the seven AERONET sites used in this investigation. NR 43 TC 23 Z9 24 U1 1 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 MAR 13 PY 2009 VL 114 AR D05209 DI 10.1029/2008JD011024 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 419PD UT WOS:000264230700003 ER PT J AU Liu, Y Wang, Y Liu, X Cai, ZN Chance, K AF Liu, Yi Wang, Yong Liu, Xiong Cai, Zhaonan Chance, Kelly TI Tibetan middle tropospheric ozone minimum in June discovered from GOME observations SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SATELLITE MEASUREMENTS; PACIFIC AB Global Ozone Monitoring Experiment (GOME) observations from 1997-2000 have revealed the Tibetan Middle Tropospheric Ozone Minimum (TMTOM), a low-ozone layer that occurs in the middle troposphere over the Tibetan Plateau (TP) in June. Ozone profiles were derived from GOME observations and validated by ozonesonde measurements at two stations (Lhasa and Xining) over the TP. The mean bias is 5-10% within the troposphere. The ozone profiles reveal the TMTOM phenomenon occurs in the middle troposphere (8-13 km) over the middle and eastern TP in June. Dynamical field analyses showed that the TMTOM accompanies the onset of the Asian summer monsoon. The low-ozone air from the Bay of Bengal is transported into the middle troposphere over the TP by southwest currents while the lower troposphere over the TP is still occupied by ozone-rich air blocked by the transport barrier of the Himalayas. The TMTOM was most prominent in June 1998 likely linked to the occurrence of the intense El Nino of 1997-1998 because the Tibetan anticyclone is of large area and has strong intensity during El Nino years. The occurrence of the TMTOM can serve as an indicator of the phase of evolution of the Asian summer monsoon. Citation: Liu, Y., Y. Wang, X. Liu, Z. Cai, and K. Chance (2009), Tibetan middle tropospheric ozone minimum in June discovered from GOME observations, Geophys. Res. Lett., 36, L05814, doi:10.1029/2008GL037056. C1 [Liu, Yi; Wang, Yong; Cai, Zhaonan] Chinese Acad Sci, Inst Atmospher Phys, Key Lab Middle Atmosphere & Global Environm Obser, Beijing 100029, Peoples R China. [Chance, Kelly] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Liu, Xiong] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. RP Liu, Y (reprint author), Chinese Acad Sci, Inst Atmospher Phys, Key Lab Middle Atmosphere & Global Environm Obser, Beijing 100029, Peoples R China. EM liuyi@mail.iap.ac.cn RI Liu, Xiong/P-7186-2014; OI Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577 FU National Science Foundation of China [40633015, 40710059003]; NASA [NNX08AN98G]; Smithsonian Institution; European Space Agency; German Aerospace Center with GOME FX We thank Yasunobu Iwasaka from Kanazawa University, Japan, and Guangyu Shi from the Institute of Atmospheric Physics, Chinese Academy of Sciences, China, for providing the ozone-sonde data at Lhasa, China; we also thank Xiangdong Zheng from the Chinese Institute of Meteorological Science for providing ozone-sonde data at Xining, China. This work was funded by the National Science Foundation of China under grants 40633015 and 40710059003. Xiong Liu was also funded by the NASA New Investigator Program (NNX08AN98G). Kelly Chance was supported by NASA and the Smithsonian Institution. We are pleased to acknowledge the ongoing cooperation of the European Space Agency and the German Aerospace Center with GOME. NR 21 TC 12 Z9 14 U1 0 U2 6 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 MAR 12 PY 2009 VL 36 AR L05814 DI 10.1029/2008GL037056 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 419LX UT WOS:000264222100007 ER PT J AU Mann, ME Schmidt, GA Miller, SK LeGrande, AN AF Mann, Michael E. Schmidt, Gavin A. Miller, Sonya K. LeGrande, Allegra N. TI Potential biases in inferring Holocene temperature trends from long-term borehole information SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SURFACE AIR-TEMPERATURE; ARCTIC PERMAFROST; NORTH-AMERICA; GISS MODELE; SNOW COVER; CLIMATE; RECONSTRUCTIONS; PALEOCLIMATE; SIMULATIONS; MIDHOLOCENE AB We use a set of global coupled ocean-atmosphere general circulation (OAGCM) experiments for timeslices over the Holocene from 9K Yr BP onwards to examine differences in Northern Hemisphere Ground Surface Temperature (GST) and Surface Air Temperature (SAT) trends. The model results are driven mainly by the orbitally-forced changes in seasonal insolation, and in particular, the increase in northern hemisphere seasonality in the early-to-mid Holocene. The model reproduces qualitatively presumed past trends in NH temperatures, though it may underestimate their magnitude. For this period, we see on average a significant increase in GST relative to SAT as a result of a competition between the effects of changing seasonal insolation, and the varying extent of insulating seasonal snow cover. The model shows a mid-Holocene peak in annual mean terrestrial Northern Hemisphere GST, but not in annual Surface Air Temperatures (SAT). We conclude that the factors influencing long-term GST trends are potentially quite complex, and that considerable care must be taken in interpreting SAT changes from the GST evidence when there is the possibility of substantial seasonal variation in warmth and snow cover. Citation: Mann, M. E., G. A. Schmidt, S. K. Miller, and A. N. LeGrande (2009), Potential biases in inferring Holocene temperature trends from long-term borehole information, Geophys. Res. Lett., 36, L05708, doi:10.1029/2008GL036354. C1 [Mann, Michael E.; Miller, Sonya K.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. [Mann, Michael E.; Miller, Sonya K.] Penn State Univ, Earth & Environm Syst Inst, University Pk, PA 16802 USA. [Schmidt, Gavin A.; LeGrande, Allegra N.] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Mann, ME (reprint author), Penn State Univ, Dept Meteorol, 503 Walker Bldg, University Pk, PA 16802 USA. EM mann@psu.edu RI Schmidt, Gavin/D-4427-2012; LeGrande, Allegra/D-8920-2012; Mann, Michael/B-8472-2017 OI Schmidt, Gavin/0000-0002-2258-0486; LeGrande, Allegra/0000-0002-5295-0062; Mann, Michael/0000-0003-3067-296X FU National Science Foundation [ATM-0542356]; NSF [ATM-05-01241]; NASA Modeling, Analysis and Prediction program FX We thank H. Pollack for providing site information for the 'HPS' borehole network. M.E.M. gratefully acknowledges support from the ATM program of the National Science Foundation (grant ATM-0542356). Holocene climate modeling at GISS was supported by NSF ATM-05-01241 and the NASA Modeling, Analysis and Prediction program. NR 34 TC 6 Z9 6 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 12 PY 2009 VL 36 AR L05708 DI 10.1029/2008GL036354 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 419LX UT WOS:000264222100002 ER PT J AU Duncan, BN Yoshida, Y Damon, MR Douglass, AR Witte, JC AF Duncan, Bryan N. Yoshida, Yasuko Damon, Megan R. Douglass, Anne R. Witte, Jacquelyn C. TI Temperature dependence of factors controlling isoprene emissions SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID OZONE MONITORING INSTRUMENT; DROUGHT; SPACE; RATES AB We investigated the relationship of variability in the formaldehyde (HCHO) columns measured by the Aura Ozone Monitoring Instrument (OMI) to isoprene emissions in the southeastern United States for 2005-2007. The data show that the inferred, regional-average isoprene emissions varied by about 22% during summer and are well correlated with temperature, which is known to influence emissions. Part of the correlation with temperature is likely associated with other causal factors that are temperature-dependent. We show that the variations in HCHO are convolved with the temperature dependence of surface ozone, which influences isoprene emissions, and the dependence of the HCHO column to mixed layer height as OMI's sensitivity to HCHO increases with altitude. Furthermore, we show that while there is an association of drought with the variation in HCHO, drought in the southeastern U. S. is convolved with temperature. Citation: Duncan, B. N., Y. Yoshida, M. R. Damon, A. R. Douglass, and J. C. Witte (2009), Temperature dependence of factors controlling isoprene emissions, Geophys. Res. Lett., 36, L05813, doi: 10.1029/2008GL037090. C1 [Duncan, Bryan N.; Yoshida, Yasuko; Douglass, Anne R.; Witte, Jacquelyn C.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Greenbelt, MD 20771 USA. [Damon, Megan R.] Northrop Grumman TASC, Chantilly, VA 20151 USA. [Yoshida, Yasuko] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Witte, Jacquelyn C.] Sci Syst & Applicat Inc, Greenbelt, MD USA. RP Duncan, BN (reprint author), NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Greenbelt, MD 20771 USA. EM bryan.n.duncan@nasa.gov RI Duncan, Bryan/A-5962-2011; Douglass, Anne/D-4655-2012 FU NASA Modeling and Analysis Program; NASA Earth Science Research Program FX This work was supported by the NASA Modeling and Analysis Program and the NASA Earth Science Research Program. We gratefully thank C. Retscher for his help with slant column data and J. Ziemke for his help with the regression analysis. We acknowledge B. Middleton, R. Martin, A. Molod and P. Palmer for helpful discussions. NR 28 TC 10 Z9 10 U1 1 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 11 PY 2009 VL 36 AR L05813 DI 10.1029/2008GL037090 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 419LW UT WOS:000264222000006 ER PT J AU Dorodnitsyn, AV AF Dorodnitsyn, A. V. TI Gravitationally distorted P Cygni profiles from outflows near compact objects SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE line: formation; radiation mechanisms: general; radiative transfer; stars: mass-loss; stars: winds, outflows; galaxies: active ID REDSHIFTED ABSORPTION-LINES; RAY BURST SPECTRA; EXPANDING ATMOSPHERES; ACCRETION DISKS; DRIVEN WINDS; BLACK-HOLE; MASS-LOSS; ENVELOPES; RADIATION; MATTER AB We consider resonant absorption in a spectral line in the outflowing plasma within several tens of Schwarzschild radii from a compact object. We take into account both Doppler and gravitational shifting effects and reformulate the theory of P Cygni profiles in these new circumstances. It is found that a spectral line may have multiple absorption and emission components depending on how far the region of interaction is from the compact object and what the distribution of velocity and opacity is. Profiles of spectral lines produced near a neutron star or a black hole can be strongly distorted by Doppler blue- or redshifting and gravitational redshifting. These profiles may have both red- and blueshifted absorption troughs. The result should be contrasted with classical P Cygni profiles, which consist of redshifted emission and blueshifted absorption features. We suggest that this property of line profiles to have complicated narrow absorption and emission components in the presence of strong gravity may help researchers to study spectroscopically the innermost parts of an outflow. C1 [Dorodnitsyn, A. V.] NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. [Dorodnitsyn, A. V.] Space Res Inst, Moscow 117997, Russia. RP Dorodnitsyn, AV (reprint author), NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Code 662, Greenbelt, MD 20771 USA. EM dora@milkyway.gsfc.nasa.gov FU Max Planck Institute for Nuclear Research (Heidelberg); NASA Postdoctoral Program at the NASA Goddard Space Flight Center FX Most of this work was carried out when the author was a postdoctoral fellow at the Max Planck Institute for Nuclear Research (Heidelberg). This research was supported in part by an appointment to the NASA Postdoctoral Program at the NASA Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. The author thanks G. S. Bisnovatyi-Kogan for the encouragement of this work and also Felix Aharonian and members of the High Energy Astrophysics Group of the Max Planck Institute for Nuclear Research for discussion. The author thanks Tim Kallman for discussions and his suggestions and help regarding the style and structure of the manuscript. NR 30 TC 8 Z9 8 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 MAR 11 PY 2009 VL 393 IS 4 BP 1433 EP 1448 DI 10.1111/j.1365-2966.2008.14171.x PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 412XV UT WOS:000263758400026 ER PT J AU Bautista, MA Ballance, C Gull, TR Hartman, H Lodders, K Martinez, M Melendez, M AF Bautista, M. A. Ballance, C. Gull, T. R. Hartman, H. Lodders, K. Martinez, M. Melendez, M. TI Scandium and chromium in the strontium filament in the Homunculus of eta Carinae SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE atomic data; atomic processes; line: formation; stars: abundances ID TRANSITION PROBABILITIES; II EMISSION; OSCILLATOR-STRENGTHS; ATOMIC STRUCTURES; FORBIDDEN LINES; FERRUM PROJECT; NI-II; SC-II; FE II; IDENTIFICATION AB We continue a systematic study of chemical abundances of the strontium filament found in the ejecta of eta Carinae. To this end we interpret the emission spectrum of Sc II and Cr II using multilevel non-local thermodynamic equilibrium models. Since the atomic data for these ions were previously unavailable, we carry out ab initio calculations of radiative transition rates and electron impact excitation rate coefficients. The observed spectrum is consistent with an electron density of the order of 10(7) cm(-3) and a temperature between 6000 and 7000 K, conditions previously determined from [Ni II], [Ti II] and [Sr II] diagnostics. The observed spectrum indicates an abundance of Sc relative to Ni more than 40 times the solar value, while the Cr/Ni abundance ratio is roughly solar. Various scenarios of depletion and dust destruction are suggested to explain such abnormal abundances. C1 [Bautista, M. A.] Virginia Polytech Inst & State Univ, Dept Phys, Blacksburg, VA 24061 USA. [Ballance, C.] Rollins Coll, Dept Phys, Winter Pk, FL 32789 USA. [Gull, T. R.; Melendez, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hartman, H.] Lund Univ, Lund Observ, SE-22100 Lund, Sweden. [Lodders, K.] Washington Univ, Dept Earth & Planetary Sci, Planetary Chem Lab, St Louis, MO 63130 USA. [Lodders, K.] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA. [Martinez, M.] IVIC, Ctr Fis, Caracas 1020A, Venezuela. [Melendez, M.] Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. RP Bautista, MA (reprint author), Virginia Polytech Inst & State Univ, Dept Phys, Blacksburg, VA 24061 USA. EM bautista@vt.edu RI Gull, Theodore/D-2753-2012; Hartman, Henrik/K-3113-2013 OI Gull, Theodore/0000-0002-6851-5380; FU Swedish Research Council (VR) FX We like to thank the anonymous referee for valuable questions and comments that let to material improvements of the paper. The observations of the strontium filament were made with the STIS on the NASA/ESA HST and were obtained by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. HH acknowledges support from the Swedish Research Council (VR). Data for this analysis were gathered under GO programs headed by Kris Davidson and GO and GTO programs headed by Theodore Gull. NR 35 TC 10 Z9 10 U1 0 U2 3 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 11 PY 2009 VL 393 IS 4 BP 1503 EP 1512 DI 10.1111/j.1365-2966.2008.14246.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 412XV UT WOS:000263758400032 ER PT J AU Spoon, HWW Armus, L Marshall, JA Bernard-Salas, J Farrah, D Charmandaris, V Kent, BR AF Spoon, H. W. W. Armus, L. Marshall, J. A. Bernard-Salas, J. Farrah, D. Charmandaris, V. Kent, B. R. TI HIGH-VELOCITY NEON LINE EMISSION FROM THE ULIRG IRAS F00183-7111: REVEALING THE OPTICALLY OBSCURED BASE OF A NUCLEAR OUTFLOW SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: ISM; ISM: jets and outflows; galaxies: active; galaxies: individual (IRAS F00183-7111, IRAS 12127-1412, IRAS 13451+1232); galaxies: ISM ID ULTRALUMINOUS INFRARED GALAXIES; SPITZER-SPACE-TELESCOPE; LYMAN BREAK GALAXIES; X-RAY; INTERSTELLAR-MEDIUM; ACTIVE GALAXIES; MIDINFRARED SPECTROSCOPY; CRYSTALLINE SILICATES; GALACTIC SUPERWINDS; SPECTROGRAPH IRS AB We report the first mid-infrared detection of highly disturbed ionized gas in the ultraluminous infrared galaxy (ULIRG) IRAS F00183-7111. The gas, traced by the 12.81 mu m [Ne II] and 15.56 mu m [Ne III] lines, spans a velocity range of -3500 to +3000 km s(-1) with respect to systemic velocity. Optical and near-infrared spectroscopic studies show no evidence for similarly high velocity gas components in forbidden lines at shorter wavelengths. We interpret this as the result of strong extinction (A(V) = 10-50) on the high-velocity gas, which identifies the base of the outflow traced in 5007 angstrom [O III] as a plausible origin. Unusual excitation conditions are implied by a comparison of the mid-infrared low-excitation neon line emission and the polycyclic aromatic hydrocarbon (PAH) emission for a sample of 56 ULIRGs. For IRAS F00183-7111, the neon/PAH ratio is 8 times higher than the average ratio. Similar mid-infrared kinematic and excitation characteristics are found for only two other ULIRGs in our sample: IRAS 12127-1412NE and IRAS 13451+1232. Both sources have an elevated neon/PAH ratio and exhibit pronounced blue wings in their 15.56 mu m [Ne III] line profiles. IRAS 13451+1232 even shows a strongly blueshifted and broad 14.32 mu m [Ne v] line. While for IRAS 13451+1232 the observed [Ne III]/[Ne II] and [Ne v]/[Ne II] line ratios indicate exposure of the blueshifted gas to direct radiation from the AGN, for IRAS F00183-7111 and IRAS 12127-1412NE the neon line ratios are consistent with an origin in fast shocks in a high-density environment, and with an evolutionary scenario in which strongly blueshifted [Ne II] and [Ne III] emission trace the (partial) disruption of the obscuring medium around a buried AGN. The detection of strongly blueshifted [Ne v] emission in IRAS 13451+1232 would then indicate this process to be much further advanced in this ULIRG than in IRAS F00183-7111 and IRAS 12127-1412NE, where this line is undetected. C1 [Spoon, H. W. W.; Bernard-Salas, J.; Farrah, D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Armus, L.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Marshall, J. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Charmandaris, V.] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece. [Charmandaris, V.] Fdn Res & Technol Hellas, IESL, GR-71110 Iraklion, Greece. [Charmandaris, V.] Observ Paris, Chercheur Associe, F-75014 Paris, France. [Kent, B. R.] Natl Radio Astron Observ, Charlottesville, VA 22901 USA. RP Spoon, HWW (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. EM spoon@isc.astro.cornell.edu RI Charmandaris, Vassilis/A-7196-2008 OI Charmandaris, Vassilis/0000-0002-2688-1956 FU NASA FX The authors thank Jan Cami, Helmut Dannerbauer, Brent Groves, Lei Hao, Timothy Heckman, Lisa Kewley, Dieter Lutz, and Xander Tielens for discussions, Catherine Buchanan, Joanna Holt, and Sylvain Veilleux for sharing their published spectra, and Mark G. Allen for providing MAPPINGS shock models ahead of publication. We also thank the slowbut dilligent referee for comments which helped to strengthen the paper. Support for this work was provided by NASA. This research has made extensive use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 60 TC 21 Z9 22 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2009 VL 693 IS 2 BP 1223 EP 1235 DI 10.1088/0004-637X/693/2/1223 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 417RR UT WOS:000264095100016 ER PT J AU Moskalenko, IV Stawarz, L Porter, TA Cheung, CC AF Moskalenko, Igor V. Stawarz, Lukasz Porter, Troy A. Cheung, Chi C. TI ON THE POSSIBLE ASSOCIATION OF ULTRA HIGH ENERGY COSMIC RAYS WITH NEARBY ACTIVE GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmic rays; galaxies: active; galaxies: individual (Cen A, Cen B, PKS 2158-380, PKS 2201+044); intergalactic medium ID GALACTIC MAGNETIC-FIELD; EXTRAGALACTIC RADIO-SOURCES; LARGE-SCALE STRUCTURE; DIGITAL SKY SURVEY; BLACK-HOLE MASS; SEYFERT-GALAXIES; X-RAY; IMAGING SURVEY; LUMINOSITY FUNCTION; UPPER LIMIT AB Data collected by the Pierre Auger Observatory (Auger) provide evidence for anisotropy in the arrival directions of cosmic rays (CRs) with energies higher than 57 EeV, which suggests a correlation with the positions of active galactic nuclei (AGNs) located within similar to 75 Mpc and 3 degrees.2 of the arrival directions. This analysis, however, does not take into account AGN morphology. A detailed study of the sample of AGNs whose positions are located within 3 degrees.2 of the CR events (and extending our analysis out to similar to 150 Mpc) shows that most of them are classified as Seyfert 2 and low-ionization nuclear emission-line region galaxies whose properties do not differ substantially from other local AGNs of the same type. Therefore, if the production of the highest energy CRs is persistent in nature, i.e., operates in a single object on long (greater than or similar to Myr) timescales, the claimed correlation between the CR events observed by Auger and the local active galaxies should be considered as resulting from a chance coincidence. In addition, most of the selected sources do not show significant jet activity, and hence, in most conservative scenarios, there are no reasons for expecting them to accelerate CRs up to the highest energies, similar to 10(20) eV. If the extragalactic magnetic fields and the sources of these CRs are coupled with matter, it is possible that the deflection angle is larger than expected in the case of a uniform source distribution due to effectively larger fields. A future analysis has to take into account AGN morphology and may yield a correlation with a larger deflection angle and/or more distant sources. We further argue that the nearby radio galaxy NGC 5128 (Cen A) alone could be associated with at least four events due to its large radio extent, and PKS 1343-60 (Cen B), another nearby radio galaxy, can be associated with more than one event due to its proximity to the Galactic plane and, correspondingly, the stronger Galactic magnetic field the ultra-high-energy CRs (UHECRs) encounter during propagation to the Earth. If the UHECRs associated with these events are indeed accelerated by Cen A and Cen B, their deflection angles may provide information on the structure of the magnetic field in the direction of these putative sources. Future gamma-ray observations (e. g., Fermi Gamma-ray Space Telescope formerly Gamma-Ray Large Area Space Telescope, and High Energy Stereoscopic System in the Southern hemisphere) may provide additional clues to the nature of the accelerators of the UHECRs in the local universe. C1 [Moskalenko, Igor V.; Stawarz, Lukasz] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94309 USA. [Porter, Troy A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Cheung, Chi C.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Moskalenko, Igor V.] Stanford Univ, Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Stawarz, Lukasz] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. RP Moskalenko, IV (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94309 USA. EM imos@stanford.edu; stawarz@slac.stanford.edu; tporter@scipp.ucsc.edu; Teddy.Cheung@nasa.gov RI Moskalenko, Igor/A-1301-2007 OI Moskalenko, Igor/0000-0001-6141-458X FU NASA Astronomy and Physics Research and Analysis Program (APRA); MEiN [1-P03D-003-29]; US Department of Energy FX I. V. M. acknowledges support from NASA Astronomy and Physics Research and Analysis Program (APRA) grant. L. S. acknowledges support by the MEiN grant 1-P03D-003-29. T. A. P. acknowledges partial support from the US Department of Energy. C. C. C. was supported by an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 146 TC 37 Z9 37 U1 1 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2009 VL 693 IS 2 BP 1261 EP 1274 DI 10.1088/0004-637X/693/2/1261 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 417RR UT WOS:000264095100019 ER PT J AU Woods, PM Willacy, K AF Woods, Paul M. Willacy, Karen TI CARBON ISOTOPE FRACTIONATION IN PROTOPLANETARY DISKS SO ASTROPHYSICAL JOURNAL LA English DT Review DE astrochemistry; planetary systems: protoplanetary disks; solar system: formation ID DENSE INTERSTELLAR CLOUDS; GALACTIC CHEMICAL EVOLUTION; T-TAURI STARS; YOUNG STELLAR OBJECTS; HERBIG-AE STARS; BOPP C/1995 O1; ORGANIC-MOLECULES; PROTOSTELLAR DISKS; ULTRAVIOLET-RADIATION; CIRCUMSTELLAR DISKS AB We investigate the gas-phase and grain-surface chemistry in the inner 30 AU of a typical protoplanetary disk (PPD) using a new model which calculates the gas temperature by solving the gas heating and cooling balance and which has an improved treatment of the UV radiation field. We discuss inner-disk chemistry in general, obtaining excellent agreement with recent observations which have probed the material in the inner regions of PPDs. We also apply our model to study the isotopic fractionation of carbon. Results show that the fractionation ratio, (12)C/(13)C, of the system varies with radius and height in the disk. Different behavior is seen in the fractionation of different species. We compare our results with (12)C/(13)C ratios in the solar system comets, and find a stark contrast, indicative of reprocessing. C1 [Woods, Paul M.; Willacy, Karen] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Woods, PM (reprint author), Univ Manchester, Jodrell Bank, Ctr Astrophys, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England. EM paul.woods@manchester.ac.uk RI Woods, Paul/E-6926-2011 OI Woods, Paul/0000-0003-4340-3590 NR 137 TC 52 Z9 52 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2009 VL 693 IS 2 BP 1360 EP 1378 DI 10.1088/0004-637X/693/2/1360 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 417RR UT WOS:000264095100028 ER PT J AU Greiner, J Kruhler, T Fynbo, JPU Rossi, A Schwarz, R Klose, S Savaglio, S Tanvir, NR McBreen, S Totani, T Zhang, BB Wu, XF Watson, D Barthelmy, SD Beardmore, AP Ferrero, P Gehrels, N Kann, DA Kawai, N Yoldas, AK Meszaros, P Milvang-Jensen, B Oates, SR Pierini, D Schady, P Toma, K Vreeswijk, PM Yoldas, A Zhang, B Afonso, P Aoki, K Burrows, DN Clemens, C Filgas, R Haiman, Z Hartmann, DH Hasinger, G Hjorth, J Jehin, E Levan, AJ Liang, EW Malesani, D Pyo, TS Schulze, S Szokoly, G Terada, K Wiersema, K AF Greiner, J. Kruehler, T. Fynbo, J. P. U. Rossi, A. Schwarz, R. Klose, S. Savaglio, S. Tanvir, N. R. McBreen, S. Totani, T. Zhang, B. B. Wu, X. F. Watson, D. Barthelmy, S. D. Beardmore, A. P. Ferrero, P. Gehrels, N. Kann, D. A. Kawai, N. Yoldas, A. Kuepcue Meszaros, P. Milvang-Jensen, B. Oates, S. R. Pierini, D. Schady, P. Toma, K. Vreeswijk, P. M. Yoldas, A. Zhang, B. Afonso, P. Aoki, K. Burrows, D. N. Clemens, C. Filgas, R. Haiman, Z. Hartmann, D. H. Hasinger, G. Hjorth, J. Jehin, E. Levan, A. J. Liang, E. W. Malesani, D. Pyo, T. -S. Schulze, S. Szokoly, G. Terada, K. Wiersema, K. TI GRB 080913 AT REDSHIFT 6.7 SO ASTROPHYSICAL JOURNAL LA English DT Review DE early universe; gamma rays: bursts; radiation mechanisms: non-thermal ID GAMMA-RAY BURSTS; PROBE WMAP OBSERVATIONS; COSMIC CHEMICAL EVOLUTION; GUNN-PETERSON TROUGH; STAR-FORMATION; LY-ALPHA; PHOTOMETRIC REDSHIFT; ENERGY INJECTION; LIGHT CURVES; HOST GALAXY AB We report on the detection by Swift of GRB 080913, and subsequent optical/near-infrared follow-up observations by GROND, which led to the discovery of its optical/NIR afterglow and the recognition of its high-z nature via the detection of a spectral break between the i' and z' bands. Spectroscopy obtained at the ESO-VLT revealed a continuum extending down to lambda = 9400 angstrom, and zero flux for 7500 angstrom< lambda < 9400 angstrom, which we interpret as the onset of a Gunn-Peterson trough at z = 6.695 +/- 0.025 (95.5% confidence level), making GRB 080913 the highest-redshift gamma-ray burst (GRB) to date, and more distant than the highest-redshift QSO. We note that many redshift indicators that are based on promptly available burst or afterglow properties have failed for GRB 080913. We report on our follow-up campaign and compare the properties of GRB 080913 with bursts at lower redshift. In particular, since the afterglow of this burst is fainter than typical for GRBs, we show that 2 m class telescopes can identify most high-redshift GRBs. C1 [Greiner, J.; Kruehler, T.; Savaglio, S.; McBreen, S.; Pierini, D.; Yoldas, A.; Afonso, P.; Clemens, C.; Filgas, R.; Hasinger, G.; Szokoly, G.] Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. [Kruehler, T.] Tech Univ Munich, D-85748 Garching, Germany. [Fynbo, J. P. U.; Watson, D.; Milvang-Jensen, B.; Vreeswijk, P. M.; Hjorth, J.; Malesani, D.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. [Rossi, A.; Klose, S.; Ferrero, P.; Kann, D. A.; Schulze, S.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Schwarz, R.] Astrophys Inst Potsdam, D-14482 Potsdam, Germany. [Tanvir, N. R.; Beardmore, A. P.; Terada, K.; Wiersema, K.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Totani, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Zhang, B. B.; Zhang, B.] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA. [Wu, X. F.; Meszaros, P.; Toma, K.; Burrows, D. N.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Wu, X. F.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. [Barthelmy, S. D.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kawai, N.] Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528551, Japan. [Yoldas, A. Kuepcue] ESO, D-85740 Garching, Germany. [Meszaros, P.] Penn State Univ, Dept Phys, Davey Lab 525, University Pk, PA 16802 USA. [Oates, S. R.; Schady, P.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Toma, K.] Natl Astron Observ Japan, Div Theoret Astron, Mitaka, Tokyo 1818588, Japan. [Aoki, K.; Pyo, T. -S.] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Haiman, Z.] Columbia Univ, Dept Astron, Pupin Phys Labs 1328, New York, NY 10027 USA. [Hartmann, D. H.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. [Jehin, E.] Univ Liege, Inst Astrophys, B-4000 Liege, Belgium. [Levan, A. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Liang, E. W.] Guangxi Univ, Dept Phys, Guangxi 53004, Peoples R China. [Szokoly, G.] Eotvos Lorand Univ, H-1117 Budapest, Hungary. RP Greiner, J (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85740 Garching, Germany. RI Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; Fynbo, Johan/L-8496-2014; Hjorth, Jens/M-5787-2014; Watson, Darach/E-4521-2015; Zhang, Binbin/C-9035-2013; Wu, Xuefeng/G-5316-2015; Rossi, Andrea/N-4674-2015; OI Kruehler, Thomas/0000-0002-8682-2384; Savaglio, Sandra/0000-0003-2354-3238; Fynbo, Johan/0000-0002-8149-8298; Hjorth, Jens/0000-0002-4571-2306; Watson, Darach/0000-0002-4465-8264; Zhang, Binbin/0000-0003-2002-116X; Wu, Xuefeng/0000-0002-6299-1263; Rossi, Andrea/0000-0002-8860-6538; Schulze, Steve/0000-0001-6797-1889; McBreen, Sheila/0000-0002-1477-618X FU XMM-Newton SOC; DFG; EU [MEIF-CT-2006-041363]; Leibniz-Prize [HA 1850/28-1]; European Southern Observatory, Chile [081.A-0135, 081.A-0856, 081.A-0966] FX We are very grateful for the excellent support by the La Silla and Paranal Observatory staff, in particular to Stephane Brillant, Michelle Doherty, Carla Gil, Rachel Gilmour, Swetlana Hubrig, Heidi Korhonen, Chris Lidman, Emanuela Pompei, Julia Scharwachter, and Linda Schmidtobreick. We acknowledge discussions with J. P. Norris, T. Sakamoto, D. Grupe, E. Rol, N. Masetti, and E. Palazzi. We also acknowledge the support of the XMM-Newton SOC and the Project Scientist in scheduling and executing the target-of-opportunity observation. We thank the referee for useful comments, and G. Stratta for providing the SN extinction model template. T. K. acknowledges support by the DFG cluster of excellence 'Origin and Structure of the Universe', A. P. B. from STFC, and P. M. V. from the EU under a Marie Curie Intra-European Fellowship, contract MEIF-CT-2006-041363. Part of the funding for GROND (both hardware as well as personnel) was generously granted from the Leibniz-Prize (DFG grant HA 1850/28-1) to Professor G. Hasinger (MPE). This work is partly based on observations collected at the European Southern Observatory, Chile under ESO proposal Nos. 081.A-0135, 081.A-0856 and 081.A-0966. The Dark Cosmology Centre is funded by the DNRF. NR 107 TC 143 Z9 144 U1 1 U2 16 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 MAR 10 PY 2009 VL 693 IS 2 BP 1610 EP 1620 DI 10.1088/0004-637X/693/2/1610 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 417RR UT WOS:000264095100051 ER PT J AU Hanasoge, SM Duvall, TL AF Hanasoge, Shravan M. Duvall, Thomas L., Jr. TI SUBWAVELENGTH RESOLUTION IMAGING OF THE SOLAR DEEP INTERIOR SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: helioseismology; Sun: interior; Sun: oscillations; waves; hydrodynamics ID TIME-DISTANCE HELIOSEISMOLOGY; MICHELSON DOPPLER IMAGER; COMPUTATIONAL ACOUSTICS; KERNELS; HOLOGRAPHY; TACHOCLINE; SCATTERING; SCHEMES AB We derive expectations for signatures in the measured travel times of waves that interact with thermal anomalies and jets. A series of numerical experiments that involve the dynamic linear evolution of an acoustic wave field in a solarlike stratified spherical shell in the presence of fully three-dimensional time-stationary perturbations are performed. The imprints of these interactions are observed as shifts in wave travel times, which are extracted from these data through methods of time-distance helioseismology (Duvall et al.). In situations where at least one of the spatial dimensions of the scatterer was smaller than a wavelength, oscillatory time shift signals were recovered from the analyses, pointing directly to a means of resolving subwavelength features. As evidence for this claim, we present analyses of simulations with spatially localized jets and sound-speed perturbations. We analyze one year's worth solar observations to estimate the noise level associated with the time differences. Based on theoretical estimates, Fresnel zone time shifts associated with the ( possible) sharp rotation gradient at the base of the convection zone are on the order of 0.01-0.1 s, well below the noise level that could be reached with the currently available amount of data (similar to 0.15 - 0.2 s with 10 yr of data). C1 [Hanasoge, Shravan M.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Duvall, Thomas L., Jr.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. RP Hanasoge, SM (reprint author), Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. EM shravan@stanford.edu RI Duvall, Thomas/C-9998-2012 FU NASA [HMI NAS5-02139] FX The computing was performed on the NASA super-computer Columbia, housed in the Ames research center. S. M. H. acknowledges funding from NASA grant HMI NAS5-02139. NR 27 TC 1 Z9 1 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2009 VL 693 IS 2 BP 1678 EP 1685 DI 10.1088/0004-637X/693/2/1678 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 417RR UT WOS:000264095100058 ER PT J AU Hedman, MM Nicholson, PD Showalter, MR Brown, RH Buratti, BJ Clark, RN AF Hedman, M. M. Nicholson, P. D. Showalter, M. R. Brown, R. H. Buratti, B. J. Clark, R. N. TI SPECTRAL OBSERVATIONS OF THE ENCELADUS PLUME WITH CASSINI-VIMS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: general; techniques: spectroscopic ID SATURNS E-RING; INFRARED OBSERVATIONS; PARTICLE PROPERTIES; SYSTEM; SPECTROMETER; SATELLITES; ATMOSPHERE; SCATTERING; FRACTURES; INTERIOR AB On 2005 November 27 (day 331), the Visual and Infrared Mapping Spectrometer instrument onboard the Cassini spacecraft obtained high signal-to-noise, spatially resolved measurements of Enceladus' particle plume. These data are processed to obtain spectra of the plume at a range of altitudes between 50 and 300 km from the surface. These spectra show that the particulate component of the plume consists primarily of fine-grained water ice. The spectral data are used to derive profiles of particle densities versus height, which are in turn converted into measurements of the velocity distribution of particles launched from the surface between 80 and 160 m s(-1) (that is, between one-third and two-thirds of the escape speed). These calculations indicate that particles with radii of 1 mu m are approximately equally likely to have launch speeds anywhere between 80 and 160 m s(-1), while particles with radii of 2 and 3 mu m have progressively steeper velocity distributions. These findings should constrain models of particle production and acceleration within Enceladus. C1 [Hedman, M. M.; Nicholson, P. D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Showalter, M. R.] SETI Inst, Mountain View, CA 94043 USA. [Brown, R. H.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Buratti, B. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Clark, R. N.] US Geol Survey, Fed Ctr, Denver, CO 80225 USA. RP Hedman, MM (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. FU Cassini project; VIMS team; Cassini Data Analysis Program FX We thank the Cassini project, the VIMS team, and the Cassini Data Analysis Program for their support of this research. NR 32 TC 38 Z9 38 U1 1 U2 16 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2009 VL 693 IS 2 BP 1749 EP 1762 DI 10.1088/0004-637X/693/2/1749 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 417RR UT WOS:000264095100064 ER PT J AU Hearty, T Song, I Kim, S Tinetti, G AF Hearty, Thomas Song, Inseok Kim, Sam Tinetti, Giovanna TI MID-INFRARED PROPERTIES OF DISK AVERAGED OBSERVATIONS OF EARTH WITH AIRS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; Earth ID EXTRASOLAR PLANET; SYNTHETIC SPECTRA; THERMAL EMISSION; DETECTABILITY; ATMOSPHERE; MARS AB We have investigated mid-infrared spectra of Earth obtained by the Atmospheric Infrared Sounder (AIRS) instrument on-board the AQUA spacecraft to explore the characteristics that may someday be observed in extrasolar terrestrial planets. We have used the AIRS infrared (R similar to 1200; 3.75-15.4 mu m) spectra to construct directly observed high-resolution spectra of the only known life bearing planet, Earth. The AIRS spectra are the first such spectra that span the seasons. We investigate the rotational and seasonal spectral variations that would arise due to varying cloud amount and viewing geometry and we explore what signatures may be observable in the mid-infrared by the next generation of telescopes capable of observing extrasolar terrestrial planets. C1 [Hearty, Thomas] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Song, Inseok] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. [Kim, Sam] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Tinetti, Giovanna] UCL, STFC, Dept Phys & Astron, London WC1E 6BT, England. RP Hearty, T (reprint author), NASA, Goddard Space Flight Ctr, Mailstop 610-2, Greenbelt, MD 20771 USA. EM Thomas.J.Hearty@nasa.gov OI Tinetti, Giovanna/0000-0001-6058-6654 FU NASA FX An anonymous referee provided several suggestions which made this paper more relevant to missions aimed at detecting extrasolar terrestrial planets. Conversations with Victoria Meadows helped plan the scope of this research. T. H. wishes to acknowledge Tom Pagano, Moustafa Chahine, and Bjorn Lambrigtsen for support in the early stages of this work and Joel Susskind and Steve Kempler for support in the later stages. John Gieselman provided computer support without which this analysis would not have been possible. Some of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. Some of the results in this paper have been derived using the HEALPix (Gorski et al. 2005) package. NR 22 TC 7 Z9 7 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2009 VL 693 IS 2 BP 1763 EP 1774 DI 10.1088/0004-637X/693/2/1763 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 417RR UT WOS:000264095100065 ER PT J AU Dale, DA Smith, JDT Schlawin, EA Armus, L Buckalew, BA Cohen, SA Helou, G Jarrett, TH Johnson, LC Moustakas, J Murphy, EJ Roussel, H Sheth, K Staudaher, S Bot, C Calzetti, D Engelbracht, CW Gordon, KD Hollenbach, DJ Kennicutt, RC Malhotra, S AF Dale, D. A. Smith, J. D. T. Schlawin, E. A. Armus, L. Buckalew, B. A. Cohen, S. A. Helou, G. Jarrett, T. H. Johnson, L. C. Moustakas, J. Murphy, E. J. Roussel, H. Sheth, K. Staudaher, S. Bot, C. Calzetti, D. Engelbracht, C. W. Gordon, K. D. Hollenbach, D. J. Kennicutt, R. C. Malhotra, S. TI THE SPITZER INFRARED NEARBY GALAXIES SURVEY: A HIGH-RESOLUTION SPECTROSCOPY ANTHOLOGY SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion; disks; galaxies: active; galaxies: jets ID POLYCYCLIC AROMATIC-HYDROCARBON; ACTIVE GALACTIC NUCLEUS; WARM MOLECULAR-HYDROGEN; STAR-FORMING REGIONS; STARBURST GALAXIES; MIDINFRARED SPECTROSCOPY; SPACE-TELESCOPE; LUMINOUS GALAXIES; IRS SPECTROSCOPY; LINE DIAGNOSTICS AB High-resolution mid-infrared spectra are presented for 155 nuclear and extranuclear regions from the Spitzer Infrared Nearby Galaxies Survey (SINGS). The fluxes for nine atomic forbidden and three molecular hydrogen mid-infrared emission lines are also provided, along with upper limits in key lines for infrared-faint targets. The SINGS sample shows a wide range in the ratio of [S III] 18.71 mu m/[S III] 33.48 mu m, but the average ratio of the ensemble indicates a typical interstellar electron density of 300-400 cm(-3) on similar to 23 '' x 15 '' scales and 500-600 cm(-3) using similar to 11 '' x 9 '' apertures, independent of whether the region probed is a star-forming nuclear, a star-forming extranuclear, or an active galactic nuclei (AGN) environment. Evidence is provided that variations in gas-phase metallicity play an important role in driving variations in radiation field hardness, as indicated by [Ne III] 15.56 mu m/[Ne II] 12.81 mu m, for regions powered by star formation. Conversely, the radiation hardness for galaxy nuclei powered by accretion around a massive black hole is independent of metal abundance. Furthermore, for metal-rich environments AGN are distinguishable from star-forming regions by significantly larger [Ne III] 15.56 mu m/[Ne II] 12.81 mu m ratios. Finally, [Fe II] 25.99 mu m/[Ne II] 12.81 mu m versus [Si II] 34.82 mu m/[S III] 33.48 mu m also provides an empirical method for discerning AGN from normal star-forming sources. However, similar to [Ne III] 15.56 mu m/[Ne II] 12.81 mu m, these mid-infrared line ratios lose their AGN/star-formation diagnostic powers for very low metallicity star-forming systems with hard radiation fields. C1 [Dale, D. A.; Schlawin, E. A.; Cohen, S. A.; Johnson, L. C.; Staudaher, S.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Smith, J. D. T.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Armus, L.; Helou, G.; Jarrett, T. H.; Murphy, E. J.; Sheth, K.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91101 USA. [Buckalew, B. A.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA. [Kennicutt, R. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Moustakas, J.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Roussel, H.] Inst Astrophys Paris, F-75014 Paris, France. [Bot, C.] Observ Astron, F-67000 Strasbourg, France. [Calzetti, D.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Engelbracht, C. W.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Gordon, K. D.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Hollenbach, D. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Malhotra, S.] Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA. RP Dale, DA (reprint author), Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. EM ddale@uwyo.edu OI Bot, Caroline/0000-0001-6118-2985; Johnson, Lent/0000-0001-6421-0953 FU NASA [1224769, 1407]; National Science Foundation FX Rajib Ganguly, Brent Groves, and Phil Maloney graciously helped with comparisons of the data to theoretical models. We are grateful for the helpful suggestions provided by the referee. Support for this work, part of the Spitzer Space Telescope Legacy Science Program, was provided by NASA through Contract Number 1224769 issued by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. This research has made use of the NASA/IPAC Extragalactic Database which is operated by JPL/Caltech, under contract with NASA. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 83 TC 51 Z9 51 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2009 VL 693 IS 2 BP 1821 EP 1834 DI 10.1088/0004-637X/693/2/1821 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 417RR UT WOS:000264095100070 ER PT J AU Acciari, VA Aliu, E Arlen, T Beilicke, M Benbow, W Bottcher, M Bradbury, SM Buckley, JH Bugaev, V Butt, Y Byrum, K Cannon, A Celik, O Cesarini, A Chow, YC Ciupik, L Cogan, P Cui, W Daniel, MK Dickherber, R Ergin, T Falcone, A Fegan, SJ Finley, JP Fortin, P Fortson, L Furniss, A Gall, D Gibbs, K Gillanders, GH Godambe, S Grube, J Guenette, R Gyuk, G Hanna, D Hays, E Holder, J Horan, D Hui, CM Humensky, TB Imran, A Kaaret, P Karlsson, N Kertzman, M Kieda, D Kildea, J Konopelko, A Krawczynski, H Krennrich, F Lang, MJ LeBohec, S Maier, G McCann, A McCutcheon, M Millis, J Moriarty, P Mukherjee, R Nagai, T Ong, RA Otte, N Pandel, D Perkins, JS Petry, D Pizlo, F Pohl, M Quinn, J Ragan, K Reyes, LC Reynolds, T Roache, E Rose, HJ Schroedter, M Sembroski, GH Smith, AW Steele, D Swordy, SP Theiling, M Toner, JA Varlotta, A Vassiliev, VV Wagner, RG Wakely, SP Ward, JE Weekes, TC Weinstein, A Williams, DA Wissel, S Wood, M Zitzer, B AF Acciari, V. A. Aliu, E. Arlen, T. Beilicke, M. Benbow, W. Boettcher, M. Bradbury, S. M. Buckley, J. H. Bugaev, V. Butt, Y. Byrum, K. Cannon, A. Celik, O. Cesarini, A. Chow, Y. C. Ciupik, L. Cogan, P. Cui, W. Daniel, M. K. Dickherber, R. Ergin, T. Falcone, A. Fegan, S. J. Finley, J. P. Fortin, P. Fortson, L. Furniss, A. Gall, D. Gibbs, K. Gillanders, G. H. Godambe, S. Grube, J. Guenette, R. Gyuk, G. Hanna, D. Hays, E. Holder, J. Horan, D. Hui, C. M. Humensky, T. B. Imran, A. Kaaret, P. Karlsson, N. Kertzman, M. Kieda, D. Kildea, J. Konopelko, A. Krawczynski, H. Krennrich, F. Lang, M. J. LeBohec, S. Maier, G. McCann, A. McCutcheon, M. Millis, J. Moriarty, P. Mukherjee, R. Nagai, T. Ong, R. A. Otte, N. Pandel, D. Perkins, J. S. Petry, D. Pizlo, F. Pohl, M. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, T. Roache, E. Rose, H. J. Schroedter, M. Sembroski, G. H. Smith, A. W. Steele, D. Swordy, S. P. Theiling, M. Toner, J. A. Varlotta, A. Vassiliev, V. V. Wagner, R. G. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Williams, D. A. Wissel, S. Wood, M. Zitzer, B. TI VERITAS OBSERVATIONS OF A VERY HIGH ENERGY gamma-RAY FLARE FROM THE BLAZAR 3C 66A SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE BL Lacertae objects: individual (3C 66A); galaxies: active; gamma rays: observations ID BL LACERTAE OBJECTS; ATMOSPHERIC CHERENKOV TELESCOPES; X-RAY; EMISSION; 3C-66A; DISCOVERY; RADIATION; ASTRONOMY; OPACITY; ARRAY AB The intermediate-frequency peaked BL Lacertae (IBL) object 3C 66A is detected during 2007-2008 in VHE ( very high energy; E > 100 GeV) gamma rays with the VERITAS stereoscopic array of imaging atmospheric Cherenkov telescopes. An excess of 1791 events is detected, corresponding to a significance of 21.2 standard deviations (sigma), in these observations (32.8 hr live time). The observed integral flux above 200 GeV is 6% of the Crab Nebula's flux and shows evidence for variability on the timescale of days. The measured energy spectrum is characterized by a soft power law with photon index Gamma = 4.1 +/- 0.4(stat) +/- 0.6(sys). The radio galaxy 3C 66B is excluded as a possible source of the VHE emission. C1 [Benbow, W.; Gibbs, K.; Kildea, J.; Perkins, J. S.; Roache, E.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Acciari, V. A.; Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Aliu, E.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Aliu, E.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Arlen, T.; Celik, O.; Chow, Y. C.; Fegan, S. J.; Ong, R. A.; Vassiliev, V. V.; Weinstein, A.; Wood, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Boettcher, M.] Ohio Univ, Dept Phys & Astron, Inst Astrophys, Athens, OH 45701 USA. [Bradbury, S. M.; Daniel, M. K.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Butt, Y.; Ergin, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Byrum, K.; Smith, A. W.; Wagner, R. G.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cannon, A.; Grube, J.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cesarini, A.; Gillanders, G. H.; Lang, M. J.; Toner, J. A.] Natl Univ Ireland, Sch Phys, Galway, Ireland. [Ciupik, L.; Fortson, L.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cogan, P.; Hanna, D.; Maier, G.; McCann, A.; McCutcheon, M.; Ragan, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Cui, W.; Finley, J. P.; Gall, D.; Pizlo, F.; Sembroski, G. H.; Varlotta, A.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Falcone, A.] Penn State Univ, Davey Lab 525, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Fortin, P.; Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Furniss, A.; Otte, N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Furniss, A.; Otte, N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Godambe, S.; Hui, C. M.; Kieda, D.; LeBohec, S.] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. [Hays, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Humensky, T. B.; Swordy, S. P.; Wakely, S. P.; Wissel, S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Imran, A.; Krennrich, F.; Nagai, T.; Pohl, M.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Kaaret, P.; Pandel, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Konopelko, A.] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA. [Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA. [Petry, D.] European So Observ, D-85748 Garching, Germany. [Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Reynolds, T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. RP Perkins, JS (reprint author), Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. EM jperkins@cfa.harvard.edu RI Hays, Elizabeth/D-3257-2012; Daniel, Michael/A-2903-2010; OI Cui, Wei/0000-0002-6324-5772; Daniel, Michael/0000-0002-8053-7910; Cesarini, Andrea/0000-0002-8611-8610; Ward, John E/0000-0003-1973-0794 FU U. S. Department of Energy; U. S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland; STFC in the UK FX This research was supported by grants from the U. S. Department of Energy, the U. S. National Science Foundation and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland, and by STFC in the UK. NR 31 TC 66 Z9 66 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 10 PY 2009 VL 693 IS 2 BP L104 EP L108 DI 10.1088/0004-637X/693/2/L104 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 419CJ UT WOS:000264196400012 ER PT J AU Enoto, T Nakagawa, YE Rea, N Esposito, P Gotz, D Hurley, K Israel, GL Kokubun, M Makishima, K Mereghetti, S Murakami, H Nakazawa, K Sakamoto, T Stella, L Tiengo, A Turolla, R Yamada, S Yamaoka, K Yoshida, A Zane, S AF Enoto, T. Nakagawa, Y. E. Rea, N. Esposito, P. Goetz, D. Hurley, K. Israel, G. L. Kokubun, M. Makishima, K. Mereghetti, S. Murakami, H. Nakazawa, K. Sakamoto, T. Stella, L. Tiengo, A. Turolla, R. Yamada, S. Yamaoka, K. Yoshida, A. Zane, S. TI SUZAKU OBSERVATION OF THE NEW SOFT GAMMA REPEATER SGR 0501+4516 IN OUTBURST SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE pulsars: individual (SGR 0501+4516); stars: magnetic fields; X-rays: stars ID MAGNETIZED NEUTRON-STARS; BOARD SUZAKU; SHORT BURSTS; GIANT FLARE; RAY; SGR-1900+14; SGR-1806-20; HETE-2 AB We present the first Suzaku observation of the new Soft Gamma Repeater, SGR 0501+4516, performed on 2008 August 26, four days after the onset of bursting activity of this new member of the magnetar family. The soft X-ray persistent emission was detected with the X-ray Imaging Spectrometer (XIS) at a 0.5-10 keV flux of 3.8 x 10-(11) erg s(-1) cm(-2), with a spectrum well fitted by an absorbed blackbody plus power-law model. The source pulsation was confirmed at a period of 5.762072 +/- 0.000002 s, and 32 X-ray bursts were detected by the XIS, four of which were also detected at higher energies by the Hard X-ray Detector (HXD). The strongest burst, which occurred at 03:16:16.9 (UTC), was so bright that it caused instrumental saturation, but its precursor phase, lasting for about 200 ms, was detected successfully over the 0.5-200 keV range, with a fluence of similar to 2.1 x 10(-7) erg cm-2 and a peak intensity of about 89 crab. The entire burst fluence is estimated to be similar to 50 times higher. The precursor spectrum was very hard, and well modeled by a combination of two blackbodies. We discuss the bursting activity and X/gamma-ray properties of this newly discovered Soft Gamma Repeater in comparison with other members of the class. C1 [Enoto, T.; Makishima, K.; Nakazawa, K.; Yamada, S.] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. [Nakagawa, Y. E.; Makishima, K.] Inst Phys & Chem Res RIKEN, Cosm Radiat Lab, Wako, Saitama 3510198, Japan. [Rea, N.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Esposito, P.; Mereghetti, S.; Tiengo, A.] INAF Ist Astrofis Spaziale & Fis Cosm Milano, I-20133 Milan, Italy. [Esposito, P.] Ist Nazl Fis Nucl, I-27100 Pavia, Italy. [Goetz, D.] CEA Saclay, DSM Irfu Serv Astrophys, F-91191 Gif Sur Yvette, France. [Hurley, K.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Israel, G. L.; Stella, L.] INAF Astron Observ Rome, I-00040 Monte Porzio Catone, RM, Italy. [Kokubun, M.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Murakami, H.] Rikkyo Univ, Dept Phys, Toshima Ku, Tokyo 1718501, Japan. [Sakamoto, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Turolla, R.] Univ Padua, Dept Phys, I-35131 Padua, Italy. [Turolla, R.; Zane, S.] Univ Coll London, MSSL, Dorking RH5 6NT, Surrey, England. [Yamaoka, K.; Yoshida, A.] Aoyama Gakuin Univ, Dept Math & Phys, Kanagawa 2298558, Japan. RP Enoto, T (reprint author), Univ Tokyo, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan. RI Rea, Nanda/I-2853-2015; XRAY, SUZAKU/A-1808-2009; OI Rea, Nanda/0000-0003-2177-6388; Tiengo, Andrea/0000-0002-6038-1090; MEREGHETTI, SANDRO/0000-0003-3259-7801; Israel, GianLuca/0000-0001-5480-6438; Esposito, Paolo/0000-0003-4849-5092 FU NWO Veni Fellowship; CNES; STFC FX We thank Valentin Pal'shin and Dmitry Frederiks for allowing us to use their Konus-Wind light curve prior to publication. Our thanks are also due to the Suzaku operation team, who successfully conducted the ToO observation. N.R. is supported by an NWO Veni Fellowship, D. G. thanks the CNES for financial support, and S.Z. acknowledges support from STFC. NR 22 TC 31 Z9 31 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 10 PY 2009 VL 693 IS 2 BP L122 EP L126 DI 10.1088/0004-637X/693/2/L122 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 419CJ UT WOS:000264196400016 ER PT J AU Furuzawa, A Ueno, D Hayato, A Ozawa, M Tamagawa, T Bamba, A Hughes, JP Kunieda, H Makishima, K Holt, SS Hwang, U Kinugasa, K Petre, R Tamura, K Tsunemi, H Yamauchi, S AF Furuzawa, Akihiro Ueno, Daisuke Hayato, Asami Ozawa, Midori Tamagawa, Toru Bamba, Aya Hughes, John P. Kunieda, Hideyo Makishima, Kazuo Holt, Stephen S. Hwang, Una Kinugasa, Kenzo Petre, Robert Tamura, Keisuke Tsunemi, Hiroshi Yamauchi, Shigeo TI DOPPLER-BROADENED IRON X-RAY LINES FROM TYCHO'S SUPERNOVA REMNANT SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: individual (Tycho, SN 1572); supernova remnants; X-rays: ISM ID BOARD SUZAKU; EMISSION; SHOCK; EXPANSION; DETECTOR; CHANDRA; WAVE; VLA AB We use Suzaku observations to measure the spatial variation of the Fe K alpha line with radius in the Tycho supernova remnant. The Fe line widths show a significant decrease from a FWHM value of 210 eV at the center to 130 eV at the rim. Over the same radial range the line center energy remains nearly constant. These observations are consistent with a scenario in which the shell of Fe-emitting ejecta in Tycho is expanding at speeds of 2800-3350 km s(-1). The minimum line width we measure is still a factor of two larger than expected from a single component plasma emission model. If thermal Doppler broadening is the dominant additional source of broadening, we infer an ion temperature of (1-3) x 10(10) K. C1 [Furuzawa, Akihiro; Ueno, Daisuke; Kunieda, Hideyo] Nagoya Univ, Grad Sch Sci, Div Particle & Astrophys Sci, Nagoya, Aichi 4648602, Japan. [Hayato, Asami; Tamagawa, Toru; Makishima, Kazuo] RIKEN, Wako, Saitama 3510198, Japan. [Hayato, Asami] Tokyo Univ Sci, Dept Phys, Shinjuku Ku, Tokyo 1628601, Japan. [Ozawa, Midori] Kyoto Univ, Grad Sch Sci, Dept Phys, Sakyo Ku, Kyoto 6068502, Japan. [Bamba, Aya; Tamura, Keisuke] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Makishima, Kazuo] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. [Holt, Stephen S.] FW Olin Coll Engn, Needham, MA 02492 USA. [Hwang, Una; Petre, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kinugasa, Kenzo] Gunma Astron Observ, Takayama, Gunma 3770702, Japan. [Tsunemi, Hiroshi] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Osaka 5600043, Japan. [Yamauchi, Shigeo] Iwate Univ, Fac Humanities & Social Sci, Morioka, Iwate 0208550, Japan. RP Furuzawa, A (reprint author), Nagoya Univ, Grad Sch Sci, Div Particle & Astrophys Sci, Furo Cho, Nagoya, Aichi 4648602, Japan. EM furuzawa@u.phys.nagoya-u.ac.jp RI XRAY, SUZAKU/A-1808-2009 FU NASA [NNG05GP87G]; Japan Society for the Promotion of Science FX We thank all members of the Suzaku team for their careful work operating the satellite and calibrating the instruments. J.P.H. acknowledges support from NASA grant NNG05GP87G. A. H. and M.O. are financially supported by the Japan Society for the Promotion of Science. NR 23 TC 10 Z9 10 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 10 PY 2009 VL 693 IS 2 BP L61 EP L65 DI 10.1088/0004-637X/693/2/L61 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 419CJ UT WOS:000264196400003 ER PT J AU Mason, RE Levenson, NA Shi, Y Packham, C Gorjian, V Cleary, K Rhee, J Werner, M AF Mason, R. E. Levenson, N. A. Shi, Y. Packham, C. Gorjian, V. Cleary, K. Rhee, J. Werner, M. TI THE ORIGIN OF THE SILICATE EMISSION FEATURES IN THE SEYFERT 2 GALAXY NGC 2110 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: individual (NGC 2110); galaxies: Seyfert; infrared: galaxies ID ACTIVE GALACTIC NUCLEI; RESOLVED MIDINFRARED SPECTROSCOPY; ULTRALUMINOUS INFRARED GALAXIES; AGN DUSTY TORI; CIRCINUS GALAXY; SPITZER SPECTRA; CLUMPY TORI; NGC-1068; NGC-2110; QSOS AB The unified model of active galactic nuclei (AGNs) predicts silicate emission features at 10 and 18 mu m in type 1 AGNs, and such features have now been observed in objects ranging from distant quasi-stellar objects to nearby LINERs. More surprising, however, is the detection of silicate emission in a few type 2 AGNs. By combining Gemini and Spitzer mid-infrared imaging and spectroscopy of NGC2110, the closest known Seyfert 2 galaxy with silicate emission features, we can constrain the location of the silicate-emitting region to within 32 pc of the nucleus. This is the strongest constraint yet on the size of the silicate-emitting region in a Seyfert galaxy of any type. While this result is consistent with a narrow-line region origin for the emission, comparison with clumpy torus models demonstrates that emission from an edge-on torus can also explain the silicate emission features and 2-20 mu m spectral energy distribution of this object. In many of the best-fitting models the torus has only a small number of clouds along the line of sight, and does not extend far above the equatorial plane. Extended silicate-emitting regions may well be present in AGNs, but this work establishes that emission from the torus itself is also a viable option for the origin of silicate emission features in active galaxies of both type 1 and type 2. C1 [Mason, R. E.] Gemini Observ, No Operat Ctr, Hilo, HI 96720 USA. [Levenson, N. A.] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. [Shi, Y.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Packham, C.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Gorjian, V.; Cleary, K.; Werner, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rhee, J.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. RP Mason, RE (reprint author), Gemini Observ, No Operat Ctr, 670 N Aohoku Pl, Hilo, HI 96720 USA. EM rmason@gemini.edu OI Levenson, Nancy A./0000-0003-4209-639X FU NSF [0237291]; University of Florida Department of Astronomy FX We thank E. Sturm for providing the spectrum of NGC 3998 and the referee, S. Honig, for a timely and helpful report. Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministrio da Cincia e Tecnologia (Brazil), and SECYT (Argentina). This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. N.A.L. acknowledges work supported by the NSF under grant 0237291 and the hospitality of the University of Florida Department of Astronomy. NR 45 TC 36 Z9 36 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 10 PY 2009 VL 693 IS 2 BP L136 EP L140 DI 10.1088/0004-637X/693/2/L136 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 419CJ UT WOS:000264196400019 ER PT J AU Schmelz, JT Saar, SH DeLuca, EE Golub, L Kashyap, VL Weber, MA Klimchuk, JA AF Schmelz, J. T. Saar, S. H. DeLuca, E. E. Golub, L. Kashyap, V. L. Weber, M. A. Klimchuk, J. A. TI HINODE X-RAY TELESCOPE DETECTION OF HOT EMISSION FROM QUIESCENT ACTIVE REGIONS: A NANOFLARE SIGNATURE? SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: corona; Sun: fundamental parameters; Sun: X-rays, gamma rays ID ATOMIC DATABASE; SOLAR-A; CORONA; ABUNDANCES; MISSION; SULFUR; PLASMA; LINES; RECONSTRUCTION; SPECTRA AB The X-Ray Telescope (XRT) on the Japanese/USA/UK Hinode (Solar-B) spacecraft has detected emission from a quiescent active region core that is consistent with nanoflare heating. The fluxes from 10 broadband X-ray filters and filter combinations were used to construct differential emission measure (DEM) curves. In addition to the expected active region peak at log T = 6.3-6.5, we find a high-temperature component with significant emission measure at log T > 7.0. This emission measure is weak compared to the main peak-the DEM is down by almost three orders of magnitude-which accounts of the fact that it has not been observed with earlier instruments. It is also consistent with spectra of quiescent active regions: no Fe XIX lines are observed in a CHIANTI synthetic spectrum generated using the XRT DEM distribution. The DEM result is successfully reproduced with a simple two-component nanoflare model. C1 [Schmelz, J. T.] Univ Memphis, Dept Phys, Memphis, TN 38152 USA. [Saar, S. H.; DeLuca, E. E.; Golub, L.; Kashyap, V. L.; Weber, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Klimchuk, J. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Schmelz, JT (reprint author), Univ Memphis, Dept Phys, Memphis, TN 38152 USA. EM jschmelz@memphis.edu RI Klimchuk, James/D-1041-2012; DeLuca, Edward/L-7534-2013 OI Klimchuk, James/0000-0003-2255-0305; DeLuca, Edward/0000-0001-7416-2895 FU NASA/SAO; NSF [ATM-0402729] FX This work was inspired by a talk given by Fabio Reale at the 2008 September Hinode-2 Meeting in Boulder, CO. We thank Fabio as well as Paola Testa, John Raymond, and Nancy Brickhouse for helpful discussions. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with ESA and the NSC (Norway). Solar physics research at the University of Memphis is supported by a Hinode subcontract from NASA/SAO as well as NSF ATM-0402729. NR 32 TC 63 Z9 63 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 10 PY 2009 VL 693 IS 2 BP L131 EP L135 DI 10.1088/0004-637X/693/2/L131 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 419CJ UT WOS:000264196400018 ER PT J AU Milkovich, SM Plaut, JJ Safaeinili, A Picardi, G Seu, R Phillips, RJ AF Milkovich, S. M. Plaut, J. J. Safaeinili, A. Picardi, G. Seu, R. Phillips, R. J. TI Stratigraphy of Promethei Lingula, south polar layered deposits, Mars, in radar and imaging data sets SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID ICE SHEETS; SUBSURFACE; MODELS; CORES AB The south polar layered deposits (SPLD) of Mars have been studied through imagery for decades. Now, two subsurface sounding radar instruments have collected data: the Mars Advanced Radar for Subsurface and Ionospheric Sounding (MARSIS) instrument on Mars Express and the Shallow Radar (SHARAD) instrument on Mars Reconnaissance Orbiter are observing the SPLD at multiple frequencies (1.8-5 and 20 MHz, respectively). Both instruments detect subsurface reflections in the Promethei Lingula region of the SPLD. MARSIS detects up to three reflections within Promethei Lingula, in addition to detecting the basal contact between the SPLD and the underlying plains. SHARAD detects 10s of reflections without penetrating to the base of the SPLD. MARSIS reflections likely correlate to the boundaries of packets of reflections in the SHARAD data; whatever change in composition of the SPLD that causes the SHARAD reflections to occur in packets may also be the source of the MARSIS reflections. In several locations, SHARAD reflections can be compared directly with images of layers; an individual reflection corresponds to 3-7 layers in images at resolutions of 6 m/pixel. Reflection surfaces are calculated using the radar observations and extrapolated to the SPLD margins where they are compared to the stratigraphy observed in images. We find that the MARSIS reflections, and thus the packet structure within the SHARAD observations, are likely related to distinctive groups of layers rather than individual layers. The radar data sets allow us to confirm several predictions concerning the interior of the SPLD from stratigraphic studies of images, including that most of the layers extend throughout the region and that they decrease in elevation toward the margin of the SPLD. C1 [Milkovich, S. M.; Plaut, J. J.; Safaeinili, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Phillips, R. J.] SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA. [Picardi, G.; Seu, R.] Univ Roma La Sapienza, INFOCOM Dept, I-00184 Rome, Italy. RP Milkovich, SM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM sarah.m.milkovich@jpl.nasa.gov NR 30 TC 10 Z9 10 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAR 10 PY 2009 VL 114 AR E03002 DI 10.1029/2008JE003162 PG 21 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 419PP UT WOS:000264232000001 ER PT J AU Kar, A Stroscio, MA Dutta, M Kumari, J Meyyappan, M AF Kar, Ayan Stroscio, Michael A. Dutta, Mitra Kumari, Jyoti Meyyappan, M. TI Observation of ultraviolet emission and effect of surface states on the luminescence from tin oxide nanowires SO APPLIED PHYSICS LETTERS LA English DT Article DE binding energy; impurity states; nanowires; photoluminescence; semiconductor materials; semiconductor quantum wires; surface states; tin compounds ID TEMPERATURE-DEPENDENCE; SNO2; PHOTOLUMINESCENCE AB Ultraviolet (UV) and orange emissions have been observed from vapor-liquid-solid grown SnO(2) nanowires. From the luminescence, the donor and acceptor binding energies have been estimated. The dependence of the orange luminescence on the diameters of tin oxide nanowires has been observed and the wavelength of the UV luminescence is found to depend on the laser power. Both the shift in the UV and the intensity of the orange luminescence is found to be dependent on the surface states of the tin oxide nanowires. C1 [Kar, Ayan; Stroscio, Michael A.; Dutta, Mitra] Univ Illinois, Dept Elect & Comp Engn, Chicago, IL 60607 USA. [Stroscio, Michael A.; Dutta, Mitra] Univ Illinois, Dept Phys, Chicago, IL 60607 USA. [Stroscio, Michael A.] Univ Illinois, Dept Bioengn, Chicago, IL 60607 USA. [Kumari, Jyoti; Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Kar, A (reprint author), Univ Illinois, Dept Elect & Comp Engn, Chicago, IL 60607 USA. EM dutta@ece.uic.edu NR 9 TC 40 Z9 41 U1 0 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 MAR 9 PY 2009 VL 94 IS 10 AR 101905 DI 10.1063/1.3097011 PG 3 WC Physics, Applied SC Physics GA 420HO UT WOS:000264280000023 ER PT J AU Liu, JJ Jones, DBA Worden, JR Noone, D Parrington, M Kar, J AF Liu, Jane J. Jones, Dylan B. A. Worden, John R. Noone, David Parrington, Mark Kar, Jay TI Analysis of the summertime buildup of tropospheric ozone abundances over the Middle East and North Africa as observed by the Tropospheric Emission Spectrometer instrument SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MODEL DESCRIPTION; UNITED-STATES; WATER-VAPOR; TRANSPORT; POLLUTION; DISTRIBUTIONS; VARIABILITY; SIMULATION; SATELLITE; CHEMISTRY AB We use the GEOS-Chem chemical transport model to interpret observations of tropospheric ozone from the Tropospheric Emission Spectrometer (TES) satellite instrument in summer 2005. Observations from TES reveal elevated ozone in the middle troposphere (500-400 hPa) across North Africa and the Middle East. Observed ozone abundances in the middle troposphere are at a maximum in summer and a minimum in winter, consistent with the previously predicted summertime "Middle East ozone maximum.'' This summertime enhancement in ozone is associated with the Arabian and Sahara anticyclones, centered over the Zagros and Atlas Mountains, respectively. These anticyclones isolate the middle troposphere over northeast Africa and the Middle East, with westerlies to the north and easterlies to the south, facilitating the buildup of ozone. Over the Middle East, we find that in situ production and transport from Asia provides comparable contributions of 30-35% to the ozone buildup. Over North Africa, in situ production is dominant (at about 20%), with transport from Asia, North America, and equatorial Africa each contributing about 10-15% to the total ozone. We find that although the eastern Mediterranean is characterized by strong descent in the middle and upper troposphere in summer, transport from the boundary layer accounts for about 25% of the local Middle Eastern contribution to the ozone enhancement in the middle troposphere. This upward transport of boundary layer air is associated with orographic lifting along the Zagros Mountains in Iran and the Asir and Hijaz Mountain ranges in Saudi Arabia, and is consistent with TES observations of deuterated water. C1 [Liu, Jane J.; Jones, Dylan B. A.; Parrington, Mark; Kar, Jay] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Noone, David] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA. [Worden, John R.] CALTECH, Jet Prop Lab, Div Earth & Space Sci, Pasadena, CA 91109 USA. RP Liu, JJ (reprint author), Univ Toronto, Dept Phys, 60 St George St, Toronto, ON M5S 1A7, Canada. EM jliu@atmosp.physics.utoronto.ca RI Parrington, Mark/E-7148-2013; Jones, Dylan/O-2475-2014; Chem, GEOS/C-5595-2014 OI Parrington, Mark/0000-0003-4313-6218; Jones, Dylan/0000-0002-1935-3725; FU Natural Sciences and Engineering Research Council of Canada (NSERC); Canadian Foundation for Climate and Atmospheric Sciences; Canadian Space Agency and Environment Canada; National Aeronautics and Space Administration; NASA Atmospheric Chemistry Modeling and Analysis Program; NASA Langley Research Center Atmospheric Science Data Center FX This work was supported by funding from the Natural Sciences and Engineering Research Council of Canada (NSERC) and the Canadian Foundation for Climate and Atmospheric Sciences. Liu thanks additional funds from Canadian Space Agency and Environment Canada. Worden's work was performed at the Jet Propulsion Laboratory, California Institute of Technology under contracts from the National Aeronautics and Space Administration. We are grateful to Mark Lawrence and two anonymous reviewers for their valuable comments. The GEOS-Chem model is managed at Harvard University with support from the NASA Atmospheric Chemistry Modeling and Analysis Program. TES data were obtained from the NASA Langley Research Center Atmospheric Science Data Center. NR 57 TC 39 Z9 39 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAR 7 PY 2009 VL 114 AR D05304 DI 10.1029/2008JD010993 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 415QU UT WOS:000263950200003 ER PT J AU Zhou, XY Smith, EJ AF Zhou, Xiaoyan Smith, Edward J. TI Solar cycle variations of heliospheric magnetic flux SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID CORONAL MASS EJECTIONS; LONG-TERM VARIATION; ULYSSES OBSERVATIONS; FIELD; INTERPLANETARY; MAXIMUM; WIND; SUN AB We extend previous studies of BR, the radial component of the heliospheric magnetic field and a measure of heliospheric magnetic flux, to include the maximum in cycle 23 so that most of 4 cycles are covered. Solar rotation averages reveal that BR systematically increases from a minimum value at sunspot minimum to a maximum value during the declining phase. This increase is interrupted by a temporary decrease associated with the disappearance and reversal of the Sun's polar cap fields. We examine variations in BR and field strength, B, and find a close correspondence consistent with the Parker model when allowance is made for the ever-present fluctuations in the heliospheric magnetic field. The solar cycle variation in BR and B is consistent with the widely accepted model of the solar field in which bipolar sunspot fields emerging at solar maximum are responsible for the erosion and reversal of the polar cap fields. Although the solar cycle change in heliospheric magnetic flux is less than a factor of 2, it is very large compared with the average flux transported into the heliosphere by an interplanetary coronal mass ejection (ICME). If the increases in B and BR at solar maximum are attributed to closed ICME fields, several hundred ICMEs must connect to the Sun for about two solar rotations before disconnecting, consistent with a recent model that attributes the increase in heliospheric flux at solar maximum to ICMEs. Future studies must distinguish between the open and closed topologies in order to evaluate their relative contributions. C1 [Zhou, Xiaoyan; Smith, Edward J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Zhou, XY (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Edward.J.Smith@jpl.nasa.gov; Xiaoyan.Zhou@jpl.nasa.gov NR 36 TC 8 Z9 8 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 MAR 7 PY 2009 VL 114 AR A03106 DI 10.1029/2008JA013421 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 415TE UT WOS:000263957300002 ER PT J AU Wu, SL Duncan, BN Jacob, DJ Fiore, AM Wild, O AF Wu, Shiliang Duncan, Bryan N. Jacob, Daniel J. Fiore, Arlene M. Wild, Oliver TI Chemical nonlinearities in relating intercontinental ozone pollution to anthropogenic emissions SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID UNITED-STATES; ASIAN EMISSIONS; NORTH-AMERICA; TRANSPORT; NOX; SENSITIVITY; EPISODES; HYDROCARBONS; PRECURSORS; EUROPE AB Model studies typically estimate intercontinental influence on surface ozone by perturbing emissions from a source continent and diagnosing the ozone response in the receptor continent. Since the response to perturbations is non-linear due to chemistry, conclusions drawn from different studies may depend on the magnitude of the applied perturbation. We investigate this issue for intercontinental transport between North America, Europe, and Asia with sensitivity simulations in three global chemical transport models. In each region, we decrease anthropogenic emissions of NO(x) and nonmethane volatile organic compounds (NMVOCs) by 20% and 100%. We find strong nonlinearity in the response to NO(x) perturbations outside summer, reflecting transitions in the chemical regime for ozone production. In contrast, we find no significant nonlinearity to NO(x) perturbations in summer or to NMVOC perturbations year-round. The relative benefit of decreasing NO(x) vs. NMVOC from current levels to abate intercontinental pollution increases with the magnitude of emission reductions. Citation: Wu, S., B. N. Duncan, D. J. Jacob, A. M. Fiore, and O. Wild (2009), Chemical nonlinearities in relating intercontinental ozone pollution to anthropogenic emissions, Geophys. Res. Lett., 36, L05806, doi: 10.1029/2008GL036607. C1 [Wu, Shiliang] Michigan Technol Univ, Dept Geol & Min Engn & Sci, Atmospher Sci Program, Houghton, MI 49931 USA. [Wu, Shiliang; Jacob, Daniel J.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02318 USA. [Wu, Shiliang; Jacob, Daniel J.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02318 USA. [Wu, Shiliang] Michigan Technol Univ, Dept Civil & Environm Engn, Houghton, MI 49931 USA. [Duncan, Bryan N.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Greenbelt, MD 20771 USA. [Duncan, Bryan N.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Fiore, Arlene M.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ 08542 USA. [Wild, Oliver] Univ Lancaster, Dept Environm Sci, Lancaster Environm Ctr, Lancaster LA1 4YQ, England. RP Wu, SL (reprint author), Michigan Technol Univ, Dept Geol & Min Engn & Sci, Atmospher Sci Program, 1400 Townsend Dr, Houghton, MI 49931 USA. RI Wild, Oliver/A-4909-2009; Duncan, Bryan/A-5962-2011 OI Wild, Oliver/0000-0002-6227-7035; FU NASA FX This work was supported by the NASA Modeling and Analysis Program. This work was inspired by the HTAP activities. NR 34 TC 34 Z9 35 U1 2 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 5 PY 2009 VL 36 AR L05806 DI 10.1029/2008GL036607 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 415PR UT WOS:000263947000003 ER PT J AU Satheesh, SK Moorthy, KK Babu, SS Vinoj, V Nair, VS Beegum, SN Dutt, CBS Alappattu, DP Kunhikrishnan, PK AF Satheesh, S. K. Moorthy, K. Krishna Babu, S. Suresh Vinoj, V. Nair, Vijayakumar S. Beegum, S. Naseema Dutt, C. B. S. Alappattu, D. P. Kunhikrishnan, P. K. TI Vertical structure and horizontal gradients of aerosol extinction coefficients over coastal India inferred from airborne lidar measurements during the Integrated Campaign for Aerosol, Gases and Radiation Budget (ICARB) field campaign SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OPTICAL-PROPERTIES; ARABIAN SEA; ATLANTIC-OCEAN; PENINSULAR INDIA; NORTH-ATLANTIC; DEPTH; IMPACTS; TRANSPORT; CLIMATE; CLOUDS AB Quantitative estimates of the vertical structure and the spatial gradients of aerosol extinction coefficients have been made from airborne lidar measurements across the coastline into offshore oceanic regions along the east and west coasts of India. The vertical structure revealed the presence of strong, elevated aerosol layers in the altitude region of similar to 2-4 km, well above the atmospheric boundary layer (ABL). Horizontal gradients also showed a vertical structure, being sharp with the e(-1) scaling distance (D-0H) as small as similar to 150 km in the well-mixed regions mostly under the influence of local source effects. Above the ABL, where local effects are subdued, the gradients were much shallower (similar to 600-800 km); nevertheless, they were steep compared to the value of similar to 1500-2500 km reported for columnar AOD during winter. The gradients of these elevated layers were steeper over the east coast of India than over the west coast. Near-simultaneous radio sonde (Vaisala, Inc., Finland) ascents made over the northern Bay of Bengal showed the presence of convectively unstable regions, first from surface to similar to 750-1000 m and the other extending from 1750 to 3000 m separated by a stable region in between. These can act as a conduit for the advection of aerosols and favor the transport of continental aerosols in the higher levels (> 2 km) into the oceans without entering the marine boundary layer below. Large spatial gradient in aerosol optical and hence radiative impacts between the coastal landmass and the adjacent oceans within a short distance of < 300 km (even at an altitude of 3 km) during summer and the premonsoon is of significance to the regional climate. C1 [Satheesh, S. K.; Vinoj, V.] Indian Inst Sci, Ctr Atmospher & Ocean Sci, Bangalore 560012, Karnataka, India. [Dutt, C. B. S.] Indian Space Res Org, Bangalore 560094, Karnataka, India. [Moorthy, K. Krishna; Babu, S. Suresh; Nair, Vijayakumar S.; Beegum, S. Naseema; Alappattu, D. P.; Kunhikrishnan, P. K.] Vikram Sarabhai Space Ctr, Space Phys Lab, Trivandrum 695022, Kerala, India. [Satheesh, S. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Satheesh, SK (reprint author), Indian Inst Sci, Ctr Atmospher & Ocean Sci, Bangalore 560012, Karnataka, India. EM satheesh@caos.iisc.ernet.in RI Vinoj, V./C-3241-2008; Alappattu, Denny/A-3825-2016; OI Vinoj, V./0000-0001-8573-6073; Alappattu, Denny/0000-0002-1432-057X; Moorthy, K. Krishna/0000-0002-7234-3868 FU NASA FX This research work was carried out under the Integrated Campaign for Aerosols, Gases, and Radiation Budget (ICARB) field campaign of ISRO-GBP. The authors thank the Department of Science and Technology, New Delhi, for supporting the Micropulse Lidar (MPL) used in this work. The authors are grateful to K. Radhakrishnan, the then Director of NRSA, the aircraft team (headed by K. Kalyanaraman and V. Raghu Venkataraman), Rasik Ravindra, and M. Sudhakar (for their excellent cooperation and support by providing the research vessel and associated facilities). Part of this research was carried out when one of the authors (S. K. S.) was supported by an appointment at the NASA Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. The authors gratefully acknowledge the NOAA Air Resources Laboratory (ARL) for the provision of the HYSPLIT transport model and NCEP for wind fields used in this paper. NR 44 TC 25 Z9 25 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAR 5 PY 2009 VL 114 AR D05204 DI 10.1029/2008JD011033 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 415QL UT WOS:000263949300004 ER PT J AU Henri, P Briand, C Mangeney, A Bale, SD Califano, F Goetz, K Kaiser, M AF Henri, P. Briand, C. Mangeney, A. Bale, S. D. Califano, F. Goetz, K. Kaiser, M. TI Evidence for wave coupling in type III emissions SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID SOLAR RADIO-BURSTS; LANGMUIR-WAVES; ULYSSES OBSERVATIONS; BICOHERENCE ANALYSIS; WIND; FREQUENCY; PLASMA; TURBULENCE; PACKETS; REGION AB Using new capabilities of waveform analyses provided by the S/WAVES instruments onboard the two STEREO spacecraft, we present for the first time a complete set of direct evidence for three-wave coupling occurring during a type III emission and involving two Langmuir waves and an ion acoustic wave. Information on the Doppler-shifted frequencies and especially the phases of the waves are used in order to check first the conservation of momentum and energy, through Fourier analyses, and second the phase locking between the waves, through bicoherence analyses. Wavelet analyses allow us to resolve for the first time the coupling regions, in which spatial length is estimated to be 18 +/- 5 km. The wave packets travel at comparable speed, and the characteristic available interaction time is about 1 s. Interpretations of the phase coupling and evaluation of the growth rate of the waves tend to favor the parametric decay, at least in the observational events considered in this work. C1 [Henri, P.; Briand, C.; Mangeney, A.; Califano, F.] Univ Paris 06, Univ Paris Diderot, Observ Paris, LESIA,CNRS, F-92190 Meudon, France. [Henri, P.; Califano, F.] Univ Pisa, Dipartimento Fis, Pisa, Italy. [Bale, S. D.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Bale, S. D.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Goetz, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Kaiser, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Henri, P (reprint author), Univ Paris 06, Univ Paris Diderot, Observ Paris, LESIA,CNRS, 5 Pl Jules Hansen, F-92190 Meudon, France. EM pierre.henri@obspm.fr RI Bale, Stuart/E-7533-2011 OI Bale, Stuart/0000-0002-1989-3596 NR 46 TC 38 Z9 38 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 MAR 5 PY 2009 VL 114 AR A03103 DI 10.1029/2008JA013738 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 415SZ UT WOS:000263956800002 ER PT J AU Fielding, EJ Lundgren, PR Burgmann, R Funning, GJ AF Fielding, Eric J. Lundgren, Paul R. Buergmann, Roland Funning, Gareth J. TI Shallow fault-zone dilatancy recovery after the 2003 Bam earthquake in Iran SO NATURE LA English DT Article ID PARKFIELD EARTHQUAKE; GEODETIC DATA; DEFORMATION; DAMAGE; VELOCITY; SLIP; RUPTURE; MOTION; ROCKS AB Earthquakes radiate from slip on discrete faults, but also commonly involve distributed deformation within a broader fault zone, especially near the surface. Variations in rock strain during an earthquake are caused by heterogeneity in the elastic stress before the earthquake, by variable material properties and geometry of the fault zones, and by dynamic processes during the rupture(1,2). Stress changes due to the earthquake slip, both dynamic and static, have long been thought to cause dilatancy in the fault zone that recovers after the earthquake(3-5). Decreases in the velocity of seismic waves passing through the fault zone due to coseismic dilatancy have been observed(6) followed by postseismic seismic velocity increases during healing(5,7,8). Dilatancy and its recovery have not previously been observed geodetically. Here we use interferometric analysis of synthetic aperture radar images to measure postseismic surface deformation after the 2003 Bam, Iran, earthquake and show reversal of coseismic dilatancy in the shallow fault zone that causes subsidence of the surface. This compaction of the fault zone is directly above the patch of greatest coseismic slip at depth. The dilatancy and compaction probably reflects distributed shear and damage to the material during the earthquake that heals afterwards. Coseismic and postseismic deformation spread through a fault zone volume may resolve the paradox of shallow slip deficits for some strike-slip fault ruptures(9). C1 [Fielding, Eric J.; Lundgren, Paul R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Buergmann, Roland] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. [Funning, Gareth J.] Univ Calif Riverside, Dept Earth Sci, Riverside, CA 92521 USA. RP Fielding, EJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Eric.J.Fielding@jpl.nasa.gov RI Funning, Gareth/F-6926-2011; OI Fielding, Eric/0000-0002-6648-8067; Funning, Gareth/0000-0002-8247-0545 FU AOE [668] FX Envisat data are copyright 2004-07 European Space Agency and were provided under AOE project 668. We thank R. Lohman for the use of data resampling programs and discussions. We thank J. Jackson, M. Talebian, D. McKenzie, J.- P. Avouac, Z. Liu, Z. H. Li, E. Cochran, F. Horowitz, G. Peltzer, Y. Ben-Zion and E. Hearn for discussions. Part of this research was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 29 TC 48 Z9 49 U1 0 U2 14 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 MAR 5 PY 2009 VL 458 IS 7234 BP 64 EP 68 DI 10.1038/nature07817 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 414AJ UT WOS:000263836000033 PM 19262670 ER PT J AU Gao, F Masek, JG Wolfe, RE AF Gao, Feng Masek, Jeffrey G. Wolfe, Robert E. TI Automated registration and orthorectification package for Landsat and Landsat-like data processing SO JOURNAL OF APPLIED REMOTE SENSING LA English DT Article DE orthorectification; precise registration; projection; Landsat; ASTER ID IMAGE REGISTRATION; COVER AB Precise registration and orthorectification of remote sensing images are the basic processes for quantitative remote sensing applications, especially for multi-temporal image analysis. In this paper, we present an automated precise registration and orthorectification package (AROP) for Landsat and Landsat-like data processing. The Landsat and Landsat-like satellite images acquired from different sensors at different spatial resolutions and projections can be re-projected, co-registered, and orthorectified to the same projection, geographic extent, and spatial resolution using a common base image through a combined resampling strategy; this allows us to perform multi-temporal image analysis directly. This paper presents and tests the AROP package on Landsat and Landsat-like data. The package is now freely available from our research web site. C1 [Gao, Feng] Earth Resources Technol Inc, Annapolis Jct, MD 20701 USA. [Gao, Feng; Masek, Jeffrey G.; Wolfe, Robert E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gao, F (reprint author), Earth Resources Technol Inc, 10810 Guilford Rd, Annapolis Jct, MD 20701 USA. RI Gao, Feng/F-3944-2010; Masek, Jeffrey/D-7673-2012; Wolfe, Robert/E-1485-2012 OI Wolfe, Robert/0000-0002-0915-1855 FU US geological survey (USGS); NASA FX This work was supported by the US geological survey (USGS) Landsat Science Team project, the NASA LDCM data blender project, the NASA ACCESS LC-ComPS project, and the NASA EOS project. The authors would like to thank Dr. Dan Slayback, Dr. Chengquan Huang, and Mr. Teng-Kui Lim for their feedback and suggestions while testing and running the AROP package. NR 14 TC 33 Z9 42 U1 1 U2 20 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 1931-3195 J9 J APPL REMOTE SENS JI J. Appl. Remote Sens. PD MAR 4 PY 2009 VL 3 AR 033515 DI 10.1117/1.3104620 PG 20 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 520SR UT WOS:000271868800001 ER PT J AU Holmes, TRH Kooi, H De Jeu, RAM Owe, M AF Holmes, T. R. H. Kooi, H. De Jeu, R. A. M. Owe, M. TI Reply to comment by J. Wang and R. L. Bras on "Estimating the soil temperature profile from a single depth observation: A simple empirical heatflow solution" SO WATER RESOURCES RESEARCH LA English DT Editorial Material C1 [Holmes, T. R. H.; Kooi, H.; De Jeu, R. A. M.] Vrije Univ Amsterdam, Dept Geoenvironm Sci, NL-1080 HV Amsterdam, Netherlands. [Owe, M.] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. RP Holmes, TRH (reprint author), Vrije Univ Amsterdam, Dept Geoenvironm Sci, De Boelelaan 1085, NL-1080 HV Amsterdam, Netherlands. EM thomas.holmes@falw.vu.nl RI Holmes, Thomas/F-4512-2010 OI Holmes, Thomas/0000-0002-4651-0079 NR 2 TC 0 Z9 0 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 J9 WATER RESOUR RES JI Water Resour. Res. PD MAR 4 PY 2009 VL 45 AR W03602 DI 10.1029/2008WR007513 PG 3 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 415UC UT WOS:000263960100003 ER PT J AU Kara, AB Wallcraft, AJ Hurlburt, HE Loh, WY AF Kara, A. B. Wallcraft, A. J. Hurlburt, H. E. Loh, W. -Y. TI Which surface atmospheric variable drives the seasonal cycle of sea surface temperature over the global ocean? SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID WATER TURBIDITY; MIXED-LAYER; MODEL; CLIMATOLOGY; SIMULATIONS; VARIABILITY; ANOMALIES; SST; SENSITIVITY; IMPACT AB The impact of near-surface atmospheric variables used in driving the seasonal cycle of climatological mean sea surface temperature (SST) is quantified over the global ocean. The six atmospheric variables are air temperature, vapor mixing ratio, wind speed, precipitation, net shortwave radiation, and net longwave radiation, the first (last) three just above (at) the sea surface. Atmospherically forced ocean general circulation model (OGCM) simulations with no data assimilation are performed using monthly and annual means of those variables under the assumption that variations in climatological monthly SSTs are driven by atmospheric variables. SSTs resulting from these simulations are compared with those from a satellite-based field to determine the impact of each atmospheric variable. Large spatial variability is found in the order of impact (most to least) of six atmospheric variables. In general, the SST seasonal cycle is driven primarily by shortwave radiation at midlatitudes, but wind speed is the major controlling variable in the Indian Ocean. Precipitation has almost no significant influence on monthly SST. Overall, shortwave radiation is the most influential variable controlling the seasonal cycle of SST over 34.3% of the global ocean. Wind speed is the second most important variable (27.2%). In tropical regions and the Arabian Sea, sources other than the atmospheric thermal forcing are found to play a significant role in regulating the SST seasonal cycle. C1 [Kara, A. B.; Wallcraft, A. J.; Hurlburt, H. E.] USN, Res Lab, Stennis Space Ctr, Div Oceanog, Mississippi State, MS 39529 USA. [Loh, W. -Y.] Univ Wisconsin, Dept Stat, Madison, WI 53706 USA. RP Kara, AB (reprint author), USN, Res Lab, Stennis Space Ctr, Div Oceanog, Code 7320,Bldg 1009, Mississippi State, MS 39529 USA. EM birol.kara@nrlssc.navy.mil FU U. S. Army Research Laboratory; U. S. Army Research Office [W911NF-05-1-0047]; Department of Defense High Performance Computing Modernization Program; United States Army Engineer Research and Development Center (ERDC) [NRL/JA/7320/08/8168] FX Appreciation is extended to anonymous reviewers whose helpful comments improved the quality of this paper. This work was funded by the Office of Naval Research (ONR) under the 6.1 project, Global Remote Littoral Forcing via Deep Water Pathways, and the project U. S. GODAE: global ocean prediction with the Hybrid Coordinate Ocean Model (HYCOM) funded under the National Ocean Partnership Program. Wei-Yin Loh's research was partially supported by the U. S. Army Research Laboratory and the U. S. Army Research Office under grant W911NF-05-1-0047. HYCOM simulations were performed under the Department of Defense High Performance Computing Modernization Program on an IBM SP POWER3 and on an HP/COMPAQ SC45 at the United States Army Engineer Research and Development Center (ERDC), Vicksburg, MS. The paper is contribution NRL/JA/7320/08/8168 and has been approved for public release. NR 26 TC 2 Z9 2 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAR 3 PY 2009 VL 114 AR D05101 DI 10.1029/2008JD010420 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 415QG UT WOS:000263948800002 ER PT J AU Gopalswamy, N AF Gopalswamy, N. TI Introduction to special section on Large Geomagnetic Storms SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Editorial Material AB Solar cycle 23 witnessed the accumulation of rich data sets that reveal various aspects of geomagnetic storms in unprecedented detail both at the Sun where the storm-causing disturbances originate and in geospace where the effects of the storms are directly felt. During two recent coordinated data analysis workshops (CDAWs) the large geomagnetic storms (D-st <= -100 nT) of solar cycle 23 were studied in order to understand their solar, interplanetary, and geospace connections. This special section grew out of these CDAWs with additional contributions relevant to these storms. Here I provide a brief summary of the results presented in the special section. C1 NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Bldg 21,Room 26,Code 695, Greenbelt, MD 20771 USA. RI Gopalswamy, Nat/D-3659-2012 NR 25 TC 1 Z9 1 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAR 3 PY 2009 VL 114 AR A00A00 DI 10.1029/2008JA014026 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 415SW UT WOS:000263956400005 ER PT J AU Strong, KT Saba, JLR AF Strong, Keith T. Saba, Julia L. R. TI A new approach to solar cycle forecasting SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Space weather prediction; Solar cycle; Magnetic fields AB We describe a novel approach for determining the timing of the solar cycle and tracking its evolution relative to other cycles. This method also has predictive capability for forecasting the cycle "onset." Based on current trends, we expect that Cycle 23 will be about I year longer than the previous two cycles. (C) 2009 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Strong, Keith T.] SP Syst, Bowie, MD 20721 USA. [Strong, Keith T.; Saba, Julia L. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Saba, Julia L. R.] Lockheed Martin Adv Technol Ctr, Palo Alto, CA 94304 USA. RP Strong, KT (reprint author), SP Syst, 12310 Longwater Dr, Bowie, MD 20721 USA. EM drkts@aol.com; julia.saba@nasa.gov FU NASA [NNX07AK36G] FX The authors would like to thank the Lockheed Martin Advanced Technology Center IRAD program for supporting the early stages of this work and the NASA Goddard Space Flight Center for providing the facilities to continue the study. Dr. Saba also acknowledges the SOHO MDI contract (NASA Grant NNX07AK36G) for partial support of the MDI data analysis. NR 9 TC 2 Z9 2 U1 0 U2 0 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 MAR 2 PY 2009 VL 43 IS 5 BP 756 EP 759 DI 10.1016/j.asr.2008.12.007 PG 4 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 420PL UT WOS:000264301600002 ER PT J AU Xu, YL Horstman, M Krisko, PH Liou, JC Matney, M Stansbery, EG Stokely, CL Whitlock, D AF Xu, Y. -L. Horstman, M. Krisko, P. H. Liou, J. -C. Matney, M. Stansbery, E. G. Stokely, C. L. Whitlock, D. TI Modeling of LEO orbital debris populations for ORDEM2008 SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Orbital debris; Environment; Modeling. Radar data analysis; Inverse problem with positive constrains; Bayesian technique AB The NASA Orbital Debris Engineering Model, ORDEM2000, is in the process of being updated to a new version: ORDEM2008. The data-driven ORDEM covers a spectrum of object size from 10 pm to greater than I m, and ranging from LEO (low Earth orbit) to GEO (geosynchronous orbit) altitude regimes, ORDEM2008 centimeter-sized populations are statistically derived from Haystack and HAX (the Haystack Auxiliary) radar data, while micron-sized populations are estimated from shuttle impact records. Each of the model populations consists of a large number of orbits with specified orbital elements, the number of objects oil each orbit (with corresponding uncertainty), and the size, type, and material assignment for each object. This paper describes the general methodology and procedure commonly used in the statistical inference of the ORDEM2008 LEO debris populations. Major steps in the population derivations include data analysis, reference-population construction, definition of model parameters in terms of reference Populations, linking model parameters with data, seeking best estimates for the model parameters, uncertainty analysis, and assessment of the outcomes. To demonstrate the population-derivation process and to validate the Bayesian statistical model applied in the population derivations throughout, this paper uses illustrative examples for the special cases of large-size (> 1 m, >32 cm, and > 10 cm) populations that are tracked by SSN (the Space Surveillance Network) and also monitored by Haystack and HAX radars operating in a staring mode. (C) 2008 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Xu, Y. -L.; Horstman, M.; Krisko, P. H.; Stokely, C. L.; Whitlock, D.] ESCG, Houston, TX 77058 USA. [Liou, J. -C.; Matney, M.; Stansbery, E. G.] NASA, Lyndon B Johnson Space Ctr, Orbital Debris Program Off, Houston, TX 77058 USA. RP Xu, YL (reprint author), ESCG, Mail Code JE104,2224 Bay Area Blvd, Houston, TX 77058 USA. EM yu-lin.xu-l@nasa.gov NR 26 TC 6 Z9 6 U1 0 U2 5 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 MAR 2 PY 2009 VL 43 IS 5 BP 769 EP 782 DI 10.1016/j.asr.2008.11.023 PG 14 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 420PL UT WOS:000264301600004 ER PT J AU Nguyen, BN Meador, MAB Tousley, ME Shonkwiler, B McCorkle, L Scheiman, DA Palczer, A AF Nguyen, Baochau N. Meador, Mary Ann B. Tousley, Marissa E. Shonkwiler, Brian McCorkle, Linda Scheiman, Daniel A. Palczer, Anna TI Tailoring Elastic Properties of Silica Aerogels Cross-Linked with Polystyrene SO ACS APPLIED MATERIALS & INTERFACES LA English DT Article DE aerogels; polystyrene; cross-linking; mesoporous materials; hybrid materials; elastic recovery ID AMINE-MODIFIED SILICA; MECHANICAL-PROPERTIES AB The effect of incorporating an organic linking group, 1,6-bis(trimethoxysilyl)hexane (BTMSH), into the underlying silica structure of a styrene cross-linked silica aerogel is examined. Vinyltrimethoxysilane (VTMS) is used to provide a reactive site on the silica backbone for styrene polymerization. Replacement of up to 88 mol % of the silicon from tetramethoxyorthosilicate with silicon derived from BTMSH and VTMS during the making of silica gels improves the elastic behavior in some formulations of the crosslinked aerogels, as evidenced by measurement of the recovered length after compression of samples to 25 % strain. This is especially true for some higher density formulations, which recover nearly 100 % of their length after compression to 25 % strain twice. The compressive modulus of the more elastic monoliths ranged from 0.2 to 3 MPa. Although some of these monoliths had greatly reduced surface areas, changing the solvent used to produce the gels from methanol to ethanol increased the surface area in one instance from 6 to 220 m(2)/g with little affect on the modulus, elastic recovery, porosity, or density. C1 [Nguyen, Baochau N.; McCorkle, Linda] Ohio Aerosp Inst, Brookpark, OH 44142 USA. [Meador, Mary Ann B.; Palczer, Anna] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Nguyen, BN (reprint author), Ohio Aerosp Inst, 22800 Cedar Point Rd, Brookpark, OH 44142 USA. EM Baochau.n.nguyen@nasa.gov; maryann.meador@nasa.gov OI Meador, Mary Ann/0000-0003-2513-7372 FU NASA's Fundamental Aeronautics Program FX Financial support from NASA's Fundamental Aeronautics Program is gratefully acknowledged. NR 16 TC 56 Z9 61 U1 6 U2 75 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1944-8244 J9 ACS APPL MATER INTER JI ACS Appl. Mater. Interfaces PD MAR PY 2009 VL 1 IS 3 BP 621 EP 630 DI 10.1021/am8001617 PG 10 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Science & Technology - Other Topics; Materials Science GA 464VL UT WOS:000267535900015 PM 20355984 ER PT J AU Gustavsson, JPR Denning, KC Segal, C Dorney, DJ AF Gustavsson, Jonas P. R. Denning, Kyle C. Segal, Corin Dorney, Daniel J. TI Incipient Cavitation Studied Under Strong Thermodynamic Effect SO AIAA JOURNAL LA English DT Article AB Incipient cavitation was studied under simulated cryogenic conditions on a NACA0015 hydrofoil in a tunnel filled with the perfluorinated ketone 2-trifluoromethyl-1, 1, 1, 2, 4, 4, 5, 5, 5-nonafluoro-3-pentlanone. Through pressure measurements on the hydrofoil, laser-illuminated high-speed photography, and flash-illuminated photography, the extent of cavitation and the characteristic frequencies of its oscillation were studied under varying speeds in the range of 1.7-6.7 m/s and several angles of attack. The results presented in this paper are limited to a 5.1-degree angle of attack. It was found that the vapor formation was much stronger in fluoroketone than in cold-water tests at similar cavitation numbers. The formed bubbles were significantly smaller and there existed an extended speed range over which fluctuation amplitudes grew with no well-defined frequency peaks, as was observed in water. C1 [Gustavsson, Jonas P. R.; Denning, Kyle C.; Segal, Corin] Univ Florida, Gainesville, FL 32611 USA. [Dorney, Daniel J.] NASA, George C Marshall Space Flight Ctr, Appl Fluid Dynam Anal Grp, Huntsville, AL 35801 USA. RP Gustavsson, JPR (reprint author), Univ Florida, Gainesville, FL 32611 USA. FU NASA Constellation University Institute Project FX This work has been supported by NASA Constellation University Institute Project. We thank Claudia Meyer, Program Manager, for her Support. NR 18 TC 3 Z9 3 U1 0 U2 8 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD MAR PY 2009 VL 47 IS 3 BP 710 EP 716 DI 10.2514/1.38987 PG 7 WC Engineering, Aerospace SC Engineering GA 414YS UT WOS:000263901700022 ER PT J AU Vickerman, MB Keith, PA Mckay, TL Gedeon, DJ Watanabe, M Montano, M Karunamuni, G Kaiser, PK Sears, JE Ebrahem, Q Ribita, D Hylton, AG Parsons-Wingerter, P AF Vickerman, Mary B. Keith, Patricia A. McKay, Terri L. Gedeon, Dan J. Watanabe, Michiko Montano, Monica Karunamuni, Ganga Kaiser, Peter K. Sears, Jonathan E. Ebrahem, Quteba Ribita, Daniela Hylton, Alan G. Parsons-Wingerter, Patricia TI VESGEN 2D: Automated, User-Interactive Software for Quantification and Mapping of Angiogenic and Lymphangiogenic Trees and Networks SO ANATOMICAL RECORD-ADVANCES IN INTEGRATIVE ANATOMY AND EVOLUTIONARY BIOLOGY LA English DT Article DE angiogenesis; lymphangiogenesis; VESGEN; retina; neovascularization; NPDR; coronary vascular development; vascular complexity; VEGF; fractal; chorioallantoic membrane; CAM; quail; avian; triamcinolone acetonide ID TRIAMCINOLONE ACETONIDE INJECTION; QUAIL CHORIOALLANTOIC MEMBRANE; INTRAVITREAL TRIAMCINOLONE; VESSEL DIAMETER; BLOOD-VESSELS; MORPHOMETRY; INHIBITION; DECREASE; SYSTEM; SWITCH AB Quantification of microvascular remodeling as a meaningful discovery tool requires mapping and measurement of site-specific changes within vascular trees and networks. Vessel density and other critical vascular parameters are often modulated by molecular regulators as determined by local vascular architecture. For example, enlargement of vessel diameter by vascular endothelial growth factor (VEGF) is restricted to specific generations of vessel branching (Parsons-Wingerter et al., Microvascular Research72: 91, 2006). The averaging of vessel diameter over many successively smaller generations is therefore not particularly useful. The newly automated, user-interactive software VESsel GENeration Analysis (VESGEN) quantifies major vessel parameters within two-dimensional (21)) vascular trees, networks, and tree-network composites. This report reviews application of VESGEN 2D to angiogenic and lymphangiogenic tissues that includes the human and murine retina, embryonic coronary vessels, and avian chorioallantoic membrane. Software output includes colorized image maps with quantification of local vessel diameter, fractal dimension, tortuosity, and avascular spacing. The density of parameters such as vessel area, length, number, and branch point are quantified according to site-specific generational branching within vascular trees. The sole user input requirement is a binary (black/white) vascular image. Future applications of VESGEN will include analysis of 3D vascular architecture and bioinformatic dimensions such as blood flow and receptor localization. Branching analysis by VESGEN has demonstrated that numerous regulators including VEGF(165), basic fibroblast growth factor, transforming growth factor beta-1, angiostatin and the clinical steroid triamcinolone acetonide induce 'fingerprint' or 'signature' changes in vascular patterning that provide unique readouts of dominant molecular signaling. Anat Rec, 292:320-332, 2009. (C) 2009 Wiley-Liss, Inc. C1 [Vickerman, Mary B.; Keith, Patricia A.; McKay, Terri L.; Gedeon, Dan J.; Ribita, Daniela; Hylton, Alan G.; Parsons-Wingerter, Patricia] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Watanabe, Michiko; Karunamuni, Ganga] Case Western Reserve Univ, Sch Med, Dept Anat, Cleveland, OH USA. [Watanabe, Michiko] Case Western Reserve Univ, Sch Med, Dept Pediat Cardiol, Cleveland, OH USA. [Montano, Monica] Case Western Reserve Univ, Sch Med, Dept Pharmacol, Cleveland, OH 44106 USA. [Kaiser, Peter K.; Sears, Jonathan E.; Ebrahem, Quteba] Cleveland Clin Fdn, Cole Eye Inst, Cleveland, OH 44195 USA. RP Parsons-Wingerter, P (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,MS 110-3, Cleveland, OH 44135 USA. EM patricia.a.parsons-wingerten@nasa.gov FU NASA [IRD04-54]; NIH [EY017528, EY017529, K12HD049091, HL65314, HL0775436, HL083048, ES013507, CA92440] FX Grant sponsor: NASA; Grant number: IRD04-54; Grant sponsor: NIH; Grant numbers: EY017528, EY017529, K12HD049091, HL65314, HL0775436, HL083048, ES013507 and CA92440. NR 25 TC 28 Z9 28 U1 0 U2 2 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 1932-8486 J9 ANAT REC JI Anat. Rec. PD MAR PY 2009 VL 292 IS 3 BP 320 EP 332 DI 10.1002/ar.20862 PG 13 WC Anatomy & Morphology SC Anatomy & Morphology GA 416CS UT WOS:000263983400003 PM 19248164 ER PT J AU Bridle, S Shawe-Taylor, J Amara, A Applegate, D Balan, ST Berge, J Bernstein, G Dahle, H Erben, T Gill, M Heavens, A Heymans, C High, FW Hoekstra, H Jarvis, M Kirk, D Kitching, T Kneib, JP Kuijken, K Lagatutta, D Mandelbaum, R Massey, R Mellier, Y Moghaddam, B Moudden, Y Nakajima, R Paulin-Henriksson, S Pires, S Rassat, A Refregier, A Rhodes, J Schrabback, T Semboloni, E Shmakova, M Van Waerbeke, L Witherick, D Voigt, L Wittman, D AF Bridle, Sarah Shawe-Taylor, John Amara, Adam Applegate, Douglas Balan, Sreekumar T. Berge, Joel Bernstein, Gary Dahle, Hakon Erben, Thomas Gill, Mandeep Heavens, Alan Heymans, Catherine High, F. William Hoekstra, Henk Jarvis, Mike Kirk, Donnacha Kitching, Thomas Kneib, Jean-Paul Kuijken, Konrad Lagatutta, David Mandelbaum, Rachel Massey, Richard Mellier, Yannick Moghaddam, Baback Moudden, Yassir Nakajima, Reiko Paulin-Henriksson, Stephane Pires, Sandrine Rassat, Anais Refregier, Alexandre Rhodes, Jason Schrabback, Tim Semboloni, Elisabetta Shmakova, Marina Van Waerbeke, Ludovic Witherick, Dugan Voigt, Lisa Wittman, David TI HANDBOOK FOR THE GREAT08 CHALLENGE: AN IMAGE ANALYSIS COMPETITION FOR COSMOLOGICAL LENSING SO ANNALS OF APPLIED STATISTICS LA English DT Article DE Inference; inverse problems; astronomy ID WEAK GRAVITATIONAL SHEAR; LARGE-SCALE STRUCTURE; NONLINEAR CLUSTER INVERSION; GALAXY SHAPE MEASUREMENT; DARK-MATTER; SYSTEMATIC-ERRORS; POLAR SHAPELETS; COSMIC SHEAR; DISTORTIONS; CALIBRATION AB The GRavitational lEnsing Accuracy Testing 2008 (GREAT08) Challenge focuses on a problem that is of crucial importance for future observations in cosmology. The shapes of distant galaxies can be used to determine the properties of dark energy and the nature of gravity, because light from those galaxies is bent by gravity from the intervening dark matter. The observed galaxy images appear distorted, although only slightly, and their shapes must be precisely disentangled from the effects of pixelisation, convolution and noise. The worldwide gravitational lensing community has made significant progress in techniques to measure these distortions via the Shear TEsting Program (STEP). Via STEP, we have run challenges within our own community, and come to recognise that this particular image analysis problem is ideally matched to experts in statistical inference, inverse problems and computational learning. Thus, in order to continue the progress seen in recent years, we are seeking an infusion of new ideas from these communities. This document details the GREAT08 Challenge for potential participants. Please visit www.great08challenge.info for the latest information. C1 [Bridle, Sarah; Shawe-Taylor, John; Balan, Sreekumar T.; Kirk, Donnacha; Witherick, Dugan; Voigt, Lisa] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Amara, Adam] Univ Hong Kong, Hong Kong, Hong Kong, Peoples R China. [Applegate, Douglas; Shmakova, Marina] Stanford Linear Accelerator Ctr, Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Berge, Joel; Moghaddam, Baback; Rhodes, Jason] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Berge, Joel; Massey, Richard; Moghaddam, Baback; Rhodes, Jason] CALTECH, Pasadena, CA 91125 USA. [Bernstein, Gary; Jarvis, Mike; Nakajima, Reiko] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Erben, Thomas; Semboloni, Elisabetta] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Heavens, Alan] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [High, F. William] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kitching, Thomas] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Berge, Joel; Moudden, Yassir; Paulin-Henriksson, Stephane; Pires, Sandrine; Rassat, Anais; Refregier, Alexandre] SAp CEA Saclay, Commissariat Energie Atom, F-91191 Gif Sur Yvette, France. [Dahle, Hakon; Kneib, Jean-Paul] Observ Astron Marseille Prov, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Gill, Mandeep] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Heymans, Catherine; Van Waerbeke, Ludovic] Univ British Columbia, Vancouver, BC V6T 1Z4, Canada. [Hoekstra, Henk] Univ Victoria, Victoria, BC V8W 2Y2, Canada. [Kuijken, Konrad; Schrabback, Tim] Leiden Univ, Leiden Observ, Huygens Lab, NL-2333 CA Leiden, Netherlands. [Lagatutta, David; Wittman, David] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Mandelbaum, Rachel] Inst Adv Study, Princeton, NJ 08540 USA. [Heymans, Catherine; Mellier, Yannick] Inst Astrophys Paris, F-75014 Paris, France. RP Bridle, S (reprint author), UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. EM sarah.bridle@ucl.ac.uk RI Witherick, Dugan/C-9403-2014; Mandelbaum, Rachel/N-8955-2014; Kneib, Jean-Paul/A-7919-2015; OI Witherick, Dugan/0000-0002-9175-0151; Mandelbaum, Rachel/0000-0003-2271-1527; Kneib, Jean-Paul/0000-0002-4616-4989; Wittman, David/0000-0002-0813-5888; Rassat, Anais/0000-0002-5476-6461; Hoekstra, Henk/0000-0002-0641-3231 FU Royal Society; European Commission; NASA FX Supported in part by the Jet Propulsion Laboratory, which is run by Caltech under a contract from NASA. NR 53 TC 61 Z9 61 U1 0 U2 2 PU INST MATHEMATICAL STATISTICS PI CLEVELAND PA 3163 SOMERSET DR, CLEVELAND, OH 44122 USA SN 1932-6157 J9 ANN APPL STAT JI Ann. Appl. Stat. PD MAR PY 2009 VL 3 IS 1 BP 6 EP 37 DI 10.1214/08-AOAS222 PG 32 WC Statistics & Probability SC Mathematics GA 522EA UT WOS:000271979400002 ER PT J AU Davies, PCW Benner, SA Cleland, CE Lineweaver, CH Mckay, CP Wolfe-Simon, F AF Davies, Paul C. W. Benner, Steven A. Cleland, Carol E. Lineweaver, Charles H. McKay, Christopher P. Wolfe-Simon, Felisa TI Signatures of a Shadow Biosphere SO ASTROBIOLOGY LA English DT Article DE Weird life; Multiple origins of life; Biogenesis; Biomarkers; Extremophiles; Alternative biochemistry ID MICROBIAL DIVERSITY; DEEP-SEA; LIFE; PHOTOSYNTHESIS; CHEMISTRY; SEDIMENTS; ARCHAEA; DESERT; EARTH; MARS AB Astrobiologists are aware that extraterrestrial life might differ from known life, and considerable thought has been given to possible signatures associated with weird forms of life on other planets. So far, however, very little attention has been paid to the possibility that our own planet might also host communities of weird life. If life arises readily in Earth-like conditions, as many astrobiologists contend, then it may well have formed many times on Earth itself, which raises the question whether one or more shadow biospheres have existed in the past or still exist today. In this paper, we discuss possible signatures of weird life and outline some simple strategies for seeking evidence of a shadow biosphere. C1 [Davies, Paul C. W.] Arizona State Univ, BEYOND Ctr Fundamental Concepts Sci, Tempe, AZ 85287 USA. [Benner, Steven A.] Fdn Appl Mol Evolut, Gainesville, FL USA. [Cleland, Carol E.] Univ Colorado, Dept Philosophy, Boulder, CO 80309 USA. [Cleland, Carol E.] Univ Colorado, Ctr Astrobiol, Boulder, CO 80309 USA. [Lineweaver, Charles H.] Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT, Australia. [Lineweaver, Charles H.] Australian Natl Univ, Res Sch Astron & Astrophys, Planetary Sci Inst, Canberra, ACT, Australia. [McKay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Wolfe-Simon, Felisa] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. RP Davies, PCW (reprint author), Arizona State Univ, BEYOND Ctr Fundamental Concepts Sci, POB 871404, Tempe, AZ 85287 USA. EM paul.davies@asu.edu NR 47 TC 39 Z9 39 U1 5 U2 38 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 MAR PY 2009 VL 9 IS 2 BP 241 EP 249 DI 10.1089/ast.2008.0251 PG 9 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 440NO UT WOS:000265707200008 PM 19292603 ER PT J AU Connelley, MS Hodapp, KW Fuller, GA AF Connelley, Michael S. Hodapp, Klaus W. Fuller, Gary A. TI A PHOTOMETRICALLY AND MORPHOLOGICALLY VARIABLE INFRARED NEBULA IN L483 SO ASTRONOMICAL JOURNAL LA English DT Article DE ISM: individual (L483); ISM: kinematics and dynamics; ISM: structure; reflection nebulae ID YOUNG STELLAR OBJECTS; MCNEILS NEBULA; FILTER SET; OUTFLOW; OUTBURST; CLOUDS; DISKS AB We present narrow and broad K-band observations of the Class 0/I source IRAS 18148-0440 that span 17 years. The infrared nebula associated with this protostar in the L483 dark cloud is both morphologically and photometrically variable on a timescale of only a few months. This nebula appears to be an infrared analog to other well known optically visible variable nebulae associated with young stars, such as Hubble's Variable Nebula. Along with Cepheus A, this is one of the first large variable nebulae to be found that is only visible in the infrared. The variability of this nebula is most likely due to changing illumination of the cloud rather than any motion of the structure in the nebula. Both morphological and photometric changes are observed on a timescale only a few times longer than the light crossing time of the nebula, suggesting very rapid intrinsic changes in the illumination of the nebula. Our narrowband observations also found that H(2) knots are found nearly twice as far to the east of the source as to its west, and that H(2) emission extends farther east of the source than the previously known CO outflow. C1 [Connelley, Michael S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Hodapp, Klaus W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. [Fuller, Gary A.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. RP Connelley, MS (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA. FU National Aeronautics and Space Administration; National Science Foundation; Ames Research Center; Oak Ridge Associated Universities through a contract with NASA FX The authors thank the referee for his/her helpful comments. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This research has made use of NASA's Astrophysics Data System. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research was supported by an appointment to the NASA Postdoctoral Program at the Ames Research Center, administered by the Oak Ridge Associated Universities through a contract with NASA. NR 33 TC 6 Z9 6 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 MAR PY 2009 VL 137 IS 3 BP 3494 EP 3500 DI 10.1088/0004-6256/137/3/3494 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 412IZ UT WOS:000263719800004 ER PT J AU Lister, ML Aller, HD Aller, MF Cohen, MH Homan, DC Kadler, M Kellermann, KI Kovalev, YY Ros, E Savolainen, T Zensus, JA Vermeulen, RC AF Lister, M. L. Aller, H. D. Aller, M. F. Cohen, M. H. Homan, D. C. Kadler, M. Kellermann, K. I. Kovalev, Y. Y. Ros, E. Savolainen, T. Zensus, J. A. Vermeulen, R. C. TI MOJAVE: MONITORING OF JETS IN ACTIVE GALACTIC NUCLEI WITH VLBA EXPERIMENTS. V. MULTI-EPOCH VLBA IMAGES SO ASTRONOMICAL JOURNAL LA English DT Review DE BL Lacertae objects: general; galaxies: active; galaxies: jets; quasars: general; radio continuum: galaxies; surveys ID SPECTRUM RADIO-SOURCES; BL-LACERTAE OBJECTS; DIGITAL SKY SURVEY; OPTICAL-IDENTIFICATION STATUS; COMPACT SYMMETRIC OBJECTS; QUASI-STELLAR OBJECTS; RAY BLAZAR CANDIDATES; BANK 966-MHZ SURVEY; PARSEC-SCALE JET; COMPLETE SAMPLE AB We present images from a long-term program (MOJAVE: Monitoring of Jets in active galactic nuclei (AGNs) with VLBA Experiments) to survey the structure and evolution of parsec-scale jet phenomena associated with bright radio-loud active galaxies in the northern sky. The observations consist of 2424 15 GHz Very Long Baseline Array (VLBA) images of a complete flux-density-limited sample of 135 AGNs above declination - 20 degrees, spanning the period 1994 August to 2007 September. These data were acquired as part of the MOJAVE and 2 cm Survey programs, and from the VLBA archive. The sample-selection criteria are based on multiepoch parsec-scale (VLBA) flux density, and heavily favor highly variable and compact blazars. The sample includes nearly all the most prominent blazars in the northern sky, and is well suited for statistical analysis and comparison with studies at other wavelengths. Our multi-epoch and stacked-epoch images show 94% of the sample to have apparent one-sided jet morphologies, most likely due to the effects of relativistic beaming. Of the remaining sources, five have two-sided parsec-scale jets, and three are effectively unresolved by the VLBA at 15 GHz, with essentially all of the flux density contained within a few tenths of a milliarcsecond. C1 [Lister, M. L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Aller, H. D.; Aller, M. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Cohen, M. H.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Homan, D. C.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Kadler, M.] Univ Erlangen Nurnberg, D-96049 Bamberg, Germany. [Kadler, M.] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany. [Kadler, M.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Kadler, M.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Kellermann, K. I.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Kovalev, Y. Y.; Ros, E.; Savolainen, T.; Zensus, J. A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Kovalev, Y. Y.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [Vermeulen, R. C.] ASTRON, NL-7990 AA Dwingeloo, Netherlands. RP Lister, ML (reprint author), Purdue Univ, Dept Phys, 525 Northwestern Ave, W Lafayette, IN 47907 USA. EM mlister@purdue.edu; haller@umich.edu; mfa@umich.edu; mhc@astro.caltech.edu; homand@denison.edu; matthias.kadler@sternwarte.uni-erlangen.de; kkellerm@nrao.edu; ykovalev@mpifr-bonn.mpg.de; ros@mpifr-bonn.mpg.de; tsavolainen@mpifr-bonn.mpg.de; azensus@mpifr-bonn.mpg.de; rvermeulen@astron.nl RI Kovalev, Yuri/J-5671-2013; OI Kovalev, Yuri/0000-0001-9303-3263; Ros, Eduardo/0000-0001-9503-4892; Savolainen, Tuomas/0000-0001-6214-1085; Kadler, Matthias/0000-0001-5606-6154 FU NSF [AST-0406923, AST0807860]; Purdue Research Foundation; NRAO; Alexander vonHumboldt fellowships at the MPIfR; NASA Postdoctoral Program at the Goddard Space Flight Center; Russian Foundation for Basic Research [01-02-16812, 05-02-17377, 08-02-00545]; Max-Planck-Gesellschaft; Academy of Finland [120516]; National Science Foundation and by funds from the University of Michigan; NASA's Astrophysics Data System; NASA/IPAC Extragalactic Database (NED) FX The authors acknowledge the other members of the MOJAVE team and students who have contributed to this work, including Christian Fromm, Kirill Sokolovsky, and Alexander Pushkarev at MPIfR as well as Andrew Merrill, Nick Mellott, Kevin O'Brien, and Amy Lankey at Purdue University. M. L. L. has been supported under NSF grants AST-0406923 & AST0807860, and a grant from the Purdue Research Foundation. Part of this work was done by M. L. L., D. C. H., and Y.Y.K. during their Jansky fellowships at the NRAO and also by Y. Y. K. and T. S. during their Alexander vonHumboldt fellowships at the MPIfR. M. K. has been supported in part by the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. RATAN-600 observations are partly supported by the Russian Foundation for Basic Research (projects 01-02-16812, 05-02-17377, 08-02-00545). T. S. has been also supported in part by the Max-Planck-Gesellschaft and by the Academy of Finland grant 120516. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research has also made use of the following resources: the University of Michigan Radio Astronomy Observatory, which is supported by the National Science Foundation and by funds from the University of Michigan, NASA's Astrophysics Data System, and the NASA/IPAC Extragalactic Database (NED). The latter is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 139 TC 199 Z9 200 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2009 VL 137 IS 3 BP 3718 EP 3729 DI 10.1088/0004-6256/137/3/3718 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 412IZ UT WOS:000263719800026 ER PT J AU Garcia-Miro, C Moll, E Vazquez, M Kuiper, TBH AF Garcia-Miro, C. Moll, E. Vazquez, M. Kuiper, T. B. H. TI Studies of CSS/GPS sources with the Deep Space Network antennas in Madrid SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT 4th Workshop on Compact Steep Spectrum and Gigahertz-Peaked Spectrum Radio Sources CY MAY 26-29, 2008 CL Riccione, ITALY SP Natl Inst Astrophys, Univ Bologna DE galaxies: compact; instrumentation: detectors; instrumentation: interferometers; radio continuum: galaxies ID DISCOVERY AB This contribution summarizes the antennas and receivers available at the Madrid Deep Space Communication Complex (MDSCC) and outlines the type of observations that can be performed to contribute to the study of the CSS/GPS sources. The last section provides guidelines on how to observe with the DSN antennas, and in particular at MDSCC. (C) 2009 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 [Garcia-Miro, C.; Moll, E.; Vazquez, M.] INTA NASA JPL, E-28008 Madrid, Spain. [Kuiper, T. B. H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Garcia-Miro, C (reprint author), INTA NASA JPL, Madrid Deep Space Commun Complex,Paseo Pintor Ros, E-28008 Madrid, Spain. EM cgmiro@mdscc.nasa.gov NR 3 TC 1 Z9 1 U1 0 U2 2 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PD MAR PY 2009 VL 330 IS 2-3 BP 137 EP 140 DI 10.1002/asna.200811140 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 420RJ UT WOS:000264306600005 ER PT J AU Bianchin, V Foschini, L Ghisellini, G Tagliaferri, G Tavecchio, F Treves, A Di Cocco, G Gliozzi, M Pian, E Sambruna, RM Wolter, A AF Bianchin, V. Foschini, L. Ghisellini, G. Tagliaferri, G. Tavecchio, F. Treves, A. Di Cocco, G. Gliozzi, M. Pian, E. Sambruna, R. M. Wolter, A. TI The changing look of PKS 2149-306 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE quasars: individual: PKS 2149-306; quasars: general; X-rays: galaxies ID RADIO-LOUD QUASARS; ACTIVE GALACTIC NUCLEI; HIGH-REDSHIFT QUASARS; XMM-NEWTON OBSERVATIONS; PHOTON IMAGING CAMERA; X-RAY-SPECTRA; EMISSION-LINE; TELESCOPE; BLAZARS; CATALOG AB Aims. We study the blazar nature of the high-redshift Flat-Spectrum Radio Quasar PKS 2149-306 (z = 2.345) by investigating its long-term behavior. Methods. We analyzed all publicly available optical-to-X-ray observations performed by XMM-Newton, Swift, and INTEGRAL. Results. PKS 2149-306 is one of four blazars at z > 2 that have been observed in the hard-X-ray regime with both the BAT and ISGRI instruments. Observations acquired almost 1 year apart in the 60-300 keV energy band in the object rest frame, exhibit no noticeable change in spectral slope associated with a flux variation of more than a factor of two. Swift data appear to show a roll-off below similar to 1 keV, which becomes increasingly evident during a similar to 3-day time-frame, that can be explained as the natural spectral break caused by the Inverse Compton onset. The broad-band spectra allow us to identify two different states. The SED modeling suggests that they can be interpreted by only a change in the bulk Lorentz factor of the jet. C1 [Bianchin, V.; Foschini, L.; Di Cocco, G.] INAF IASF Bologna, I-40129 Bologna, Italy. [Ghisellini, G.; Tagliaferri, G.; Tavecchio, F.; Wolter, A.] Osserv Astron Brera, INAF, I-23807 Merate, Italy. [Treves, A.] Univ Insubria, Dipartimento Sci, Como, Italy. [Gliozzi, M.] George Mason Univ, Fairfax, VA 22030 USA. [Pian, E.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. [Sambruna, R. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Bianchin, V (reprint author), INAF IASF Bologna, Via Gobetti 101, I-40129 Bologna, Italy. EM bianchin@iasfbo.inaf.it RI Foschini, Luigi/H-3833-2012; OI Foschini, Luigi/0000-0001-8678-0324; Wolter, Anna/0000-0001-5840-9835; Ghisellini, Gabriele/0000-0002-0037-1974; Tagliaferri, Gianpiero/0000-0003-0121-0723; Pian, Elena/0000-0001-8646-4858 FU ASI/INAF [I/088/06/0] FX This research has made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We acknowledge the use of public data from the Swift data archive. We acknowledge partial support from ASI/INAF Contract I/088/06/0. NR 40 TC 6 Z9 6 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 MAR PY 2009 VL 496 IS 2 BP 423 EP 428 DI 10.1051/0004-6361/200811128 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 422CS UT WOS:000264405300014 ER PT J AU Pinilla-Alonso, N Brunetto, R Licandro, J Gil-Hutton, R Roush, TL Strazzulla, G AF Pinilla-Alonso, N. Brunetto, R. Licandro, J. Gil-Hutton, R. Roush, T. L. Strazzulla, G. TI The surface of (136108) Haumea (2003 EL61), the largest carbon-depleted object in the trans-Neptunian belt SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Kuiper Belt; solar system: formation; techniques: spectroscopic; astrochemistry ID NEAR-INFRARED SPECTROSCOPY; KUIPER-BELT; WATER ICE; ION IRRADIATION; OPTICAL-CONSTANTS; 50000 QUAOAR; MU-M; METHANE; TNOS; REFLECTANCE AB Context. Previously known as 2003 EL61, (136108) Haumea, is the largest member of a group of trans-Neptunian objects (TNOs) with similar orbits and "unique" spectral characteristics in the form of a neutral slope in the visible and the deepest water ice absorption bands observed in the trans-Neptunian belt (TNb). Studying the surface of 2003 EL61 provides useful constraints of the origin of this particular group of TNOs and about the outer Solar System's history. Aims. We attempt to study the composition of the surface of 2003 EL61. Methods. We present visible and near-infrared spectra of 2003 EL61 obtained with the 4.2 m WHT and the 3.6 m TNG telescopes at the "Roque de losMuchachos" Observatory (Canary Islands, Spain). Near-infrared spectra were obtained at different rotational phases covering almost one complete rotational period. Spectra are fitted using scattering models based on Hapke theory and constraints on the surface composition are derived. Results. The observations confirm previous results that the 2003 EL61 spectrum is neutral in color and exhibits deep water-ice absorption bands. They also provide new facts about the surface of this object: the lack of significant variations in the spectral slope (in the near-infrared) and the depth of the water-ice absorption bands at different rotational phases clearly evident in the data, suggest that the surface of 2003 EL61 is homogeneous. The scattering models indicate that a 1:1 intimate mixture of crystalline and amorphous water ice is the most probable surface composition of this big TNO, and constrain the presence of other minor constituents to a maximum traction of 8%. Conclusions. The derived composition suggests that: a) cryovolcanism is unlikely to be the resurfacing process that retains the surface of this TNO, and the other members of this population, covered mainly by water ice; b) the surface is older than 10(8) yr which constrains the timescale of any catastrophic event. such as the collision suggested to be the origin of this population, to at least 10(8) yr; c) the surface of 2003 EL61 is depleted of carbon-bearing species. According to the orbital parameters of the population, this implies that is a possible source of carbon-depleted, Jupiter-Family comets. C1 [Pinilla-Alonso, N.] Fdn Galileo Galilei & Telescopio Nazl Galileo, Tenerife, Spain. [Brunetto, R.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Brunetto, R.; Strazzulla, G.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy. [Licandro, J.] Inst Astrofis Canarias, Tenerife 38205, Spain. [Gil-Hutton, R.] San Juan Natl Univ, San Juan, Argentina. [Roush, T. L.] NASA, Ames Res Ctr, Moffett Field, Moffett Field, CA 94035 USA. RP Pinilla-Alonso, N (reprint author), Fdn Galileo Galilei & Telescopio Nazl Galileo, POB 565,38700 S-C de La Palma, Tenerife, Spain. EM npinilla@tng.iac.es NR 44 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 MAR PY 2009 VL 496 IS 2 BP 547 EP 556 DI 10.1051/0004-6361/200809733 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 422CS UT WOS:000264405300027 ER PT J AU Gastaldello, F Buote, DA Temi, P Brighenti, F Mathews, WG Ettori, S AF Gastaldello, Fabio Buote, David A. Temi, Pasquale Brighenti, Fabrizio Mathews, William G. Ettori, Stefano TI X-RAY CAVITIES, FILAMENTS, AND COLD FRONTS IN THE CORE OF THE GALAXY GROUP NGC 5044 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cooling flows; galaxies: clusters: general; galaxies: clusters: individual (NGC 5044); X-rays: galaxies: clusters ID COOLING FLOW CLUSTERS; ACTIVE GALACTIC NUCLEI; DEEP CHANDRA OBSERVATION; AMES ELLIPTIC GALAXIES; XMM-NEWTON; PERSEUS CLUSTER; MOLECULAR GAS; HOT GAS; VORONOI TESSELLATIONS; SPITZER OBSERVATIONS AB We present a two-dimensional analysis of the bright nearby galaxy group NGC 5044 using the currently available Chandra and XMM data. In the inner 10 kpc, a pair of cavities are evident together with a set of bright X-ray filaments. If the cavities are interpreted as gas displaced by relativistic plasma inflated by an active galactic nucleus, even in the absence of extended 1.4 GHz emission, this would be consistent with a recent outburst as also indicated by the extent of dust and H alpha emission. The soft X-ray filaments coincident with H alpha and dust emission are cooler than those which do not correlate with optical and infrared emission. We suggest that dust-aided cooling contributes to form warm (T similar to 10(4) K) gas, emitting Ha radiation. At 31 kpc and 67 kpc, a pair of cold fronts are present, indicative of sloshing due to a dynamical perturbation caused by accretion of a less-massive group, also suggested by the peculiar velocity of the brightest galaxy NGC 5044 with respect to the mean group velocity. C1 [Gastaldello, Fabio] INAF, IASF Milano, I-20133 Milan, Italy. [Gastaldello, Fabio; Buote, David A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Temi, Pasquale] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA. [Temi, Pasquale] SETI Inst, Mountain View, CA 94043 USA. [Brighenti, Fabrizio] Univ Bologna, Dept Astron, I-40127 Bologna, Italy. [Brighenti, Fabrizio; Mathews, William G.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Ettori, Stefano] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Ettori, Stefano] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy. RP Gastaldello, F (reprint author), INAF, IASF Milano, Via Bassini 15, I-20133 Milan, Italy. RI Gastaldello, Fabio/N-4226-2015; Ettori, Stefano/N-5004-2015 OI Gastaldello, Fabio/0000-0002-9112-0184; Ettori, Stefano/0000-0003-4117-8617 FU ASI-INAF [I/023/05/0, I/088/06/0]; NASA [NNG04GE76G] FX We thank N. Caon for kindly providing the Ha image used in Figure 11 and for useful discussions; S. Giacintucci for sharing her results prior to publication and for useful discussions; P.J. Humphrey for the use of his Chandra data reduction and analysis code; J. Sanders for the use of his contour binning code; L. Zappacosta for a critical reading of the manuscript; and the anonymous referee for a careful reading and for suggestions that improved the work presented here. We made use of the WVT binning algorithm by Diehl & Statler (2006), which is a generalization of Cappellari & Copin's (2003) Voronoi binning algorithm. F. G., F. B., and S. E. acknowledge the financial contribution from contract ASI-INAF I/023/05/0 and I/088/06/0. D. A. B. gratefully acknowledges partial support from NASA grant NNG04GE76G, issued through the Office of Space Sciences Long-Term Space Astrophysics Program. NR 95 TC 40 Z9 40 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2009 VL 693 IS 1 BP 43 EP 55 DI 10.1088/0004-637X/693/1/43 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 414ZE UT WOS:000263903300004 ER PT J AU Guyon, O Matsuo, T Angel, R AF Guyon, Olivier Matsuo, Taro Angel, Roger TI CORONAGRAPHIC LOW-ORDER WAVE-FRONT SENSOR: PRINCIPLE AND APPLICATION TO A PHASE-INDUCED AMPLITUDE CORONAGRAPH SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation: adaptive optics; techniques: high angular resolution ID LYOT CORONAGRAPHS; MASK; SENSITIVITY; APODIZATION AB High-contrast coronagraphic imaging of the immediate surrounding of stars requires exquisite control of low-order wave-front aberrations, such as tip-tilt (pointing) and focus. We propose an accurate, efficient, and easy to implement technique to measure such aberrations in coronagraphs which use a focal plane mask to block starlight. The coronagraphic low-order wave-front sensor (CLOWFS) produces a defocused image of a reflective focal plane ring to measure low-order aberrations. Even for small levels of wave-front aberration, the proposed scheme produces large intensity signals which can easily be measured, and therefore does not require highly accurate calibration of either the detector or optical elements. The CLOWFS achieves nearly optimal sensitivity and is immune from noncommon path errors. This technique is especially well suited for high-performance low inner working angle coronagraphs. On phase-induced amplitude apodization (PIAA)-type coronagraphs, it can unambiguously recover aberrations which originate from either side of the beam shaping introduced by the PIAA optics. We show that the proposed CLOWFS can measure sub-milliarcsecond telescope pointing errors several orders of magnitude faster than would be possible in the coronagraphic science focal plane alone, and can also accurately calibrate residual coronagraphic leaks due to residual low-order aberrations. We have demonstrated approximate to 10(-3)lambda/D pointing stability in a laboratory demonstration of the CLOWFS on a PIAA-type coronagraph. C1 [Guyon, Olivier] Subaru Telescope, Natl Astron Observ Japan, Hilo, HI 96720 USA. [Matsuo, Taro] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Angel, Roger] Univ Arizona, Steward Observ, Tucson, AZ 85719 USA. RP Guyon, O (reprint author), Subaru Telescope, Natl Astron Observ Japan, Hilo, HI 96720 USA. EM guyon@naoj.org NR 14 TC 65 Z9 65 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2009 VL 693 IS 1 BP 75 EP 84 DI 10.1088/0004-637X/693/1/75 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 414ZE UT WOS:000263903300007 ER PT J AU Grasset, O Schneider, J Sotin, C AF Grasset, O. Schneider, J. Sotin, C. TI A STUDY OF THE ACCURACY OF MASS-RADIUS RELATIONSHIPS FOR SILICATE-RICH AND ICE-RICH PLANETS UP TO 100 EARTH MASSES SO ASTROPHYSICAL JOURNAL LA English DT Article DE Earth; planets and satellites: general; methods: numerical; planetary systems; equation of state ID EXTRA-SOLAR PLANETS; M-CIRCLE-PLUS; OCEAN-PLANETS; SUPER-EARTHS; SOLID EXOPLANETS; GIANT PLANETS; HIGH-PRESSURE; HARPS SEARCH; SYSTEM; ABUNDANCES AB A mass-radius (M-R) relationship is proposed for solid planets and solid cores ranging from 1 to 100 Earth-mass planets. It relies on the assumption that solid spheres are composed of iron and silicates, around which a variable amount of water is added. The M-R law has been set up assuming that the planetary composition is similar to the averaged composition for silicates and iron obtained from the major elements ratio of 94 stars hosting exoplanets. Except on Earth for which a tremendous amount of data is available, the composition of silicate mantles and metallic cores cannot be constrained. Similarly, thermal profiles are poorly known. In this work, the effect of compositional parameters and thermal profiles on radii estimates is quantified. It will be demonstrated that uncertainties related to composition and temperature are secondary compared to the effect of the amount of water. The super-Earth family includes four classes of planets: iron-rich, silicate-rich, water-rich, or with a thick atmosphere. For a given mass, the planetary radius increases significantly from the iron-rich to the atmospheric-rich planet. Even if some overlaps are likely, M-R measurements could be accurate enough to ascertain the discovery of an Earth-like planet. The present work describes how the amount of water can be assessed from M-R measurements. Such an estimate depends on several assumptions including (1) the accuracy of the internal structure model and (2) the accuracy of mass and radius measurements. It is shown that if the mass and the radius are perfectly known, the standard deviation of the amount of water is about 4.5%. This value increases rapidly with the radius uncertainty but does not strongly depend on the mass uncertainty. C1 [Grasset, O.] Univ Nantes, Lab Planetol & Geodynam, UMR CNRS 6112, F-44035 Nantes, France. [Schneider, J.] Observ Paris, UMR CNRS 8102, Lab Univers & Theories, Paris, France. [Sotin, C.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Grasset, O (reprint author), Univ Nantes, Lab Planetol & Geodynam, UMR CNRS 6112, F-44035 Nantes, France. FU NASA FX The authors want to thank G. Tinetti for her valuable comments on detection perspectives and an anonymous reviewer for her/his constructive remarks. Part of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 54 TC 65 Z9 65 U1 2 U2 17 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2009 VL 693 IS 1 BP 722 EP 733 DI 10.1088/0004-637X/693/1/722 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 414ZE UT WOS:000263903300060 ER PT J AU Chiang, E Kite, E Kalas, P Graham, JR Clampin, M AF Chiang, E. Kite, E. Kalas, P. Graham, J. R. Clampin, M. TI FOMALHAUT'S DEBRIS DISK AND PLANET: CONSTRAINING THE MASS OF FOMALHAUT B FROM DISK MORPHOLOGY SO ASTROPHYSICAL JOURNAL LA English DT Article DE celestial mechanics; circumstellar matter; planetary systems; planetary systems: protoplanetary disks; stars: individual (Fomalhaut) ID 3/1 COMMENSURABILITY; SOLAR-SYSTEM; ACCRETION; SATELLITES; SPECTRA; ORIGIN; MODEL; PARTICLES; DYNAMICS; BEHAVIOR AB Following the optical imaging of exoplanet candidate Fomalhaut b (Fom b), we present a numerical model of how Fomalhaut's debris disk is gravitationally shaped by a single interior planet. The model is simple, adaptable to other debris disks, and can be extended to accommodate multiple planets. If Fom b is the dominant perturber of the belt, then to produce the observed disk morphology it must have a mass M(pl) < 3M(J), an orbital semimajor axis a(pl) > 101.5 AU, and an orbital eccentricity e(pl) = 0.11-0.13. These conclusions are independent of Fom b's photometry. To not disrupt the disk, a greater mass for Fom b demands a smaller orbit farther removed from the disk; thus, future astrometric measurement of Fom b's orbit, combined with our model of planet-disk interaction, can be used to determine the mass more precisely. The inner edge of the debris disk at a approximate to 133 AU lies at the periphery of Fom b's chaotic zone, and the mean disk eccentricity of e approximate to 0.11 is secularly forced by the planet, supporting predictions made prior to the discovery of Fom b. However, previous mass constraints based on disk morphology rely on several oversimplifications. We explain why our constraint is more reliable. It is based on a global model of the disk that is not restricted to the planet's chaotic zone boundary. Moreover, we screen disk parent bodies for dynamical stability over the system age of similar to 100 Myr, and model them separately from their dust grain progeny; the latter's orbits are strongly affected by radiation pressure and their lifetimes are limited to similar to 0.1 Myr by destructive grain-grain collisions. The single planet model predicts that planet and disk orbits be apsidally aligned. Fomalhaut b's nominal space velocity does not bear this out, but the astrometric uncertainties may be large. If the apsidal misalignment proves real, our calculated upper mass limit of 3MJ still holds. If the orbits are aligned, our model predicts M(pl) = 0.5M(J), a(pl) = 115 AU, and e(pl) = 0.12. Parent bodies are evacuated from mean-motion resonances with Fom b; these empty resonances are akin to the Kirkwood gaps opened by Jupiter. The belt contains at least 3M(circle plus) of solids that are grinding down to dust, their velocity dispersions stirred so strongly by Fom b that collisions are destructive. Such a large mass in solids is consistent with Fom b having formed in situ. C1 [Chiang, E.; Kalas, P.; Graham, J. R.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Chiang, E.; Kite, E.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. [Clampin, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Chiang, E (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM echiang@astro.berkeley.edu RI Clampin, mark/D-2738-2012 FU NSF [AST-0507805]; Berkeley Fellowship FX This work was supported by NSF grant AST-0507805. E. K. acknowledges support from a Berkeley Fellowship. We thank M. Fitzgerald, Y. Lithwick, E. Mamajek, C. Marois, N. Murray, K. Stapelfeldt, and M. Wyatt for discussions. An anonymous referee rapidly provided a thoughtful report, at the behest of ApJ Scientific Editor F. Rasio, for which we are grateful. NR 36 TC 125 Z9 125 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2009 VL 693 IS 1 BP 734 EP 749 DI 10.1088/0004-637X/693/1/734 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 414ZE UT WOS:000263903300061 ER PT J AU Bussmann, RS Dey, A Lotz, J Armus, L Brand, K Brown, MJI Desai, V Eisenhardt, P Higdon, J Higdon, S Jannuzi, BT Le Floc'h, E Melbourne, J Soifer, BT Weedman, D AF Bussmann, R. S. Dey, Arjun Lotz, J. Armus, L. Brand, K. Brown, M. J. I. Desai, V. Eisenhardt, P. Higdon, J. Higdon, S. Jannuzi, B. T. Le Floc'h, E. Melbourne, J. Soifer, B. T. Weedman, D. TI HUBBLE SPACE TELESCOPE MORPHOLOGIES OF z similar to 2 DUST OBSCURED GALAXIES. I. POWER-LAW SOURCES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: fundamental parameters; galaxies: high-redshift ID STAR-FORMING GALAXIES; ULTRALUMINOUS INFRARED GALAXIES; DEEP-FIELD-SOUTH; ACTIVE GALACTIC NUCLEUS; HIGH-REDSHIFT GALAXIES; SCUBA SUPER-MAP; X-RAY SURVEY; SUBMILLIMETER GALAXIES; SIGNIFICANT POPULATION; DISTANT GALAXIES AB We present high-spatial resolution optical and near-infrared imaging obtained using the ACS, WFPC2, and NICMOS cameras aboard the Hubble Space Telescope of 31 24 mu m bright z approximate to 2 Dust Obscured Galaxies (DOGs) identified in the Bootes Field of the NOAO Deep Wide-Field Survey. Although this subset of DOGs have mid-IR spectral energy distributions dominated by a power-law component suggestive of an AGN, all but one of the galaxies are spatially extended and not dominated by an unresolved component at rest-frame UV or optical wavelengths. The observed V-H and I-H colors of the extended components are 0.2-3 magnitudes redder than normal star-forming galaxies. All but one have axial ratios > 0.3, making it unlikely that DOGs are composed of an edge-on star-forming disk. We model the spatially extended component of the surface brightness distributions of the DOGs with a Sersic profile and find effective radii of 1-6 kpc. This sample of DOGs is smaller than most submillimeter galaxies (SMGs), but larger than quiescent high-redshift galaxies. Nonparametric measures (Gini and M(20)) of DOG morphologies suggest that these galaxies are more dynamically relaxed than local ULIRGs. We estimate lower limits to the stellar masses of DOGs based on the rest-frame optical photometry and find that these range from similar to 10(9)-10(11) M(circle dot). If major mergers are the progenitors of DOGs, then these observations suggest that DOGs may represent a postmerger evolutionary stage. C1 [Bussmann, R. S.] Univ Arizona, Steward Observ, Dept Astron, Tucson, AZ 85721 USA. [Dey, Arjun; Lotz, J.; Jannuzi, B. T.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Armus, L.; Desai, V.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Brown, M. J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Eisenhardt, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Higdon, J.; Higdon, S.] Georgia So Univ, Statesboro, GA 30460 USA. [Melbourne, J.; Soifer, B. T.] CALTECH, Opt Observ, Pasadena, CA 91125 USA. [Weedman, D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Bussmann, RS (reprint author), Univ Arizona, Steward Observ, Dept Astron, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM rsbussmann@as.arizona.edu RI Brown, Michael/B-1181-2015 OI Brown, Michael/0000-0002-1207-9137 FU HST [GO10890]; NASA through a grant from the Space Telescope Science Institute [HST-GO10890]; NASA [NAS5-26555] FX R. S. B. gratefully acknowledges financial assistance from HST grant GO10890, without which this research would not have been possible. Support for Program number HST-GO10890 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. The research activities of A. D. and B. T. J. are supported by NOAO, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. Support for E. Le Floc'h was provided by NASA through the Spitzer Space Telescope Fellowship Program. NR 83 TC 39 Z9 40 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2009 VL 693 IS 1 BP 750 EP 770 DI 10.1088/0004-637X/693/1/750 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 414ZE UT WOS:000263903300062 ER PT J AU Fragile, PC Meier, DL AF Fragile, P. Chris Meier, David L. TI GENERAL RELATIVISTIC MAGNETOHYDRODYNAMIC SIMULATIONS OF THE HARD STATE AS A MAGNETICALLY DOMINATED ACCRETION FLOW SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies: active; MHD; relativity; X-rays: stars ID BLACK-HOLE ACCRETION; FORCE-FREE MAGNETOSPHERE; SAGITTARIUS-A; ELECTRONS; GEOMETRY; MODEL; DISKS; FIELD; EVOLUTION; SPECTRUM AB We present one of the first physically motivated two-dimensional general relativistic magnetohydrodynamic numerical simulations of a radiatively cooled black hole accretion disk. The fiducial simulation combines a total-energy-conserving formulation with a radiative cooling function, which includes bremsstrahlung, synchrotron, and Compton effects. By comparison with other simulations we show that in optically thin advection-dominated accretion flows (ADAFs), radiative cooling can significantly affect the structure, without necessarily leading to an optically thick, geometrically thin accretion disk. We further compare the results of our radiatively cooled simulation to the predictions of a previously developed analytic model for such flows. For the very low stress parameter and accretion rate found in our simulated disk (alpha approximate to 0.003, (M) over dot/(M) over dot(EDD) approximate to 5 x 10-(6)), we closely match a state called the "transition" solution between an outer ADAF and what would be a magnetically dominated accretion flow (MDAF) in the interior. The qualitative and quantitative agreement between the numerical and analytic models is quite good, with only a few well understood exceptions. According to the analytic model then, at significantly higher alpha or (M) over dot we would expect a full MDAF to form. The collection of simulations in this work also provides important data for interpreting other numerical results in the literature, as they span the most common treatments of thermodynamics, including simulations evolving (1) the internal energy only; (2) the internal energy plus an explicit cooling function; (3) the total energy without cooling; and (4) the total energy including cooling. We find that the total energy formulation is a necessary prerequisite for proper treatment of radiative cooling in magneto-rotational instability accretion flows, as the internal energy formulation produces a large unphysical numerical cooling of its own. We also find that the relativistic cooling functions must be handled carefully numerically in order to avoid equally unphysical heating or cooling runaways. C1 [Fragile, P. Chris] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA. [Meier, David L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Fragile, PC (reprint author), Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA. EM fragilep@cofc.edu; David.L.Meier@jpl.nasa.gov FU JPL/Caltech; JPL [1304153]; South Carolina Space Grant Consortium; Jet Propulsion Laboratory, California Institute of Technology FX We thank Sera Markoff and Masanori Nakamura for their discussions and careful reading of this manuscript. We would like to recognize Joseph Niehaus for his contributions to testing the Cosmos++ code. P. C. F. gratefully acknowledges the support of a Faculty R&D grant from the College of Charleston and a REAP grant from the South Carolina Space Grant Consortium. Part of the research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract to the National Aeronautics and Space Administration. Part of this research also was performed when the authors attended extended workshops at the UCLA Institute for Pure and Applied Mathematics and the UCSB Kavli Institute for Theoretical Physics. D. L. M. is grateful to JPL/Caltech for financial support, and to UCLA for their hospitality during his sabbatical. This work also was supported by JPL subcontract 1304153. Computing resources were provided by the JPL Supercomputing Facility and the Texas Advanced Computing Center (TACC). NR 29 TC 48 Z9 48 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2009 VL 693 IS 1 BP 771 EP 783 DI 10.1088/0004-637X/693/1/771 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 414ZE UT WOS:000263903300063 ER PT J AU Liu, W Petrosian, V Dennis, BR Holman, GD AF Liu, Wei Petrosian, Vahe Dennis, Brian R. Holman, Gordon D. TI CONJUGATE HARD X-RAY FOOTPOINTS IN THE 2003 OCTOBER 29 X10 FLARE: UNSHEARING MOTIONS, CORRELATIONS, AND ASYMMETRIES SO ASTROPHYSICAL JOURNAL LA English DT Review DE acceleration of particles; Sun: flares; Sun: magnetic fields; Sun: X-rays, gamma rays ID CORONAL MASS EJECTIONS; FIELD LINE SHRINKAGE; SOLAR-FLARES; MAGNETIC RECONNECTION; PARTICLE-ACCELERATION; IMPULSIVE PHASE; 2-RIBBON FLARE; BREMSSTRAHLUNG RADIATION; SPECTRAL CHARACTERISTICS; STOCHASTIC ACCELERATION AB We present a detailed imaging and spectroscopic study of the conjugate hard X-ray (HXR) footpoints (FPs) observed with the Ramaty High Energy Solar Spectroscopic Imager (RHESSI) in the 2003 October 29 X10 flare. The double FPs first move toward and then away from each other, mainly parallel and perpendicular to the magnetic neutral line, respectively. The transition of these two phases of FP unshearing motions coincides with the direction reversal of the motion of the loop-top (LT) source, and with the minima of the estimated loop length and LT height. We find temporal correlations between the HXR flux, spectral index, and magnetic field strength of each FP. The HXR flux exponentially correlates with the magnetic field strength, which also anticorrelates with the spectral index before the second HXR peak's maximum, suggesting that particle acceleration sensitively depends on the magnetic field strength and/or reconnection rate. Asymmetries are observed between the FPs: on average, the eastern FP is 2.2 times brighter in HXR flux and 1.8 times weaker in magnetic field strength, and moves 2.8 times faster away from the neutral line than the western FP; the estimated coronal column density to the eastern FP from the LT source is 1.7 times smaller. The two FPs have marginally different spectral indices. The eastern-to-western FP HXR flux ratio and magnetic field strength ratio are anticorrelated only before the second HXR peak's maximum. Neither magnetic mirroring nor column density alone can explain the totality of these observations, but their combination, together with other transport effects, might provide a full explanation. We have also developed novel techniques to remove particle contamination from HXR counts and to estimate effects of pulse pileup in imaging spectroscopy, which can be applied to other RHESSI flares in similar circumstances. C1 [Liu, Wei; Dennis, Brian R.; Holman, Gordon D.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Liu, Wei; Petrosian, Vahe] Stanford Univ, Ctr Space Sci & Astrophys, Dept Phys, Stanford, CA 94305 USA. RP Liu, W (reprint author), NASA, Goddard Space Flight Ctr, Solar Phys Lab, Heliophys Sci Div, Code 671, Greenbelt, MD 20771 USA. EM weiliu@sun.stanford.edu RI Dennis, Brian/C-9511-2012; Holman, Gordon/C-9548-2012 NR 121 TC 37 Z9 37 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2009 VL 693 IS 1 BP 847 EP 867 DI 10.1088/0004-637X/693/1/847 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 414ZE UT WOS:000263903300071 ER PT J AU Sakamoto, T Sato, G Barbier, L Barthelmy, SD Cummings, JR Fenimore, EE Gehrels, N Hullinger, D Krimm, HA Lamb, DQ Markwardt, CB Palmer, DM Parsons, AM Stamatikos, M Tueller, J Ukwatta, TN AF Sakamoto, T. Sato, G. Barbier, L. Barthelmy, S. D. Cummings, J. R. Fenimore, E. E. Gehrels, N. Hullinger, D. Krimm, H. A. Lamb, D. Q. Markwardt, C. B. Palmer, D. M. Parsons, A. M. Stamatikos, M. Tueller, J. Ukwatta, T. N. TI E-peak ESTIMATOR FOR GAMMA-RAY BURSTS OBSERVED BY THE Swift BURST ALERT TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: bursts ID INTRINSIC SPECTRA; FLASHES; ENERGY; CATALOG; MODEL; ENERGETICS; MISSION; HETE-2; BAT AB We report a correlation based on a spectral simulation study of the prompt emission spectra of gamma-ray bursts (GRBs) detected by the Swift Burst Alert Telescope (BAT). The correlation is between the E-peak energy, which is the peak energy in the nu F-nu spectrum, and the photon index (Gamma) derived from a simple power-law (PL) model. The E-peak-Gamma relation, assuming the typical smoothly broken PL spectrum of GRBs, is log E-peak = 3.258 - 0.829 Gamma (1.3 <= Gamma <= 2.3). We take into account not only a range of E-peak energies and fluences, but also distributions for both the low-energy photon index and the high-energy photon index in the smoothly broken PL model. The distribution of burst durations in the BAT GRB sample is also included in the simulation. Our correlation is consistent with the index observed by BAT and E-peak measured by the BAT, and by other GRB instruments. Since about 85% of GRBs observed by the BAT are acceptably fit with the simple PL model because of the relatively narrow energy range of the BAT, this relationship can be used to estimate E-peak when it is located within the BAT energy range. C1 [Sakamoto, T.; Cummings, J. R.; Krimm, H. A.; Markwardt, C. B.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Sakamoto, T.; Cummings, J. R.] Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Baltimore, MD 21250 USA. [Stamatikos, M.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA. [Fenimore, E. E.; Palmer, D. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Markwardt, C. B.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Sato, G.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Lamb, D. Q.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Hullinger, D.] Moxtek Inc, Orem, UT 84057 USA. [Ukwatta, T. N.] George Washington Univ, Dept Phys, Washington, DC 20052 USA. RP Sakamoto, T (reprint author), NASA, Goddard Space Flight Ctr, CRESST, Code 661, Greenbelt, MD 20771 USA. RI Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; Tueller, Jack/D-5334-2012; Parsons, Ann/I-6604-2012 NR 58 TC 54 Z9 54 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 MAR 1 PY 2009 VL 693 IS 1 BP 922 EP 935 DI 10.1088/0004-637X/693/1/922 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 414ZE UT WOS:000263903300077 ER PT J AU Wise, JH Cen, RY AF Wise, John H. Cen, Renyue TI IONIZING PHOTON ESCAPE FRACTIONS FROM HIGH-REDSHIFT DWARF GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: theory; galaxies: dwarf; galaxies: formation; galaxies: high-redshift; radiative transfer ID MICROWAVE-ANISOTROPY-PROBE; LYMAN CONTINUUM ESCAPE; PRIMORDIAL HII-REGIONS; STAR-FORMATION HISTORY; POPULATION-III STARS; LOW-MASS GALAXIES; METAL-FREE STARS; INTERGALACTIC MEDIUM; COSMIC REIONIZATION; RADIATIVE FEEDBACK AB It has been argued that low-luminosity dwarf galaxies are the dominant source of ionizing radiation during cosmological reionization. The fraction of ionizing radiation that escapes into the intergalactic medium from dwarf galaxies with masses less than similar to 10(9.5) solar masses plays a critical role during this epoch. Using an extensive suite of very high resolution (0.1 pc), adaptive mesh refinement, radiation hydrodynamical simulations of idealized and cosmological dwarf galaxies, we characterize the behavior of the escape fraction in galaxies between 3 x 10(6) and 3 x 10(9) solar masses with different spin parameters, amounts of turbulence, and baryon mass fractions. For a given halo mass, escape fractions can vary up to a factor of two, depending on the initial setup of the idealized halo. In a cosmological setting, we find that the time-averaged photon escape fraction always exceeds 25% and reaches up to 80% in halos with masses above 10(8) solar masses with a top-heavy initial mass function (IMF). The instantaneous escape fraction can vary up to an order of magnitude in a few million years and tends to be positively correlated with star formation rate. We find that the mean of the star formation efficiency times ionizing photon escape fraction, averaged over all atomic cooling (T(vir) >= 8000 K) galaxies, ranges from 0.02 for a normal IMF to 0.03 for a top-heavy IMF, whereas smaller, molecular cooling galaxies in minihalos do not make a significant contribution to reionizing the universe due to much lower star formation rates. These results provide the physical basis for cosmological reionization by stellar sources, predominately atomic cooling dwarf galaxies. C1 [Wise, John H.] NASA, Lab Observat Cosmol, Goddard Space Flight Ctr, Greenbelt, MD 21114 USA. [Cen, Renyue] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Wise, JH (reprint author), NASA, Lab Observat Cosmol, Goddard Space Flight Ctr, Greenbelt, MD 21114 USA. EM john.h.wise@nasa.gov FU Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA; [AST-0407176]; [NNG06GI09G] FX We thank an anonymous referee for useful suggestions. J. H. W. thanks Tom Abel for useful discussions. We performed these calculations on Orange at SLAC, Discover at NASA/GSFC, Abe and Cobalt at NCSA, and Queenbee at LSU. This research was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. We gratefully acknowledge financial support by grants AST-0407176 and NNG06GI09G. NR 96 TC 136 Z9 136 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2009 VL 693 IS 1 BP 984 EP 999 DI 10.1088/0004-637X/693/1/984 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 414ZE UT WOS:000263903300082 ER PT J AU Mewaldt, RA Leske, RA Stone, EC Barghouty, AF Labrador, AW Cohen, CMS Cummings, AC Davis, AJ von Rosenvinge, TT Wiedenbeck, ME AF Mewaldt, R. A. Leske, R. A. Stone, E. C. Barghouty, A. F. Labrador, A. W. Cohen, C. M. S. Cummings, A. C. Davis, A. J. von Rosenvinge, T. T. Wiedenbeck, M. E. TI STEREO OBSERVATIONS OF ENERGETIC NEUTRAL HYDROGEN ATOMS DURING THE 2006 DECEMBER 5 SOLAR FLARE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: corona; Sun: coronal mass ejections (CMEs); Sun: flares; Sun: particle emission; Sun: X-rays, gamma rays ID PARTICLE-ACCELERATION; GAMMA-RAY; CHARGE-TRANSFER; DECAY; IONS; MAGNETOSPHERE; ABUNDANCES; COLLISIONS; TELESCOPE; PROTONS AB We report the discovery of energetic neutral hydrogen atoms (ENAs) emitted during the X9 solar event of 2006 December 5. Beginning similar to 1 hr following the onset of this E79 flare, the Low Energy Telescopes (LETs) on both the STEREO A and B spacecraft observed a sudden burst of 1.6-15 MeV protons beginning hours before the onset of the main solar energetic particle event at Earth. More than 70% of these particles arrived from a longitude within +/-10 degrees of the Sun, consistent with the measurement resolution. The derived emission profile at the Sun had onset and peak times remarkably similar to the GOES soft X-ray profile and continued for more than an hour. The observed arrival directions and energy spectrum argue strongly that the particle events <5 MeV were due to ENAs. To our knowledge, this is the first reported observation of ENA emission from a solar flare/coronal mass ejection. Possible origins for the production of ENAs in a large solar event are considered. We conclude that the observed ENAs were most likely produced in the high corona and that charge-transfer reactions between accelerated protons and partially stripped coronal ions are an important source of ENAs in solar events. C1 [Mewaldt, R. A.; Leske, R. A.; Stone, E. C.; Labrador, A. W.; Cohen, C. M. S.; Cummings, A. C.; Davis, A. J.] CALTECH, Pasadena, CA 91125 USA. [Barghouty, A. F.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. [von Rosenvinge, T. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wiedenbeck, M. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mewaldt, RA (reprint author), CALTECH, Pasadena, CA 91125 USA. FU NASA [SA2715-26309]; NASA's Office of Chief Engineer; [NAS5-03131] FX This work was supported by NASA at Caltech and JPL under subcontract SA2715-26309 from the University of California, Berkeley, under NASA contract NAS5-03131. The work at Marshall Space Flight Centerwas supported by the TEI Program of NASA's Office of Chief Engineer. We thank NOAA for GOES X-ray data, Mike Kaiser for STEREO/ WAVES data, Chris Russell for STEREO magnetic field data, and the RHESSI team for. gamma- ray data. We also appreciate discussions with Eric Christian, Sam Krucker, Bob Lin, Ron Murphy, and Gerry Share. NR 29 TC 19 Z9 20 U1 0 U2 1 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 MAR 1 PY 2009 VL 693 IS 1 BP L11 EP L15 DI 10.1088/0004-637X/693/1/L11 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 407RS UT WOS:000263382600003 ER PT J AU Rawlins, MA Steele, M Serreze, MC Vorosmarty, CJ Ermold, W Lammers, RB McDonald, KC Pavelsky, TM Shiklomanov, A Zhang, JL AF Rawlins, Michael A. Steele, Michael Serreze, Mark C. Voeroesmarty, Charles J. Ermold, Wendy Lammers, Richard B. McDonald, Kyle C. Pavelsky, Tamlin M. Shiklomanov, Alexander Zhang, Jinlun TI Tracing Freshwater Anomalies Through the Air-Land-Ocean System: A Case Study from the Mackenzie River Basin and the Beaufort Gyre SO ATMOSPHERE-OCEAN LA English DT Article ID VAPOR TRANSPORT; FLOW REGULATION; DRAINAGE-BASIN; ARCTIC-OCEAN; VARIABILITY; DISCHARGE; PRECIPITATION; BALANCE; MODEL AB Mackenzie River discharge was at a record low in water year (WY) 1995 (October 1994 to September 1995), was near average in WY 1996, and was at a record high in WY 1997. The record high discharge in WY 1997, with above average flow each month, was followed by a record high flow in May 1998, then a sharp decline. Through diagnosing these changing flows and their expression in the Beaufort Sea via synthesis of observations and model output, this study provides insight into the nature of the Arctic's freshwater system. The low discharge in WY 1995 manifests negative anomalies in P-E and precipitation, recycled summer precipitation, and dry surface conditions immediately prior to the water year. The complex hydrograph for WY 1996 reflects a combination of spring soil moisture recharge, buffering by rising lake levels, positive P-E anomalies in summer, and a massive release of water held in storage by Bennett Dam. The record high discharge in WY 1997 manifests the dual effects of reduced buffering by lakes and positive P-E anomalies for most of the year. With reduced buffering, only modest P-E the following spring led to a record discharge in May 1998. As simulated with a coupled ice-ocean model, the record low discharge in WY 1995 contributed to a negative freshwater anomaly on the Mackenzie shelf lasting throughout the winter of 1995/96. High discharge from July-October 1996 contributed approximately 20% to a positive freshwater anomaly forming in the Beaufort Sea in the autumn of that year. The remainder was associated with reduced autumn/winter ice growth, strong ice melt the previous summer, and positive P-E anomalies over the ocean itself. Starting in autumn 1997 and throughout 1998, the upper ocean became more saline owing to sea-ice growth. C1 [Rawlins, Michael A.; McDonald, Kyle C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Steele, Michael; Ermold, Wendy; Zhang, Jinlun] Univ Washington, Appl Phys Lab, Polar Sci Ctr, Seattle, WA 98195 USA. [Serreze, Mark C.] Univ Colorado, Natl Snow & Ice Data Ctr, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Voeroesmarty, Charles J.; Lammers, Richard B.; Shiklomanov, Alexander] Univ New Hampshire, Inst Study Earth Oceans & Space, Water Syst Anal Grp, Durham, NH 03824 USA. [Pavelsky, Tamlin M.] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90095 USA. RP Steele, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM michael.rawlins@jpl.nasa.gov FU National Science Foundation's Arctic System Science (ARCSS); Office of Polar Programs Arctic Section; National Aeronautics and Space Administration's (NASA) Cryospheric Program; [ARC-0229769]; [ARC-0230427]; [ARC-0230429]; [ARC-029651]; [OPP-0094532]; [OPP-0230243]; [OPP-9910264]; [NNG04GH04G]; [NNG04GH52G]; [NNG04GJ39G]; [NAG59617] FX This work was supported by the National Science Foundation's Arctic System Science (ARCSS) program, the Office of Polar Programs Arctic Section, and grants ARC-0229769, ARC-0230427, ARC-0230429, ARC-029651, OPP-0094532, OPP-0230243, and OPP-9910264. We also acknowledge support from the National Aeronautics and Space Administration's (NASA) Cryospheric Program and grants NNG04GH04G, NNG04GH52G, NNG04GJ39G, and NAG59617. The authors thank Charon Birkett, Steve Frolking and Dominik Wisser for helpful discussions. Andrew Slater is thanked for assistance with the SWE estimates. Portions of the work were carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract to the National Aeronautics and Space Administration. NR 32 TC 9 Z9 9 U1 1 U2 11 PU CMOS-SCMO PI OTTAWA PA BOX 3211, STATION D, OTTAWA, ON K1P 6H7, CANADA SN 0705-5900 J9 ATMOS OCEAN JI Atmos.-Ocean PD MAR PY 2009 VL 47 IS 1 BP 79 EP 97 DI 10.3137/OC301.2009 PG 19 WC Meteorology & Atmospheric Sciences; Oceanography SC Meteorology & Atmospheric Sciences; Oceanography GA 436GK UT WOS:000265400500005 ER PT J AU Shim, C Li, QB Luo, M Kulawik, S Worden, H Worden, J Eldering, A Diskin, G Sachse, G Weinheimer, A Knapp, D Montzca, D Campos, T AF Shim, Changsub Li, Qinbin Luo, Ming Kulawik, Susan Worden, Helen Worden, John Eldering, Annmarie Diskin, Glenn Sachse, Glen Weinheimer, Andy Knapp, David Montzca, Deedee Campos, Teresa TI Satellite observations of Mexico City pollution outflow from the Tropospheric Emissions Spectrometer (TES) SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Mega-city pollution; TES; O-3-CO correlation; INTEX-B; Mexico city ID CARBON-MONOXIDE; UNITED-STATES; OZONE; VARIABILITY; MEGACITIES; CHEMISTRY; PACIFIC; AEROSOL; EASTERN; MODEL AB Concurrent tropospheric O-3 and CO vertical profiles from the Tropospheric Emission Spectrometer (TES) during the MILAGRO/INTEX-B aircraft campaigns over the Mexico City Metropolitan Area (MCMA) and its surrounding regions were used to examine Mexico City pollution outflow on a regional scale. The pollution outflow from the MCMA occurred predominantly at 600-800 hPa as evident in O-3, CO, and NOx enhancements in the in situ aircraft observations. TES O-3 and CO are sensitive to the MCMA pollution outflow due to their relatively high sensitivities at 600-800 hPa. We examined O-3, CO, and their correlation at 600-800 hPa from TES retrievals, aircraft measurements, and GEOS-Chem model results. TES captures much of the spatial and day-to-day variability of O-3 seen in the in situ data. TES CO, however, shows much less spatial and day-to-day variability compared with the in situ observations. The Delta O-3/Delta CO slope is significantly higher in the TES data (0.43) than the in situ data (0.28) due partly to the lack of variability in TES CO. Extraordinarily high Delta O-3/Delta CO slope (0.81) from TES observations at 618 hPa over the Eastern U.S. was previously reported by Zhang et al. [Zhang, L.. Jacob, D.J., Bowman, K.W., et al.. 2006. Ozone-CO correlations determined by the TES satellite instrument in continental outflow regions. Geophys. Res. Lett. 33, L18804.10.1029/2006GL026399.]. Thus the application of TES CO-O-3 correlation to map continental pollution outflow needs further examination. Published by Elsevier Ltd. C1 [Shim, Changsub; Li, Qinbin; Luo, Ming; Kulawik, Susan; Worden, John; Eldering, Annmarie] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Li, Qinbin] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA. RP Shim, C (reprint author), CALTECH, Jet Prop Lab, M-S 183-501,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM cshim@jpl.nasa.gov RI Chem, GEOS/C-5595-2014 FU California Institute of Technology; Jet Propulsion Laboratory (JPL); PL Research and Technology Development (RTD) program; Human Resources Development Fund (HRDF); NASA Atmospheric Composition Modeling and Analysis program (ACMAP); TES; NASA Atmospheric Chemistry Modeling and Analysis Program FX This work is performed at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under contract with the NASA. C. Shim and Q. Li were jointly supported by the JPL Research and Technology Development (R&TD) program, Human Resources Development Fund (HRDF), NASA Atmospheric Composition Modeling and Analysis program (ACMAP), and the TES project at JPL. The GEOS-Chem model is managed at Harvard University with support from the NASA Atmospheric Chemistry Modeling and Analysis Program. We thank Melody Avery for the in-Situ 03 measurements. We thank Lin Zhang for very helpful discussions. NR 48 TC 12 Z9 12 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD MAR PY 2009 VL 43 IS 8 BP 1540 EP 1547 DI 10.1016/j.atmosenv.2008.11.026 PG 8 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 417IX UT WOS:000264070800008 ER PT J AU Cong, ZY Kang, SC Smirnov, A Holben, B AF Cong, Zhiyuan Kang, Shichang Smirnov, Alexander Holben, Brent TI Aerosol optical properties at Nam Co, a remote site in central Tibetan Plateau SO ATMOSPHERIC RESEARCH LA English DT Article DE Aerosol optical properties; AERONET; Tibetan Plateau; Sun photometer ID SKY RADIANCE MEASUREMENTS; AERONET; ANTARCTICA; ABSORPTION; THICKNESS; NETWORK; REGION; SEASON; DEPTH; SUN AB To reduce uncertainties in the assessment of aerosol effects on regional climate and validate the satellite products, aerosol optical measurements were made at a remote site, Nam Co Station (AERONET) in central Tibetan Plateau, since August 2006. Very low aerosol optical values were observed with annual mean Aerosol Optical Depth (AOD) of 0.05 at 500 nm during August 2006 to July 2007. Angstrom parameters were also low with an average of 0.42 +/- 0.27, Angstrom parameter varies greatly over a narrow range of AOD, indicating the occurrence of different types of aerosol particles. The seasonal variation of the monthly average AOD shows maximum values in the spring (April, May) and remains high values in summer monsoon season (June, July, August, and September). The former corresponds to the prevalence of soil dust particle in spring and the later reflects the enhanced human activities in summer. The seasonal variation of columnar size distribution is also consistent with this result. Distinct seasonal variation of water vapor content was observed, with high that occurred in summer monsoon season. Nam Co appears to represent a clean continental background site for atmospheric composition investigation. This work could fill the gap which exists in our knowledge on the global aerosol distribution over the huge high elevation area (i.e. Tibetan Plateau). (C) 2008 Elsevier B.V. All rights reserved. C1 [Cong, Zhiyuan; Kang, Shichang] Chinese Acad Sci, Inst Tibetan Plateau Res, Beijing 100085, Peoples R China. [Kang, Shichang] Chinese Acad Sci, State Key Lab Cryospher Sci, Lanzhou 730000, Peoples R China. [Smirnov, Alexander] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Smirnov, Alexander; Holben, Brent] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD USA. RP Kang, SC (reprint author), Chinese Acad Sci, Inst Tibetan Plateau Res, 18 Shuangqing Rd, Beijing 100085, Peoples R China. EM Shichang.kang@itpcas.ac.cn RI Smirnov, Alexander/C-2121-2009; 丛, 志远/E-5237-2012 OI Smirnov, Alexander/0000-0002-8208-1304; 丛, 志远/0000-0002-7545-5611 FU National Natural Science Foundation of China [40605034, 40771187, 40830743]; National Basic Research Program of China [2005CB422004]; Chinese Academy of Sciences FX This study is supported by the National Natural Science Foundation of China (40605034, 40771187, 40830743), the National Basic Research Program of China (2005CB422004), and "Knowledge Innovation Program" of Chinese Academy of Sciences. We thank all of the staff at Nam Co Station for maintaining the sun photometer. NR 27 TC 42 Z9 45 U1 3 U2 21 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0169-8095 J9 ATMOS RES JI Atmos. Res. PD MAR PY 2009 VL 92 IS 1 BP 42 EP 48 DI 10.1016/j.atmosres.2008.08.005 PG 7 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 411OE UT WOS:000263658100004 ER PT J AU Landi, E Bhatia, AK AF Landi, E. Bhatia, A. K. TI Atomic data and spectral line intensities for Ca XVII SO ATOMIC DATA AND NUCLEAR DATA TABLES LA English DT Article ID BE-LIKE IONS; BERYLLIUM ISOELECTRONIC SEQUENCE; HIGHLY IONIZED CALCIUM; COLLISION STRENGTHS; OSCILLATOR-STRENGTHS; RATE COEFFICIENTS; CROSS-SECTIONS; EMISSION-LINES; TRANSITIONS; NI AB Electron impact collision strengths, energy levels, oscillator strengths, and spontaneous radiative decay rates are calculated for Ca XVII. The configurations used are 2s(2), 2s2p, 2p(2), 2131', 2141' and 2s51', with I s, p, and I' = s, p, d giving rise to 92 fine-structure levels in intermediate coupling. Collision strengths are calculated at seven incident energies (15, 30. 75, 112.5, 150, 187.5 and 225 Ry) for the transitions within the three lowest configurations corresponding to the 10 lowest energy levels, and at five incident energies (75, 112.5, 150, 187.5 and 225 Ry) for transitions between the lowest five levels and the n = 3,4, 5 configurations, Calculations have been carried out using the distorted wave approximation. Excitation rate coefficients are calculated as a function of electron temperature by assuming a Maxwellian electron velocity distribution. Using the excitation rate coefficients and the radiative transition rates of the present work, and R-Matrix results for the 2s(2), 2s2p, 2p2 configurations available in the literature, statistical equilibrium equations for level populations are solved at electron densities covering the range of 10(11)-10(14) Cm(-3) at an electron temperature of log T(e)(K) = 6.7, corresponding to the maximum abundance of Ca XVII. Spectral line intensities are calculated, and their diagnostic relevance is discussed. This dataset will be made available in the next version of the CHIANTI database. (C) 2008 Elsevier Inc. All rights reserved. C1 [Landi, E.] USN, Res Lab, Washington, DC 20375 USA. [Landi, E.] ARTEP Inc, Columbia, MD 21044 USA. [Bhatia, A. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Landi, E (reprint author), USN, Res Lab, Washington, DC 20375 USA. EM landi@poppeo.nrl.navy.mil RI Landi, Enrico/H-4493-2011 FU Enrico Landi [NNH06CD24C, NNG04ED07P]; NASA FX The work of Enrico Landi is supported by the NNH06CD24C, NNG04ED07P, and other NASA grants. Calculations were carried out using Discover computer of the NASA Center for Computation Science. We warmly thank the referee for Valuable comments and suggestions. NR 33 TC 3 Z9 3 U1 0 U2 1 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0092-640X J9 ATOM DATA NUCL DATA JI Atom. Data Nucl. Data Tables PD MAR PY 2009 VL 95 IS 2 BP 155 EP 183 DI 10.1016/j.adt.2008.10.003 PG 29 WC Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Physics GA 418SL UT WOS:000264168900003 ER PT J AU Vargas-Angel, B AF Vargas-Angel, Bernardo TI CORAL HEALTH AND DISEASE ASSESSMENT IN THE US PACIFIC REMOTE ISLAND AREAS SO BULLETIN OF MARINE SCIENCE LA English DT Article ID BLACK BAND DISEASE; GREAT-BARRIER-REEF; OCEAN; SEDIMENTATION; DYNAMICS; BIOLOGY; HOST; LINE AB During 2006 and 2007, the first comprehensive, quantitative coral disease assessment was conducted at seven coral islands and atolls in the central Pacific: Johnston, Palmyra, Kingman, and Wake Atolls, and Howland, Baker, and Jarvis Islands. Collectively, they are referred to as Pacific Remote Island Areas (PRIA), spanning over 4000 km and nearly 20 degrees latitude. Distribution and prevalence of disease were determined from 25-m belt transects at 80 sites, covering an area of over 22,000 m(2) of reef habitat. Six broad disease categories were recognized affecting 12 different scleractinian genera; prevalence was computed based on the estimated total number of coral colonies per survey site. The most geographically and taxonomically widespread disease was skeletal growth anomalies detected at nearly 40% of sites and on six different anthozoan genera. In contrast, the most prevalent disease was acute tissue loss (or white syndrome) which was hosted by four scleractinian genera, including Acropora, Montipora, Goniastrea, and Platygyra. Pigmentation response and other sublethal lesions, such as algal and cyanophyte infections, and tube-worm infestations, were infrequent and occurred in low prevalences. The overall abundance of coral diseases in the U.S. PRIA was low; however, patterns of prevalence varied among coral genera and indicated a few taxa were disproportionately affected by disease, namely the Acroporidae and Poritidae. Of potential concern is white syndrome, which results in severe and rapid tissue loss, particularly on the tabular Acropora cytherea (Dana, 1846) at Johnston Atoll. C1 Univ Hawaii, Joint Inst Marine & Atmospher Res, Natl Ocean & Atmospher Adm,Coral Reef Ecosyst Div, Natl Marine Fisheries Serv,Pacific Fisheries Sci, Honolulu, HI 96814 USA. RP Vargas-Angel, B (reprint author), Univ Hawaii, Joint Inst Marine & Atmospher Res, Natl Ocean & Atmospher Adm,Coral Reef Ecosyst Div, Natl Marine Fisheries Serv,Pacific Fisheries Sci, 1125 B Ala Moana Blvd, Honolulu, HI 96814 USA. EM Bernardo.VargasAngel@noaa.gov FU NOAA Pacific Islands Fisheries Science Center's Coral Reef Ecosystem Division FX This work was supported by the NOAA Coral Reef Conservation Program, Institutional, logistic, and financial support were provided by the NOAA Pacific Islands Fisheries Science Center's Coral Reef Ecosystem Division. Institutional and logistical assistance were also provided by the U.S. Fish and Wildlife Service (Howland, Baker, Jarvis, Palmyra, and Kingman National Wildlife Refuges) and the U.S. Air Force (Wake Atoll). The officers and crew of the NOAA Ship HfIALAKAi are gratefully acknowledged for support with dive and small boat operations. J. Maragos and J. Kenyon conducted field colony counts, B. Dejoseph assisted with the computation of coral generic densities, and J. Helyer with the preparation of site maps. The author also wants to thank R. Schroeder, A. Hall, P. Vroom, R. Brainard, and two anonymous reviewers, whose comments substantially improved this manuscript. NR 48 TC 28 Z9 29 U1 0 U2 18 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 J9 B MAR SCI JI Bull. Mar. Sci. PD MAR PY 2009 VL 84 IS 2 BP 211 EP 227 PG 17 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 419KX UT WOS:000264219500006 ER PT J AU Gultepe, I Pearson, G Milbrandt, JA Hansen, B Platnick, S Taylor, P Gordon, M Oakley, JP Cober, SG AF Gultepe, I. Pearson, G. Milbrandt, J. A. Hansen, B. Platnick, S. Taylor, P. Gordon, M. Oakley, J. P. Cober, S. G. TI THE FOG REMOTE SENSING AND MODELING FIELD PROJECT SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID LAND-SURFACE SCHEME; BULK MICROPHYSICS PARAMETERIZATION; SCANNING DOPPLER RADAR; WEATHER FORECAST MODEL; LOW STRATUS DETECTION; RADIATION FOG; BLOWING SNOW; PART I; OPERATIONAL IMPLEMENTATION; NUMBER CONCENTRATION AB The main purpose of this work is to describe a major field project on fog and summarize the preliminary results. Three field phases of the Fog Remote Sensing and Modeling (FRAM) project were conducted over the following two regions of Canada: 1) the Center for Atmospheric Research Experiments (CARE), in Toronto, Ontario (FRAM-C), during the winter of 2005/06, and 2) Lunenburg, Nova Scotia (FRAM-L), during June 2006 and June 2007. Fog conditions observed during FRAM-C were continental in nature, while those conditions observed during FRAM-L were of marine origin. The main objectives of the project were to attain 1) a better description of fog environments, 2) the development of microphysical parameterizations for model applications, 3) the development of remote sensing methods for fog nowcasting/forecasting, 4) an understanding of issues related to instrument capabilities and improvement of the analysis, and 5) an integration of model data with observations to predict and detect fog areas and particle phase. During the project phases, various measurements at the surface, including droplet and aerosol spectra, ice crystal number concentration, visibility, 3D turbulent wind components, radiative fluxes, precipitation, liquid water content profiles, and cloud ceiling, were collected together with satellite measurements. These observations will be studied to better forecast/nowcast fog events in association with results obtained from numerical forecast models. It is suggested that improved scientific understanding of fog will lead to better forecasting/nowcasting skills, benefiting the aviation, land transportation, and shipping communities. C1 [Gultepe, I.; Hansen, B.; Cober, S. G.] Environm Canada, Cloud Phys & Severe Weather Res Sect, Sci & Technol Branch, Meteorol Res Div, Toronto, ON M3H 5T4, Canada. [Pearson, G.] Environm Canada, Natl Lab Marine & Coastal Meteorol, Dartmouth, NS, Canada. [Milbrandt, J. A.] Environm Canada, Sci & Technol Branch, Numer Weather Predict Res Sect, Meteorol Res Div, Dorval, PQ, Canada. [Platnick, S.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Taylor, P.; Gordon, M.] York Univ, Dept Earth & Space Sci & Engn, Toronto, ON M3J 2R7, Canada. [Oakley, J. P.] Univ Manchester, Sch Elect & Elect Engn, Manchester, Lancs, England. RP Gultepe, I (reprint author), Environm Canada, Cloud Phys & Severe Weather Res Sect, Sci & Technol Branch, Meteorol Res Div, Toronto, ON M3H 5T4, Canada. EM ismail.gultepe@ec.gc.ca RI Platnick, Steven/J-9982-2014 OI Platnick, Steven/0000-0003-3964-3567 FU Canadian National Search and Rescue Secretariat and Environment Canada; ISDAC; U. S. Department of Energy [DE-FG02-08ER64554]; ARM Aerial Vehicle Program; DOE Atmospheric Sciences Program (ASP); Environment Canada and the National Research Council of Canada; ARM program archive; U. S. DOE; Office of Science; Office of Biological and Environmental Research; Environmental Sciences Division; European [COST-722] FX Funding for this work was provided by the Canadian National Search and Rescue Secretariat and Environment Canada. ISDAC was supported by the Office of Biological and Environmental Research of the U. S. Department of Energy (Grant No. DE-FG02-08ER64554) through the Atmospheric Radiation Measurement (ARM) program and the ARM Aerial Vehicle Program with contributions from the DOE Atmospheric Sciences Program (ASP), and Environment Canada and the National Research Council of Canada. Data were obtained from the ARM program archive, sponsored by the U. S. DOE, Office of Science, Office of Biological and Environmental Research, Environmental Sciences Division. Some additional funding was also provided by the European COST-722 fog initiative project office. Authors are thankful to G. Isaac for instrumental support, M. Wasey and R. Reed of Environment Canada for technical support, and J. W. Strapp for discussions on the TP3000 MWR during FRAM. NR 69 TC 76 Z9 86 U1 3 U2 28 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD MAR PY 2009 VL 90 IS 3 BP 341 EP + DI 10.1175/2008BAMS2354.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 430ZT UT WOS:000265031800005 ER PT J AU Gu, GJ AF Gu, Guojun TI Intraseasonal variability in the equatorial Atlantic-West Africa during March-June SO CLIMATE DYNAMICS LA English DT Article DE Tropical intraseasonal oscillations; Tropical convection and precipitation; Tropical Atlantic-West Africa ID MADDEN-JULIAN OSCILLATION; TROPICAL ATLANTIC; CONVECTION ANOMALIES; GLOBAL TROPICS; RAINFALL; MONSOON; SUMMER; PRECIPITATION; TEMPERATURE; PREDICTION AB Intraseasonal (30-80 days) variability in the equatorial Atlantic-West African sector during March-June is investigated using various recently-archived satellite measurements and the NCEP/DOE AMIP-II reanalysis daily data. The global connections of regional intraseasonal signals are first examined for the period of 1979-2006 through lag-regression analyses of convection (OLR) and other dynamic components against a regional intraseasonal convective (OLR) index. The eastward-propagating features of convection can readily be seen, accompanied by coherent circulation anomalies, similar to those for the global tropical intraseasonal mode, i.e., the Madden-Julian oscillation (MJO). The regressed TRMM rainfall (3B42) anomalies during the TRMM period (1998-2006) manifest similar propagating features as for the regressed OLR anomalies during 1979-2006. These coherent features hence tend to suggest that the regional intraseasonal convective signals might be mostly a regional response to, or closely associated with the MJO, and probably contribute to the MJO's global propagation. Atmospheric and surface intraseasonal variability during March-June of 1998-2006 are further examined using the high-quality TRMM Microwave Imager (TMI) sea surface temperature (SST), columnar water vapor, and cloud liquid water, and the QuikSCAT oceanic winds (2000-2006). Enhanced (suppressed) convection or positive (negative) rainfall anomalies approximately cover the entire basin (0A degrees-10A degrees N, 30A degrees W-10A degrees E) during the passage of intraseasonal convective signals, accompanied by anomalous surface westerly (easterly) flow. Furthermore, a unique propagating feature seems to exist within the tropical Atlantic basin. Rainfall anomalies always appear first in the northwestern basin right off the coast of South America, and gradually extend eastward to cover the entire basin. A dipolar structure of rainfall anomalies with cross-equatorial surface wind anomalies can thus be observed during this evolution, similar to the anomaly patterns on the interannual time scale discovered in past studies. Coherent intraseasonal variations and patterns can also be found in other physical components. C1 [Gu, Guojun] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Gu, Guojun] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. RP Gu, GJ (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 613-1, Greenbelt, MD 20771 USA. EM guojun.gu-1@nasa.gov FU NOAA's Climate Program Office [NA05QAR4311133]; NASA's Precipitation Mission FX The author thanks Dr. Robert F. Adler for his consistent support during the course of this study. Mr. David Bolvin prepared the TRMM (TMPA/3B42) rainfall product. TMI SST, columnar water vapor and cloud liquid water, and QuikSCAT surface winds were downloaded from http://www.remss.com.TheNCEP/DOE Reanalysis II product and daily OLR data were provided by the NOAA-CDC, Boulder, CO, from its website: http://www.cdc.noaa.gov. This study was supported by NOAA's Climate Program Office under grant NA05QAR4311133 and by NASA's Precipitation Mission. NR 39 TC 7 Z9 7 U1 0 U2 3 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0930-7575 J9 CLIM DYNAM JI Clim. Dyn. PD MAR PY 2009 VL 32 IS 4 BP 457 EP 471 DI 10.1007/s00382-008-0428-0 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 396JS UT WOS:000262588600002 ER PT J AU Conklin, DJ Lillywhite, HB Bishop, B Hargens, AR Olson, KR AF Conklin, Daniel J. Lillywhite, Harvey B. Bishop, Barbara Hargens, Alan R. Olson, Kenneth R. TI Rhythmic contractility in the hepatic portal "corkscrew" vein of the rat snake SO COMPARATIVE BIOCHEMISTRY AND PHYSIOLOGY A-MOLECULAR & INTEGRATIVE PHYSIOLOGY LA English DT Article DE Gravity; Snake; Vascular smooth muscle; Vasomotion; Vein; Venous return ID LONGITUDINAL SMOOTH-MUSCLE; SOUTH-AMERICAN RATTLESNAKE; ISOLATED SMALL ARTERIES; CROTALUS-DURISSUS; MYOGENIC RESPONSE; LOWER-VERTEBRATES; ENDOTHELIUM; PRESSURE; GRAVITY; ADRENOCEPTOR AB Terrestrial, but not aquatic, species of snakes have hepatic portal veins with a corkscrew morphology immediately posterior of the liver. Relatively large volumes of venous blood are associated with this region, and the corkscrew vein has been proposed to function as a bidirectional valve that impedes gravitational shifts of intravascular volume. To better understand the functional significance of the corkscrew anatomy, we investigated the histology and contractile mechanisms in isolated corkscrew segments of the hepatic portal vein of a yellow rat snake (Pantherophis obsoletus). Morphologically, the corkscrew portal vein is here shown to have two distinct layers of smooth muscle - an inner circular layer, and an outer longitudinal layer, separated by a layer of collagen, - whereas only a single circular layer of smooth muscle is present in the adjacent posterior caval vein. Low frequency (similar to 0.3 cycles*min(-1)) spontaneous and catecholamine-induced rhythms were observed in 11% and 89% of portal vein segments, respectively, but neither spontaneous nor agonist-induced cycling was observed in adjacent posterior (non-corkscrew) caval veins. Catecholamines, angiotensin 11, or stretch increased the amplitude and/or frequency of contractile cycles. Ouabain, verapamil or indomethacin, but not tetrodotoxin, alpha-, or beta-adrenergic receptor antagonists, inhibited cyclical contractions indicating a dependence of these cycles on Na(+)/K(+) ATPase, extracellular Ca(2+) and prostanoid(s). These data suggest that the rhythmic contractility of the corkscrew segment of the ophidian portal vein may act in conjunction with its morphological features to improve venous return and to prevent retrograde shifts of blood that might otherwise pool in posterior veins. (C) 2008 Elsevier Inc. All rights reserved. C1 [Lillywhite, Harvey B.] Univ Florida, Dept Zool, Gainesville, FL 32611 USA. [Conklin, Daniel J.; Lillywhite, Harvey B.; Hargens, Alan R.] NASA, Ames Res Ctr, Div Life Sci, Moffett Field, CA 94035 USA. [Conklin, Daniel J.; Bishop, Barbara] Univ Louisville, Inst Mol Cardiol, Louisville, KY 40202 USA. [Hargens, Alan R.] Univ Calif San Diego, UCSD Med Ctr, San Diego, CA 92103 USA. [Olson, Kenneth R.] Indiana Univ, Sch Med S Bend, South Bend, IN 46617 USA. RP Lillywhite, HB (reprint author), Univ Florida, Dept Zool, 122 Bartram Hall,POB 118525, Gainesville, FL 32611 USA. EM hbl@zoo.ufl.edu FU NSF [IBN 91-05247]; NASA [199-14-12-04]; National Research Council Senior Research Associateship FX This work was supported by: NSF IBN 91-05247 (KRO), NASA grant 199-14-12-04 (ARH), and a National Research Council Senior Research Associateship (HBL). NR 30 TC 0 Z9 0 U1 0 U2 1 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 1095-6433 J9 COMP BIOCHEM PHYS A JI Comp. Biochem. Physiol. A-Mol. Integr. Physiol. PD MAR PY 2009 VL 152 IS 3 BP 389 EP 397 DI 10.1016/j.cbpa.2008.11.013 PG 9 WC Biochemistry & Molecular Biology; Physiology; Zoology SC Biochemistry & Molecular Biology; Physiology; Zoology GA 413GB UT WOS:000263779800015 PM 19049826 ER PT J AU Kincaid, RK Alexamdrov, N Holroyd, MJ AF Kincaid, Rex K. Alexamdrov, Natalia Holroyd, Michael J. TI An Investigation of Synchrony in Transport Networks SO COMPLEXITY LA English DT Article DE networks; power laws; degree distribution; synchronization ID COMPLEX NETWORKS AB The cumulative degree distributions of transport networks, such as air transportation networks and respiratory neuronal networks, follow power laws. The significance of power laws with respect to other network performance measures, such as throughput and synchronization, remains an open question. Evolving methods for the analysis and design of air transportation networks must be able to address network performance in the face of increasing demands and the need to contain and control local network disturbances, such as congestion. Toward this end, we investigate functional relationships that govern the performance of transport networks; for example, the links between the first nontrivial eigenvalue, lambda(2), of a network's Laplacian matrix-a quantitative measure of network synchronizability-and other global network parameters. In particular among networks with a fixed degree distribution and fixed network assortativity (a measure of a networks preference to attach nodes based on a similarity or difference), those with small lambda(2) are shown to be poor synchronizers, to have much longer shortest paths and to have greater clustering in comparison to those with large lambda(2). A simulation of a respiratory network adds data. to our investigation. This study is a beginning step in developing metrics and design variables for the analysis and active design of air transport networks. (C) 2008 Wiley Periodicals, Inc. Complexity 14:34-43,2009 C1 [Kincaid, Rex K.] Coll William & Mary, Dept Math, Williamsburg, VA 23185 USA. [Alexamdrov, Natalia] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Holroyd, Michael J.] Univ Virginia, Dept Comp Sci, Charlottesville, VA 22903 USA. RP Kincaid, RK (reprint author), Coll William & Mary, Dept Math, Williamsburg, VA 23185 USA. EM rrkinc@math.wm.edu NR 22 TC 5 Z9 5 U1 0 U2 3 PU HINDAWI LTD PI LONDON PA ADAM HOUSE, 3RD FLR, 1 FITZROY SQ, LONDON, WIT 5HE, ENGLAND SN 1076-2787 EI 1099-0526 J9 COMPLEXITY JI Complexity PD MAR-APR PY 2009 VL 14 IS 4 BP 34 EP 43 DI 10.1002/cplx.20245 PG 10 WC Mathematics, Interdisciplinary Applications; Multidisciplinary Sciences SC Mathematics; Science & Technology - Other Topics GA 421XQ UT WOS:000264392000004 ER PT J AU Wimmer, G Schuecker, C Pettermann, HE AF Wimmer, G. Schuecker, C. Pettermann, H. E. TI Numerical simulation of delamination in laminated composite components - A combination of a strength criterion and fracture mechanics SO COMPOSITES PART B-ENGINEERING LA English DT Article DE Layered structures; Delamination; Finite element analysis ID MODELS AB An approach for the numerical treatment of delamination in laminated composite components is presented. A first ply failure criterion is employed to predict delamination initiation, while delamination propagation is analyzed using linear elastic fracture mechanics. The combination of initiation and propagation criteria yields a conservative estimation of the load earring capacity of a structure. Furthermore, the growth stability, the sensitivity of the results with respect to a change in the interface properties. and the non-linear structural response caused by the delamination growth process are determined. Two structures are investigated, which show the capability of the proposed approach, a curved laminate and a double lap shear test specimen. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Wimmer, G.; Pettermann, H. E.] Vienna Univ Technol, Inst Lightweight Design & Struct Biomech, Network Mat & Engn, AAR, A-1040 Vienna, Austria. [Schuecker, C.] NASA, Postdoctoral Program, Hampton, VA 23618 USA. RP Wimmer, G (reprint author), Vienna Univ Technol, Inst Lightweight Design & Struct Biomech, Network Mat & Engn, AAR, Gusshausstr 27-29, A-1040 Vienna, Austria. EM wimmer@ilsb.tuwien.ac.at FU Austrian Aeronautics Research (AAR)/Network for Materials and Engineering by the Austrian Federal Ministry of Economics and Labor FX The funding of the Austrian Aeronautics Research (AAR)/Network for Materials and Engineering by the Austrian Federal Ministry of Economics and Labor is gratefully acknowledged. NR 25 TC 26 Z9 28 U1 2 U2 12 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1359-8368 J9 COMPOS PART B-ENG JI Compos. Pt. B-Eng. PD MAR PY 2009 VL 40 IS 2 BP 158 EP 165 DI 10.1016/j.compositesb.2008.10.006 PG 8 WC Engineering, Multidisciplinary; Materials Science, Composites SC Engineering; Materials Science GA 411EI UT WOS:000263630500008 ER PT J AU Kwak, D AF Kwak, Dochan TI CFD activities at NASA Ames Research Center - Review of selected topics SO COMPUTERS & FLUIDS LA English DT Editorial Material C1 NASA, Ames Res Ctr, NASA Adv Supercomp Div, Moffett Field, CA 94035 USA. RP Kwak, D (reprint author), NASA, Ames Res Ctr, NASA Adv Supercomp Div, Moffett Field, CA 94035 USA. EM Dochan.Kwak@nasa.gov NR 0 TC 0 Z9 0 U1 1 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0045-7930 J9 COMPUT FLUIDS JI Comput. Fluids PD MAR PY 2009 VL 38 IS 3 BP 481 EP 481 DI 10.1016/j.compfluid.2008.10.001 PG 1 WC Computer Science, Interdisciplinary Applications; Mechanics SC Computer Science; Mechanics GA 396DE UT WOS:000262571600001 ER EF